astronomical society of australia annual scientific meeting

Astronomical Society of Australia Annual Scientific Meeting 2013

CONTENTS

WELCOME 2 PROGRAM 3 Sunday, 7th July 3 Monday, 8th July 3 Tuesday, 9th July 5

Wednesday, 10th July 7 Thursday, 11th July 18 Thursday, 11th July 9

Friday, 12th July 11 ORGANISING COMMITTEE 12 DELEGATE INFORMATION 13 The organisers office 13 Registration 13 Speaker preparation instructions 13 Poster sparklers 13 Displaying your poster 13 Internet access 13 Recycling your name badges and lanyards 14 Useful phone numbers 14 Accommodation 14

VENUE 15 Parking 16

SOCIAL AND SPECIAL EVENTS PROGRAM 17 Sunday, 7th July 17 Monday, 8th July 17 Tuesday, 9th July 17 Wednesday, 10th July 18 Thursday, 11th July 19 Friday, 12th July 19

POSTER LISTING 20 ABSTRACTS 24 Oral abstracts 24

Poster abstracts 59 SPONSOR AND SUPPORTER PROFILES 86 ATTENDEE LIST 88 INDEX OF ABSTRACT AUTHORS 92


WELCOME The Monash Centre for Astrophysics (MoCA) is proud to welcome attendees of the 2013 Astronomical Society of Australia's Annual Scientific Meeting to Monash University's Clayton Campus. MoCA was formally established in 2011, comprising researchers and students from the Schools of Physics and Mathematical Sciences at Monash University. Formerly the Centre for Stellar and Planetary Astrophysics (CSPA), the centre was formed in 2001 to serve as a national focus for theoretical astrophysics in the areas of stellar and planetary science. In recent years, the breadth of astrophysics research at Monash has widened substantially. Current research within MoCA can be divided into seven active areas:

Stellar nucleosynthesis,

Solar physics,

Galaxy evolution,

High-energy astrophysics,

Smoothed particle hydrodynamics,

Stellar and planetary dynamics, and

General relativity. MoCA is one of the most diverse astrophysics research groups in Australia, and our goal is to maintain our leading role in theory while building further on our observational research strengths. For more information about MoCA see the centre's web page at http://moca.monash.edu. This year sees the ASA's premier meeting returning to Monash after a long hiatus. The Clayton campus is also undergoing a period of restoration and renovation in 2013, with the recently completed New Horizons Centre (hosting members of MoCA as well as the School of Physics and CSIRO); the Green Chemical Futures building beginning construction; and substantial refurbishment of undergraduate student teaching and social spaces. We hope that whether this is your first time in Melbourne, or you are a regular visitor to Monash, you will be pleasantly surprised by what you find. We wish you an enjoyable stay and an entertaining and productive meeting.

Duncan Galloway on behalf of the 2013 ASA ASM LOC


PROGRAM [S] denotes student presentation [#] denotes abstract number

SUNDAY, 7TH JULY 2013 Registration Opens 4:00pm - 8:00pm Banquet Halls Welcome Reception 6:00pm - 8:00pm Banquet Halls

MONDAY, 8TH JULY 2013 Opening and Ellery Introduction 8:45am - 9:10am Central One Theatre Chair: Michael Brown 8:45 AM Duncan Galloway, Conference Chair

Conference Introduction 8:50 AM Dr Alan Finkel, Chancellor of Monash University

Opening of Conference 9:05 AM Kate Brooks, President of Astronomical Society of Australia

Ellery Lecture Introduction Ellery Lecture 9:10am - 10:30am Central One Theatre Chair: Michael Brown 9:10 AM Rachel Webster, University of Melbourne

What can a gravitationally-lensed quasar teach us? [1] 10:00 AM Julia Bryant, University of Sydney

SAMI and the SAMI galaxy Survey [2] Morning Tea 10:30am - 11:00am Banquet Halls Galaxies 11:00am - 12:15pm Central One Theatre Chair: Michael Brown 11:00 AM Julie Banfield, CSIRO Astronomy and Space Science

The Australia Telescope Large Area Survey: Data Release and Early Science [3] 11:15 AM Laura Hoppmann (S), ICRAR/UWA

Deep 21-cm HI Observations with the Arecibo Telescope [4] 11:30 AM Luca Cortese, Swinburne University of Technology

The role of the cluster environment on the star formation cycle of galaxies [5] 11:45 AM Paola Oliva-Altamirano (S), Swinburne University of Technology

Galaxy and Mass Assembly (GAMA): Testing galaxy formation models through the most massive objects in the universe [6]

12:00 PM Iraklis Konstantopoulos, Australian Astronomical Observatory The Evolution of Galaxies in Compact Groups [7]

Poster Sparkler Talks 12:15pm - 12:20pm Central One Theatre Chair: Michael Brown


ASA Chapter Sparklers 12:20pm - 12:30pm Central One Theatre Chair: Michael Brown

The Astronomical Society of Australia's Education and Public Outreach Chapter

Women In Astronomy Chapter

Early Career Researcher Chapter

Australian National Institute for Theoretical Astrophysics Chapter Lunch 12:30pm - 2:00pm Banquet Halls Speed Meet a Mentor 12:45pm - 1:45pm West Wing Cellar Chair: Tanya Hill Some lunch will be provided in the West Wing Cellar for those attending the lunchtime session. Solar System and Extra-Solar Planets 2:00pm - 3:15pm Central One Theatre Chair: Daniel Bayliss 2:00 PM Michele Bannister, NRC - Herzberg

Small worlds, big puzzles: insights from the Solar System's outer frontiers [8] 2:30 PM Duncan Wright, UNSW

First results from the AAT search for Habitable-Zone Exoplanets orbiting Late M-dwarfs [9] 2:45 PM Jonathan Horner, UNSW School of Physics

Dynamical Constraints on Multi-Planet Exoplanet Systems [10] 3:00 PM Francesco Pignatale (S), Swinburne University of Technology

Unveiling the 2D Chemistry of Protoplanetary Discs [11] Poster Sparkler Talks 3:15pm - 3:30pm Central One Theatre Chair: Daniel Bayliss Afternoon Tea 3:30pm - 4:00pm Banquet Halls Galaxies, HI and Radio Continuum 4:00pm - 5:30pm Central One Theatre Chair: Samantha Penny 4:00 PM Barbara Catinella, Swinburne University of Technology

HI properties of massive galaxies [12] 4:30 PM Louise Webster Prize

Andy Green, Australian Astronomical Observatory The connection between star formation and turbulence [13]

5:00 PM Sarah Reeves (S), University of Sydney A search for intervening HI absorption in nearby, gas-rich galaxies [14]

5:15 PM Benjamin McKinley, Australian National University The giant lobes of Centaurus A observed with the Murchison Widefield Array [15]

Poster Session One 5:30pm - 6:30pm Banquet Halls Refreshments will be provided. See poster listing for names of poster presenters. Early Career Researcher Social Mixer 5:45pm - 6:45pm Banquet Halls Chair: David Parkinson


TUESDAY, 9TH JULY 2013 Heads of Department Meeting 8:00am – 9:00am Room 115, Building 28 (Maths Building) eResearch, Science Communication and Outreach 9:00am - 9:30am Central One Theatre Chair: Simon O’Toole 9:00 AM Christopher Fluke, Swinburne University of Technology

Further adventures in three-dimensional visualisation: Leaping into your data [16] 9:15 AM Darren Croton, Swinburne University of Technology

Building model universes in the "cloud": the Theoretical Astrophysical Observatory (TAO) [17] The Importance of Science Communication (Panel Discussion) 9:30am - 10:30am Central One Theatre Chair: Simon O’Toole

Brian Schmidt, Australian National University

Graham Phillips, ABC

Katie Mack, University of Melbourne

Paul Dalgarno, The Conversation Morning Tea and Press Event 10:30am - 11:00am Banquet Halls The press event will be held in the West Wing Cellar. Dwarf Galaxies and Star Clusters 11:00am - 12:15pm Central One Theatre Chair: Christopher Usher 11:00 AM Samantha Penny, Monash University, MoCA

The origin and evolution of dwarf galaxies [18] 11:30 AM Sarah Sweet, University of Queensland

Tidal dwarf galaxy candidates in gas-rich groups [19] 11:45 AM Christina Blom, Swinburne University

Globular Cluster Studies Uncover remarkable details of Ongoing Accretion in the Haloes of two nearby Early-type Galaxies [20]

12:00 PM Gary Da Costa, Australian National University The [Fe/H] Abundance Dispersion in the Remote Halo Globular Cluster NGC 5824 [21]

Poster Sparkler Talks 12:15pm - 12:30pm Central One Theatre Chair: Christopher Usher Lunch 12:30pm - 2:00pm Banquet Halls Australian National Institute for Theoretical Astrophysics 12:45pm - 1:45pm Central One Theatre Chair: Darren Croton Some lunch will be provided in the Central One Theatre Foyer for those attending the lunchtime session. A New Era in Australian Radio Astronomy: MWA 2:00pm - 3:30pm Central One Theatre Chair: Douglas Bock 2:00 PM Steven Tingay, Curtin University

The Murchison Widefield Array, low frequency Precursor to the Square Kilometre Array [22] 2:20 PM Randall Wayth, Curtin University

The MWA All-sky Survey [23] 2:35 PM Rachel Webster, University of Melbourne

MWA: Epoch of Reionisation [24]


2:50 PM Martin Bell, Sydney University Transients and variables with the Murchison Widefield Array [25]

3:00 PM Cathryn Trott, Curtin University Information Theory and the MWA [26]

3:10 PM Natasha Hurley-Walker, Curtin Institute of Radio Astronomy MWA Observations of the Galactic Plane and Magellanic Clouds [27]

3:20 PM Emil Lenc, University of Sydney First polarisation results with the MWA [28]

Afternoon Tea 3:30pm - 4:00pm Banquet Halls A New Era in Australian Radio Astronomy: ASKAP and SKA 4:00pm - 5:30pm Central One Theatre Chair: Steven Tingay 4:00 PM Antony Schinckel, CSIRO

The Australian SKA Pathfinder – an update [29] 4:15 PM Lisa Harvey-Smith, CSIRO

Update on the Australian SKA Pathfinder (ASKAP) [30] 4:30 PM Brian Boyle, DIICCSRTE

The Australian SKA Project office [31] 4:45 PM Philip Diamond, SKA Organisation

Designing the SKA [32] 5:00 PM Stuart Wyithe, University of Melbourne

Science with SKA1 - Low frequency [33] 5:15 PM Lister Staveley-Smith, University of Western Australia

Science with SKA1-survey [34] Australia Telescope National Facility Community Meeting 5:45pm - 7:30pm Banquet Halls Chair: Douglas Bock Finger food and some drinks will be provided with a short presentation. Harley Wood Lecture 7:30pm - 8:30pm Central One Theatre Chair: Hamed Moradi and Duncan Galloway 7:30 PM Charley Lineweaver, Australian National University

The Birth, Life and Death of our Planet......and of the Universe [35]


WEDNESDAY, 10TH JULY 2013

Supernovae, High Energy and Fundamental Astrophysics 9:00am - 10:30am Central One Theatre Chair: Duncan Galloway 9:00 AM Alexander Heger, Monash University

Supernovae from the First Stars [36] 9:30 AM Eric Howell, University Western Australia

Are Ultra-long and Sub-luminous gamma-ray bursts distinct populations? [37] 9:45 AM Fang Yuan, Australian National University

Locations of Peculiar Supernovae as a Diagnostic of Their Origins [38] 10:00 AM Roland Crocker, ANU

The implications of the giant, magnetized outflows from the Galactic Centre [39] 10:15 AM Luciano Rezzolla, Max-Planck Institute for Gravitational Physics

The missing link: from merging neutron stars to magnetic jets [40] Morning Tea 10:30am - 11:00am Banquet Halls Astronomical Society of Australia Annual General Meeting 11:00am - 12:30pm Central One Theatre Lunch 12:30pm - 2:00pm Banquet Halls The Astronomical Society of Australia's Education and Public Outreach Chapter 12:45pm - 1:45pm Central One Theatre Chair: Christopher Fluke Some lunch will be provided in the Central One Theatre Foyer for those attending the lunchtime session. PARALLEL SESSION - Cosmology 2:00pm - 3:30pm Central One Theatre Chair: Darren Croton 2:00 PM Christina Magoulas (S), University of Melbourne

Measuring the bulk flow from the 6dFGS peculiar velocity survey [41] 2:15 PM Jeff Cooke, Swinburne University

Supernova discoveries at z > 2 and their host galaxies [42] 2:30 PM Jun Koda, Swinburne University of Technology

Peculiar velocity power spectrum [43] 2:45 PM Jaehong Park (S), The University of Melbourne

The cross-power spectrum between 21cm emission and galaxies in hierarchical galaxy formation models [44]

3:00 PM Gregory Poole, University of Melbourne DRAGONS: The Dark Ages Reionization and Galaxy Formation Simulation Program [45]

3:15 PM Michael Childress, Australian National University SN 2012fr: A Luminous Normal Type Ia Supernova in NGC 1365 [46]

PARALLEL SESSION - Protostars, Star Formation and the ISM 2:00pm - 3:30pm Campus Centre Cinema Chair: Andrew Walsh 2:00 PM Christophe Pinte, UMI-FCA Santiago

Dust grain size sorting in the TW Hydrae protoplanetary disk [47] 2:15 PM Catarina Ubach (S), Swinburne University

A multi-wavelength study of the GQ Lup protoplanetary disc [49] 2:30 PM Tracey Hill, Joint ALMA Observatory

The role of ridges in high-mass star formation - high resolution insights from Herschel [48] 2:45 PM James Green, CSIRO Astronomy and Space Science

MAGMO: Mapping the Galactic Magnetic field through OH masers [50]


3:00 PM Aaron Rizzuto (S), Macquarie University The Membership and Multiplicity of Sco-Cen [51]

3:15 PM Michael Ashley, University of New South Wales Terahertz observations of star forming regions from Antarctica [52]

Afternoon Tea 3:30pm - 4:00pm Banquet Halls PARALLEL SESSION - Galaxies, HI and Radio Continuum 4:00pm - 5:00pm Central One Theatre Chair: Naomi McClure-Griffiths 4:00 PM Joanne Dawson, University of Tasmania

Making a SPLASH with the Dish [53] 4:15 PM Vanessa Moss (S), University of Sydney/CSIRO Astronomy and Space Science

High velocity clouds in the Galactic All Sky Survey: Catalogue [54] 4:30 PM Helga Denes (S), Swinburne University of Technology

Finding galaxies with unusual HI content [55] 4:45 PM James Allison, University of Sydney

The cold gas in nearby radio galaxies with HIPASS [56] PARALLEL SESSION - Solar and Stellar Astrophysics 4:00pm - 5:00pm Campus Centre Cinema Chair: Stephen Marsden 4:00 PM Jan Staff, Macquarie University

Jets and planetary nebulae [57] 4:15 PM Taissa Danilovich (S), Chalmers University of Technology

Mass-loss and the circumstellar environment of S type AGB stars [58] 4:30 PM Paul Cally, Monash University

MHD Mode Conversion in Stellar Atmospheres [59] 4:45 PM Donna Burton (S), University of Southern Queensland

Doppler Imaging of AB Doradus [60] New Opportunities with the Gemini Observatory 5:00pm - 5:30pm Chair: Stuart Wyithe Central One Theatre 5:00 PM Markus Kissler-Patig, Gemini Observatory

New Opportunities with the Gemini Observatory [61] Refreshments will be provided after this session in the Central One Theatre lobby. Poster Session Two 5:30pm - 6:30pm Banquet Halls Refreshments will be provided. National Committee for Astronomy Meeting 6:00pm - 8:00pm Conference Room, Conference Centre Chair: Stuart Wyithe


THURSDAY, 11TH JULY 2013

Stellar and Archaeoastronomy 9:00am - 10:30am Central One Theatre Chair: Alexander Heger 9:00 AM Amanda Karakas, Australian National University

Stellar yields from low and intermediate-mass stars [62] 9:30 AM Andrew Casey (S), RSAA, ANU

Adopting the Aquarius Stream: Is the Aquarius Stream the result of a disrupted classical Globular Cluster? [63]

9:45 AM Ioannis Gonidakis, CSIRO The circumstellar environment of the Mira Variable TX Cam, as revealed by long-term high-resolution interferometric observations of SiO masers [64]

10:00 AM Michael Ireland, Australian Astronomical Observatory The FunnelWeb Survey with the UKST [65]

10:15 AM Duane Hamacher, University of New South Wales Cultural Astronomy in the Torres Strait [66]

Morning Tea 10:30am - 11:00am Banquet Halls Galaxies, Active Galactic Nuclei 11:00am - 12:15pm Central One Theatre Chair: Christopher Fluke 11:00 AM Stas Shabala, University of Tasmania

Triggering and feedback from Active Galactic Nuclei [67] 11:30 AM Kevin Pimbblet, Monash University

The duty cycle of galaxy cluster AGN [68] 11:45 AM Rebecca Davies (S), RSAA, ANU

NGC7130: An Insight into Ionising sources of Composite Galaxies [69] 12:00 PM Bok Prize Lecture Benjamin Pope (S), Sydney Institute for Astronomy

Dancing in the Dark: Kernel Phase Interferometry of Ultracool Dwarfs [70] The Next Decadal Plan for Australian Astronomy 12:15pm - 12:30pm Central One Theatre Chair: Christopher Fluke 12:15 PM Stuart Wyithe, University of Melbourne

The 2016-25 Decadal Plan for Australian Astronomy [71] Lunch 12:30pm - 2:00pm Banquet Halls Women in Astronomy 12:45pm - 1:45pm Central One Theatre Chair: Lisa Harvey-Smith Some lunch will be provided in the Central One Theatre Foyer for those attending the lunchtime session. PARALLEL SESSION - Galaxies 2:00pm - 3:30pm Central One Theatre Chair: Darren Croton 2:00 PM Christopher Usher (S), Swinburne University of Technology

Do All Galaxies' Globular Clusters Have the Same Stellar Populations? [72] 2:15 PM Sarah Martell, Australian Astronomical Observatory

Multiple stellar populations in intermediate-age star clusters [73] 2:30 PM Nicholas Scott, Swinburne University of Technology

How environment affects early-type galaxies - insights from integral-field spectroscopy surveys [74]


2:45 PM Michelle Cluver, Australian Astronomical Observatory Galaxies that Flash as they Crash [75]

3:00 PM Jacob Crossett (S), Monash University UV Strong Red Sequence Cluster Galaxies: Their Environment and Morphology [76]

3:15 PM Nicolas Bonne (S), MoCA, Monash University What Shapes the Local Universe K-Band Galaxy Luminosity Function? [77]

PARALLEL SESSION - Protoplanets, Extrasolar Planets and Planetary Nebulae 2:00pm - 3:30pm Campus Centre Cinema Chair: Duncan Wright 2:00 PM Daniel Bayliss, ANU

Transiting Exoplanets from HATSouth [78] 2:15 PM Karen Lewis, Tokyo Institute of Technology

Moon Radius Limits for Planets with Spotted Host Stars: Scatter in the Folded Light-curve [79] 2:30 PM Brett Addison (S), University of New South Wales

Recently Discovered Exoplanetary System in Spin-Orbit Misalignment from Rossiter-Mclaughlin Measurements [80]

2:45 PM Kimberly Bott (S), University of New South Wales Modelling the Atmospheric Structure and Composition of Hot Jupiter HD 189733b [81]

3:00 PM Sarah Maddison, Swinburne University The intriguing transitional disk HD142527 - planet formation in action? [82]

3:15 PM Quentin Parker, Macquarie University/AAO Planetary nebulae: Windows into the soul of stellar Death [83]

Afternoon Tea 3:30pm - 4:00pm Banquet Halls PARALLEL SESSION - Galaxies, including High Redshift Galaxies 4:00pm - 5:30pm Central One Theatre Chair: Emma Ryan-Weber 4:00 PM Tim Dolley (S), MoCA

The Environment of z<1 Star Forming Galaxies [84] 4:15 PM Glenn Kacprzak, Swinburne University of Technology

Tracing Outflows and Accretion: A Bimodal Azimuthal Dependence of the Circumgalactic Medium [85]

4:30 PM Lee Spitler, Australian Astronomical Observatory / Macquarie University A first glimpse into the complete galaxy population 12 billion years ago [86]

4:45 PM Michele Trenti, University of Cambridge The first galaxies: bright and faint [87]

5:00 PM Edoardo Tescari, University of Melbourne Properties of simulated galaxies at z~4-7 [88]

5:15 PM Antonios Katsianis (S), University of Melbourne Properties of high redshift galaxies in cosmological hydrodynamical simulations [89]

PARALLEL SESSION - High Energy Astrophysics 4:00pm - 5:30pm Campus Centre Cinema Chair: Duncan Galloway 4:00 PM Thomas Russell (S), ICRAR

Disk-jet coupling in Galactic black hole X-ray binaries [90] 4:15 PM Sean Farrell, The University of Sydney

Unveiling the Variable X-ray Sky [91] 4:30 PM Roberto Soria, Curtin University

Black hole mass in an ultraluminous X-ray source [92] 4:45 PM Sammanani Premachandra, Monash University

Precision ephemerides for gravitational-wave searches: Sco X-1 & Cyg X-2 [93]


5:00 PM Hauke Worpel (S), MoCA Evidence for accretion rate change during type I X-ray bursts [94]

5:15 PM Phoebe de Wilt (S), University of Adelaide Unveiling Unidentified TeV Gamma-Ray Sources at 12mm with Mopra [95]

Conference Dinner 7:00pm - 10:30pm Dragon Boat Palace, 149 Lonsdale Street, Melbourne Buses will depart from the Robert Blackwood Hall, Monash Clayton Campus at 6:15pm. Buses will start returning back to Monash from Melbourne at 9:30pm.

FRIDAY, 12TH JULY 2013 Galaxies 9:00am - 10:15am Central One Theatre Chair: Heath Jones 9:00 AM Chris Power, University of Western Australia

Do we have robust astrophysical tests of dark matter? [96] 9:30 AM Simon Mutch, The University of Melbourne

A formation history model of galaxy growth [97] 9:45 AM Michael Brown, Monash University

Star Formation in Red Spiral Galaxies [98] 10:00 AM Charlene Heisler Prize

Emily Wisnioski, MPE From 13 to 600+: the Future of High-z IFU Surveys [99]

Morning Tea 10:15am - 11:00am Banquet Halls Facilities 11:00am - 12:30pm Central One Theatre Chair: Heath Jones 11:00 AM Matthew Bailes, Swinburne University of Technology

Discovery of a population of millisecond duration radio bursts [100] 11:15 AM Rogier Windhorst, Arizona State University

How the James Webb Space Telescope can measure First Light, Reionization, and Galaxy Assembly: Science and Project Update as of 2013 [101]

11:30 AM Kyler Kuehn, AAO Optical Spectroscopy from TAIPAN to the GMT's MANIFEST [102]

11:45 AM Andrew Hopkins, Australian Astronomical Observatory The ASKAP/EMU Data Challenge [103]

12:00 PM Doug Simons, CFHT CFHT Status Report and Future Plans [104]

12:15 PM Closing Remarks Lunch 12:30pm - 2:00pm Banquet Halls Australian Synchrotron Tour 12:45pm - 1:45pm Australian Synchrotron, Blackburn Road, Clayton Meet at the registration desk to walk to the Australian Synchrotron and sign is as a group.


ORGANISING COMMITTEE

ASTRONOMICAL SOCIETY OF AUSTRALIA LOCAL ORGANISING COMMITTEE

Duncan Galloway (chair & treasurer) Kevin Pimbblet (secretary) Daniel Price (venues) Simon Campbell (travel & accommodation) Danielle White (ASN Events, logistics) Samantha Penny & Michael Brown (public lecture & media) Allie Ford Heath Jones John Lattanzio Andrew Prentice Terrence Tricco

ASTRONOMICAL SOCIETY OF AUSTRALIA SCIENTIFIC ORGANISING COMMITTEE

Michael Brown (Monash; chair) Daniel Price (Monash; ANITA rep) Cathy Trott (Curtin; WIA) Chris Fluke (Swinburne; EPOC) Lisa Kewley (RSAA) Jonti Horner (UNSW) Chiara Tonini (Swinburne) Baerbel Koribalski (CASS) Amanda Bauer (AAO)


DELEGATE INFORMATION

THE ORGANISER’S OFFICE – ASN EVENTS

The Organiser’s office is located in the Banquet Halls (Northern part of building 10). Any enquiries can be directed to an ASN Events staff member other than those about accommodation which should be dealt with directly at your hotel. The conference office hours are:

Sunday: 4:00pm – 8:00pm Monday: 7:30am – 6:30pm Tuesday: 8:00am – 8:30pm Wednesday: 8:00am – 6:30pm Thursday: 8:00am – 6:00pm Friday: 8:00am – 2:00pm

REGISTRATION

The registration fee includes:

Conference materials

Morning tea, lunch and afternoon tea

Welcome reception ticket

Conference dinner ticket

GST/Tax

SPEAKER PREPARATION INSTRUCTIONS

Presentations must be delivered from computers provided in the presentation room (A PC and MAC will be available). All PCs are running Windows XP and they have Office 2010, VLC media player, all standard browsers and Adobe Acrobat Reader. A late-model Apple Macintosh with suitable presentation software will also be provided. You should transfer your presentation to the provided machines well before your session, and ensure that the formatting is correct and that any animations, video or sound files are working correctly. The AV Technician will be located in the session room and will be available before sessions commence in the morning and in breaks. The audio-visual equipment is being supplied and manned by committee volunteers. Please see the registration desk for any questions.

POSTER SPARKLERS

For those delegates that are presenting a one minute presentation of their poster, please ensure that you are lined up next to the stage in order of your presentation. Your presentation slide which was already given to the organisers will be loaded for you. If you have made changes to your slide, please inform the registration desk well in advance of your presentation. There will be a countdown clock viewable for you, once your one minute is up, please move off the stage.

DISPLAYING YOUR POSTER

Posters will be on display for the duration of the conference. Posters can be put up from 4:00pm on Sunday 7

th July

and must be taken down by the end of lunch on Friday 12th

July. Poster presenters are asked to man their poster during both sessions; refreshments will be provided during both sessions. Posters will need to be a maximum of 1.2 metres high and 1 metre wide. Your poster placement corresponds with the abstract number given in this handbook. All posters can be attached to the poster boards with Velcro, please visit the registration desk for additional supplies.

INTERNET ACCESS

Wireless access will be available and is free for all delegates at Monash University. You will find your login and password details in your name badge. Instructions for using the wireless with this account are as follows:


1. Join the "guest-wireless" network 2. Open a browser window and load any page 3. In the netlogin window that appears, type your username, which is “ext-<username>”. For example, John Smith would be JSmith and should type in "ext-JSmith" (not case sensitive). Your username can be found in your name badge. 4. Enter the password, which is "password" (this *is* case sensitive). 5. A popup window should appear to confirm that you have authenticated to guest-wireless If attendees can already connect via eduroam, it is not necessary to use the guest-wireless network.

RECYCLING YOUR NAME BADGES AND LANYARDS

There will be a box at the registration desk to place your lanyards and name badges if you do not wish to keep them.

USEFUL PHONE NUMBERS

ASN Events Onsite: Bree – 0407 097 539 Danielle – 0413 932 387 Kristie – 0422 114 347 Monash University Clayton Campus - 03 9905 4000

ACCOMMODATION

Bruce Country Motor Inn 445 Blackburn Road, Mount Waverley, VIC Ph: 03 9803 5411 Gateway on Monash Boutique Hotel 630 Blackburn Road, Notting Hill, VIC Ph: 03 9561 4455 Ibis Melbourne Glen Waverley 297 Springvale Road, Glen Waverley, VIC Ph: 03 9518 7117 Mannix College Wellington Road, Monash University, Clayton, VIC Ph: 03 9544 8895 Novotel Melbourne Glen Waverley 285 Springvale Road, Glen Waverly, VIC Ph: 03 8561 2345


VENUE

1 2 3 4 1 - Main Lecture Hall - Central 1 Theatre (Building 63) 2 - Breakout Rooms – Campus Centre Cinema and West Wing Cellar (Building 10) 3 - Mannix College - Accommodation 4 - Posters and Catering – Banquet Halls (Campus Centre, Building 10)


PARKING

During non-teaching weeks you may park in the blue sections of the multi-level car parks without a permit. These are situated in the two multiplex car parks which are on opposite sides of campus. These are indicated by signs and blue painted lines on the asphalt. Parking in any other area (including uncovered blue sections) without a ticket or permit may result in a fine.

Multiplex car parks:

N 1 multi-level car park (map reference: B2)

SE 4 multi-level car park (map reference: E5) Also the Wellington Road car park, at the corner of Blackburn & Wellington Roads is free all year round. The car park will be closed once it is full.

Full details can be found via ask.Monash: https://monash.custhelp.com/app/answers/detail/a_id/2524/kw/parking


SOCIAL AND SPECIAL EVENTS PROGRAM Sunday, 7

th July – Welcome Reception

Monday, 8th

July – Speed Meet a Mentor Monday, 8

th July - Early Career Researcher Social Mixer

Tuesday, 9th

July – MWA Press Event Tuesday, 9

th July - Australian National Institute for Theoretical Astrophysics Chapter Lunchtime Meeting

Tuesday, 9th

July - Australia Telescope National Facility Community Meeting Tuesday, 9

th July - Harley Wood Lecture

Wednesday, 10th

July - Astronomical Society of Australia's Education and Public Outreach Chapter Lunchtime Meeting Thursday, 11

th July - Women in Astronomy Chapter Lunchtime Meeting

Thursday, 11th

July – Conference Dinner Friday, 12

th July - Australian Synchrotron Tour

SUNDAY, 7TH JULY The Welcome Reception - The welcome reception will be held from 6:00pm for all delegates to attend in the Banquet Halls. Partners are welcome to purchase a ticket (in advance). Please visit the registration desk for availability. The welcome reception wine is being sponsored and provided by Tyrell’s Wines. The conference thanks Tyrell’s Wines for their generous support.

MONDAY, 8TH JULY Speed Meet a Mentor – The Speed Meet a Mentor will take place in the West Wing Cellar (please visit the venue section on directions). Everyone is invited to participate in this “speed dating” version of a mentoring session. Attendees will be paired up for a quick chat before moving on to the next conversation. For mentorees it’s an opportunity to build confidence, broaden networks, and discover mentoring. For mentors it’s a chance to meet those who are keen to learn from your experience and knowledge. Organised by the Women in Astronomy and Early Career Research chapters of the ASA, Speed Meet a Mentor, connects you into the ASA’s strong professional network. Delegates were asked to select they wanted to attend during registration. If you would like to attend and have not indicated you would like to go, please visit the registration desk. Early Career Researcher Social Mixer – The Early Career Researcher Social Mixer will take place in the Banquet Halls from 5:45pm – 6:45pm. The Early Career Researcher chapter is a new chapter of the ASA - and it wants you! Whether you are an ECR who wants the mentoring, networking and training opportunities the chapter will provide, a postgrad student just finishing up their PhD and wondering about their future career, or an established researcher who would be willing to act as a mentor to ECRs, this is the chapter for you. Come along to our social mixer on Monday evening to drink some wine and find out more.

TUESDAY, 9TH JULY MWA Press Event – The formal launch of Murchison Widefield Array (MWA) Operations will mark the MWA as the first of three Square Kilometre Array (SKA) precursor telescopes to be fully operational for science. Having recently completed construction, commissioning and verification, the MWA will start its full science mission in July 2013, with astronomers beginning detailed observations to reveal the first billion years of the Universe, as well as a wide range of solar, galactic and extragalactic science. The development and commissioning of the MWA is the outcome of nearly nine years of work by an international consortium of 13 institutions across four countries (Australia, USA, India and New Zealand), led by Western Australia’s Curtin University. Please join the Federal Minister for Science and Research, Senator Don Farrell, as he launches MWA Operations at 10.30am, in the West Wing Cellar. The launch will include presentations from Curtin University’s Professor Steven Tingay, Director of the MWA, and Professor Phil Diamond, Director General of the SKA Organisation. Morning tea will also be provided, along with cool giveaways.


Australian National Institute for Theoretical Astrophysics Chapter Lunchtime Meeting – From 12:45pm – 1:45pm in Central One Theatre the Australian National Institute for Theoretical Astrophysics (ANITA) will hold their annual town hall meeting. Please join us over lunch, theorists and observers alike, to discuss future issues and opportunities in theoretical and numerical astrophysics, the annual ANITA report, funding opportunities, and upcoming theory meetings in Australia. Some lunch will be provided in the Central One Theatre Foyer for those attending the lunchtime session. Australia Telescope National Facility Community Meeting – The meeting will be held from 5:45pm – 7:30pm in the Banquet Halls. CSIRO Astronomy and Space Science invites the astronomical community to a Town Hall-style discussion on the Australia Telescope National Facility (ATNF). Topics will include ASKAP early science and future Parkes instrumentation. This session will be one of a series of forums over the coming months in which the community is invited to interact with CASS on the strategy for the ATNF telescopes. The ATNF currently consists of the Parkes Telescope, Australia Telescope Compact Array, and access to the Mopra Telescope and NASA's Canberra Deep Space Communication Complex (Tidbinbilla) Telescopes. The Australian SKA Pathfinder (ASKAP) will also be part of the ATNF. The session will include a short presentation, Q&A, and feedback forum. Wine and cheese will be served afterwards.

Harley Wood Lecture – The public lecture will be delivered by Charles H. Lineweaver and will take place from 7:30pm – 8:30pm in the Central One Theatre. All delegates are welcome to attend. An astrophysicist, Charles H. Lineweaver is an associate professor at the Australian National University’s Planetary Science Institute (PSI), a joint venture of the ANU Research School of Astronomy and Astrophysics and Research School of Earth Science. His research involves analysis of the statistical distribution of exoplanets, the cosmic microwave background radiation, and cosmological prerequisites for the formation of terrestrial planets and life.

Educated at Ludwig-Maximillians-Universität in Munich where he was awarded highest honors in physics, Dr. Lineweaver earned a BA in history from the State University of New York at Binghamton, an MA in English from Brown University, a BS is physics from Ludwig Maximillian's University in Munich, and a Ph.D. in physics at the University of California, Berkeley in 1994. He was a member of the COBE satellite team, led by George Smoot (2006 Physics Nobel Prize), that discovered the temperature fluctuations in the cosmic microwave background. He was a postdoctoral fellow at the Observatoire Astronomique in Strasbourg and, successively, a vice chancellor’s postdoctoral research fellow and Australian Research Council (ARC) fellow at the University of New South Wales (UNSW) where he taught one of the most popular general studies courses "Are We Alone?" A member of the editorial board of Astrobiology Magazine, he is the author of more than seventy papers published in scientific journals or in volumes of collected works. His research areas include cosmology (determination of the age and composition of the universe) exoplanetology (the statistical analysis of exoplanets) and astrobiology (using our new knowledge of cosmology to constrain life in the Universe). His research has been published in Science, Nature, the Astrophysical Journal, Astrobiology, Scientific American, American Journal of Physics, and Microbiology Australia. He is the son of a high school biology teacher and has lived in or travelled through 72 countries, has spoken 4 languages semi-fluently at one time or another, and was a semi-professional soccer player in Germany. Personal homepage: http://www.mso.anu.edu.au/~charley

WEDNESDAY, 10TH JULY The Astronomical Society of Australia's Education and Public Outreach Chapter Lunchtime Meeting – The EPOC Chapter meeting will be held from 12:45pm – 1:45pm in the Central One Theatre. Some lunch will be provided in the Central One Theatre Foyer for those attending the lunchtime session. The Education and Public Outreach Chapter (EPOC) is open to all ASA members who share a common interest in communicating astronomy to students of all ages and the general public. At this lunchtime meeting, you will get to meet and network with other EPOC members, as we share our experiences, and discuss opportunities and future plans for the Chapter.


THURSDAY, 11TH JULY Women in Astronomy Chapter Lunchtime Meeting – The WIA Chapter meeting will be held from 12:45pm – 1:45pm in Central One Lecture Theatre. Some lunch will be provided in the Central One Theatre Foyer for those attending the lunchtime session. Action on women's representation relies on the active participation of all ASA members. Men are welcome and strongly encouraged to attend this lunch. The Women in Astronomy lunch session will allow members to learn about the activities of the ASA Chapter for Women in Astronomy discuss future plans and provide their feedback to the committee. This year, a major topic for discussion will be a planned 'Women in Astronomy Awards' scheme that is proposed to provide a framework for universities and institutes to implement changes that support the aims of the Chapter. It is hoped that this scheme will make a positive change to the working environments of all ASA members. Discussion topics will include:

Aims and objectives of the Chapter

Steering Committee 'who's who'

Plans for the Women in Astronomy Workshop 2013

Action plan for institutes leading to 'the Women in Astronomy Awards'

Discussion The Conference Dinner – The conference dinner will be held from 7pm at the Dragon Boat Palace Restaurant in Melbourne (Dragon Boat Palace, 149 Lonsdale Street, Melbourne). A banquet menu including some drinks and entertainment will be provided. The conference have organised buses to transfer delegates between Monash Clayton and Dragon Boat Palace. The buses will depart Monash Clayton at 6:15pm for arrival in Melbourne at 7:00pm. The buses on the way back will depart the restaurant at 9:30pm, 10:00pm and 10:30pm (however is dependent on numbers). You will have been allocated a place on the conference bus if you have not let the conference organisers know that you do not require the bus transfers and specifically for the way back you will be allocated on the 9:30pm return bus. If you have selected to attend the dinner you will find the ticket in the back of your name tag. If you haven’t indicated that you would like a ticket, please visit the registration desk for availability. Partners are welcome to purchase a ticket (in advance).

FRIDAY, 12TH JULY Australian Synchrotron Tour – A tour of the Australian Synchrotron has been arranged for 12:45pm – 1:45pm. The tour is currently fully subscribed; please see the registration desk for any cancellations if you would like to attend the tour. For those attending the tour, please ensure that you have read the safety information available on the conference website. Please meet at the registration desk at 12:35pm and the group will walk together over to the Australian Synchrotron. Once arrived at the Synchrotron you will be asked to sign in for the tour.


POSTER LISTING Eromanga Adermann, Sydney Institute for Astronomy [201] Searching for Intermediate Mass Black Holes in Early Type Galaxies Featuring Prominent Dust Lanes Shaila Akhter, UNSW School of Physics [202] Clustering of dense molecular gas in the Milky Way Galaxy Mohammad Ali Nawaz, ANU [203] Interaction of Hydra A jets with the Intracluster medium Rebecca Allen, Swinburne University [204] Using Scaling Relations to Examine the Effects of Environment on High Redshift Galaxy Evolution Richard Beare, Monash Centre for Astrophysics [205] New Measurements of the Evolving Growth Rates of Galaxies Georgios Bekiaris, Swinburne University of Technology [206] Investigating Kinematic Modelling of Disk Galaxies Using GPUs Sarah Bird, Tuorla Observatory, University of Turku [207] Testing a Velocity Dispersion Model of the Milky Way Halo's Stars Tui Britton, Macquarie University [208] Māori Astronomical Traditions of Meteors Michael Brown, Monash University [209] Galaxy spectral energy distributions from the ultraviolet to the mid-infrared Sarah Bruzzese, ICRAR/UWA [210] Is the initial mass function universal? The case of NGC 2915 Pierluigi Cerulo, Swinburne University of Technology [211] Morphological Transformation of Red Sequence Galaxies in High Redshift Galaxy Clusters Kate Chow, CSIRO [212] The Australia Telescope Large Area Survey: The composite properties of young AGN Jordan Collier, University of Western Sydney [213] Wide-Field Infrared Survey Explorer Observations of Infrared Faint Radio Sources Camila Correa, University of Melbourne [214] Mass assembly history of main sequence galaxy halos Valentina D'Orazi, Macquarie University [215] Lithium abundances in the globular cluster NGC 6218 (M12) Ashkbiz Danehkar, Macquarie University [216] Evolution of planetary nebulae with hydrogen-deficient central stars Dimitri Douchin, Macquarie University / Universite Montpellier 2 [217] Estimating the fraction of binary central stars of planetary nebulae using the IR-excess method Mark Durre, Swinburne University of Technology [218] NGC2110 – Young Star Clusters in the Circumnuclear Torus Tobias Feger, Macquarie University [219] A stable wavelength comb for precise radial velocity measurements


Michael Fitzgerald, Macquarie University [220] A Review of High School Astronomy Student Research Projects over the last two decades Bi-Qing For, ICRAR/UWA [221] The twisted Magellanic Stream and its Leading Arm(s) Caroline Foster, Australian Astronomical Observatory [222] Outer triaxiality of a ‘Fast Rotator’ Gregory Goldstein, University of Western Sydney [223] A Catalogue of Radio AGN behind the LMC Michael Goodwin, Australian Astronomical Observatory [224] Starbugs enabling technologies and applications Elise Hampton, RSAA, ANU [225] The search for TeV particle accelerators in the star forming HII complex G5.89-0.39 using Chandra Paul Hancock, University of Sydney [226] Radio Faint Gamma-Ray Burst Afterglows Alex Hill, CSIRO Astronomy & Space Science [227] Magnetic fields in the Smith Cloud Louise Howes, Australian National University [228] Discovery of the oldest stars in the Galactic bulge Richard Hunstead, Sydney Institute for Astronomy [229] How accurate is SuperCOSMOS astrometry? Minh Huynh, University of Western Australia [230] The ATLAS 5.5 GHz survey of the extended Chandra Deep Field South: catalogue, source counts and spectral indices James Jackson, Boston University [231] Galactic Structure from the MALT 90 Survey: High-Mass Star-Formation in Distant Spiral Arms Andrew Jacob, Sydney Observatory [232] The Fall and Rise of Sydney Observatory Andrew Jacob, Sydney Observatory [233] Making visible the women who measured stars in Australia Akila Jeeson-Daniel, University of Melbourne [234] Clumping factors of H and He from EoR simulations Christopher Jordan, University of Tasmania [235] First results for MALT-45: A 7mm survey of the southern Galaxy Sreeja Kartha, Swinburne University [236] Wide-field imaging studies of globular cluster systems in three intermediate mass early-type galaxies Champlain Kenyi, University of NSW, Sydney [237] Spectroscopic Fitting of the Terrestrial Atmosphere for Improved Planetary Atmosphere Observations and Greenhouse Gas Monitoring Dane Kleiner, Monash University [238] A test for galaxy pre-processing using large-scale structure in the local Universe


Rebecca Lange, ICRAR, UWA [239] GAMA: The local mass-size relationship revisited Paul Lasky, University of Melbourne [240] Magnetic Fields in Relativistic Neutron Stars Sarah Leslie, Research School of Astronomy and Astrophysics [241] The Energy Source and Dynamics of Infared Luminous Galaxy ESO148-IG02 Karen Lewis, Tokyo Institute of Technology [242] Decoding the Message from Silicon in Stardust Mainstream Silicon Carbide Grains John Lopez, UNSW School of Physics [243] Molecular Gas Dynamics near Sagittarius A* Vicki Lowe, University of New South Wales, CSIRO Astronomy and Space Science [244] Variations between star formation environments Stephen Marsden, USQ [245] Bcool Australia Nigel Maxted, The University of Adelaide [246] Dense gas towards the supernova remnants RX J1713.7-3946 and W28 Bernard Meade, Swinburne University of Technology [247] Do tiled display walls improve feature recognition in large astronomical images? Martin Meyer, ICRAR/UWA [248] Tully-Fisher Relations without Galaxy Inclinations Scott Meyer, ICRAR [249] HI stacking can be used to measure edge-on rotation velocities for use in the Tully-Fisher relation Guido Moyano Loyola, Swinburne University of Technology [250] Stars on the run: escaping from stellar clusters Themiya Nanayakkara, CAS [251] Colour bimodality of galaxies at high redshift Belinda Nicholson, University of Melbourne [252] Is The Fundamental Plane Fundamental? Robert Nilsson, Monash University and Lulea University of Technology, Sweden [253] Properties of coronal rains in the Sun Samuel Oronsaye, ICRAR/Curtin University [254] Pulsar Studies with the Murchison Widefield Array (MWA) David Palamara, MoCA (Monash Centre for Astrophysics) [255] The clustering of GAMA galaxies: dependence on color, luminosity, mass and redshift Nicola Pastorello, Swinburne University [256] Globular Cluster and Stellar Metallicity Radial Profiles in Early-Type Galaxies Samantha Penny, Monash University, MoCA [257] The GAMA void galaxy sample Kevin Pimbblet, Monash University [258] The role of stellar mass and environment for cluster blue fraction, AGN, and star formation


Chris Power, University of Western Australia [259] The Halo Mass Function & Future Galaxy Surveys Andrew Prentice, Monash University [260] Mercury, Titan and Ganymede: new theoretical models for bulk chemical composition, internal physical structure and origin which match the latest spacecraft data Hayden Rampadarath, ICRAR, Curtin University [261] Multi-Epoch Very Long Baseline Interferometric Observations of the Nuclear Starburst Region of NGC~253: Improved modeling of the supernova and star-formation rates Glen Rees, Macquarie University [262] The radio properties of mass selected IR Galaxies out to Z=3 Stuart Ryder, Australian Astronomical Observatory [263] The First Supernova Discovered with GeMS/GSAOI Graeme Salter, UNSW [264] Direct Imaging of Long Period Radial Velocity Exoplanet Systems with NICI Giulia Savorgnan, Swinburne University of Technology [265] The supermassive black hole mass - Sérsic index (and other) relation(s) for bulges and elliptical galaxies Richard Scalzo, Australian National University [266] Type Ia Supernova Bolometric Light Curves and Ejected Mass Estimates from the Nearby Supernova Factory Stas Shabala, University of Tasmania [267] The relationship between lobe luminosity and kinetic power of AGN jets Genevieve Shattow, Swinburne [268] Measuring the environments of proto-clusters in the high redshift universe Luke Shingles, Australian National University [269] The Chemical Evolution of Heavy Elements in Globular Clusters Izabela Spaleniak, Macquarie University [270] Integrated photonic lanterns with gratings: miniature spectral filters for near-infrared spectroscopy Elodie Thilliez, Swinburne University of Technology [271] A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved with Herschel Georgios Vernardos, Swinburne University of Technology [272] Adventures in the microlensing cloud: eResearch tools for zooming into the heart of quasars Andrew Walsh, Curtin University [273] High spatial resolution observations of water masers in HOPS Kathrin Wolfinger, Swinburne [274] Exploring the Ursa Major region Graeme Wong, University of Western Sydney [275] The physical conditions of the Lupus molecular clouds Tim Young, University of New South Wales [276] Giants in Vela: The high energy tail of Vela's pulsed radio emission Christian Wolf, ANU [277]

Photometric Redshifts: Template-based vs. Empirical


ABSTRACTS

ORAL ABSTRACTS

1

WHAT CAN A GRAVITATIONALLY-LENSED QUASAR TEACH US? Rachel Webster

1

1. University of Melbourne, Parkville, VIC, Australia The third gravitationally lensed quasar that was discovered is also one of the most unusual: in Q2237+0305 the lensing galaxy is ten times closer than might be expected. Since it is relatively nearby, the lensing galaxy and its surrounds can be explored at much higher resolution than is usually possible. This talk will follow an historical timeline, tracing our developing understanding of both the microlensing of quasars and the potential uses of lensing both as a quasi-high resolution telescope, and as a tracer of dark matter distributions.

2

SAMI AND THE SAMI GALAXY SURVEY Julia Bryant

1 2

1. CAASTRO, Sydney, Australia 2. University of Sydney, NSW, Australia SAMI (Sydney university AAO MOS IFS) is a new multi-object IFU for the Anglo-Australian Telescope. It is the first on-sky application of innovative photonic imaging bundles called hexabundles, which will remove the aperture effects that have biased previous single-fibre multi-object astronomical surveys. A major galaxy survey using SAMI is now underway (http://sami-survey.org/) and has the potential to revolutionise our understanding of galaxies, with spatially-resolved spectroscopy of 3400 targets planned over the next 3 years. Scientific objectives of the SAMI galaxy survey will be outlined and I will present some early science results showing the effectiveness of hexabundles on sky and the potential of the survey. URL for supporting material - http://sami-survey.org/

3

THE AUSTRALIA TELESCOPE LARGE AREA SURVEY: DATA RELEASE AND EARLY SCIENCE Julie Banfield

1 , and the ATLAS Team

1. CSIRO Astronomy and Space Science, Marsfield, NSW, Australia The Australia Telescope Large Area Survey (ATLAS) is the widest deep radio survey to date, covering ~7 square degrees at 1.4 GHz down to 15µJy/beam. ATLAS covers two fields, the Chandra Deep Field South (CDFS) and the European Large Area ISO Survey South 1 (ELAIS S1), where we have catalogued ~5000 source components. These data compliment the current multi-wavelength coverage from X-Rays to Radio wavelengths. The primary science goal of ATLAS is to study the formation and evolution of galaxies and I will present the data release and a first look at the science ATLAS will contribute to the broader astronomical community.

4 (S)

DEEP 21-CM HI OBSERVATIONS WITH THE ARECIBO TELESCOPE Laura Hoppmann

1 , Lister Lister Staveley-Smith

1 , Wolfram Freudling

2

1. ICRAR/UWA, Crawley, WA, Australia 2. ESO, Garching, Bayern, Germany The star formation rate (SFR) in galaxies, as measured by optical, UV and far-infrared observations, appears to increase by an order of magnitude over the redshift interval of z=0 to z≈1. However, little accurate information about the co-evolution of neutral hydrogen is available. Measurements are limited to sparse and model-dependent


observations of damped Lyman-α systems at high redshifts or to observations of 21cm radio emission line at very low redshift. However, the unique sensitivity of the Arecibo telescope can be used to directly detect 21-cm HI emissions from galaxies at cosmological distances. Previous detections have involved optically pre-selected galaxies and are therefore biased in their selection criteria. Here we present results from the ongoing Arecibo Ultra Deep Survey (AUDS) which is a blind 21-cm survey with the Arecibo L-band Feed Array (ALFA). We use data from AUDS to accurately derive the HI mass function and constrain the cosmic HI density ΩHI at redshifts greater than zero for the first time.

5

THE ROLE OF THE CLUSTER ENVIRONMENT ON THE STAR FORMATION CYCLE OF GALAXIES Luca Cortese

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia Even though it has been known for decades that the properties of galaxies are tightly linked to the environment they inhabit, we still miss a coherent picture on the role played by the cluster environment on galaxy evolution. Until very recently, one of the main problems has been the lack of information about the properties of the different baryonic components (e.g.,gas, stars, dust and metals) taking part in the star formation cycle of galaxies and their variation with local density. Now, wide-area multi-wavelength surveys are finally under way, making it possible to investigate separately the effects of the environment on the different constituents of galaxies. In this talk, I will combine multiwavelength data (e.g., GALEX-UV, SDSS-optical, Arecibo-HI, Herschel-FIR/submm) for the Herschel Reference Survey, a volume-, magnitude-limited sample of nearby galaxies, to explore how the cold gas, dust and metal content and star formation activity of galaxies vary when moving from the field to the center of the Virgo cluster. I will conclude describing how upcoming multi-wavelength surveys will soon allow us to extend the same kind of analysis to galaxy groups, thus bridging the gap between cluster and field populations.

6 (S)

GALAXY AND MASS ASSEMBLY (GAMA): TESTING GALAXY FORMATION MODELS THROUGH THE MOST MASSIVE OBJECTS IN THE UNIVERSE Paola Oliva-Altamirano

1 , Sarah Brough

2 , Chris Lidman

2 , Warrick Couch

1 , Edward Taylor

3

1. Swinburne University of Technology, Hawthorn east, VIC, Australia 2. Australian Astronomical Observatory, Sydney, Australia 3. University of Melbourne, Melbourne, VIC, Australia Brightest Cluster Galaxies (BCGs) represent the most luminous systems known at present epochs. The extent to which such extreme galaxies have acquired their particular properties from their privileged location at the centres of clusters and/or their high density environment is of key astrophysical interest. Unfortunately, the assembly history and evolution of these giant galaxies is still poorly understood. We analyse the growth of BCGs in the last 3.5 billion years using a large sample from the Galaxy and Mass Assembly Survey (GAMA), 1220 BCGs/BGGs, and compare our results with the Semi-Analytic Models (SAMs) of De Lucia \& Blaizot (2007) and Tonini et al. (2012). The growth is analyse taking into account the BCG Stellar Mass-Halo Mass correlation, in other words, we compare the BCG stellar mass of like-to-like clusters. We find no significant growth between redshifts 0.3 and 0, whereas SAMs predict that BCGs have acquired 30\% of their stellar mass over this period of cosmic time. We also examine the position of the BCGs with respect to their Dark Matter Halo and find that around 14\% of the BCGs are not lying at the centre of the dark matter halo potential well and this could be an indicator of recent cluster mergers. In a further analysis, we find that around 40\% of the BCGs harbor on-going star formation, with rates in a range 0-4 M$_{\odot}$ per year, in agreement with the new recipes used in Tonini et al. (2012). While BCGs might not be completely dormant, the fraction of their mass being converted into new stars is still very low.


7

THE EVOLUTION OF GALAXIES IN COMPACT GROUPS Iraklis Konstantopoulos

1

1. Australian Astronomical Observatory, North Ryde, NSW, Australia Galaxies are seldom found in isolation. As a small unit of large clusters, individual members are subject to the volition of their groupings and evolve most commonly through interactions and mergers. In the parameter-space between too many friends and none at all lie compact galaxy groups. The ones classified by Hickson

1 (Hickson compact groups, or

HCGs) share the distinctive characteristics of low membership, isolation and high density. They exhibit low velocity dispersions, which result in prolonging interactions, when such events occur, or quasi-secular evolution, when they do not. They are also HI-deficient, to a very intriguing extent. I will be discussing multi-wavelength observations of a sample of 12 HCGs

2 3 and explore several themes, including the usage of gas, the dwarf galaxy membership, and the

apparent rapid morphological transformation of compact group galaxies. 1. Hickson, 1982, ApJ, 255, 382 2. Konstantopoulos et al., 2012, ApJ, 745, 30 3. Konstantopoulos et al., 2010, ApJ, 723, 197

8

SMALL WORLDS, BIG PUZZLES: INSIGHTS FROM THE SOLAR SYSTEM'S OUTER FRONTIERS Michele Bannister

1

1. NRC - Herzberg, Victoria, BC, Canada The cold, distant outer regions of our Solar System that lie beyond Neptune's orbit have provided an exciting past decade of discoveries. The small worlds in these volumes are the remnant planetesimals of the protoplanetary disk. Their surprisingly rich variety of dynamically defined populations, on orbits that are mostly now isolated and preserved from further interaction, provide evidence for major restructuring of the giant planetary architecture in the early history of the Solar System. The mechanisms of how this happened, sharply or smoothly, are an active area of theoretical debate: no model yet provides a match to all aspects of the observed populations. The sixteen hundred trans-Neptunian objects that are known have been discovered in the last two decades through sky surveys with optical telescopes. Upcoming surveys using wide-field imagers on 4m to 8m-class telescopes promise to draw in the details of this history. Understanding the tangled set of dynamical and physical properties in our most accessible of planetary systems will have implications for our wider understanding of the evolution of planetary systems.

9

FIRST RESULTS FROM THE AAT SEARCH FOR HABITABLE-ZONE EXOPLANETS ORBITING LATE M-DWARFS Duncan Wright

1 , Christopher Tinney

1 , Robert Wittenmyer

1

1. UNSW, Kensington, NSW, Australia Finding Earth-like planets orbiting in the ‘habitable zone’ of other stars is one of the major goals of modern astronomy. Detecting Earth-like planets, in Earth-like orbits around Sun-like stars is currently beyond reach of any facility except Kepler (and is problematic even then). What is possible now, is the detection of Earth-like planets in habitable-zone orbits around low-mass stars using the radial velocity technique. Early indications from both Doppler planet searches and Kepler are that rocky planets around low-mass stars are common. A new program searching for habitable-zone exoplanets orbiting M4-M6 dwarfs on the Anglo-Australian Telescope began in late 2012. This program uses the new CYCLOPS fibre-feed working in the near infra-red to obtain high-precision velocities. This talk outlines the techniques used to analyse these data, the precision achieved, and the first results from this survey.


10

DYNAMICAL CONSTRAINTS ON MULTI-PLANET EXOPLANET SYSTEMS Jonathan Horner

1 , Robert A Wittenmyer

1

1. UNSW School of Physics, SYDNEY, NSW, Australia As a direct result of ongoing efforts to detect more exoplanetary systems, an ever-increasing number of multiple-planet systems are being announced. But how many of these systems are truly what they seem? In many cases, such systems are announced solely on the basis of orbital fits to observational data, and no attempt is made to see whether the proposed orbits are actually dynamically feasible. As a result, it is certain that "planetary systems" are being announced that involve planets moving on orbits that would be dynamically unstable on timescales of just a few hundred years. Here, we present the results of detailed dynamical simulations that investigate the orbital stability and evolution of a number of recently announced multi-planet exoplanetary systems. These simulations have enabled us to create highly detailed dynamical maps of those systems, allowing us to better constrain the orbits of the planets contained therein

1 4 . In some cases, our results have even led to the very existence of the planets themselves being called into

question2 3 .

1. Horner, J. et al., 2012a, Monthly Notices of the Royal Astronomical Society, 425, 749 2. Horner, J. et al., 2012b, Monthly Notices of the Royal Astronomical Society, 427, 2812 3. Horner, J. et al., 2011, Monthly Notices of the Royal Astronomical Society: Letters, 416, L11 4. Wittenmyer, R. A., Horner, J. & Tinney, C. G., 2012, The Astrophysical Journal, 761, 165

11 (S)

UNVEILING THE 2D CHEMISTRY OF PROTOPLANETARY DISCS Francesco Pignatale

1 , Sarah Maddison

1 , Kurt Liffman

2 , Geoffrey Brooks

3

1. Swinburne University of Technology, Hawthorn, Vic, Australia 2. MSE, CSIRO, Melbourne, Vic, Australia 3. FEIS, Swinburne University of Technology, Melbourne, Vic, Australia Planets, meteorites and all the objects of our Solar System result from different physical and chemical processes which occurred during the protoplanetary disc phase. IR observations of protoplanetary discs provide insights into the chemistry of the surface layers, but do not provide any information on the chemistry of the disc interior and the midplane where planets form. Theoretical radial condensation sequences are in general agreement with the bulk composition of the Solar System planets, but they can not explain the chemistry of rare objects like carbonaceous and enstatite chondrites, and the carbon-rich content of asteroids. Hence, more detailed modeling is required. We utilize a chemical equilibrium code and a 2D disc model to derive the largest chemical simulation of the Solar Nebula, and, for the first time, simultaneously compute the chemical composition within all regions of the disc, from its surface to the midplane, for over 400 gases and solid compounds. In this talk I will present an overview of the resulting 2D chemical distribution, focusing on some key compounds such as silicates, and show that: (1) the chemistry derived from IR observations are not representative of the bulk chemistry of the disc midplane; (2) we have identified the potential zone in which enstatite chondrites could have formed, supporting recent evidence that these objects and the surface of Mercury shared similar bulk compositions ; and (3) the 2D disc hosts carbon-rich reservoirs, which could have led to the formation of carbon-rich asteroids, and from which the gas giants might have accreted their atmospheres. These new results were only achievable with the 2D chemical distribution, which provides new insight not possible with 1D condensation sequences.

12

HI PROPERTIES OF MASSIVE GALAXIES Barbara Catinella

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia Quantifying how the gas content depends on galaxy properties and their environment is of paramount importance for constraining models of galaxy formation. Equally important is to perform such studies on large and unbiased samples of galaxies, in order to obtain results that are truly representative of the local population. I will present results based on the recently completed GALEX Arecibo SDSS Survey (GASS), which was designed to provide such a representative sample for massive galaxies. I will discuss how the atomic hydrogen (HI) content of


massive systems depends on their structural and star formation properties, as well as on their environment, and will point out the relevance of these findings for the future surveys that will be carried out with the Square Kilometer Array and its pathfinders.

13

LOUISE WEBSTER PRIZE THE CONNECTION BETWEEN STAR FORMATION AND TURBULENCE Andy Green

1

1. Australian Astronomical Observatory, North Ryde, NSW, Australia This is the story of the discovery of a simple correlation among all star forming galaxies, a correlation which is not unexpected, but which still remains largely unexplained. The discovery itself has answered far fewer questions than it has created. I will describe how we know that star formation and gas turbulence are correlated in galaxies, and why that discovery has enabled a much greater search to understand not only the correlation itself, but also the evolution of star forming galaxies in general.

14 (S)

A SEARCH FOR INTERVENING HI ABSORPTION IN NEARBY, GAS-RICH GALAXIES Sarah Reeves

1 2 3 , Elaine Sadler

1 3

1. ARC Centre of Excellence for All-Sky Astrophysics, Sydney, Australia 2. CSIRO Astronomy and Space Science (CASS), Sydney, Australia 3. University of Sydney, NSW, Australia The 21cm HI absorption-line provides an ideal probe of the gas distribution and kinematics in galaxies well beyond the local universe (z > 0.3). However, we currently lack the understanding to infer galaxy properties from absorption-line data alone. To address this, we are conducting a search for intervening HI absorption in a sample of 20 nearby, gas-rich galaxies. Using observations with the ATCA we are able to detect both absorption and emission from the target galaxies. We investigate how detection-rate varies with distance from the galaxies, and make detailed comparisons of the absorption- and emission-line features to improve our understanding of the interpretation of absorption-line data. In our pilot sample of six, we have made two tentative detections, which we now plan to follow-up with further observations. We also use VLBI observations to investigate how the properties of the background source might affect the detection rate. In this talk I will present the results from pilot sample, and more recent observations, and discuss implications for future absorption-line surveys.

15

THE GIANT LOBES OF CENTAURUS A OBSERVED WITH THE MURCHISON WIDEFIELD ARRAY Benjamin McKinley

1 , Frank Briggs

1 , Bryan Gaensler

2 , Ilana Feain

3 , MWA Builders List

1. Australian National University, Canberra, ACT, Australia 2. University of Sydney, Sydney, Australia 3. CSIRO, Sydney, Australia Due to our fortuitous position in space, we have access to an ideal laboratory to study one particular radio galaxy in great detail: Centaurus A. Since its discovery in 1948

1 as the discrete radio source associated with the nearby (3.8

Mpc) elliptical galaxy NGC5128, it has been intensely studied across a wide range of wavelengths and physical scales. The most striking features of Centaurus A are the giant radio lobes, which, due to the galaxy’s close proximity, have an unusually large angular extent of approximately 8 by 4 degrees on the sky, presenting a practical challenge to radio astronomers. Feain et al

3 have produced the first high-resolution images of the giant lobes to date, achieving 50 arcsec

(600 pc) resolution at 1.4 GHz with the Australia Telescope Compact Array and unveiling a complex morphological structure. The spatially-resolved spectral properties of the lobes at low radio frequencies are interesting as they provide clues as to the particle acceleration history of the lobes and the physical processes which caused their current morphology. However, low-frequency spectral-index maps have so far been hampered by the low spatial resolution of the images below 1.4 GHz

2 or small frequency ranges

5. The Murchison Widefield Array (MWA

4,6), with a spatial


resolution of several arcmins and observing frequencies between 80 and 300 MHz, is ideally suited to providing the low-frequency maps needed to examine the spectra of the giant lobes of Centaurus A in detail. I will summarise the initial low-frequency studies conducted with the MWA 32-tile prototype

7 and present the latest observations of

Centaurus A conducted during the recent science commissioning of the full 128-tile instrument. 1. Bolton, J. G., 1948, Nature, 162, 141 2. Combi, J. A., Romero, G. E., Arnal, E. M., 1998, A&A, 333, 298 3. Feain, I. J., Ekers, R. D., Murphy, T., et al, 2009, ApJ, 707, 114 4. Lonsdale, C. J., Cappallo, R. J., Morales, M. F., et al, 2009, in Proc. IEEE, 97, 8 5. Stefan, I. I., Carilli, C. L., Green, D. A., et al, 2012, arXiv:1212.1624 6. Tingay, S. J., Goeke, R., Bowman, J. D., et al, 2013, PASA, 30, 7 7. McKinley et al, in prep

16

FURTHER ADVENTURES IN THREE-DIMENSIONAL VISUALISATION: LEAPING INTO YOUR DATA Christopher Fluke

1 , David Barnes

2

1. Swinburne University of Technology, Hawthorn, VIC, Australia 2. Monash Biomedical Imaging, Monash University, Clayton, Australia Two long-standing problems in three-dimensional visualisation are the need for 1) a method to publish interactive 3D data as part of a research paper and 2) an intuitive, low-cost, desktop-based 3D pointing device. The S2PLOT programming library was developed with the 3D data visualisation needs of astronomers in mind. Along with providing a simple, yet powerful, programming interface for C/C++/Fortran codes at the desktop, S2PLOT provides a solution for the first problem through its pathway for creating interactive 3D figures for PDF documents. This capability has now been enhanced, enabling the creation of 3D-PDFs directly from LaTeX documents using only free, open source software. A solution to the second problem is now also in hand, thanks to the new Leap Motion Controller gesture-based device. We will demonstrate how S2PLOT continues to help astronomers to get in touch with their 3D data and share it with the world.

17

BUILDING MODEL UNIVERSES IN THE "CLOUD": THE THEORETICAL ASTROPHYSICAL OBSERVATORY (TAO) Darren Croton

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia In this talk I will discuss the use of new technologies to build and deliver cosmological-scale galaxy formation models to the community. Combining high performance computing, a "web 2.0" front-end architecture, and cloud-based processing and storage, the NeCTAR funded "Theoretical Astrophysical Observatory" (TAO) will allow astronomers construct their own mock light cones from a range of different simulations and galaxy models, filter the output through virtual telescopes, and download the results for their own scientific use. TAO will be of value to both large survey teams and individuals, and should serve a wide range of scientific needs.

18

THE ORIGIN AND EVOLUTION OF DWARF GALAXIES Samantha Penny

1

1. Monash University, MoCA, Clayton, VIC, Australia This talk will focus on dwarf galaxies, the most numerous galaxy type in the Universe. These low mass galaxies are fundamental in understanding galaxy evolution, and galaxy formation models must be able to predict and describe their properties. However, recent observations suggest mutiple origins for the dwarf galaxy populations of nearby groups and clusters, suggesting they are not a simple, homogeneous population. In this talk, I will review our current understanding of dwarf galaxy formation and evolution. Using deep observations of nearby galaxy clusters, I will also show that the line between low mass galaxies and massive star clusters is becoming increasingly blurred, with


increasing evidence that some ultra compact dwarfs are the stripped remnants of dwarf ellipticals rather than being massive globular clusters.

19

TIDAL DWARF GALAXY CANDIDATES IN GAS-RICH GROUPS Sarah M Sweet

1 , Michael J Drinkwater

1 , Gerhardt Meurer

2 , Virginia Kilborn

3 , Kenji Bekki

2 , Helga Denes

4

1. University of Queensland, Qld, Australia 2. ICRAR, UWA, Perth, Australia 3. Swinburne, Melbourne, Victoria, Australia 4. Swinburne, Melbourne, Victoria, Australia We have uncovered an interesting population of star-forming dwarf galaxies in Local Group-like groups of galaxies. The dwarf galaxies in these groups have very high Halpha equivalent widths, are quite compact, and are mostly not obviously attached to a host galaxy. Integral field spectroscopy with WiFeS reveals that these dwarfs have a wide range of metallicity, some significantly above that expected for their small size. Many also have strong signs of rotation and low mass-to-light ratios measured within 1.5 effective radii. Such observations indicate that these particular dwarfs are not newly forming in their own cold dark matter haloes, because we would then expect them to have low metallicities and high mass-to-light ratios. Rather, they appear to have formed in clumps of pre-enriched tidal debris flung off of interacting giant galaxies. We have recently also obtained DEIMOS multi-object spectroscopy to measure rotation curves of the more likely candidates, out to 3 effective radii. Observations of falling rotation curves and low mass-to-light ratios will indicate that these are indeed tidal dwarf galaxies.

20

GLOBULAR CLUSTER STUDIES UNCOVER REMARKABLE DETAILS OF ONGOING ACCRETION IN THE HALOES OF TWO NEARBY EARLY-TYPE GALAXIES Christina Blom

1

1. Swinburne University, Hawthorn, VIC, Australia It is thought that giant early type galaxies accrete large numbers of smaller galaxies during the later stages of their evolution. Observers have only recently uncovered the low surface brightness light showing these accretion events as they happen. The photometric discoveries of intra-group/intra-cluster light tantalise us with the potential chemical and dynamical information that could be gleaned from spectroscopic observations, but these spectroscopic observations are just out of reach with current instruments. I will discuss how I have used photometric and spectroscopic observations of globular clusters, situated in tidally stripped stellar streams and accreting onto NGC 4365 and NGC 4111, to extract some of the chemical and dynamical details contained in the stellar streams. Globular clusters are much more easily observed than diffuse stellar light and can be used to illuminate the properties of galaxy/group haloes. NGC 4365 is a group dominant elliptical galaxy, 6 Mpc behind the Virgo Cluster, showing a number of rare properties, including the combination of a kinematically distinct core and a ~90 degree kinematic misalignment as well as a unique 3

rd globular cluster subpopulation. It is currently accreting another strange galaxy NGC 4342, which has itself

been the subject of much recent debate regarding its own dark matter halo. NGC 4111 is an S0 galaxy, also the dominant member of a group 15 Mpc away and we have discovered a stellar stream extending from another group galaxy UGC 7094 to the centre of NGC 4111. I will present results from wide-field imaging and state-of-the-art spectroscopy from the DEep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck II telescope.


21

THE [FE/H] ABUNDANCE DISPERSION IN THE REMOTE HALO GLOBULAR CLUSTER NGC 5824 Gary Da Costa

1

1. Australian National University, Weston Creek, ACT, Australia Star-to-star variations in light elements such as O and Na are ubiquitous within the Galaxy's globular cluster population. However, there are relatively few clusters which show internal variations in the heavier elements such as Fe and Ca. The stellar system omega Cen has long been known to possess a substantial internal abundance range, and more recently, smaller intrinsic [Fe/H] abundance dispersions have been established in other globular clusters such as M22 and M54. In a recent paper (Saviane et al 2012, A&A, 504, A27) we suggested that the luminous (MV = -8.9) outer halo (Rgc = 26 kpc) globular cluster NGC5824 also possesses a small intrinsic [Fe/H] dispersion. The result was based on spectra at the Ca triplet of 17 red giants. Here I will present the results of an extensive follow-up spectroscopic study of red giants in the cluster based on Ca triplet spectroscopy obtained at the VLT with FORS2 and at Gemini-South with GMOS. I will compare the resulting abundance distribution for NGC5824 with those for M22, M54 and omega Cen and comment on the possible connection between globular clusters like these and the disruption of dwarf galaxies during the formation of the Galaxy's halo.

22

THE MURCHISON WIDEFIELD ARRAY, LOW FREQUENCY PRECURSOR TO THE SQUARE KILOMETRE ARRAY Steven Tingay

1

1. Curtin University, Bentley, WA, Australia I'll introduce the segment of the special session on the Murchison Widefield Array (MWA) by giving an overview of this next generation low frequency interferometer. The MWA is the low frequency Precursor for the Square Kilometre Array; construction was completed in late 2012, science commissioning was completed in June, and the instrument has now entered its full science operations phase. The MWA is the first of the three SKA Precursors to be fully operational for science and will support four main science themes: 1) the search for signals related to the first luminous objects in the Universe, from the Epoch of Reionisation; 2) a wide range of galactic and extragalactic science based around wide-field surveys; 3) searches for common and exotic transient and variable phenomena on timescales from millisseconds to years; 4) studies of the Sun and the Earth's ionosphere. I'll describe the instrument, its capabilities, its operational parameters and an overview of the first round of successful observing proposals, initial results from the science commissioning phase, and the intimate connection between the MWA and the international SKA pre-construction phase that will be executed over the next three years. The full MWA system description is given by Tingay et al. (2013, PASA, 30, 7) and a full description of the MWA science themes is given by Bowman et al. (2013, PASA, 30, 31).

23

THE MWA ALL-SKY SURVEY Randall Wayth

1

1. Curtin University, Perth, WA, Australia The extraordinary field of view of the MWA gives it impressive survey capabilities. The GaLactic and Extragalactic All-sky MWA (GLEAM) survey will cover the entire sky visible to the MWA over a range of radio frequencies yielding a comprehensive census of the low frequency radio sky. GLEAM will allow astronomers to study a wide range of astrophysical objects, from the very small (pulsars and their wind nebulae) to the very large (cosmic ray acceleration mechanisms in galaxy clusters). Local to our Galaxy, GLEAM will enable astronomers to study Galactic magnetism, supernova remnants and the interstellar medium in unprecedented detail. On cosmic scales, GLEAM will allow astronomers to find and study the most distant radio sources, advancing our understanding of the evolution of the Universe during its early times. The exceptional survey speed of the MWA will enable astronomers to regularly revisit large regions of the sky, thereby allowing studies of the radio sky in the time domain. The MWA is unrivaled in its ability to systematically study large regions of the sky for transient and variable radio sources, thereby opening a new domain of astronomy that complements similar programs on optical and other telescopes. URL for supporting material - http://www.mwatelescope.org/


24

MWA: EPOCH OF REIONISATION Rachel Webster

1 , & MWA EoR Collaboration

1. University of Melbourne, Parkville, VIC, Australia The MWA was designed to as a large-N small-d prototype telescope optimised to detect the Epoch of Re-ionisation. This talk will present the first published results from the MWA EoR collaboration, describing the limits obtained from a few hours of data on the 32-tile prototype. A description of the potential of the MWA array to measure the EoR signal will be presented, with a brief discussion of both new techniques already developed, and the challenges yet to be understood.

25

TRANSIENTS AND VARIABLES WITH THE MURCHISON WIDEFIELD ARRAY Martin Bell

1

1. Sydney University, Redfern, NSW, Australia In this talk I will present results from a survey conducted with the prototype MWA instrument. In this survey almost 60 repeat observations were obtained of an area of sky ~2000 deg

2, to a flux limit of >300 mJy. I will present the

results of a statistical analysis of the variability of sources within these fields on day, week and year timescales. In will relate this to the current ‘state-of-the-art’ of transient and variable radio surveys, and I will demonstrate how competitive the MWA is at leading an assault on the dynamic low frequency radio sky, in future operations.

26

INFORMATION THEORY AND THE MWA Cathryn Trott

1

1. Curtin University, Bentley, WA, Australia The science we can perform with an instrument is determined by the information contained within the data and the ability of our methods to extract this information. Next-generation low frequency wide-field radio interferometers, such as the Murchison Widefield Array (MWA) in Western Australia, are capable of delivering exciting new science results, but present new challenges to understanding our instrument and designing our analysis methods. In this talk I will present some of the information theory techniques being used to understand the limitations of MWA datasets, as a crucial testbed for SKA-low design. I will then present one example of where an understanding of the instrument informs the strategies used to detect the Epoch of Reionisation signal from high redshift neutral hydrogen.

27

MWA OBSERVATIONS OF THE GALACTIC PLANE AND MAGELLANIC CLOUDS Natasha Hurley-Walker

1

1. Curtin Institute of Radio Astronomy, Perth, WA, Australia Located in the Southern Hemisphere, the MWA is an ideal instrument for observing the low-frequency radio emission from the Galactic Plane, as well as the Small and Large Magellanic Clouds. I will present an overview of the science possible from these observations, challenges inherent in working with interferometric measurements of the diffuse sky, and show some preliminary MWA commissioning results.


28

FIRST POLARISATION RESULTS WITH THE MWA Emil Lenc

1 2

1. CAASTRO, Redfern, NSW, Australia 2. University of Sydney, Redfern, NSW, Australia While the Murchison Widefield Array is now in the processes of passing the baton from the commissioning phase to operations, a great deal of experience has been accumulated in this early phase of the instrument. Here I will present an overview of long-wavelength polarimetry with the MWA together with recent results obtained during commissioning that demonstrate its polarimetric capabilities.

29

THE AUSTRALIAN SKA PATHFINDER – AN UPDATE Antony E.T. Schinckel

1 for the ASKAP Team (1)

1. CSIRO Astronomy and Space Science, Epping, NSW, Australia The Australian Square Kilometer Array Pathfinder (ASKAP) will be the fastest cm-wave survey instrument in radio astronomy. ASKAP will consist of 36 12-meter 3-axis antennas in a 6 km diameter configuration providing up to 10 arcsec of resolution. Each antenna is equipped with a large checkerboard phased array feed (PAF) operating from 0.7 to 1.8 GHz, and digital beamformer preceding the correlator. The 96 dual-polarization elements (192 receivers) of the PAF and the subsequent beamformer will provide about 30 beams (at 1.4 GHz) to produce a 30 square degree field-of-view, allowing rapid, deep surveys of the entire visible sky. The antenna incorporates a third axis to fix the parallactic angle with respect to the entire optical system (blockage and phased array feed). The first antenna was deployed at the MRO in late 2009, and the last was commissioned in June 2012, with installation of receivers, beamformers and the correlator now underway. Currently three antennas have Mk I Phased Array Feeds and their beamformers installed. CSIRO has commenced early commissioning of these as part of the BETA project to test and further develop PAFs and Beamforming for ASKAP. Development of the Mk II PAF and digital systems (which have significant improvements over the Mk I systems) is also progressing well. The site of ASKAP is the Murchison Radio-astronomy Observatory, 315 kilometres north east of Geraldton, Western Australia, a new radio astronomy observatory being developed by CSIRO. The MRO and surrounding region has been selected as one of the sites for the SKA. A description of the ASKAP system, status and plans will be presented. URL for supporting material - http://www.atnf.csiro.au/projects/askap

30

UPDATE ON THE AUSTRALIAN SKA PATHFINDER (ASKAP) Lisa Harvey-Smith

1

1. CSIRO, Epping, NSW, Australia CSIRO's Australian SKA Pathfinder (ASKAP) is a radio interferometer in the remote Murchison region of Western Australia, equipped with phased array radio receivers for an ultra-fast survey capability. Whilst the full suite of receivers is still under construction, early engineering test results from only three dishes are giving us tantalising glimpses of things to come. In this talk, CSIRO's ASKAP Project Scientist will describe the status of ASKAP, present latest results from technical commissioning tests and discuss the plans for the commencement of scientific observations.


31

THE AUSTRALIAN SKA PROJECT OFFICE Brian Boyle

1

1. DIICCSRTE, Canberra, ACT, Australia I will summarize the work of the Australian SKA Project office in Canberra and outline it's role in preparing Australia to host the Square Kilometre Array project.

32

DESIGNING THE SKA Philip Diamond

1

1. SKA Organisation, Macclesfield, Chesh, United Kingdom Update on the status of the design process for the SKA and discuss the SKA baseline design.

33

SCIENCE WITH SKA1 - LOW FREQUENCY Stuart Wyithe

1

1. University of Melbourne, Parkville, Vic, Australia SKA1 - Low is proposed to be a low-frequency aperture array, operating at ~ 50MHz - 350MHz. The primary science case for SKA1-low is detection of the 21-cm HI-line during the Epoch of Reionization at redshifts from between 5 and 25. Secondary science cases include HI-line absorption against continuum sources, low radio frequency observations of pulsars, and magnetized plasmas both in the Galaxy and intergalactic space. This talk will briefly summarise these science cases and associated requirements, focussing on the Epoch of Reionization.

34

SCIENCE WITH SKA1-SURVEY Lister Staveley-Smith

1

1. University of Western Australia, Crawley, WA, Australia The survey component of Phase 1 of the SKA will be located in Western Australia, and will consist of 96 antennas, each equipped with a phased array feed. The instrument will be a substantial improvement on ASKAP in terms of sensitivity and survey speed. I will review the recently published baseline design and outline the primary science goals of this instrument, noting possible synergies with surveys being planned at other wavelengths.

35

THE BIRTH, LIFE AND DEATH OF OUR PLANET......AND OF THE UNIVERSE Charley Lineweaver

1

1. Australian National University, Canberra, ACT, Australia People, planets, stars and even universes are born, they live for a while and then die. I will review what we know about the origin of the earth and the origin of the life on it -- the coming extinction of this life and the death of the Earth and Sun. The second law of thermodynamics is relevant to the birth and death of the universe. I will try to explain why. The main goal of the lecture is to paint a picture of how we got here and how we fit into the universe.


36

SUPERNOVAE FROM THE FIRST STARS Alexander Heger

1

1. Monash University, Clayton, VIC, Australia The first stars to form in the universe may have had very different properties from later generation of stars. They were uniquely made form just primordial gas and also their formation process and characteristic masses may have been quite different. No direct observations of these star are possible at this time, however, so our ability to study these early stars is limited to indirect measurements and numerical simulations. For example, stellar forensics based on nucleosynthesis patterns preserved in subsequent generations of stars may be used in an attempt to reconstruct the properties of the first stars. The overarching big questions are: What are the typical masses of this first generation of stars? What is the initial mass function? And how did these stars live and die? This will determine how the universe transitioned from the first stars to the formation of the first galaxies, and what observations of them may be possible in the future. Early simulation of formation of the first stars and simple theoretical arguments suggested the these first stars may have been quite massive, possibly massive enough to explode as pair instability supernova. Interestingly, there is an increasing number of observations suggesting that even in the present universe very massive stars form and live to explode as powerful pair instability supernovae. But is this also outcome we should generally expect for the majority of the first stars and is it supported by observations of the "ashes" of the first stars?

37

ARE ULTRA-LONG AND SUB-LUMINOUS GAMMA-RAY BURSTS DISTINCT POPULATIONS? Eric Howell

1 , David Coward

1 , B Gendre

2 3 , G Stratta

3 , J. Atteia

4 5 , S. Basa

6 , M. Boer

7 8 , S. Cutini

2 , V. D'Elia

2 , A.

klotz4 5 , L. Piro

9

1. University Western Australia, Perth, WA, Australia 2. ASI Science Data Center, Galileo Galilei, I-00044 , Frascati, Italy 3. Osservatorio Astronomico di Roma, OAR-INAF, via Frascati 33, I-00040, Monte Porzio Catone, , Rome, Italy 4. Universit´e de Toulouse, UPS-OMP, IRAP, Toulouse, France 5. CNRS, IRAP, 14, avenue Edouard Belin, F-31400, Toulouse, France 6. Aix Marseille Universit´e, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388,

Marseille, France 7. CNRS, ARTEMIS, UMR 7250, Boulevard de l’Observatoire, BP 4229, F-06304 Nice Cedex 4, Nice, France 8. CNRS, Observatoire de Haute-Provence, F-04870 Saint Michel l’Observatoire, Marseille, France 9. Istituto di Astrofisica e Planetologia Spaziali di Roma, INAF, via fosso del cavaliere 100, I-00133, Roma, Italy Multiwavelength observations have shown gamma ray bursts to be the most luminous and distant transient events in the Universe. Originally categorised into two populations through their duration and spectral hardness: long/soft and short/hard; subsequent observations have suggested the existence of a number of sub-populations of burst. These include a sub-luminous population and a recently identified ultra-long population. Using a novel approach based on the arrival time records of the bursts we show how different source populations can be untangled by virtue of their intrinsic rate densities. Furthermore, we present an analysis of GRB 111209A, a burst observed for 7 hours, and suggest that this member of an ultra-long population resulted from the collapse of a low-metallicity blue super giant star. 1. E. Howell and D. Coward, 2013, A redshift–observation time relation for gamma-ray bursts: evidence of a

distinct sub-luminous population, MNRAS, 428, 167 2. B. Gendre, G. Stratta, J.L. Atteia, S. Basa, M. Boar, D. Coward, S. Cutini, V. D’Elia, E. Howell, A. Klotz, and L.

Piro, 2013, The Utra-long gamma-ray burst 111209A: The collapse of a blue supergiant, ApJ 766, 30, 2013


38

LOCATIONS OF PECULIAR SUPERNOVAE AS A DIAGNOSTIC OF THEIR ORIGINS Fang Yuan

1 2 , Chiaki Kobayashi

3 , Brian P Schimidt

1 2 , Philipp Podsiadlowski

4 , Stuart A Sim

2 5 , Richard A Scalzo

1 2

1. Australian National University, Weston Creek, ACT, Australia 2. ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Canberra, Australia 3. University of Hertfordshire, Hatfield, UK 4. Oxford University, Oxford, UK 5. Queen's University Belfast, Belfast, UK One of the key questions for understanding supernovae is the nature of their progenitors. For very nearby core-collapse supernovae, direct identifications of pre-explosion progenitor stars have led to the tightest constraints on their physical characteristics - but this is only possible in a handful of cases. Recently, an increasing number of unusual transients occurring far away from galaxies have been discovered by wide-field transient surveys. For these outlying events, direct observation of the local stellar population is impossible, due to low surface brightness. In this paper, we study a class of peculiar sub-luminous "calcium-rich" supernovae which exhibit locations consistently well outside their host galaxies' centres. We compare their distribution with globular clusters and stellar populations through the results of self-consistent cosmological simulations. A statistical analysis shows that their distribution is consistent with globular clusters or a very old metal-poor population. Because several of the objects have photometric limits which exclude an underlying globular cluster, we can conclude that this population represents an exotic explosion process involving the oldest most metal poor stars in the local universe. Recent large transient experiments indicate that there are other classes of objects that occur at atypically large distances from their host galaxies. The methods developed in this paper can be used in the future to help identify the progenitors of these unusual classes of objects as sufficient numbers become available to undertake a statistical analysis.

39

THE IMPLICATIONS OF THE GIANT, MAGNETIZED OUTFLOWS FROM THE GALACTIC CENTRE Roland Crocker

1

1. ANU, Weston Creek, ACT, Australia Using polarimetry data collected for the S-PASS survey by the Parkes radio telescope, Carretti, Crocker et al.

1 have

recently discovered giant, magnetized outflows from the Galactic nucleus. I explain the implications of these outflows for understanding the global mass and energy flows through the centre of the Galaxy and show how these outflows - and the coincident Fermi Bubbles found in gamma-ray data - are the result of star-formation occurring in this region rather than activity of the Galaxy's super-massive black hole. The S-PASS data also imply that very strong magnetic fields - surpassing 10 microgauss - extend many kiloparsecs into the Galactic halo. 1. Carretti et al. 2013 Nature, 493, 66

40

THE MISSING LINK: FROM MERGING NEUTRON STARS TO MAGNETIC JETS Luciano Rezzolla

1

1. Max-Planck Institute for Gravitational Physics, Potsdam, AAA, Germany Short Gamma-Ray Bursts (SGRBs) are among the most luminous explosions in the universe, releasing in less than one second the energy emitted by our Galaxy over one year. Despite decades of observations, the nature of their ``central-engine'' remains unknown. I will show how the dynamics of a binary of magnetized neutron stars leads to a rapidly-spinning black hole surrounded by a hot and highly-magnetized torus. The development of magnetohydrodynamical instabilities in the torus can amplify by several orders of magnitude the initially turbulent magnetic field, yielding an ordered poloidal field of ~ 10

15 G along the black-hole spin-axis, within a half-opening angle of 30 deg, which may

naturally launch a relativistic jet. I will show that the broad consistency of these ab-initio calculations with SGRB observations provides important confirmations that the merger of magnetized neutron stars can provide the basic physical conditions for the central-engine of SGRBs.


41 (S)

MEASURING THE BULK FLOW FROM THE 6DFGS PECULIAR VELOCITY SURVEY Christina Magoulas

1 , Christopher Springob

2 , Matthew Colless

3 , Jeremy Mould

4 , Heath Jones

1. University of Melbourne, Melbourne, VIC, Australia 2. University of Western Australia, Perth, W.A., Australia 3. Australian National University, Canberra, VIC, Australia 4. Swinburne University, Melbourne, VIC, Australia While recent years have seen rapid growth in the number of galaxy peculiar velocity measurements, disagreements remain about the extent to which the peculiar velocity field - a tracer of the distribution of mass, agrees with both lambda-CDM expectations and with velocity field models derived from redshift surveys. The 6dF Galaxy Survey includes Fundamental Plane (FP) distances and peculiar velocities for nearly 10,000 early-type galaxies, making it the largest and most homogenous galaxy peculiar velocity sample to date. In this presentation, we describe how we have used the 6dFGS velocity field to measure the local bulk flow and determine the range and influence of large-scale motions in the local universe. We also compare the galaxy density and peculiar velocity fields to establish the distribution of dark and luminous matter and better constrain key cosmological parameters such as the redshift-space distortion parameter.

42

SUPERNOVA DISCOVERIES AT Z > 2 AND THEIR HOST GALAXIES Jeff Cooke

1 , Mark Sullivan

2 , Avishay Gal-Yam

3 , Raymond Calrberg

4 , Emma Ryan-Weber

1 , Richard Ellis

5 , Chuck

Horst6 , Yuuki Omori

7 , Gonzalo Diaz

1

1. Swinburne University, Hawthorn, VIC, Australia 2. Oxford University, Oxford, UK 3. Weizmann Institute, Rehovot, Israel 4. University of Toronto, Toronto, Canada 5. Caltech, Pasadena, CA, USA 6. San Diego State University, San Diego, USA 7. McGill University, Montreal, Canada I will discuss our image-stacking, galaxy monitoring method that has successfully detected 15 supernovae at z > 2 in the Canada-France-Hawaii Telescope Legacy Survey Deep fields. I will present supernova light curves and late-time Keck spectra which include two recently discovered super-luminous, pair-instability supernova candidates at z = 2.05 and z = 3.90. Our supernova program monitors z > 2 Lyman break galaxies. I will compare the rest-frame ultraviolet photometric and spectroscopic properties of the supernova host galaxies with respect to the complete (~100,000) galaxy sample and discuss observed trends and implications. Because Population III stars are believed to exist down to z ~ 2, and clouds of pristine gas capable of forming Population III stars have been discovered at z ~ 3, our technique to detect z > 2 supernovae offers the first viable means to provide observational examples of the deaths of the first stars. Upcoming DES DECam, Hyper-SuprimeCam, and LSST surveys are poised to detect >50,000 supernovae at z ~ 2 - 6 that will fully characterize high redshift events and enable tight constraints on their progenitors and the form of the high-redshift IMF.

43

PECULIAR VELOCITY POWER SPECTRUM Jun Koda

1 , Andrew Johnson

1 , Chris Blake

1 , Tamara Davis

2 , Morag Scrimgeour

3 , Chris Springob

3

1. Swinburne University of Technology, Hawthorn, Vic, Australia 2. School of Mathematics and Physics, University of Queensland, Brisbane, QLD, Australia 3. International Centre for Radio Astronomy Research (ICRAR), University of Western Australia, Crawley, WA,

Australia Measuring galaxy peculiar velocities provides powerful new tests of the theory of gravity on cosmological scales, that are complementary to other cosmic probes. We present new cosmological fits to the most powerful existing dataset, the 6-degree Field Galaxy Survey velocity sample, which (in disagreement with some previous velocity data) are in concordance with the standard cosmological model. We explain our improvements in data analysis and modelling of velocity power spectrum. Looking forward, we also present new forecasts for how future velocity surveys performed with the Australian Square Kilometre Array Pathfinder will produce competitive tests of cosmology.


44 (S)

THE CROSS-POWER SPECTRUM BETWEEN 21CM EMISSION AND GALAXIES IN HIERARCHICAL GALAXY FORMATION MODELS Jaehong Park

1

1. The University of Melbourne, Parkville, VIC, Australia The correlation between 21cm fluctuations and galaxies is sensitive to the astrophysical properties of the galaxies that drove reionization. Thus, detailed measurements of the cross-power spectrum and its evolution could provide a powerful measurement both of the properties of early galaxies and the process of reionization. We will present the evolution of the cross-power spectrum between 21cm emission and galaxies using a model which combines the hierarchical galaxy formation model GALFORM implemented within the Millennium-II dark matter simulation, with a semi-numerical scheme to describe the resulting ionization structure. We will also show predicted observational uncertainties of the cross-correlation coefficient based on specifications of the Murchison Widefield Array combined with galaxy surveys of varying area and depth.

45

DRAGONS: THE DARK AGES REIONIZATION AND GALAXY FORMATION SIMULATION PROGRAM Gregory Poole

1

1. University of Melbourne, Parkville, Vic, Australia DRAGONS is an ambitious simulation program well-underway at the University of Melbourne aiming to describe the formation of the first galaxies and the co-evolution of the inter-galactic medium during the epoch of reionization. I will describe how DRAGONS will use an integrated suite of state-of-the-art hydro-dynamic, N-body and semi-analytic models of galaxy formation to achieve this goal and present the program's ongoing progress.

46

SN 2012FR: A LUMINOUS NORMAL TYPE IA SUPERNOVA IN NGC 1365 Michael J. Childress

1

1. Australian National University, Weston Creek, ACT, Australia SN 2012fr was a luminous normal Type Ia supernova in the nearby barred spiral galaxy NGC 1365. We obtained 65 optical spectra of SN 2012fr from nine telescopes spanning four continents over a two month period beginning two days after the date of explosion. High-velocity features at early epochs and a plateau in the velocity of intermediate mass elements at late epochs indicate complex layering of the ejected material. Absorption features in the maximum light spectrum indicate SN 2012fr lies on the borders between "subclasses" of Type Ia supernovae proposed in two recent classification schemes. Finally, distance measurements to NGC 1365 obtained as part of the HST Key Project on the extragalactic distance scale enable the use of SN 2012fr as a fundamental calibrator for measuring the Hubble constant.

47

DUST GRAIN SIZE SORTING IN THE TW HYDRAE PROTOPLANETARY DISK Christophe Pinte

1 , Francois Menard

1 , Maddison Sarah

2 , Pantin Eric

3 , Gonzalez Jean-Francois

4 , Ubach Catarina

2

1. UMI-FCA Santiago, Santiago, Chile 2. Swinburne, Melbourne, Australia 3. CEA, Paris, France 4. CRAL, Lyon, France Proto-planetary disks are the birthplaces of planets. During the very first stages of planet formation, the dust particles grow by coagulation. In parallel, the gas drag on dust particles results in vertical settling and subsequent radial migration towards the central star. Dust migration and settling are central processes for the formation of planets as they concentrate material in the disk mid-plane and increase the local density, a necessary process for efficient dust grain growth and subsequent planet building. Hydrodynamical simulations show that radial migration of the dust is most efficient for grains of mm and cm sizes and should occur on timescales smaller than 100 000 years.


In this contribution, we present 7 mm observations of the disk surrounding the T Tauri star TW Hydra, obtained with the ATCA interferometer (and planned cycle 1 ALMA 3mm observations). These observations allow us to measure the full extension of the disk as well as its brightness profile. The comparison with data obtained at shorter wavelengths (850 microns, which probe the distribution of smaller grains), shows a less rapid falloff of the amplitude as a function of uv-distance, suggesting radial migration of mm/cm-sized grains. The analysis of these data, with state-of-the-art radiative transfer models, allows us to establish, for the first time, quantitative constraints on the degree of dust migration in a T Tauri disk. We discuss the implications of our findings on planet formation.

48

THE ROLE OF RIDGES IN HIGH-MASS STAR FORMATION - HIGH RESOLUTION INSIGHTS FROM HERSCHEL Tracey Hill

1 , Frederique Motte

2 , Philippe Andre

2 , Pierre Didelon

2 , Doris Arzoumanian

2

1. Joint ALMA Observatory, Vitacura, -, Chile 2. AIM Paris-Saclay (CEA), Gif-sur-Yvette, Ile de France, France High mass stars are dynamic entities which tend to have a rather profound impact on their environment. Despite this, there remain many open questions about their formation and evolution.The Herschel Space Observatory, along with its dedicated key programs, is transforming our understanding of high-mass star formation, in particular providing key insights into the environment in which massive stars form. Herschel recently unveiled the highly filamentary structure of star forming complexes and the molecular constituents of the ISM where star formation takes place.We recently identified, from the HOBYS key program, high-column density supercritical filaments which appear to be the preferential sites of high-mass star formation. These ridges may result from the constructive convergence of flows (Hill et al., 2011) or from filament mergers (Hennemann et al., 2012). More recently we showed (Hill et al., 2012) that the Vela C ridge tends to have a filament width similar to that seen in low-mass star forming regions (Arzoumanian et al., 2011). Additionally, the Vela C ridge tends to display similar characteristics as Serpens South (from the Gould Belt survey) a low to intermediate mass region. Such results test suggestions of a column density threshold seen in numerical simulations. I will also discuss the impact of OB clusters on their immediate environment. In particular, in M16 (the Eagle Nebula, home to the pillars of creation), I will show how such a cluster may impact the evolution of the next generation of stars (Hill et al., 2012b). URL for supporting material – http://adsabs.harvard.edu/abs/2011A%26A...533A..94H http://adsabs.harvard.edu/abs/2012A%26A...542A.114H http://adsabs.harvard.edu/abs/2012A%26A...548L...6H

49 (S)

A MULTI-WAVELENGTH STUDY OF THE GQ LUP PROTOPLANETARY DISC Catarina Ubach

1 , Sarah Maddison

1 , Christopher Wright

2 , Francois Menard

3

1. Swinburne University, Hawthorn, VIC, Australia 2. ADFA@UNSW, Canberra, Australia 3. UMIFA-FCA, CNRS/INSU France, Santiago, Chile To observe the first stages planet formation around the 1Myr old classical T Tauri star GQ Lup, a multi-wavelength survey at 3, 7 and 15 mm was conducted with ATCA. We found the flux is temporally stable in all three wavebands, suggesting the flux is dominated by thermal dust emission. Our results also suggest that the protoplanetary disc contains large cm-sized pebbles and has an outer disc radius greater than 200 AU. Our disc size contradicts previous 1.3 mm SMA observations by Dai et al. (2010)

1 , who suggested a compact disc with an outer radius confined to 25 –

75 AU best fitted the data. Since their model did not account for the longer wavelength data, which provides information about larger grains that affect the temperature distribution and dust disc mass estimates, we used the radiative transfer code MCFOST to fit our longer millimetre observations along with the SMA data and shorter wavelength observations from the literature. Here we present the results for both our multi-wavelength survey and the full parameter sweep. 1. Dai et al., 2010, AJ, 139, 626


50

MAGMO: MAPPING THE GALACTIC MAGNETIC FIELD THROUGH OH MASERS James Green

1 , Naomi McClure-Griffiths

1 , James Caswell

1 , Tim Robishaw

2 , Lisa Harvey-Smith

1 , Sui Ann Mao

3

1. CSIRO Astronomy and Space Science, Epping, NSW, Australia 2. DRAO, Penticton, Canada 3. University of Wisconsin, Maddison, USA We have completed observations for a project to examine large-scale magnetic fields pervading regions of high-mass star formation. Through correlating targeted observations of ground-state OH maser emission towards more than 500 sites of high mass star formation, this project aims to test if the orientations of weak large-scale magnetic fields can be maintained in the contraction (and field amplification) to the high densities encountered in regions of high-mass star formation. Our observations were made with the Australia Telescope Compact Array, using the new broadband backend, to capture all four ground-state transitions in full polarisation simultaneously. These observations were made towards sites of high-mass star formation traced by 6.7-GHz methanol masers detected in the Methanol Multibeam Survey. I will discuss the detections, local- and large-scale magnetic field properties and the implications for the role of magnetic fields in high-mass star formation.

51 (S)

THE MEMBERSHIP AND MULTIPLICITY OF SCO-CEN Aaron C Rizzuto

1 , Michael J Ireland

1

1. Macquarie University, North Ryde, NSW, Australia OB associations provide a glimpse into a group of stars directly after formation. The nearest OB association to the sun is the Sco-Cen association, and is also the nearest region of massive star formation. Sco-Cen provides a rich laboratory for the study of the output of star formation. Despite the relatively complete high-mass membership, the G to M-type PMS membership is highly incomplete. We have developed a Bayesian membership selection that assigns a membership probability based on position, proper motion, and photometry from all sky catalogues. Potential members will then be confirmed through spectroscopic youth indicators such as Li6708 and H-alpha using the WiFeS instrument on the 2.3m telescope. This will allow us to simultaneously search for massive planetary companions, such as GSC 06214-00210b analogs using spectroastrometric techniques. We have also characterised the multiplicity of the high-mass Sco-Cen stars using long baseline interferometry and all-sky data. We observed a 58 stars in the Sco-Cen region of sky, which were bluer that B-V = -0.1 and brighter than 5

thmagnitude using the Sydney University Stellar

Interferometer. We detected 24 companions, 15 of which were new detections. We then used all-sky data such as 2MASS and APASS magnitudes and UCAC4 proper motions to identify companions beyond 5 arcseconds separation. Combining our interferometric and all-sky surveys with the highly complete imaging and spectroscopic work in the literature, we used a Bayesian technique to derive the parameters of the Sco-Cen B-type multiplicity distribution. We find a companion frequency of 1.25, and estimate that as many as 23% of Sco-Cen B-type stars are single. This raises questions as to the angular momentum removal methods involved in the formation of high-mass stars. We also present preliminary results dating different parts of Sco-Cen with precision orbit measurements using long baseline interferometry and AO observations.

52

TERAHERTZ OBSERVATIONS OF STAR FORMING REGIONS FROM ANTARCTICA Michael C.B. Ashley

1 , Craig A. Kulesa

2 , Michael G. Burton

1 , John W.V. Storey

1

1. University of New South Wales, Sydney, NSW, Australia 2. University of Arizona, Tucson, USA In January 2012 we installed a 0.6m terahertz telescope (HEAT) on the PLATO-R observatory at Ridge A in Antarctica (Ashley 2013). HEAT is surveying the Galactic Plane in the atomic carbon lines at 492GHz and 809GHz and carbon monoxide at 806GHz. The spatial resolution of the survey is a few arcminutes, and the spectral resolution is 1 km/s. This is the deepest and highest resolution survey conducted at these frequencies. Velocity cubes from the 2012 season are now available on-line and are of a quality that is otherwise only obtainable from space. Numerous molecular clouds are resolved and can be overlayed with CO maps at lower frequencies taken with the Mopra telescope.


Ridge A, 150km from Dome A, the highest point on the Antarctic plateau, has shown itself to be a superlative terahertz site. For example, during March 2013, a relatively "wet" part of the year, the average precipitable water vapour was only 0.14mm. At 1.5THz the atmospheric opacity at Ridge A was below 1.5 for 85 days from January to October 2012, compared with 5 days for the same period on the Chajnantor plain. Even more importantly the opacity is highly stable, with our 2012 data suggesting that the sky noise is less that half that of the South Pole on average (Kulesa et al 2012). This is better than expected from a linear scaling of the total water vapour content at the two sites. The HEAT telescope was upgraded with an improved detector during a servicing mission in early 2013, with plans to reach the ionised carbon line at 1.9THz in 2014. 1. Ashley, M. C. B, 2013, "Care and feeding of an Antarctic telescope", in press, Physics Today, May 2013. 2. Kulesa, C. A., et al, 2012, "Opportunities for terahertz facilities on the high plateau", IAU Symp 288, 256.

53

MAKING A SPLASH WITH THE DISH Joanne Dawson

1 , Andrew Walsh

2 , Maria Cunningham

3 , Paul Jones

3 , Shari Breen

4 , Naomi McClure-Griffiths

4 ,

Cormac Purcell5 , Vicki Lowe

3 , Courtney Jones

1 , Vasaant Krishnan

1 , John Dickey

1 , Jimi Green

4 , Ettore Carretti

4 ,

Jose Gomez6 , Simon Ellingsen

1 , Jim Caswell

4 , Hiroshi Imai

7 , Steven Gibson

8 , Nadia Lo

9 , Patrick Hennebelle

10

1. University of Tasmania, Hobart, TAS, Australia 2. Curtin University, Perth, Australia 3. UNSW, Sydney, Australia 4. CSIRO Astronomy and Space Science, Sydney, Australia 5. University of Sydney, Sydney, Australia 6. Instituto de Astrofísica de Andalucía, Granada, Spain 7. Kagoshima University, Kagoshima, Japan 8. Western Kentucky University, Bowling Green, USA 9. Universidad de Chile, Santiago, Chile 10. Observatoire de Paris, Paris, France The process by which dense, star-forming clouds form from the diffuse ISM is an important part of galaxy evolution, and a major unsolved problem in modern astrophysics. To construct a comprehensive observational picture, multiple tracers are needed that can follow the ISM through all stages of its evolution. However, we lack large-scale spectral line tracers of the diffuse molecular regime, in which hydrogen is in the form of H2 but CO abundances are low. Such "transition-state" gas is the missing link that probes the earliest stages of the molecular cloud formation process, but is completely missed by traditional molecular line surveys. The ground state OH lines at 1612, 1665, 1667 and 1720 MHz may provide an answer to this problem. With low critical densities and enhanced abundances in diffuse molecular gas, OH is an effective - but underexploited - tracer of the CO-dark molecular ISM. SPLASH (the Southern Parkes Large-Area Survey in Hydroxyl) is a large, unbiassed and fully-sampled survey of OH emission, absorption and masers that will map the Galactic Plane and Galactic Centre at unprecedented scales and sensitivities. This dataset will answer critical questions on the global distribution of diffuse OH, the degree to which it traces hidden molecular gas, and its role as a probe of molecular cloud formation. As a blind and sensitive survey of all four ground-state transitions, SPLASH is also detecting a large number new OH masers, facilitating a broad range of astrophysical studies, from star formation, to evolved stars, to SNRs. I will report on the science aims and strategy of SPLASH, and present initial results from its first two semesters, which have revealed a rich and complex distribution of OH emission and absorption in a subsection of the Southern Milky Way.


54 (S)

HIGH VELOCITY CLOUDS IN THE GALACTIC ALL SKY SURVEY: CATALOGUE Vanessa A. Moss

1 2 , Naomi M. McClure-Griffiths

2 , Tara Murphy

1 3 , D.J. Pisano

4 5 , Jonathan K. Kummerfeld

1 , James

R. Curran3

1. Sydney Institute for Astronomy, School of Physics, University of Sydney, Camperdown, NSW, Australia 2. CSIRO Astronomy and Space Science, ATNF, Epping, NSW, Australia 3. School of Information Technologies, University of Sydney, Camperdown, NSW, Australia 4. School of Physics, West Virginia University, Morgantown, West Virginia, United States 5. Adjunct Assistant Astronomer, National Radio Astronomy Observatory, Green Bank, West Virginia, United

States We present a catalogue of high velocity clouds (HVCs) from the second release of the Galactic All Sky Survey in neutral hydrogen. Our catalogue resolves for the first time the velocity width distribution of southern-sky HVCs, revealing a median cloud line-width of 19 km/s, and also probes further into the boundary between gas of Galactic and extragalactic origin than typical catalogues of HVCs. Our data was taken with the Parkes radio telescope and has been stray-radiation corrected, consisting of 57 mK sensitivity, 1 km/s velocity resolution and 16' angular resolution. The GASS catalogue of HVCs improves on previous studies with its unprecedented combination of spectral and angular resolution in an all-southern-sky survey, allowing us to investigate how the dynamic and interacting population of anomalous velocity clouds in the Milky Way can offer insights into HI gas at the bridge between the disk and the halo of our Galaxy.

55 (S)

FINDING GALAXIES WITH UNUSUAL HI CONTENT Helga Denes

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia There is more and more evidence that some galaxies in groups show similar trends to galaxies in clusters, such as redder colours and gas deficiency, highlighting that gas stripping mechanisms are not only important on galaxy cluster scales but also in galaxy groups. The question is though, which mechanisms are important in low density environments? To answer this, we need to identify galaxies with recent or ongoing gas stripping in these environments. A good tool for this are optical-HI scaling relations which make it possible to find galaxies with significantly less HI than an average galaxy of the same type. I derived new, multi wavelength scaling relations by comparing the HI content of galaxies in the HI Parkes All Sky Survey (HIPASS) with optical and near infrared datasets available for southern galaxies. I will present these scaling relations and their application of identifying HI deficient galaxies in low density environments. I will also use these relations for predicting the HI content of galaxies for upcoming large scale surveys such as WALLABY, the ASKAP HI All Sky Survey.

56

THE COLD GAS IN NEARBY RADIO GALAXIES WITH HIPASS James R Allison

1 , Elaine M Sadler

1 2

1. University of Sydney, Sydney, NSW, Australia 2. ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Sydney, NSW, Australia Absorption of 21cm wavelength radiation in neutral atomic hydrogen (HI) provides the observer with a powerful tool to map the line-of-sight kinematics of neutral gas in galaxies. Observations of the 21cm transition have been used to observe highly broadened and doppler-shifted lines towards radio-loud active galactic nuclei (AGNs). The study of such absorption lines provides direct evidence of the presence of cold neutral gas in/out-flows, indicating that the interaction between the AGN with the interstellar medium is common. Using a novel technique, developed for future all-sky absorption surveys with the Square Kilometer Array pathfinders

1,

we have successfully detected cold HI gas in nearby radio galaxies in the first-generation HI Parkes All-Sky Survey (HIPASS). I will present results from this search and follow-up observations with the Australia Telescope Compact Array (ATCA). Furthermore, I will discuss our recent observations of the cold HI gas feeding compact young radio galaxies with both ATCA and the Australian Long Baseline Array

2,3.

1. Allison J. R., Sadler E. M., Whiting M. T., 2012a, PASA, 29, 221 2. Allison J. R., Curran S. J., Emonts B. H. C., Geréb K., Mahony E. K., Reeves S., Sadler E. M., Tanna A., Whiting

M. T., Zwaan M. A., 2012b, MNRAS, 423, 2601


3. Allison J. R., Curran S. J., Sadler. E. M., Reeves S. N., 2013, MNRAS, 430, 157 URL for supporting material - http://www.physics.usyd.edu.au/~jra/cv/cv.html

57

JETS AND PLANETARY NEBULAE Jan E Staff

1

1. Macquarie University, NSW, Australia Planetary nebulae marks the transition of some intermediate mass stars to a white dwarf. The outer envelopes of the star is ejected creating the planetary nebula, while the core, which can no longer sustain fusion processes, shrink and cool to a white dwarf. Approximately 80% of all planetary nebulae are not spherical, and many exhibit bipolar lobes and jets. The jets are sometimes bent, indicating that the disk launching them may be precessing. Interestingly, jets in planetary nebulae share many similarities with jets from young stellar objects. I will show simulations of jets from a precessing disk, and discuss what conditions can lead to launching the observed jets.

58 (S)

MASS-LOSS AND THE CIRCUMSTELLAR ENVIRONMENT OF S TYPE AGB STARS Taissa Danilovich

1 , Kay Justtanont

1 , Hans Olofsson

1

1. Chalmers University of Technology, Onsala, SE, Sweden At the end of their main sequence lifetimes, stars similar to our sun will ascend the asymptotic giant branch (AGB) of the H-R diagram. The AGB phase is a period of intense mass-loss as the star ejects its outer layers. The ejecta go on to form molecules and condense into dust in a circumstellar envelope. The composition of the dust and the molecular chemistry of the circumstellar envelope depend on the chemical make-up of the star, and most specifically on the carbon to oxygen ratio. We will be presenting our research on S type AGB stars, which have C/O close to 1. These stars are in a period of transition from oxygen rich to carbon rich and exhibit some characteristics of both types. We have conducted detailed radiative transfer modelling of several S stars based on observations obtained from Herschel/HIFI as part of the HIFISTARS and SUCCESS guaranteed time key projects and will present our results. By studying the mass-loss properties and circumstellar environments of AGB stars we can estimate the extent to which AGB stars contribute to the chemical enrichment of the ISM.

59

MHD MODE CONVERSION IN STELLAR ATMOSPHERES Paul Cally

1

1. Monash University, Clayton, Vic, Australia Magnetohydrodynamic waves come in three flavours: fast, slow, and Alfvén. Most astronomers know this. But these types are not set in stone. Waves can change their type as they pass through various regions. In this presentation, I review conversion between fast and slow as occurs in stellar active regions, and fast to Alfvén as occurs in stellar atmospheres. Implications are discussed.

60 (S)

DOPPLER IMAGING OF AB DORADUS Donna M Burton

1 , Brad D Carter

1 , Stephen C Marsden

1

1. University of Southern Queensland, Coonabarabran, NSW, Australia I present the results of Doppler Imaging observations of the active young K dwarf star AB Doradus from 2008 to 2013 using the ANU 2.3m telescope with its Echelle spectrograph. Doppler Imaging is a well established method for probing


stellar magnetic dynamos which generate magnetic fields and activity cycles. Dark surface spot features on rapidly-rotating stars cause "bumps" in the line profiles of such stars. Doppler Imaging then inverts a time series of these "bumps" to produce a map of the surface spot features on a star.

61

NEW OPPORTUNITIES WITH THE GEMINI OBSERVATORY Markus Kissler-Patig

1

1. Gemini Observatory, Hilo, HI, United States Observatory's new director, Markus Kissler-Patig, will present an update of the facility and introduce some new opportunities for astronomers at Gemini. Gemini operates twin 8-m telescopes, one in Hawaii and the other in Chile. The departure of the UK from Gemini's international partnership at the end of 2012 provided the chance to re-evaluate the services offered to Gemini users and opened new opportunities in two domains. First, Gemini will welcome discussions with groups wanting to bring their instruments for campaigns. This visiting instrument program will complement the suite of workhorse instruments offered by the Observatory, and will allow scientific breakthroughs not possible with the regular suite of instruments. Second, the Gemini Observatory is exploring cross-partnership large or long programs. Gemini is considering dedicating 20% of Gemini time to high-impact large or long collaborative programs selected through a yearly call. In addition to these two major initiatives, several new instruments are expected in 2013: Flamingos-2, the Gemini Multi-conjugate adaptive optics System (GeMS), and the Gemini Planet Imager (GPI). Gemini and its Users Committee are also examining the possibility of offering some fraction of time in a fast turn around mode, as well as "eavesdropping" for remote observing. We remain very interested in having astronomers visit the telescopes. We encourage all astronomers to come to this presentation to learn about these new opportunities, and to provide feedback how the Gemini Observatory can optimally support your research.

62

STELLAR YIELDS FROM LOW AND INTERMEDIATE-MASS STARS Amanda Karakas

1

1. Australian National University, Canberra, ACT, Australia The chemical yields from stars are a key ingredient in chemical evolution models. Stars with masses as low as 0.9 solar masses, which have an age less than that of our Galaxy at low metallicity, can contribute to the chemical evolution of elements. Stars less than about 10 solar masses experience recurrent mixing events that can significantly change the surface composition of the envelope, with observed enrichments in carbon, nitrogen, fluorine, and heavy elements synthesized by the slow neutron capture process (the s-process). These stars release their nucleosynthesis products through stellar outflows or winds, in contrast to massive stars that explode as core collapse supernovae. In this talk I will review stellar yields for stars up to 10 solar masses, including a brief discussion of their uncertainties and shortcomings. I will also discuss efforts by various groups to address these issues and provide homogeneous yields for low and intermediate-mass stars covering a broad range of metallicities.

63 (S)

ADOPTING THE AQUARIUS STREAM: IS THE AQUARIUS STREAM THE RESULT OF A DISRUPTED CLASSICAL GLOBULAR CLUSTER? Andrew Casey

1 , Stefan Keller

1 , Alan Alves-Brito

1 , Anna Frebel, Gary Da Costa

1 , Amanda Karakas

1 , Kevin

Schlaufman1 , Heather Jacobson, QinQin Yu, David Yong

1 , Ken Freeman

1

1. RSAA, ANU, Canberra, ACT, Australia Stellar streams occur from the tidal disruption of a stellar system as it orbits the galaxy, providing ongoing evidence for the hierarchical assembly of galaxies. Usually these streams are distant, and their parent system -- typically a globular cluster or a dwarf galaxy -- are identified before any associated stream. The Aquarius Stream was discovered serendipitously by the RAVE survey and in these respects it is quite distinct: it is relatively close (within 10 kpc) and has no associated parent stellar system. Follow-up spectroscopic data from Wylie de-Boer et al. (2012)


suggested that stars in the stream have the same metallicity, and that these stars exhibit chemical abundances that are synonymous with globular cluster stars. Thus, they propose the Aquarius Stream is the result of a disrupted globular cluster. Since the stream is close, the parent ought to be a close by -- and presumably already known -- globular cluster. However, no such parent globular cluster has yet been associated. We have performed a detailed chemical abundance analysis on five stream members with high S/N, high-resolution spectra taken using the MIKE spectrograph on the Magellan Clay telescope. While our velocities match those taken with low-resolution spectra, our data indicates the stream is not chemically coherent: we find a large range of metallicities even over this small sample. Additionally, we find no strong chemical evidence for globular cluster origin. No Na-O anti-correlation is present, and we find a positive Mg-Al abundance relationship, both inconsistent with that expected from stars enriched in a globular cluster environment. Chemically, from our data the Aquarius Stream appears indistinguishable from the Milky Way thick disk population. Despite that, the stream members do have similar velocities. We propose and show evidence for a non-accreted origin where the Aquarius Stream has resulted from a perturbation or some minor merger with the Milky Way's thick disk, demonstrating that the structure of the Milky Way is more complex than we think.

64

THE CIRCUMSTELLAR ENVIRONMENT OF THE MIRA VARIABLE TX CAM, AS REVEALED BY LONG-TERM HIGH-RESOLUTION INTERFEROMETRIC OBSERVATIONS OF SIO MASERS Ioannis Gonidakis

1 , Phil Diamond

2 , Athol Kemball

3

1. CSIRO, Epping, NSW, Australia 2. SKA Telescope, Lower Withington, Macclesfield, UK 3. University of Illinois at Urbana-Champaign, Urbana, USA We present the results from the long-term monitoring campaign of the SiO masers toward TX Cam. Observations of the target source were conducted in bi-weekly or monthly intervals for five years with the Very Long Baseline Array (VLBA), covering three complete stellar cycles. The highlight of our project is the production of a movie, showing the evolution of the masers in the extended atmosphere of the star and revealing the properties of this complex area. Peculiar kinematics of several features in our movie suggest that they can be attributed to the existence of shock waves permeating the masering region. The morphology, kinematics and variability of the SiO masers are studied in detail and compared with other observations and theoretical models.

65

THE FUNNELWEB SURVEY WITH THE UKST Michael Ireland

1 2 , Chris Tinney

3

1. Dept of Physics and Astronomy, Macquarie University, NSW, Australia 2. Australian Astronomical Observatory, North Ryde, NSW, Australia 3. School of Physics, University of New South Wales, Kensington, NSW, Australia Throughout stellar and exoplanetary astrophysics, magnitude-limited medium-resolution spectral surveys have been key for determining which stars are young, which are evolved, and to which population each star belongs. However, this basic data is available for only the ~200,000 stars in the hundred-year old HD catalog. The AAO's Starbugs technology will enable an entirely new generation of rapid, medium-resolution stellar spectroscopic survey. No other competing technology comes even close to providing the rapid redeployment required for surveys targetting millions of bright stars. The FunnelWeb survey will exploit this technology on the planned TAIPAN spectrograph, to target the 2 million stars with V=5.7-12 south of +30 degrees at medium resolution, in only 100 clear nights of observing time. The resulting survey data set would become the 21st century's HD catalogue with both an order of magnitude more stars and an order of magnitude more independent spectral information per star - identifying young stars to use as targets for direct imaging searches for exoplanets; providing an input catalogue for NASA's TESS transit search mission; linking the RAVE and GALAH Galactic archaeology surveys; providing a spectral library for all-sky asteroseismology; mapping out stellar populations and the 3D dust distribution in the nearest kpc in detail; and enabling numerous other stellar astrophysics projects. Community members interested in joining this new program are encouraged to get involved by registering for the upcoming FunnelWeb Science Workshop.


66

CULTURAL ASTRONOMY IN THE TORRES STRAIT Duane W. Hamacher

1

1. University of New South Wales, Sydney, NSW, Australia Torres Strait Islanders are a Melanesian sea-faring people whose traditional country comprises 48,000 km

2 of shallow

waters and roughly 100 islands between the tip of Queensland and Papua New Guinea. Islander laws and customs are informed by the story of Tagai – a creation deity represented in the sky as a constellation spanning across the Milky Way. The story of Tagai encompasses four themes for governing the Islander way of life. The first is that Islanders are a sea-faring people who share a common way of life. Stellar navigation is such an important component of Islander culture that a navigation star was incorporated into the Islander flag. The second theme links the stars of Tagai as custodians of knowledge for future generations. The third relates to the laws and customs that are instructed by Tagai. And the fourth theme discusses the cycle of life as a period of time and renewal based on the rising and setting of particular stars. Thus, astronomical knowledge was recruited, structured, and weaved into oral traditions and material culture that informed Islander morals and values. Despite this, many aspects of Islander astronomy are not well understood and little has been researched or written on the subject in the last 100 years. My current research on Islander astronomy is helping to fill this gap through ethnographic, archaeological, linguistic, and historical studies of Torres Strait Islander people and culture.

67

TRIGGERING AND FEEDBACK FROM ACTIVE GALACTIC NUCLEI Stas Shabala

1

1. University of Tasmania, Hobart, TAS, Australia Accretion of matter by supermassive black holes residing at the centres of galaxies is responsible for triggering Active Galactic Nuclei (AGNs), the most energetic objects in the Universe. Observational and theoretical evidence collected in recent years strongly suggests that these objects play a crucial role in galaxy formation and evolution. They do this via the process of AGN feedback, where a fraction of the AGN energy output couples to the surrounding gas. AGN feedback regulates gas cooling, and has been invoked to explain the lack of a cooling catastrophe in galaxy clusters, and the dearth of widespread star formation in massive galaxies at low redshift. AGN can also enhance star formation; this mode of feedback may be important at high redshift. I will review the evidence for AGN feedback, and discuss the different feedback modes. I will argue that understanding the processes that trigger AGN activity is crucial to quantifying feedback, and will outline how studying the complete "galaxy/environment - AGN triggering - feedback" cycle will help us understand the physics of this complex problem.

68

THE DUTY CYCLE OF GALAXY CLUSTER AGN Kevin Pimbblet

1 , Stanislav Shabala, Chris Haines, Amelia Fraser-McKelvie, David Floyd

1. Monash University, Clayton, Vic, Australia Mergers have frequently been cited as a method to fuel and feed the growth of AGN. Given that the fuel source for AGN is in the gas phase, any physical environmental mechanism that has the potential to disturb the morphology of a galaxy such as harassment may also produce an enhancement of AGN activity, not simply mergers. But there exists a strong body of literature that also holds that environment plays little to no role in the incidence of AGN. Here, we present an analysis of spectroscopically-identified optical AGN down to a cluster magnitude of M*+1 in a sample of 6 self-similar SDSS galaxy clusters at z=0.07. These clusters are specifically selected to lack significant substructure at bright limits in their central regions so that we are largely able to eliminate the local action of merging clusters on the frequency of AGN. We will detail how the AGN incidence varies with cluster position and in velocity phase-space as a function of mass, before turning to how AGN "retire" using the WHAN diagnostic to separate weak AGN from "retired galaxies", in which the main ionization mechanism comes from old stellar populations. We demonstrate that cluster AGN have no special position inside galaxy clusters: they are neither preferentially located in the infall regions, nor situated at local maxima of galaxy density which is at apparent odds with results from X-ray analysis. Our results suggest that if interactions with other galaxies are responsible for triggering AGN activity, the time-lag between trigger and AGN enhancement must be sufficiently long to obfuscate the encounter site and wipe out the local galaxy density signal.


69 (S)

NGC7130: AN INSIGHT INTO IONISING SOURCES OF COMPOSITE GALAXIES Rebecca L Davies

1 , Jeffrey A Rich

2 , Lisa J Kewley

1 3 , Michael A Dopita

1 3 4

1. RSAA, ANU, Weston, ACT, Australia 2. Carnegie Observatories, Pasadena, USA 3. University of Hawaii, Manoa, USA 4. King Abdulaziz University, Jeddah, Saudi Arabia We use the Wide-Field Spectrograph (WiFeS) on the ANU 2.3m telescope to investigate the power sources of the composite activity in the luminous infrared galaxy NGC7130. We show that NGC7130 is a spectacularly clean case of starburst + AGN activity. We observe clear and distinct rings of gas ionised by increasing fractions of AGN activity towards the nucleus. We use our data to robustly estimate the relative contribution of star-formation and AGN activity to the EUV radiation field in NGC7130, and our integral field data allows us to estimate the radius of the narrow line region. This analysis paves the way for a large investigation into the power mechanisms responsible for the composite optical class of galaxies.

70 (S)

BOK PRIZE LECTURE DANCING IN THE DARK: KERNEL PHASE INTERFEROMETRY OF ULTRACOOL DWARFS Benjamin Pope

1

1. Sydney Institute for Astronomy, Redfern, NSW, Australia The formation and evolution of extremely low-mass stars is at present poorly understood. Having masses much smaller than the typical observed and predicted collapsing mass of protostellar environments, there has been controversy as to whether field brown dwarfs form from turbulent collapse directly, or as embryos ejected from nascent multiple systems. The aim of this research is to shed light on the formation and evolution of brown dwarfs using a recently-developed interferometric image post-processing technique called kernel phase interferometry. This makes use of self-calibrating observables which are robust against small wavefront errors from turbulence or instrumental aberrations, achieving higher contrast and angular resolution than is possible with other approaches. The study of ultracool dwarf binaries is therefore also a test case for resolving much fainter planetary companions in future surveys. In this talk, I present a re-analysis of archival Hubble Space Telescope (HST) snapshot images of nearby L dwarfs using kernel-phase interferometry. This new study reveals five new detections of dwarf companions, precise astrometry on known binaries in the sample and detection constraints on possible high-contrast companions.

71

THE 2016-25 DECADAL PLAN FOR AUSTRALIAN ASTRONOMY Stuart Wyithe

1

1. University of Melbourne, Parkville, Vic, Australia The National Committee for Astronomy (NCA) carries out a formal strategic planning process on a 10-year time scale. This provides the opportunity for Australian astronomy to carry out a stock take of its capabilities, assess its impact both nationally and internationally, provide a vision for the future and to set priorities and develop strategies on how that vision might be implemented. As the currency of the last Decadal Plan for Australian Astronomy concludes in 2015, it is now time to consider the next Decadal planning process for the period 2016-25. In this talk the NCA will present a proposed outline for the formulation of the next Decadal Plan. The community will be invited to provide feedback on this process.


72 (S)

DO ALL GALAXIES' GLOBULAR CLUSTERS HAVE THE SAME STELLAR POPULATIONS? Christopher Usher

1 , The SLUGGS Survey

1. Swinburne University of Technology, Hawthorn, VIC, Australia Optical colours are typical used to infer the metallicities of extragalactic globular clusters. However the form of the colour-metallicity relation has been a matter of debate. As part of the SLUGGS survey of nearby early-type galaxies and their globular cluster systems we have used the DEIMOS multi-object spectrograph on Keck to obtain spectra of thousands of globular clusters. Previously we have used the strength of the near infrared calcium triplet to derive metallicities showing that galaxies’ globular cluster metallicity distributions are bimodal like their globular cluster colour distributions. However we see evidence that different galaxies have different globular cluster colour-metallicity relations. Different colour-metallicity relations would imply that globular clusters in different galaxies have different ages, chemical abundances or stellar mass functions. We have now stacked our spectra by colour within each galaxy to allow us to measure the strength of weaker metal lines allowing us to confirm our CaT metallicities. By empirically comparing line ratios we can identify how globular clusters differ between galaxies.

73

MULTIPLE STELLAR POPULATIONS IN INTERMEDIATE-AGE STAR CLUSTERS Sarah L Martell

1 , Sonia Duffau

2 , Antonino P Milone

3 , Graeme H Smith

4 , Michael M Briley

5 , Eva K Grebel

6

1. Australian Astronomical Observatory, Sydney, NSW, Australia 2. LSW/ZAH, University of Heidelberg, Heidelberg, Baden-Wuerttemberg, Germany 3. Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT, Australia 4. Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA 5. Physics and Astronomy , Appalachian State University, Boone, NC, USA 6. ARI/ZAH, University of Heidelberg, Heidelberg, Baden-Wuerttemberg, Germany I will describe a recent observational project aimed at understanding the formation of multiple stellar populations in star clusters. Using moderate-resolution VLT/FORS2 spectra of stars in the intermediate-age clusters NGC 1651 and NGC 1751 in the Large Magellanic Cloud, we have found that the complex age structure known from precision photometry is matched by complex light-element abundances. This result carries important new implications for the formation of star clusters in various galactic environments.

74

HOW ENVIRONMENT AFFECTS EARLY-TYPE GALAXIES - INSIGHTS FROM INTEGRAL-FIELD SPECTROSCOPY SURVEYS Nicholas Scott

1 , Roger Davies

2 , Michele Cappellari

2 , Alister W Graham

1 , Ryan Houghton

2 , Kevin Pimbblet

3

1. Swinburne University of Technology, Hawthorn, VIC, Australia 2. Subdepartment of Astrophyiscs,, University of Oxford, Oxford, United Kingdom 3. School of Physics, Monash University, Melbourne, Victoria, Australia Nature vs. nurture is one of the most hotly debated topics in galaxy evolution, with no clear consensus on what role, if any, the environment of a galaxy plays in determining its physical properties. The advent of large, 3D integral field spectroscopy surveys of galaxies in the local Universe has opened up an exciting new avenue to address this question. By determining, for the first time, spatially resolved properties of statistically significant samples of galaxies spanning the full range of environments, we can now hope to disentangle the subtle but key signatures of the environmental transformation of galaxies. The ATLAS

3D survey

1 , the first truly large-scale integral field survey of nearby galaxies, found a strong dependence of

the kinematics of the stars within an early-type galaxy on its local environment. To follow up this exciting new result, a series of smaller integral field projects have studied the early-type galaxy populations in a range of nearby environments including the Fornax, Virgo, Coma and Abell1689 clusters as well as the general field. I will present the results of each of these individual projects, then describe the overall picture they present of how early-type galaxy kinematics vary with environment and how these results help reveal the processes responsible for the environmental transformation of galaxies. Finally I will outline how Australian astronomy, through SAMI and other instruments, is perfectly positioned to lead the way in the area of large-scale 3D galaxy evolution studies. 1. Cappellari et al., 2011, MNRAS, 413, 813


75

GALAXIES THAT FLASH AS THEY CRASH Michelle E. Cluver

1 , Philip N. Appleton

2 , Patrick Ogle

2 , Thomas H. Jarrett

3 , Jesper Rasmussen

4

1. Australian Astronomical Observatory, North Ryde, NSW, Australia 2. IPAC/Caltech, Pasadena, CA, USA 3. Dept. of Astronomy, University of Cape Town, Cape Town, South Africa 4. Dark Cosmology Centre, Copenhagen, Denmark Compact Groups are dense environments where galaxies are strongly interacting and have been shown to experience accelerated evolution from late-types, with copious star-formation, to early-type disk systems. I will present recent results from a Spitzer Space Telescope mid-infrared spectroscopy study of a sample of 23 Hickson Compact Groups; here we find evidence for excess excited molecular hydrogen emission in galaxies nearing the red sequence (in mid-infrared colour and specific star formation). What mechanism is responsible for heating the H2 and is shock-excited molecular hydrogen an important clue to evolution in less dense environments?

76 (S)

UV STRONG RED SEQUENCE CLUSTER GALAXIES: THEIR ENVIRONMENT AND MORPHOLOGY Jacob P Crossett

1 , Kevin A Pimbblet

1 , John P Stott

2 , Heath Jones

1

1. Monash University, Clayton, Vic, Australia 2. School of Physics, University of Durham, Durham City, United Kingdom While it is commonly accepted that most spheroidal galaxies on the red sequence contain largely older stellar populations, it has been suggested that a small amount of recent star formation may have occurred within the last billion years. This residual star formation is observationally determined by high NUV flux, and is found to be present in over 10% of early-type galaxies down of a magnitude of R=-18 in five massive clusters from the Las Campanas/AAO Rich Cluster Survey at z~0.1. I will present results using Galex NUV-R colour magnitude diagrams to determine the broad morphological and environmental properties of these galaxies with this residual star formation to explain their formation. I will show that despite optical colours corresponding to the red sequence, these galaxies are not found to resemble early-type galaxies, but reside in low density (~100 Gal/Mpc

2) at predominantly high (>2Mpc) radii from

their host cluster centre. In addition to this, their morphology portrays a low concentration, Sersic index=1 profile. This suggests evidence of "quenching" of star formation in late type galaxies, as opposed to a residual burst of star formation.

77 (S)

WHAT SHAPES THE LOCAL UNIVERSE K-BAND GALAXY LUMINOSITY FUNCTION? Nicolas J Bonne

1 , Michael Brown

1

1. MoCA, Monash University, Clayton, VIC, Australia We have calculated morphology and colour selected K-band luminosity functions for 13,489 galaxies in the local Universe. Each galaxy has an established morphological type and redshift measurement. We select galaxies by a magnitude limit of 2MASS Ks < 10.75 and a redshift limit of 704 < cz < 20,000 km/s. We find that the bright end of our luminosity function is dominated by a population of high stellar mass, red spiral galaxies, with a total of 1,221 red spirals spread over the entire function. These red spirals are able to account for the difference in shape between luminosity functions of colour and morphology. If red spirals are formed through the truncation of star formation, these objects must be relics of a much earlier age. Alternatively, these red spirals may not be passive, continuing to form stars and grow. Regardless, where do these spirals fit into our current idea of galaxy evolution?


78

TRANSITING EXOPLANETS FROM HATSOUTH Daniel Bayliss

1

1. ANU, Weston Creek, ACT, Australia HATSouth is the world’s first network of automated and homogeneous telescopes that is capable of year-round 24-hour monitoring of positions over an entire hemisphere of the sky. The goal of the network is to discover and characterize a large number of transiting exoplanets, reaching out to long periods and down to small planetary radii. HATSouth also probes a population of lower mass stars including m-dwarfs which are not monitored in shallower exoplanet transit surveys. HATSouth monitors extended areas on the sky, deriving high precision light curves for a large number of stars, searching for the signature of planetary transits, and confirming and characterizing planetary candidates with larger telescopes. The project employs six telescope units spread over three prime locations with large longitude separation in the southern hemisphere: Las Campanas Observatory (Chile), HESS site (Namibia), and Siding Spring Observatory (Australia). Each of the HATSouth units holds four 0.18 m diameter telescope tubes on a common mount producing a 64 sq. deg. field-of-view on the sky. We will present an overview of the HATSouth network, summarize operations over the first 2.5 years, and present the current HATSouth exoplanet discoveries to date, including the characterization of these exoplanetary systems.

79

MOON RADIUS LIMITS FOR PLANETS WITH SPOTTED HOST STARS: SCATTER IN THE FOLDED LIGHT-CURVE Karen M Lewis

1 , Bun'ei Sato

1 , Shigeru Ida

1

1. Tokyo Institute of Technology, Ookayama, Japan Limits on large moons of extrasolar planets, when combined with observations of the Solar System, allow tests of models of planet and moon formation, migration and structure. Unfortunately, if the host stars of transiting planets, one of the most promising places to search for moons, are spotted, effects such as spot crossing events and long term photometric trends make moon detection challenging. Consequently we extend current moon detection methods, in particular the scatter in the folded light-curve method, to allow its use for spotted stars, by excising the planetary transit and fitting the photometric trends. We present and discuss robust exo-moon radius thresholds calculated for one planet and one planet candidate, both with highly spotted host stars, using archived Kepler transiting planet data. For the case of HAT-P 11 b we can rule out moons with radii less than 0.9 Earth radii and for KOI 1353.01 moons with 2% of the host star's radius. This work demonstrates that detection of Earth-sized, and super Earth-sized moons of transiting planets is feasible, even when the host star is highly spotted.

80 (S)

RECENTLY DISCOVERED EXOPLANETARY SYSTEM IN SPIN-ORBIT MISALIGNMENT FROM ROSSITER-MCLAUGHLIN MEASUREMENTS Brett Addison

1 , Chris Tinney

1 , Duncan Wright

1

1. University of New South Wales, UNSW Sydney, NSW, Australia Over 800 extrasolar planets have been discovered over the past two decades at an ever-increasing pace. In addition to finding new planets, a detailed analysis of their structure, composition, and other bulk properties is needed in order to understand the processes involved in their formation, evolution and migration. The Exoplanetary Science group at the University of New South Wales is utilising the new CYCLOPS2 fibre feed in conjunction with the UCLES spectrograph at the Anglo-Australian Telescope to carry out high precision Doppler spectroscopy of candidate transit planet systems. In addition, our team is carrying out measurements of the Rossiter-McLaughlin (RM) effect in transiting exoplanets. The RM anomaly for transiting planets allows the measurement of the alignment between a planet's orbital plane and its host star's spin axis, known as spin-orbit alignment. This measurement is a crucial component for studying the processes involved in planetary formation and migration. We have carried out measurements of this anomaly for a recently discovered exoplanetary system. Preliminary results indicate that this system is significantly in spin-orbit misalignment by about -90 degrees. I will discuss this exciting result and its potential implications for other planetary systems.


81 (S)

MODELLING THE ATMOSPHERIC STRUCTURE AND COMPOSITION OF HOT JUPITER HD 189733B Kimberly Bott

1 , Jeremy Bailey

1 , Lucyna Kedziora-Chudczer

1

1. University of New South Wales, Kensington, NSW, Australia Past analysis of HD 189733b's atmosphere has been a cause for some debate, with conflicting findings regarding water and sodium abundances and the presence of a high altitude haze. I will present our model of HD 189733b's cloud structure and atmospheric composition using VSTAR (Versatile Software for Transfer of Atmospheric Radiation). Since the effective temperature of the planet is expected to be approximately 5000K, newly available high-temperature spectral line lists were used. Our result will be compared to previous models and an assessment of the practicality of a model-focused approach to exoplanet spectral analysis will be made.

82

THE INTRIGUING TRANSITIONAL DISK HD142527 - PLANET FORMATION IN ACTION? Sarah Maddison

1 , Chris Wright

2 , Simon Casassus

3

1. Swinburne University, Hawthron, VIC, Australia 2. ADFA, University of New South Wales, Canberra, ACT, Australia 3. Universidad de Chile, Casilla, Santiago, Chile When giant planets form in protoplanetary disks, they are expected to dynamically clear out a gap. During this transition phase while the planet is still forming, gap-crossing gas streams are expected to continue accreting material onto the growing planet from the over-density at the outer gap edge. Large dust grains are expected to pile-up at the outer gap edge, while small grains can cross the gap with the gas. The near face-on transitional disk HD142527 offers an excellent 'laboratory' to study planet formation in action. ALMA 345 GHz continuum and ATCA 34 GHz (7-mm band) images show that the dust emission is shaped like a horseshoe in the outer disk, while ALMA CO (3-2) observations show residual gas inside the cavity and denser HCO+ gas in gap-crossing filaments. The ATCA 7mm observations show a peak in the dust flux in the horseshoe, corresponding to molecular line decrements (in both CO and HCO+), as well as diffuse 7mm emission roughly corresponding to the ALMA filaments where no counterpart is seem in the 345 GHz continuum. We discuss the implications for planet formation in this intriguing transitional disk.

83

PLANETARY NEBULAE: WINDOWS INTO THE SOUL OF STELLAR DEATH Quentin A Parker

1

1. Macquarie University/AAO, Sydney, NSW, Australia The study of Planetary Nebulae (PNe) is crucial to understand late stage stellar evolution and the chemical evolution of our entire Galaxy. The ionised shell exhibits strong emission lines that are excellent laboratories for plasma physics. PNe are visible to great distances where their strong lines permit determination of the size, expansion velocity and age of the PN, so probing the physics and timescales of stellar mass loss. We can use them to derive luminosity, temperature and mass of their central stars, and the chemical composition of the ejected gas. Their radial velocities trace a galaxy’s kinematic properties and test whether the galaxy contains a substantial amount of dark matter while their ensemble brightness distribution in coherent systems provide a powerful cosmological standard candle. Their complex shapes provide clues to their formation, evolution, mass-loss processes, and the shaping role that may be played by magnetic fields, binary central or even massive planets. As the central star fades to a WD and the nebula expands, the integrated flux, surface brightness and radius change in predictable ways. PNe are thus powerful astrophysical tools, providing a unique window into the soul of late stage stellar evolution. In this talk I will present some specific examples of the current on-going research at MQ that seeks to exploit the above science drivers with a particular emphasis on new multi-wavelength capabilities. URL for supporting material - http://physics.mq.edu.au/astronomy/


84 (S)

THE ENVIRONMENT OF Z<1 STAR FORMING GALAXIES Tim Dolley

1 , Michael Brown

1

1. MoCA, Monash University, VIC, Australia Many feedback processes can contribute to the regulation and truncation of star formation in galaxies. Knowing the environment of galaxies is important to understand which are the dominant mechanisms. Galaxy clustering tells us the host dark matter halo mass, and their distribution within these halos. We measured the clustering of a morphology selected sample of z<0.1 spiral galaxies, as a function of specific star formation rate (SSFR). We find that the typical dark matter halo mass of spiral galaxies is independent of SSFR. We detect what appears to be the signature of recent or ongoing mergers in the clustering of galaxies with enhanced SSFRs. We extend our analysis to higher redshift, by measuring the clustering of star forming galaxies from 0.2<z<1.0, usingSpitzer 24µm imaging. We show that at z<0.8 star formation is truncated in dark matter halos of M≈10

12.5Mʘ. The most luminous star forming

galaxies at z<0.8 are typically still undergoing star formation in the local universe, in groups and less dense environments. We see an increase in clustering and halo mass at 0.8<z<1.0, where we are observing star forming progenitors of elliptical galaxies, in denser environments.

85

TRACING OUTFLOWS AND ACCRETION: A BIMODAL AZIMUTHAL DEPENDENCE OF THE CIRCUMGALACTIC MEDIUM Glenn G. Kacprzak

1 , Chris W. Churchill

2 , Nikole M. Nielsen

2

1. Swinburne University of Technology, Hawthorn, VIC, Australia 2. Department of Astronomy , New Mexico State University, Las Cruces, NM, USA MgII absorption-lines detected in the spectra of background quasars allow us to probe the cool metal-enriched halo gas associated with foreground galaxies. This technique allows us to directly study the complex halo gas which provides the fuel for star-forming disks. We will discuss the series of observations that likely explain the origins of MgII absorption systems. We will present how the orientation of foreground absorbing galaxies influences the MgII absorption strengths and gas covering fractions as probed with background quasars/galaxies. We will show the bi-model distribution of galaxy positions angles, relative to the background source, demonstrating that the absorption arises along the projected galaxy minor and major axis. This suggests that the absorption arises from outflows along the minor axis and accretion along the major axis. We show how the predictions of simple outflow and inflow models are consistent with these observations.

86

A FIRST GLIMPSE INTO THE COMPLETE GALAXY POPULATION 12 BILLION YEARS AGO Lee Spitler

1

1. Australian Astronomical Observatory / Macquarie University, North Ryde, NSW, Australia Traditional optical searches for distant galaxies has yielded large samples of star-forming galaxies. Unfortunately, these searches were not sensitive to old or dusty distant galaxies and so our knowledge about galaxies in the early Universe was not complete. Using deep infrared imaging products from the ZFOURGE survey, we are now able to look at the complete distant galaxy population and study the evolutionary relationships between star-forming, old and dusty galaxies ~12 billion light years ago. I will present the first unbiased glimpse into the redshift z=3-4 galaxy population and show that large numbers of massive dusty and old galaxies existed very early in the Universe.

87

THE FIRST GALAXIES: BRIGHT AND FAINT Michele Trenti

1

1. University of Cambridge, Cambridge, UK, United Kingdom The search for the agents of reionization is elusive: While it is well established that the process is completed by redshift z~6 (and likely already at z~8-10), the observed population of galaxies at z>6 appears insufficient to even


maintain the hydrogen ionized. Thus, the leading hypothesis is that the majority of star formation during the first billion years after the Big Bang was in elusive, small mass and very faint galaxies. In this context, I will show how searches for both bright and faint galaxies are needed to quantify accurately the galaxy luminosity function and star formation at z>8. I will present results on our search for the brightest of reionizing galaxies with the Hubble BoRG survey, as well as discuss how we can use GRBs host galaxy surveys at high-z to quantify star formation in faint dwarf galaxies that are beyond the direct reach of Hubble. 1. Trenti et al. 2012, ApJL, 749, 38 2. Trenti et al. 2011, ApJL, 727, 39 3. Tacchella, Trenti & Carollo 2013, ApJL accepted, arxiv:1211.2825 4. Bradley, Trenti et al. 2012, ApJ, 760, 108

88

PROPERTIES OF SIMULATED GALAXIES AT Z~4-7 Edoardo Tescari

1

1. University of Melbourne, Parkville, VIC, Australia I will present the first results of the AustraliaN GADGET-3 early Universe Simulations (ANGUS) project. The aim of this project is to run state-of-the-art cosmological hydrodynamical simulations with an improved version of GADGET-3, to better understand the interplay between galaxies and intergalactic medium at z>2. In particular, I will discuss the results of two papers where we explored the star formation rate function, the galaxy stellar mass function and the star formation rate-stellar mass relation of z ~ 4-7 galaxies.

89 (S)

PROPERTIES OF HIGH REDSHIFT GALAXIES IN COSMOLOGICAL HYDRODYNAMICAL SIMULATIONS Antonios Katsianis

1 , Edoardo Tescari

1 , J. Stuart B. Wyithe

1

1. University of Melbourne, Melbourne, Victo, Australia We investigate the evolution of the Star Formation Rate Function (SFRF), star formation rate−stellar mass relation (SFR−M⋆) and Galaxy Stellar Mass Function (GSMF) of z ∼ 4-7 galaxies using high-resolution and large box size cosmological Smoothed Particle Hydrodynamics (SPH) simulations run with the new code P-GADGET3(XXL). We explore the effects of different feedback prescriptions (galactic winds and AGN feedback) and different initial stellar mass functions and metal cooling. We show that our fiducial model, with strong winds and efficient AGN feedback, is able to reproduce the observed SFRF at redshift z ∼ 4-7 and the observed GSMF obtained from UV selected samples at redshift 6 ≤ z ≤ 7, while at z ∼ 4 we are more consistent with recent results from IR selected samples. However, a tension between the simulated SFR−M⋆ realtion and GSMF with the ones observed exists. By combining the simulated SFR−M⋆ relation with the observed star formation rate functions, we argue that this disagreement may be the result of the uncertainty in the assumed observational Luv−M⋆ conversion and, especially, in the normalization of the observed SFR−M⋆ relation.

90 (S)

DISK-JET COUPLING IN GALACTIC BLACK HOLE X-RAY BINARIES Thomas D Russell

1

1. ICRAR, Perth, WA, Australia There is a universal connection between the accretion and ejection phenomena; a relationship that is observed in black holes of all masses. Quantifying this connection is the first step to understanding how jets are launched, accelerated and collimated. X-ray binaries (or microquasars) are ideal systems to study this relation, as they evolve on human timescales. In occasional outbursts, their luminosities increase by several orders of magnitude, with the thermal X-ray emission from the accretion disk and the radio emission from the relativistic jets undergoing dramatic changes. I present recent results from an intensive, multi-wavelength observing campaign of the microquasar MAXI J1836-194 during its 2011 outburst. Broadband radio to X-ray data taken over the course of the outburst show dramatic changes in the jet spectrum, closely linked to the evolution of the accretion disk. During the peak of the outburst we see that the inner radius of the accretion disk moves inwards to ~85 km, the disk temperature peaks and


the jet luminosity decreases. Then, as the outburst declines, the inner disk radius returns to much larger radii, the disk cools and the jet luminosity recovers to pre-outburst levels. These simultaneous, high cadence observations provide an unprecedented insight into the accretion processes occurring during an outburst, allowing us to observe an evolving compact jet and the corresponding changes within the accretion regime. This has implications for the launching of jets on all scales, from microquasars to their larger-scale analogues, AGN.

91

UNVEILING THE VARIABLE X-RAY SKY Sean Farrell

1 , Kitty Lo

1 , Tara Murphy

1 , Bryan Gaensler

1

1. The University of Sydney, Redfern, NSW, Australia Variable X-ray sources represent some of the most extreme physical phenomena in the Universe and provide probes of intense magnetic fields, strong gravitational fields, and extremely high temperatures. The types of objects that display variable X-ray emission include stars, accreting compact objects (black holes, neutron stars, and white dwarfs), and even planets. The type of X-ray variability observed can be broadly grouped into explosive (flaring), periodic, and aperiodic variability. The shape of the X-ray spectrum and the variability properties of a given source can provide information on the underlying physical mechanism of the X-ray emission and therefore the nature of the source. I will present a study of the 2,267 variable X-ray sources in the XMM-Newton 2XMMi-DR2 catalogue, highlighting some interesting results regarding the spectral and timing properties of different source populations. I will also discuss recent work investigating the use of machine learning techniques in the automatic classification of the variable X-ray sources in 2XMM. Such techniques have been found to be highly successful in identifying unknown objects. They therefore have important implications for the automatic classification of astrophysical sources detected in large sky surveys such as those to be performed by the MWA, ASKAP, SkyMapper, and eROSITA telescopes.

92

BLACK HOLE MASS IN AN ULTRALUMINOUS X-RAY SOURCE Roberto Soria

1 , Christian Motch

2 , Manfred W Pakull

2 , Fabien Grise

3 , Greg Pietrzynski

4

1. Curtin University, Bentley, WA, Australia 2. Observatoire Astronomique, University of Strasbourg, Strasbourg, France 3. Instituto de Astrofísica de Canarias, San Cristóbal de La Laguna, Spain 4. Warsaw University, Warsaw , Poland ULXs are the most luminous subclass of black hole X-ray binaries, often an order of magnitude more luminous than those known in our Galaxy. It is still hotly debated whether ULXs are powered by proportionally more massive black holes, or instead contain stellar-mass black holes accreting above their Eddington limit ("ultraluminous accretion state"). Thus, measuring black hole masses in ULXs would greatly enhance our understanding of black hole formation and of different regimes of accretion physics. Unfortunately, because of their distance, ULX optical counterparts are generally too faint to permit dynamical mass measurements. However, we have found a ULX in NGC 7793 (distance of about 3.7 Mpc) with a well-resolved B9I supergiant donor star. At V ~ 20.5 mag, it is bright enough for photometric and spectroscopic studies. We discovered a 65.2-day orbital period with a 0.5 mag amplitude in the V-band lightcurve, due to X-ray heating of the donor star. From the amplitude of the Balmer and He II 4686 radial velocity variations, and from our modelling of the optical lightcurve, we constrain the mass of the black hole to be less than about 15 solar masses. Therefore, our result suggests that the ultraluminous X-ray state is associated to supercritical accretion. Finally, we will discuss other intriguing properties of this source, still under investigation, such as an eclipsing precessing disk and a possible Doppler-shifted line from a relativistic jet.


93

PRECISION EPHEMERIDES FOR GRAVITATIONAL-WAVE SEARCHES: SCO X-1 & CYG X-2 Sammanani S Premachandra

1, Duncan K Galloway

1 2 , Danny Steeghs

3 , Tom Marsh

3 , Jorge Casares

4 , Remon

Cornelisse4

1. School of Physics, Monash University, Clayton, Vic 3800, Australia 2. School of Mathematical Sciences, Monash University, Clayton, Vic 3800, Australia 3. University of Warwick, Coventry, United Kingdom 4. Instituto de Astrofisica, La Laguna, Tenerife Accreting neutron stars in low-mass X-ray binaries (LMXBs) are candidate persistent gravitational wave (GW) sources, which may be detectable with next generation interferometers such as Advanced LIGO/VIRGO within this decade. However, the kind of searches possible will likely be limited principally by the uncertainty in the binary system parameters. I will present the revised binary system parameters for Sco X-1 and Cyg X-2 based on the 13-year and 45-year baseline, respectively. I will also present the estimates of the likely precision of the parameters that can be achieved throughout Advanced LIGO/VIRGO period and quantify the improvement in search sensitivity via the number of templates (models).

94 (S)

EVIDENCE FOR ACCRETION RATE CHANGE DURING TYPE I X-RAY BURSTS Hauke Worpel

1 , Duncan K. Galloway

1 , Daniel J. Price

1

1. MoCA, Clayton, VIC, Australia The standard approach for time-resolved X-ray spectral analysis of thermonuclear bursts involves subtraction of the pre-burst emission as background. This approach implicitly assumes that the persistent flux remains constant throughout the burst. We reanalyzed 332 photospheric radius expansion bursts observed from 40 sources by the Rossi X-ray Timing Explorer, introducing a multiplicative factor fa to the persistent emission contribution in our spectral fits. We found that for the majority of spectra the best-fit value of fa is significantly greater than 1, suggesting that the persistent emission typically increases during a burst. Elevated fa values were not found solely during the radius expansion interval of the burst, but were also measured in the cooling tail. The modified model results in a lower average value of the χ

2 fit statistic, indicating superior spectral fits, but not yet to the level of formal statistical

consistency for all the spectra. We interpret the elevated fa values as an increase of the mass accretion rate onto the neutron star during the burst, likely arising from the effects of Poynting-Robertson drag on the disk material. We measured an inverse correlation of fa with the persistent flux, consistent with theoretical models of the disc response. We suggest that this modified approach may provide more accurate burst spectral parameters, as well as offering a probe of the accretion disk structure.

95 (S)

UNVEILING UNIDENTIFIED TEV GAMMA-RAY SOURCES AT 12MM WITH MOPRA Phoebe de Wilt

1 , Gavin Rowell

1

1. University of Adelaide, Adelaide, SA, Australia Data from the H2O Galactic Plane Survey (HOPS) and additional Mopra mm observations have been used to search for dense gas toward unidentified Galactic TeV gamma-ray sources seen by the High Energy Spectroscopic System (H.E.S.S.). Previous searches for counterparts have concentrated on large scale molecular and atomic gas, aiming to determine if they arise from acceleration cosmic-rays and/or electrons. However the morphology and dynamics of dense gas can provide additional insight into the conditions of the ISM towards the gamma-ray emission. In this work, dense and disrupted molecular gas traced at 12 mm wavelengths has been used to provide further insight to the origin of several bright unidentified TeV sources.


96

DO WE HAVE ROBUST ASTROPHYSICAL TESTS OF DARK MATTER? Chris Power

1

1. University of Western Australia, Crawley, WA, Australia The Lambda Cold Dark Matter model is well established as the framework within which we study the origin and growth of structure in the Universe from the earliest cosmic epoch to the present day. Yet a recurring theme for the LCDM model over the last two decades has been that it faces a crisis on small-scales, predicting an overabundance of low-mass galaxies whereas comparatively few are observed. Can this tension be explained by appealing to known astrophysical processes, or does it signal the need for a fundamental overhaul of the dark matter model itself? I will review the current state of affairs, highlighting where our theoretical understanding needs to be improved, and I will discuss the kind of observations that might help us test dark matter models in the most robust fashion.

97

A FORMATION HISTORY MODEL OF GALAXY GROWTH Simon J Mutch

1

1. The University of Melbourne, Melbourne, VIC, Australia I will introduce a new, simple model that self-consistently connects the growth of galaxies to the formation history of their host dark matter halos. Using just two simple, phenomenologically motivated equations that depend only on dark matter halo properties, our "formation history" model is capable of reproducing the observed z=0 red and blue stellar mass functions. By adding redshift as a second input variable to the model I will further show that an improved reproduction of the stellar mass function out to z=3 can be achieved. Finally, I will discuss the general utility of this new model for exploring a broad range of topics associated with galaxy formation and evolution, and for creating mock galaxy samples which have a number of advantages over those generated by other techniques. URL for supporting material - http://arxiv.org/abs/1304.2774

98

STAR FORMATION IN RED SPIRAL GALAXIES Michael Brown

1

1. Monash University, Clayton, VIC, Australia It is often assumed that red galaxies have effectively stopped forming stars and grow mostly via merging with other galaxies. However, the presence of massive red spiral galaxies in the nearby Universe (e.g., Bonne et al., in prep.) suggests this picture may be flawed. These galaxies cannot be produced by simply truncating star-formation in present-day blue spiral galaxies. We have used SDSS, 2MASS, WISE and NVSS to identify nearby galaxies with very low star formation rates and determine the environments in which these galaxies reside. Using archival 21-cm data, we have determined if these galaxies could rekindle their star formation or if star formation has been permanently truncated.

99

CHARLENE HEISLER PRIZE FROM 13 TO 600+: THE FUTURE OF HIGH-Z IFU SURVEYS Emily Wisnioski

1

1. MPE, Garching, BY, Germany My thesis presents the kinematics of 13 star-forming galaxies at z>1 selected from the WiggleZ Survey for having extreme star-formation, forming the largest AO sample to date at this redshift. Over the past 8 years ~300 galaxies have been observed at z>1 with IFUs using ~300hrs of 8-10m telescope time. These observations have lead to key findings, many of which are reflected in the WiggleZ IFU sample, such as: high velocity dispersions, large fractions of disk galaxies, asymmetries between kinematic and photometric axes, and massive star-forming regions capable of hosting galactic scale winds. However, questions the surveys were designed to answer remain open as the currently


studied ~300 galaxies are an amalgamation of many heterogeneous targeted samples across a wide redshift range (z=1-4) analysed with a variety of techniques. Taking advantage of the previous targeted surveys and the new multiplexed KMOS instrument, the upcoming KMOS-3D survey will tackle key questions by tracing the evolution of velocity dispersions, kpc-scale star formation, and outflows over 5 Gyrs between 0.7<z<2.5 using ~600 mass-selected galaxies from the 3D-HST survey.

100

DISCOVERY OF A POPULATION OF MILLISECOND DURATION RADIO BURSTS Matthew Bailes

1 , HITRUN TEAM

1. SWINBURNE UNIVERSITY OF TECHNOLOGY, Balwyn North, Vic, Australia The High Time Resolution Universe Survey for Pulsars and Fast Transients team has commenced processing its high-latitude data and discovered four millisecond-duration radio transients at extremely high dispersion. The transients comply with extraordinary accuracy to the cold plasma dispersion and scattering relations expected from genuine celestial sources. If the dispersion is from the intergalactic medium, we infer cosmological distances of up to z=1 for the sources. Our derived event rate suggests that over 1000 times a day the sky is lit up by short bursts of ~1 Jy radio emission from the distant Universe that are unique cosmological probes. In this talk I will discuss the bursts, some potential sources, their potential for cosmology and a radical and inexpensive GPU correlator for the Molonglo telescope that should find over 100 sources per year by exploiting its high gain and very large field of view.

101

HOW THE JAMES WEBB SPACE TELESCOPE CAN MEASURE FIRST LIGHT, REIONIZATION, AND GALAXY ASSEMBLY: SCIENCE AND PROJECT UPDATE AS OF 2013 Rogier A. Windhorst

1

1. Arizona State University, Tempe,, AZ, United States We review how the 6.5 meter James Webb Space Telescope (JWST) --- after its launch planned for 2018 --- can measure the epochs of First Light, Reionization, and Galaxy Assembly, building on recent results from the Hubble Wide Field Camera 3. Significant technical progress has been made on the design and fabrication of JWST: more than 80% of its launch mass has been built, passed final design, or is being built as of Spring 2013. All JWST's 18 flight mirrors have been gold-coated with an optical performance that meets or exceed specs. Two of JWST's scientific instruments were delivered to NASA GSFC in 2012, with the last two to follow in 2013. We show what combination of area, depth, and wavelength coverage are needed for JWST to detect a sufficient number of First Light objects, and to measure their evolving luminosity function (LF). JWST will map the epoch of First Light through Pop III-star dominated objects at redshifts z=8--20, and its transition to the first Pop II stars in dwarf galaxies at z<9. JWST will measure the evolution of the steep faint-end of the dwarf galaxy LF at z=6--15, which likely provided the UV-flux needed to start and finish cosmic Reionization. I will also discuss: 1) simulations of deep JWST images, using lower redshift restframe UV--optical HST images as templates; (2) if ultradeep JWST images will run into the instrumental or natural confusion limits; (3) to what extent gravitational lensing bias from foreground object halos may affect the search for First Light objects at redshifts z>8--10. A new generation of algorithms may be needed to automatically detect, measure and classify objects in very crowded, ultradeep JWST fields; and (4) the optimum mix of random deep JWST fields, and lensing fields centered on foreground clusters or groups. URL for supporting material – http://www.jwst.nasa.gov/ http://www.asu.edu/clas/hst/www/jwst/


102

OPTICAL SPECTROSCOPY FROM TAIPAN TO THE GMT'S MANIFEST Kyler Kuehn

1

1. AAO, North Ryde, NSW, Australia TAIPAN is an optical spectroscopic survey that will observe of order 2 million stars and 500,000 galaxies over a significant fraction of the Southern hemisphere. The TAIPAN instrument is currently under construction, and is designed to make use of the novel Starbugs fibre positioner system. With 150 fully-parallelized and independently-steerable Starbug-driven fibres, TAIPAN will also serve as a prototype and testbed for the technologies necessary for the larger MANIFEST fibre positioner system, which will in turn play a crucial role in realising the scientific capabilities of the planned Giant Magellan Telescope. We describe the TAIPAN instrument requirements, design specifications, and current status, as well as the five-year astronomical survey program that it will undertake starting in 2015. We also describe the path from the present design of TAIPAN to the future realisation of the significantly more complex MANIFEST facility.

103

THE ASKAP/EMU DATA CHALLENGE Andrew Hopkins

1

1. Australian Astronomical Observatory, North Ryde, NSW, Australia At the second annual SPARCS workshop held in Sydney on 30 May - 1 June 2012, many tests of radio continuum source finding tools and techniques were presented and discussed. A consensus was reached that a blind source finding challenge would be a valuable addition to our current approaches for understanding the strengths and limitations of the many source-finding tools presently available. The goal of the current Data Challenge is to assess the (1) completeness, (2) reliability, (3) accuracy, and (4) common failure modes, for a variety of source-finding tools. The Data Challenge ran from 30 November 2012 to 15 January 2013, with 8 teams registering to test 11 source finder tools on a set of three simulated ASKAP continuum images. Here I present the outcomes of the Data Challenge, highlighting strengths and weakness of the particular tools tested, and identifying the next steps forward.

104

CFHT STATUS REPORT AND FUTURE PLANS Doug Simons

1

1. CFHT, Kamuela, HI, United States After a brief summary of recent metrics illustrating the scientific success of CFHT, the future of the Observatory is described through various initiatives designed to broaden the CFHT partnership, develop new capabilities, and take steps toward the replacement of CFHT with a powerful new facility (ngCFHT) dedicated to highly multiplexed wide-field spectroscopy. CFHT, in the context of the evolving landscape on Mauna Kea will also be discussed, as CFHT positions itself among a backdrop of some older facilities possibly being decommissioned while new Mauna Kea facilities are on the planning horizon.


POSTER ABSTRACTS

201

SEARCHING FOR INTERMEDIATE MASS BLACK HOLES IN EARLY TYPE GALAXIES FEATURING PROMINENT DUST LANES Eromanga Adermann

1 , Sean Farrell

1 , Anne Green

1

1. Sydney Institute for Astronomy, Redfern, NSW, Australia Current theories suggest that intermediate mass black holes (~100 - 100,000 solar masses) played an important role in the formation of supermassive black holes. The study of intermediate mass black holes may therefore shed light on how supermassive black holes formed and evolved. One of the most promising methods for identifying intermediate mass black holes is through observations of the X-ray emission produced by accretion processes, though X-ray luminosities apparently above the Eddington limit for a low mass black hole can theoretically be produced by high mass X-ray binaries containing stellar mass black holes, accreting at very high rates and possibly emitting anisotropically. Though convincing observational evidence for the existence of intermediate mass black holes has thus far been sparse, the ultraluminous X-ray source HLX-1, located in the dusty early type galaxy ESO 243-49, is a very strong candidate, with an X-ray luminosity far in excess of the Eddington limit for a stellar mass black hole. Recent studies have indicated that HLX-1 is the remnant of a dwarf galaxy that was accreted < 200 Myr ago by ESO 243-49, suggesting that intermediate mass black holes may be the result of galaxy interaction. We sought to explore this idea further by searching for non-nuclear X-ray sources with luminosities above the stellar mass black hole Eddington limit in early type galaxies with prominent dust lanes (such as those present in ESO 243-49), which are believed to be traces of recent minor mergers. The low star formation rates in these galaxies mean that any such sources are unlikely to be extreme high mass X-ray binaries containing stellar mass black holes, and would thus constitute excellent intermediate mass black hole candidates. Here we present the results of our search for active intermediate mass black hole candidates in early type galaxies with prominent dust lanes, performed using archival XMM-Newton and Chandra X-ray data in a sample of galaxies taken from GalaxyZoo.

202

CLUSTERING OF DENSE MOLECULAR GAS IN THE MILKY WAY GALAXY Shaila Akhter

1

1. UNSW School of Physics, SYDNEY, NSW, Australia Giant molecular clouds are the hosts for massive star formation, which occurs within dense condensation within the more diffuse gas. The HOPS Mopra telescope survey of the southern Galactic plane identified many regions of dense gas using transitions of the molecule ammonia. We are now examining these regions in greater depth, and here we describe how we are decomposing the areas of ammonia emission into 3-dimensional clumps. While 3-D clump finding is now routinely undertaken, the hyperfine structure of ammonia presents extra difficulties, and we discuss ways of getting around this problem. This study is a first step in understanding the clumping and multiplicity of dense (possibly) protostellar clumps throughout differing regions of the Milky Way Galaxy.

203

INTERACTION OF HYDRA A JETS WITH THE INTRACLUSTER MEDIUM Mohammad Ali Nawaz

1 , Geoff Bicknell

1 , Alex Wagner

2

1. Research School of Astronomy and Astrophysics, ANU, Canberra, ACT, Australia 2. Center for Computational Sciences, University of Tsukuba, Ibaraki, Japan We have performed 2D axisymmetric and 3D, relativistic hydrodynamic simulations of the interaction of the Hydra A jets with the cluster environment. The motivation for this study is to model the radio and X-ray structures of the radio galaxy Hydra A and to understand in detail the interaction of radio sources with cooling flows. Our basic interpretation of the radio morphology is the following: A disruptive Mach disk at ~6 kpc is responsible for the bright knot between 6-10 kpc in the northern jet. The abrupt transition of the jet to a plume like structure in the northern side is a result of the Mach disk. The gradual transition to turbulence in the southern side is mediated by less disruptive conical shocks. We suggest that the northern jet is highly over-pressured with respect to the environment, because this is a prerequisite for the formation of a Mach disk. Accordingly, the southern jet is less over-pressured. The precession of the jets produces the curved structure and the rotational symmetry of the radio source.


Using minimum energy estimates and the theory of expanding bubbles we have estimated the kinetic power of the jets to be 6×10

44 erg s

-1. We have successfully reproduced the inner 50 kpc structures of the Hydra A radio source with

our numerical simulations, including the bright knot in the northern jet, the turbulent transition of the jets to plume-like structures, and the curved morphology of the jets. From a parameter space study of the jet power and the jet velocity we obtain a relationship between the position of the Mach disk and the jet velocity. We estimate a jet velocity of ~0.1c from this relationship, which is approximately consistent with other estimates based on Doppler boosting.

204

USING SCALING RELATIONS TO EXAMINE THE EFFECTS OF ENVIRONMENT ON HIGH REDSHIFT GALAXY EVOLUTION Rebecca Allen

1 , Glenn Kacprzak

1 , Karl Glazebrook

1 , Lee Spitler

2

1. Swinburne University, Hawthorn, Vic, Australia 2. Macquarie University, North Ryde, NSW, Australia The galaxy size-mass relation is a key tool used to confirm galaxy formation and evolution scenarios and can be further implemented to address the role of environment. Disagreement exists regarding the extent to which environment affects galaxy evolution at redshifts above z~1. Using the Z-FOURGE medium-band survey we selected a sample of ~40 cluster and ~300 field galaxies having photometric redshifts between 2<z<2.2. We then stacked the publicly available HST galaxy images in order to accurately measure the typical light profiles of cluster and field galaxies. We directly compared the radial surface brightness profiles, sizes, and Sérsic indices of the field and cluster galaxies in different environments. We find that high mass (10

10<(M/Mʘ)<10

11) cluster galaxies are larger and less compact than their field

counterparts while low mass galaxies (109<(M/Mʘ)<10

10) in both environments appear to be similar. This implies that

higher mass cluster galaxies are evolving at an accelerated rate compared to galaxies in the field and that minor mergers could be the driver of this rapid growth.

205

NEW MEASUREMENTS OF THE EVOLVING GROWTH RATES OF GALAXIES Richard Beare

1 , Michael Brown

1 , Kevin Pimbblet

1

1. Monash Centre for Astrophysics, Clayton, Victoria, Australia Using a sample of ~400,000 galaxies in the Bootes field (~10 times larger than previous studies), we have accurately measured the evolving B-band luminosity function of red and blue galaxies at z<1.2. We find that the comoving space density of red galaxies approximately doubles from z~1.1 to z~0.1, while that of blue galaxies remains relatively unchanged. By contrast the luminosity density of red galaxies changes little over the same redshift range, while that of blue galaxies approximately halves. By comparing our measurements of the luminosity density evolution of red galaxies with those to be expected from passive evolution alone, we deduce that red galaxies have increased in stellar mass by a factor of ~4 from z~1.1 to z~0.1, and we attribute this to the combined effect of mergers and blue galaxies crossing the green valley as they cease to form stars. We also measure how the rate of growth of massive galaxies evolves with redshift, and find rapid growth at z~1 and far less growth at z~0.4. For massive red galaxies, we compare our observations with those to be expected from passive evolution alone, and deduce that massive red galaxies double in mass from z~1.1 to z~0.5 and then change little in mass from z~0.5 to z~0.1. As there are insufficient massive blue galaxies at z>0.5 that could cease star formation and become massive red galaxies, we infer that the observed growth in massive red galaxies from z~1.1 to z~0.5 is due almost entirely to mergers.

206

INVESTIGATING KINEMATIC MODELLING OF DISK GALAXIES USING GPUS Georgios Bekiaris

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia Galaxy Kinematics allow us to gain a better understanding of the formation and evolution of disk galaxies. By utilizing Integral Field Spectroscopy (IFS) we can obtain spatially resolved spectra and investigate galaxy kinematics in great


detail. Large IFS surveys of thousands of galaxies are being planned for the coming years and will produce a tremendous amount of data. The currently available computer software for IFS data processing and galaxy kinematic modelling does not take full advantage of the computational strength of the modern hardware, thus making the procedure very time consuming. Our aim is to accelerate kinematic modelling of disk galaxies by exploiting the power of the highly parallel processors available on the Graphics Processing Units (GPUs) and other general purpose computing devices. We explore both grid-based and Markov Chain Monte Carlo (MCMC) methods for parameter estimation and we evaluate the results. For the development of the software the gSTAR supercomputing facility is used.

207

TESTING A VELOCITY DISPERSION MODEL OF THE MILKY WAY HALO'S STARS Sarah Bird

1 , Chris Flynn

2 , William E Harris

3 , Mauri Valtonen

1

1. Tuorla Observatory, University of Turku, Turku, ., Finland 2. Swinburne University of Technology, Melbourne, Victoria, Australia 3. McMaster University, Hamilton, Ontario, Canada We use simulations to test the stability of a model of the velocity dispersion of the Milky Way stellar halo, with applications to the Gaia mission.

208

MĀORI ASTRONOMICAL TRADITIONS OF METEORS Tui Britton

1

1. Macquarie University, Sydney, NSW, Australia We examine Māori astronomical traditions for representations of meteors. We find that religion, story, and ceremony highlight the broad perception of meteors found throughout the Māori culture. Meteors were often personified as gods but were also seen as omens of death and destruction. This research contributes to the Meteor Beliefs Project and is featured in WGN – Journal of the International Meteor Organization

209

GALAXY SPECTRAL ENERGY DISTRIBUTIONS FROM THE ULTRAVIOLET TO THE MID-INFRARED Michael Brown

1

1. Monash University, Clayton, VIC, Australia We present an atlas of 120 spectral energy distributions for nearby galaxies, with wavelength coverage spanning from the UV to the mid-infrared. We combined ground-based optical spectrophotometry with infrared spectroscopy from Spitzer and Akari, with gaps in spectral coverage being filled using MAGPHYS models. The spectroscopy and models were normalised, constrained and verified using matched aperture photometry measured using imagery from Swift, GALEX, SDSS, 2MASS, Spitzer and WISE. The availability of 27 photometric bands allowed us to identify and mitigate systematic errors present in the data, including an error in the WISE W4 filter curve. Comparison of our spectral energy distributions with other template libraries and the observed colors of galaxies indicates that we have smaller systematic errors than existing atlases while spanning a broader range of galaxy types.


210

IS THE INITIAL MASS FUNCTION UNIVERSAL? THE CASE OF NGC 2915 Sarah Bruzzese

1

1. International Centre for Radio Astronomy Research, Perth, WA, Australia The initial mass function (IMF) is very important to many aspects of astrophysics; it allows us to determine galactic properties such as the stellar mass of a galaxy, and is crucial in understanding star formation histories and galaxy evolution. Theoretically we expect the IMF to change with star forming conditions

1. However, observations of stars in

the Milky Way and Magellenic clouds show no significant variation2. This has led to heated debate over whether the

IMF is universal or not. We are addressing this question by determining the form of the IMF in nearby galaxies. With the capabilities of the Hubble Space Telescope we can detect individual massive stars (M ≥ 2.5 Mʘ), allowing us to constrain the form of the upper-end IMF by statistically comparing simulated and observed colour-magnitude diagrams. We constrain the upper-mass limit, and the power-law slope for a variety of plausible star formation histories. We present results for the first object in our study, the outer-disk of NGC 2915, a blue compact dwarf galaxy at a distance of 4 Mpc. NGC 2915 is of interest due to its high mass-to-light ratio and low stellar density in its gas-rich outer-disk

4.

1. Bate & Bonnell 2005, MNRAS 2. Kroupa 2001, MNRAS 3. Bastian et al. 2010, ARA&A 4. Meurer et al. 1996, AJ

211

MORPHOLOGICAL TRANSFORMATION OF RED SEQUENCE GALAXIES IN HIGH REDSHIFT GALAXY CLUSTERS Pierluigi Cerulo

1 , Warrick J Couch

2 , Chris Lidman

2

1. Swinburne University of Technology, Hawthorn, VIC, Australia 2. Australian Astronomical Observatory, North Ryde, NSW, Australia I present the results of a detailed analysis of the morphological properties of red sequence galaxies in a X-ray detected cluster at redshift z=0.98. Overall, the red sequence is dominated by elliptical and S0 galaxies. The fraction of S0s decreases at faint luminosities, where disc-dominated systems tend to become more frequent. From the comparison with a sample of local galaxy clusters, I discuss possible scenarios for the evolution of galaxies of different morphologies. I finally show the ongoing application of the analysis developed for this cluster to a sample of galaxy clusters at 0.8 < z < 1.5 and its implications for the investigation of the environmental drivers of galaxy evolution.

212

THE AUSTRALIA TELESCOPE LARGE AREA SURVEY: THE COMPOSITE PROPERTIES OF YOUNG AGN Kate E Chow

1

1. CSIRO, Epping, NSW, Australia The Australia Telescope Large Area Survey (ATLAS) is the widest deep radio survey attempted so far, covering ≈7 deg

2 across its two fields, the Chandra Deep Field South (CDFS) and the European Large Area ISO Survey South 1

Region (ELAIS-S1). ATLAS has extensive multiwavelength data, including optical, infrared and X-ray, to complement its ≈15µJy rms 1.4 GHz radio data. At these faint radio flux densities, star-forming galaxies begin to dominate the source population, and there is evidence for a composite population of sources with ongoing star formation that also contain an AGN. Understanding these faint radio source populations is essential for understanding galaxy evolution and what role is played by the AGN. I present preliminary results investigating the faint population of Compact Steep Spectrum sources in ATLAS, thought to be one of the earliest stages of the AGN life-cycle and possibly composite AGN/star-forming objects. Exploring this population will aid us in understanding the evolution of AGN as a whole and help to shed light on what triggers AGN.


213

WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF INFRARED FAINT RADIO SOURCES Jordan D Collier

1 2 , Julie K Banfield

2 3 , Ray P Norris

2 , Dominic H F M Schnitzeler

2 4 , Amy Kimball

5 6 , Miroslav

Filipovic1 , Thomas H Jarrett

7 , Carol J Lonsdale

8

1. University of Western Sydney, Kingswood, NSW, Australia 2. CSIRO Astronomy and Space Science, Marsfield, NSW, Australia 3. Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT, Australia 4. Max-Planck-Institut fur Radioastronomie, Universitat Bonn, Bonn, Germany 5. Dept. of Astronomy, University of Washington, Seattle, WA, USA 6. National Radio Astronomy Observatory, Charlottesville, VA, USA 7. Infrared Processing and Analysis Center, Pasadena, CA, USA 8. North American ALMA Science Center, National Radio Astronomy Observatory, Charlottesville, VA, USA We present a population of 1317 Infrared Faint Radio Sources (IFRSs) that are reliably detected in the infrared, generated by cross-correlating the Wide-Field Infrared Survey Explorer (WISE) all-sky survey with major radio surveys. We present the first spectroscopic redshifts of IFRSs, as well as the first X-ray counterparts of IFRSs, one of which is the only match from the ROSAT All-Sky Survey. We propose that they represent a population of radio-loud Active Galactic Nuclei (AGN) at z > 2. Evidence for this comes primarily from (1) spectroscopic redshifts for 18 sources, (2) a comparison between the WISE infrared colours, and (3) the radio morphology. 18 spectroscopic redshifts reveal their matching sources to be primarily broadline QSOs at 2 < z < 3. The WISE colours of the sources we present inhabit the same space occupied by obscured AGN, QSOs and Seyferts. The majority of sources are unresolved, but 213 sources contain morphologies of large-scale radio galaxies, showing that a significant portion of this sample consists of radio-loud AGN. We suggest that these are closer versions of the extreme IFRSs believed to be large redshifts (z > 3). 1. Wright E. L., WISE Team 2009, in American Astronomical Society Meeting Abstracts #214 Vol. 214 of

American Astronomical Society Meeting Abstracts, WISE - the Wide-field Infrared Survey Explorer. p. 217.01

214

MASS ASSEMBLY HISTORY OF MAIN SEQUENCE GALAXY HALOS Camila Correa

1 , Alan Duffy

1 , Stuart Wyithe

1

1. University of Melbourne, Parkville, VIC, Australia We use cosmological hydrodynamical simulations from OWLS project to build halo merger trees and study the mass assembly history of main sequence galaxy halos. We propose a simple 1-parameter formula for the mass assembly history (MAH) of halos as a function of redshift. We find that it simultaneously presents a close fit to the mean total mass trajectories of halos and its time derivative provides an accurate estimate of the total accretion rate. We make detailed comparisons of analytically derived accretion rates, as well as MAHs derived from other N-body simulations, and find excellent agreement (with one exception of an often used scheme). We show that by using the present day halo mass (M0) as a unique parameter in our model, we can easily determine the halo mass and accretion rate at earlier epochs.

215

LITHIUM ABUNDANCES IN THE GLOBULAR CLUSTER NGC 6218 (M12) Valentina D'Orazi

1 , George Angelou

2 , Angela Bragaglia

3 , Eugenio Carretta

3 , Raffaele Gratton

4 , Sara Lucatello

4

1. Macquarie University, North Ryde, NSW, Australia 2. Monash University, Clayton, VIC 3800, Australia 3. INAF - Bologna, Bologna, Italy 4. INAF - Padova, Padova, Italy The historic notion of globular clusters as simple stellar populations is now proven to be too simplistic . In the last years a large number of observational studies have revealed the presence of large internal variations in their light-element content (e.g., C, O, N, Na, Mg, and Al). This extremely peculiar chemical pattern, which is not observed in open clusters and field stars, points to inter-cluster pollution processes and to the existence of multiple stellar generations. Although the first level of the game is clear, several fundamental issues are still open, related to e.g. the nature of the light-element distributions and to their relationship with the cluster structural parameters (such as mass, horizontal branch morphology). We present in this contribution lithium abundances for a large sample of giant stars in the globular clutter NGC 6218: thanks to its fragile nature (Li starts burning at only T~2.5 MK), lithium represents a


very powerful diagnostic in this context and can provide strong observational constraints to the multiple population scenario in globular clusters. The comparison with models and the implications for cluster formation and internal pollution mechanisms is also discussed.

216

EVOLUTION OF PLANETARY NEBULAE WITH HYDROGEN-DEFICIENT CENTRAL STARS Ashkbiz Danehkar

1 , Quentin Parker

1 2

1. Macquarie University, Sydney, NSW, Australia 2. Australian Astronomical Observatory, Epping, NSW, Australia Although most central stars of planetary nebulae show hydrogen-rich surface abundances, a small fraction (5-20%) display an expanding hydrogen-deficient stellar atmosphere, which cannot be explained by radiation pressure. This is the so-called wind momentum problem. It is currently far from clear what are the physical mechanisms and evolutionary paths which expel the outer hydrogen layer from these carbon-oxygen degenerate pre-white dwarfs, and transforms it into a fast stellar wind. We present WiFeS/IFU observations of a carefully selected sample of planetary nebulae having hydrogen-deficient central stars. Our new results will shed light on the formation of these stars via better elucidation of their characteristics in combination with photoionization models of planetary nebulae.

217

ESTIMATING THE FRACTION OF BINARY CENTRAL STARS OF PLANETARY NEBULAE USING THE IR-EXCESS METHOD Dimitri Douchin

1 , orsola DeMarco

2

1. Macquarie University / Universite Montpellier 2, Sydney, NSW, Australia 2. MQAAASTRO Centre, Macquarie University, Sydney, NSW, Australia There is no quantitative theory to explain why a high 80% of all planetary nebulae are non-spherical. The Binary Hypothesis states that a companion to the progenitor of a central star of planetary nebula is required to shape the nebula and even for a planetary nebula to be formed at all. A way to test this hypothesis is to estimate the binary fraction of central stars of planetary nebulae and to compare it with that of the main sequence population. Preliminary results from photometric variability and the infrared excess techniques indicate that the binary fraction of central stars of planetary nebulae is higher than that of the main sequence, implying that PNe could preferentially form via a binary channel. I will show new photometric results resulting from the analysis of an extended sample, yielding an up-to-date binary fraction of central stars of planetary nebulae.

218

NGC2110 – YOUNG STAR CLUSTERS IN THE CIRCUMNUCLEAR TORUS Mark Durre

1 , Jeremy Mould

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia We have observed the nucleus of NGC2110 (a Seyfert S0 galaxy with a radio jet) with the Keck OSIRIS instrument (using AO) across the infrared in the J, H and Z bands, with a resolution of 5 pc per pixel. The circumnuclear torus is resolved into a number of luminous star clusters, which are each comparable to the mass and luminosity of the Arches Cluster at the centre of the Milky Way. The cluster age, star forming rates and interstellar reddening are estimated. An upper limit to the kinematically determined mass of a central supermassive black hole is calculated.


219

A STABLE WAVELENGTH COMB FOR PRECISE RADIAL VELOCITY MEASUREMENTS Tobias Feger

1 , Joao Bento

1 , Mike Ireland

1

1. Macquarie University, North Ryde, NSW, Australia We present a novel, stable and inexpensive wavelength scale reference based on a photonic cavity with the potential of mass replication for current and future (arrays of) radial velocity spectrographs. The primary purpose of using a photonic cavity is to obtain a dense sinusoidal wavelength comb with spectral coverage between 450-650nm. Its basic setup is an unbalanced all-fibre white light Mach-Zehnder interferometer assembled out of two off-the-shelf available fibre couplers. To reach a good long-term stability the interferometer is actively locked by monitoring phase deviations of an extremely stable atomic line. The full system operates in closed loop, i.e. any phase shift measured by a photo receiver will be actively corrected using a phase feedback component (e.g. fibre heater). The setup, its characterization and results from long-term stability tests are being presented with this poster.

220

A REVIEW OF HIGH SCHOOL ASTRONOMY STUDENT RESEARCH PROJECTS OVER THE LAST TWO DECADES Michael T Fitzgerald

1

1. Macquarie University, Chatswood, NSW, Australia The technological capacity for relevant and authentic high school-based student astronomical research using research grade telescopes and data has exploded over the last twenty years. From the early 1990s when the earliest remote controllable small (12-24") optical telescopes staggered onto pre-internet bulletin boards up until the present day where sophisticated large aperture (1m-2m+) optical, as well as a variety of radio, telescopes are able to be accessed remotely and robotically via broadband, many projects have attempted to leverage these technologies to undertake student-led research within the classroom. While the technologies themselves have been largely engineering successes, effective educational use of these technologies in a high school classroom context currently lags behind, although not without their notable successes. In this talk I will briefly summarise the results of a recently completed review, based on a deep literature review as well as interviews with most of the key project personnel, of high-school focussed astronomy research projects over the last 20 years. I will outline the major projects and their successes, but will largely focus on outlining those factors uncovered that prevent such projects from being as successful in motivating and educating high school students as their potential suggests.

221

THE TWISTED MAGELLANIC STREAM AND ITS LEADING ARM(S) Bi-Qing For

1

1. ICRAR/UWA, Perth, WA, Australia The Magellanic Stream and Leading Arm which originated from the Magellanic Clouds are spectacular gaseous features. They extend for tens of kpcs and span for ~200 degree in the southern sky. The close proximity of the Magellanic Clouds to the Milky Way provides an excellent opportunity to study interacting galaxy system. I utilized the data from Galactic All-Sky Survey (GASS) and ATCA high-resolution Magellanic Stream survey to study the properties of high velocity clouds that presumbly associated with the Magellanic Stream and Leading Arm. Morphological classification is given for these HVCs and HVCs catalogs in this vicinity are presented. I will also present the the newly discovered population of clouds that forms the LA IV and a new diffuse bridge-like feature connecting the LA II and III complexes.


222

OUTER TRIAXIALITY OF A ‘FAST ROTATOR’ Caroline Foster

1

1. Australian Astronomical Observatory, North Ryde, NSW, Australia As part of their pioneering work, the ATLAS3D team have shown that several morphologically elliptical galaxies are centrally kinematically disky. Hence, while global morphology suggests that ellipticals are ellipsoidal/triaxial in shape, their central kinematics are more consistent with (inclined) oblate systems. We obtain galaxy light kinematics of the centrally kinematically disky elliptical NGC 4473 out to 2.5 effective radii. While we confirm previous results in the central regions, we find that at large galactocentric radii NGC 4473 exhibits an interesting kinematic transition. In the outskirts, we observe clear minor and major axis rotation, a tell-tale sign of triaxiality. Hence, we conclude that the stellar halo of NGC 4473 is consistent with being triaxial as also inferred from its Hubble type. We conclude that NGC 4473 is centrally axisymmetric with an important transition into an outer ‘kinematically decoupled halo’ (KDH), in agreement with theoretical expectations.

223

A CATALOGUE OF RADIO AGN BEHIND THE LMC Gregory Goldstein

1 , Miroslav Filipovic, Nicholas Tothill, Evan Crawford

1. Univ Western Sydney, Greenwich, NSW, Australia We have prepared a catalogue of 230 known and recently identified radio AGN in a defined 7 x 7 degree area (the field of the Spitzer SAGE survey, described in Meixner et al (2006)) behind the LMC using multiwavelength studies. Identification of new AGN behind the LMC and other nearby galaxies remains important in several areas of research. Over the last 6 years over 7000 AGN candidates have been detected behind the LMC, in particular using microlensing studies such as MACHO and OGLE, and the Spitzer SAGE IR. Radio AGN were detected as LMC background sources in ATCA and MOST radio images; by mid-IR spectrum using criteria of Stern et al (2005); by optical variability (MACHO, OGLE); in catalogues/published studies as AGN/quasars with spectroscopic redshifts; and with X-ray counterparts. A total of 230 AGN candidates were included in the catalogue. Candidates were identified as AGN in at least two of the above categories. Radio AGN were classified as point or extended based on appearance, the major axis size, and the ratio of peak/integrated flux density at 36, 20, 6, and 3 cm wavelengths. There were 124 point, 80 extended, and 26 paired sources; 35 AGN had flat radio spectum, 145 steep and 45 ultra steep; 159 had a AGN IR spectrum, 64 had X-ray counterpart, 25 had a redshift. The angular separations of the radio source and the optical/IR/xray sources have been measured. As expected by the AGN unification theory, flat spectrum radio AGN have a smaller separation of the radio-optical/IR sources than steep spectrum. 15 of the 124 radio AGN that were point sources (12.0%) met criteria for “faint infrared radio sources”. A detailed catalogue of radio AGN is being published online. The catalogue will in addition provide a list of 181 confirmed AGN (with spectroscopic redshifts) in the study area that do NOT have radio counterparts. Thus of a total (181+25) 206 AGN with redshifts in the area, 12.1% have radio counterparts. 1. Stern et al, The Astrophysical Journal, 631:163–168, 2005 September 20 2. Meixner et al The Astronomical Journal, 132:2268–2288, 2006 December

224

STARBUGS ENABLING TECHNOLOGIES AND APPLICATIONS Michael Goodwin

1

1. Australian Astronomical Observatory, North Ryde, NSW, Australia Starbugs is an ongoing R&D project at the AAO to develop parallel fibre positioning technology to feed multi-object spectrographs. Starbugs are miniaturized robotic devices that can accurately ‘discrete step’ over large area focal surfaces to position payloads. Starbugs are the leading candidates for future based fibre positioning instrument concepts developed by the AAO, such as TAIPAN, HECTOR and MANIFEST. Starbugs are also suitable for positioning a diverse range of compact payloads to utilize the focal surface efficiently over wide-fields. Examples of these payloads include multiple integral field units, coherent imaging bundles for field acquisition and guiding, wavefront sensors and


correctors for multi-object adaptive optics and liquid atmospheric dispersion corrector. We describe these applications and technologies enabled by Starbugs that provide new and exciting scientific capabilities.

225

THE SEARCH FOR TEV PARTICLE ACCELERATORS IN THE STAR FORMING HII COMPLEX G5.89-0.39 USING CHANDRA Elise Hampton

1 , Gavin Rowell

1 , Dieter Horns

2 , Yasunobu Uchiyama

3 , Stefan Funk

3 , Stefan Wagner

4

1. University of Adelaide, Adelaide, SA, Australia 2. Institut fuer Experimental Physik, Universitaet Hamburg, Hamburg, Germany 3. Kavli Institute for Particles Physics and Cosmology, Stanford, USA 4. Universitaet Heidelberg, Heidelberg, Germany Several TeV gamma-ray sources have been found towards star forming HII regions, opening up the possibility that such star formation regions may accelerate particles to very high energies. We have analysed an 80ks Chandra observation of the G5.89-0.39 HII complex, comprising of a conventional HII region and an ultra compact (UC) HII region, and surrounding area towards the W28 SNR. The results of the analysis identify 159 X-ray sources in the Chandra observation with 17 X-ray sources identified within the HII region (G5.89-0.39A) and 17 X-ray sources identified within the UC HII region (G5.89-0.39B). The luminosities of the sources identified within the HII complex are consistent with B-type stars. Spectral analysis of the X-ray sources in the HII complex is consistent with known values of the area and indicates a match to a thermal APEC spectral fit. Possible localised soft diffuse X-ray emission has been identified in some areas of the Chandra observation. An analysis of the K-α iron line shows the potential for colliding winds associated with the conventional HII region. We also calculate an unabsorbed X-ray luminosity for the suspected ionising source of the UC HII region, J18003084-2404046 (Feldt et al. 2003).

226

RADIO FAINT GAMMA-RAY BURST AFTERGLOWS Paul J Hancock

1 , Bryan M Gaensler

1 , Tara Murphy

1

1. University of Sydney, NSW, Australia The detection rate of gamma-ray burst (GRB) afterglows is only 30% at radio wavelengths, much lower than in the X-ray ( 95%) or optical ( 70%) bands. The cause of this low radio detection rate has previously been attributed to limited observing sensitivity. We use visibility stacking to test this idea, and conclude that the low detection rate is instead due to two intrinsically different populations of GRBs, radio bright and radio faint. The radio bright GRBs also have higher gamma-ray fluence, isotropic energies, X-ray fluxes and optical fluxes than the radio faint GRBs, confirming the existence of two physically distinct populations. We suggest that the gamma-ray efficiency of the prompt emission is responsible for the difference between the two populations.

227

MAGNETIC FIELDS IN THE SMITH CLOUD Alex S Hill

1 , Robert A Benjamin

2 , Sui Ann Mao

3 4 , Felix J Lockman

5 , Naomi M McClure-Griffiths

1

1. CSIRO Astronomy & Space Science, Epping, NSW, Australia 2. Department of Physics, University of Wisconsin-Whitewater, Whitewater, WI, USA 3. NRAO, Socorro, NM, USA 4. Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA 5. NRAO, Green Bank, WV, USA The accretion of gas is an important component of galaxy evolution by providing fresh fuel for star formation. However, it is unknown whether and how infalling gas can reach galactic disks. The Smith Cloud is perhaps the best-studied example of a high velocity cloud interacting with the Galactic halo 3 kpc below the midplane, a case study of the active accretion in the Milky Way. We analyse H I, Hα, and Faraday rotation data for the Smith Cloud. We find filamentary structures in both H I and Hα which suggest shocked and decelerated bow waves from the interaction between the cloud and the halo ISM. There are also enhancements in Faraday rotation measure aligned with the Hα


filaments, suggesting a magnetic field of > 3 μG in these filaments which may pervade the rest of the Smith Cloud. This object promises to provide an excellent case study for magnetohydrodynamic simulations of gas accretion.

228

DISCOVERY OF THE OLDEST STARS IN THE GALACTIC BULGE Louise M Howes

1 , Martin Asplund

1 , Stefan Keller

1

1. Australian National University, Weston, ACT, Australia Despite frequent attempts over many years, the elusive first stars of the Universe have yet to be found. Searches for these "Population III" objects have targeted the old and metal-poor Galactic halo. However according to models of the formation of galaxies like the Milky Way, the oldest stars should lie in the centre of the Galaxy - in the bulge. Until now, problems with overcrowding and extinction have made searching the bulge an impossible task; the most metal-poor star previously known has [Fe/H]=-2.1. Our dedicated search, using SkyMapper photometry to pre-select low metallicity candidates, will discover >100 bulge stars with [Fe/H]<-3, all confirmed using AAOmega on the AAT. Here we present the first results of the ongoing survey: >2000 stars with [Fe/H]<-1, and from the pilot study, high-resolution spectroscopy of 12 stars (8 with MIKE on Magellan, and 4 as part of the Gaia-ESO survey using FLAMES UVES on the VLT). These high-resolution data have confirmed the discovery of the bulge's most metal-poor stars yet. They have allowed us to derive detailed chemical abundances of these stars, including alpha and s-process elements, which we have compared to the other components of the Galaxy. At the time of writing, we are currently following up another 8000 candidates with 9 nights at the AAT, the exciting results of which will be described on our poster! URL for supporting material - www.mso.anu.edu.au/~louise

229

HOW ACCURATE IS SUPERCOSMOS ASTROMETRY? Adam L. Schaefer

1 , Richard W. Hunstead

1 , Helen M. Johnston

1

1. Sydney Institute for Astronomy, The University of Sydney, NSW, Australia The Schmidt telescope surveys of the northern and southern sky form an invaluable resource for seeking counterparts at other wavelengths and for transferring coordinates onto CCD images. But how reliable are the positions from the Schmidt surveys, given the complex distortions introduced by the bending of the glass plates to the telescope's focal surface? SuperCOSMOS provides the best image sampling of the various digitized versions of the UK and Palomar Schmidt surveys, and in this paper we compare SuperCOSMOS optical positions with milliarcsecond radio positions that define the International Celestial Reference Frame (ICRF). The comparison sample has been confined to stellar objects brighter that magnitude 20, and Galactic latitude > 10 deg. Mean position offsets in both hemispheres are <0.1 arcsec in both coordinates, with rms scatter <0.2 arcsec. However, there are significant systematic errors in both hemispheres, particularly in the north.

1

1. Hambly, N. C. et al., 2001, MNRAS 326, 1279

230

THE ATLAS 5.5 GHZ SURVEY OF THE EXTENDED CHANDRA DEEP FIELD SOUTH: CATALOGUE, SOURCE COUNTS AND SPECTRAL INDICES

Minh Huynh1 , Andrew Hopkins

2 , Emil Lenc

3 , Minnie Mao

4 , Enno Middelberg

5 , Ray Norris

6 , Kate Randall

6

1. University of Western Australia, Crawley, WA, Australia 2. Australian Astronomical Observatory, Sydney, NSW, Australia 3. University of Sydney, Sydney, NSW, Australia 4. NRAO, Socorro, New Mexico, USA 5. Ruhr-Universitat, Bochum, Germany 6. CSIRO, Sydney, NSW, Australia Star-forming galaxies are thought to dominate the sub-mJy radio population, but recent work has shown that low-luminosity active galactic nuclei (AGNs) can still make a significant contribution to the faint radio source population.


Spectral indices are an important tool for understanding the emission mechanism of the faint radio sources. We have observed the extended Chandra Deep Field South at 5.5 GHz using a mosaic of 42 pointings with the Australia Telescope Compact Array. Our image reaches an almost uniform sensitivity of ~12 μJy rms over 0.25 deg

2 with a

restoring beam of 4.9 arcsec × 2.0 arcsec, making the ATLAS 5.5 GHz survey one of the deepest 6 cm surveys to date. We present the 5.5 GHz catalogue and source counts from this field. We take advantage of the large amount of ancillary data in this field to study the 1.4 to 5.5 GHz spectral indices of the sub-mJy population. For the full 5.5 GHz selected sample we find a flat median spectral index, αmed = -0.40, which is consistent with previous results. However, the spectral index appears to steepen at the faintest flux density levels (S5.5 GHz < 0.1 mJy), where αmed= -0.68. We performed stacking analysis of the faint 1.4 GHz selected sample (40<S1.4 GHz<200 μJy) and found a steep average spectral index, α = -0.8, consistent with synchrotron emission. We also found a weak trend of steepening spectral index with redshift. Several young AGN candidates are identified using spectral indices, suggesting that gigahertz peaked-spectrum sources are as common in the mJy population as they are at Jy levels.

231

GALACTIC STRUCTURE FROM THE MALT 90 SURVEY: HIGH-MASS STAR-FORMATION IN DISTANT SPIRAL ARMS James Jackson

1 , Scott Whitaker

1 , Jill Rathborne

2 , Jonathan Foster

3

1. Boston University, Boston, MA, United States 2. CASS, CSIRO, Marsfield, NSW, Australia 3. Astronomy Department, Yale University, New Haven, Connecticut, USA Using mm-wave molecular data from the Millimetre Astronomy Legacy Team 90 GHz Survey (MALT 90), we have determined the radial velocities and kinematic distances to 1,912 high-mass star-forming regions. This is the largest sample of star-forming regions for which reliable distances have been determined. We resolve the near-far kinematic distance ambiguity by searching for absorption or self-absorption features in the 21 cm H I spectra toward each of the molecular clumps. The distribution of the high-mass star-forming clumps clearly traces Galactic spiral arm features including the Scutum-Centaurus Arm, the Norma Arm, and the Sagittarius Arm. Of particular interest is the first detection of the most distant portion of the Scutum-Centaurus Arm at the far kinematic distance (~10 kpc from the Sun). Since high-mass star-formation occurs almost exclusively in spiral arms, these dense star-forming clumps may provide the best tracers of spiral structure in the Milky Way.

232

THE FALL AND RISE OF SYDNEY OBSERVATORY Andrew Jacob

1 , Toner Stevenson

1

1. Sydney Observatory, Sydney, NSW, Australia Sydney Observatory ceased astronomical research over 30 years ago when the Museum of Applied Arts and Sciences was granted responsibility for the site. It is now a museum of astronomy and a public observatory. The preservation and interpretation of astronomical heritage continues with the collection of 20,000 astronomical glass plates and associated records being returned and funding to reinstall the third dome received. A new digital planetarium is now in regular use, major astronomical events have been webcast and we continue to interact with the public through social media. A daytime school program in meteorology has been introduced and one in indigenous studies, including indigenous astronomy, is in preparation. URL for supporting material - http://www.sydneyobservatory.com.au/


233

MAKING VISIBLE THE WOMEN WHO MEASURED STARS IN AUSTRALIA Toner M Stevenson

1 2 , Andrew Jacob

2 3

1. Museum Studies, The University of Sydney, Sydney 2. Sydney Observatory, Millers Point, NSW, Australia 3. Curatorial, Powerhouse Museum, Sydney In Australia a significant number of women were employed to measure, log and calculate the position of stars for the Astrographic Catalogue at Adelaide, Sydney, Melbourne and Perth Observatories. This poster considers the social perception of the ‘nature ‘of women, the feminising of the observatory and the attitudes of the press to the employment of women in a scientific endeavour. It highlights Mary Emma Greayer who was employed as a computer in 1890 at Adelaide Observatory and Charlotte Emily Fforde Peel, a measurer and assistant computer from 1898 at Melbourne Observatory. Rather than an anonymous group of ‘women who measure’, it argues that individuals, such as Greayer and Peel, produced new research and had agency within the observatory not previously recognised as such.

234

CLUMPING FACTORS OF H AND HE FROM EOR SIMULATIONS Akila Jeeson-Daniel

1

1. University of Melbourne, Parkville, Vic, Australia In this work, we calculate the clumping factors of HII,HeII and HeIII in the IGM at various redshifts using a suite of Epoch of Reionization simulations. The Epoch of Reionization simulations were produced using Gadget and the ionizing radiative transfer performed using CRASH with the parameters calibrated to various observations at z~6. We also discuss the effect of environment on clumping factor calculations.

235

FIRST RESULTS FOR MALT-45: A 7MM SURVEY OF THE SOUTHERN GALAXY Christopher H Jordan

1 , Andrew Walsh, Maxim Voronkov, Simon Ellingsen

1 , Vicki Lowe

1. University of Tasmania, Hobart, TAS, Australia MALT-45 is an untargeted Galactic plane survey searching for tracers of high mass star formation (HMSF) at 7mm. With the recent upgrades to the Australia Telescope Compact Array, we have been able to push the limits on observational efficiency to obtain a very sensitive blind survey in a short amount of time. Specifically, MALT-45 uses a fast on-the-fly mapping with 6 seconds per pointing, which results in a quarter-square-degree region being mapped in approximately 14 hours. Each region is Nyquist sampled and collects data in 12 spectral lines. The primary spectral lines of MALT-45 include: CS (1-0) - a high density gas tracer, which contrasts well with NH3 (1,1) from the similar HOPS survey; 44 GHz Class I methanol masers - the brightest of the Class I lines, it is poorly understood, and MALT-45 is one of the first surveys to thoroughly search for these masers; SiO (1-0) v=1,2,3 - typically associated with evolved stars, there have been rare associations with HMSF, and MALT-45 offers the potential to detect more. Other lines include thermal SiO (1-0) v=0, thermal methanol, C34S, OCS, and radio recombination lines H51a and H53a. Perhaps the most significant and innovative aspect of MALT-45 is the usage of ATCA autocorrelations. Each antenna of the ATCA is similar to Mopra, and by using all 6 antennae simultaneously, have a 6 fold increase in sensitivity per unit observation time. The autocorrelation data was only recently made available by the ATCA upgrade with the Compact Array Broadband Backend, and tools have been developed to allow this data processing. We present the first 5 square-degrees (l = 330 - 335, b = -0.5 - +0.5) of the Galactic plane mapped by MALT-45.


236

WIDE-FIELD IMAGING STUDIES OF GLOBULAR CLUSTER SYSTEMS IN THREE INTERMEDIATE MASS EARLY-TYPE GALAXIES Sreeja Kartha

1

1. Swinburne University, Hawthorn, VIC, Australia We present the results from a study of globular cluster systems belonging to three early-type galaxies : NGC 720 (E5), NGC 1023 (S0) and NGC 2768 (S0). The galaxies were observed in multi-band wide-field images using the Subaru and Canada France Hawaii Telescopes. For NGC 1023 and NGC 2768, we made use of archival HST data. This work is a first time investigation of globular cluster systems to large galactocentric radii (∼100 kpc) for NGC 720 and NGC 2768. The radial extent of globular cluster systems is characterised to be 68 ± 6 kpc for NGC 720, 20 ± 2 kpc for NGC 1023 and 63 ± 3 kpc for NGC 2768. We have determined the total number of globular clusters and hence the specific frequency for the individual galaxies. The azimuthal distribution of globular cluster systems are investigated and found to be similar to the host galaxy properties. We have examined for globular cluster bimodality and found the three galaxies have strong blue and red subpopulations. We also present a new correlation of globular cluster system sizes and host galaxy effective radii.

237

SPECTROSCOPIC FITTING OF THE TERRESTRIAL ATMOSPHERE FOR IMPROVED PLANETARY ATMOSPHERE OBSERVATIONS AND GREENHOUSE GAS MONITORING Daniel V Cotton

1 , Champlain Kenyi

2 , Jeremy Bailey

3 , Lucyna Kedziora-Chudczer

4

1. School of Physics, The University of New South Wales, Sydney, NSW, Australia 2. School of Physics, The University of New South Wales, Sydney, NSW, Australia 3. School of Physics, The University of New South Wales, Sydney, NSW, Australia 4. School of Physics, The University of New South Wales, Sydney, NSW, Australia Summary: Ground-based observations are usually limited to spectral windows between the strong absorptions of species in the terrestrial atmosphere. When observing solar system- and exoplanetary atmospheres these same atomic and molecular absorptions are of interest. To get precise determinations of molecular abundances in planetary observations from ground-based telescopes, the effects of the Earth’s atmosphere need to be accurately removed. This task is complicated by variations in the concentrations of telluric absorbing species. The strong absorptions by carbon dioxide and water are among the most important and problematic. What we as astronomers seek to eliminate is of great interest to environmental and atmospheric scientists. The concentrations of telluric water vapour, carbon dioxide and methane are the subject of emerging greenhouse gas monitoring programs. We have developed code to work with the highly developed and well-regarded VSTAR radiative transfer atmospheric fitting software to attack these problems. ATMOF – ATMOspheric Fitting – makes use of VSTAR models of the terrestrial atmosphere as plug-in modules; it uses the Levenberg-Marquardt method to vary the mixing ratios of molecules in the models to fit calibration data (either standard star or solar observations) and determine the state of the atmosphere. The model is then used to remove telluric absorptions from observations of planets – producing a pure spectrum. Here we report on our progress in developing ATMOF for these dual purposes.

238

A TEST FOR GALAXY PRE-PROCESSING USING LARGE-SCALE STRUCTURE IN THE LOCAL UNIVERSE Dane Kleiner

1 , Kevin A Pimbblet

1 , D Heath Jones

1 , Baerbel Koribalski

2

1. Monash University, Clayton, VIC, Australia 2. CSIRO Astronomy and Space Science, Marsfield, NSW, Australia We present $sim$ 173 filaments of galaxies detected in 6dFGS and 2dFGRS out to a redshift of $z <$ 0.05. Selected by mass, we will measure the SFR, morphology and gas content of galaxies within these filaments to test if the filamentary environment provides the right conditions to transform galaxies for the first time. We will also compare how the properties of groups of galaxies within filaments compare to groups not embedded in this large scale structure. Specifically, we aim to test if galaxies are being pre-processed in filaments as they get funnelled into denser environments.


239

GAMA: THE LOCAL MASS-SIZE RELATIONSHIP REVISITED Rebecca Lange

1

1. ICRAR, UWA, Crawley, WA, Australia I will present a revised mass-size relationship of local galaxies using GAMA data (Galaxy And Mass Assembly survey) in a redshift range of 0.014<z<0.1. Furthermore, I will present the comparison of the mass-size relationship of spheroids, disks and galaxy components, showing that it is important to study not only the global properties of galaxies but also the properties of the components in order to improve our understanding of galaxy formation and evolution.

240

MAGNETIC FIELDS IN RELATIVISTIC NEUTRON STARS Paul Lasky

1

1. University of Melbourne, Melbourne, VIC, Australia The internal topology, strength and dynamics of magnetic fields in strongly magnetised neutron stars play a crucial role in the secular and dynamical evolution of these exotic objects. I will present both analytic calculations and nonlinear simulations of strongly magnetised neutron stars, with particular emphasis on determining stable magnetic field equilibrium states. The existence of various new branches of solutions in the context of magnetar physics and gravitational wave observations will be presented.

241

THE ENERGY SOURCE AND DYNAMICS OF INFARED LUMINOUS GALAXY ESO148-IG02 Sarah K Leslie

1 , Jeffery A Rich

2 , Lisa J Kewley

1 3 , Michael A Dopital

1 3 4

1. Research School of Astronomy and Astrophysics, Weston, ACT, Australia 2. Carnegie Observatories, Pasadena, California, USA 3. Institute for Astronmy, University of Hawaii, Honolulu, HI 4. Astronomy Department, Faculty of Science, King Abdulaziz University, Jeddah, Saudi Arabia We present integral field data of the infrared luminous merger galaxy ESO 148-IG02 obtained from the ANU Wide Field Spectrograph (WiFeS). We apply AGN and shock models to investigate the relative contribution from star formation, shock excitation and AGN activity to the optical emission in this key merger stage. We find that ESO148-IG02 has a flat metallicity gradient, consistent with recent gas inflow. Using kinematic information we separate the line emission maps into a northern non-rotating star formation region with low velocity dispersion, and a southern rotating system with high velocity dispersion which is influenced by AGN activity. We show that the two overlapping galaxies can be separated using the kinematic information, demonstrating the power of integral field spectroscopy.

242

DECODING THE MESSAGE FROM SILICON IN STARDUST MAINSTREAM SILICON CARBIDE GRAINS Karen M Lewis

1 , Maria Lugaro

2 , Brad K Gibson

2 3 , Kate Pilkington

2 3

1. Tokyo Institute of Technology, Ookayama, Japan 2. Monash Centre for Astrophysics (MoCA) , Monash University, Melbourne, Victoria, Australia 3. Jeremiah Horrocks Institute, University of Central Lancashire , Preston, UK SiC mainstream grains are presolar grains believed to form in the envelopes of carbon rich asymptotic giant branch (AGB) stars with masses between 1.5 and 3 solar masses. These grains represent a conundrum as the

29Si and

30Si

abundances indicate that they formed in stars of super-solar metallicity, before the solar system formed. To shed light on this problem, we use silicon isotopic abundances to derive an age metallicity relation for the stars believed to have produced the SiC mainstream grains. For 2732 mainstream SiC grains listed in the Presolar Grain Database, we use the

29Si abundances with the latest GCE models to derive [Fe/H], and

30Si abundances along with the models of

Zinner et al. (2006) to determine an approximate birth age for the AGB star in which the grain formed. Comparing our age metallicity relation with observational relationships derived for stars in the solar neighbourhood, we find that the spread of [Fe/H] is in agreement, but the mean [Fe/H] in our relation is higher by 0.2 dex. We propose that this


difference is because stars with higher [Fe/H] produce more dust and are consequently over-represented in our age metallicity diagram, a finding consistent with other works in the literature. This result offers a solution for the long-standing problem of silicon in stardust SiC grains, confirms the necessity of coupling chemistry and dynamics in simulations of the chemical evolution of our Galaxy, and constrains the modelling of dust condensation in stellar winds as a function of the metallicity.

243

MOLECULAR GAS DYNAMICS NEAR SAGITTARIUS A* John AP Lopez

1

1. UNSW School of Physics, SYDNEY, NSW, Australia Arguably one of the most important scientific advances in our understanding of black holes and galaxy formation is the discovery of a supermassive black hole (SMBH) associated with the radio source Sagittarius A*, at the center of our own Milky Way Galaxy. Results are presented here from molecular line emission on the kinematics and chemistry of clouds surrounding Sgr A* within a radius of ~ 0.2 degrees, which is within the Central Molecular Zone (CMZ). In particular, our data shows interesting chemistry in a cloud named: GC M-0.13-0.08 (Southern cloud / 20 kms

-1 cloud),

indicative of shocked gas and exposure to high levels of UV radiation. We discuss whether this is due to the general environment of Sgr A* or whether massive star formation is taking place in situ within the cloud. These observations were undertaken at 3mm and 7mm with the NANTEN2 & Mopra radio telescopes.

244

VARIATIONS BETWEEN STAR FORMATION ENVIRONMENTS Vicki Lowe

1 2 , Maria Cunningham

2

1. CSIRO Astronomy and Space Science, Sydney, Australia 2. University of New South Wales, Sydney, Australia The life cycles of high-mass stars (≥ 8Mʘ) have a major impact on the evolution of galaxies, while in turn, the position of a molecular cloud in the Galaxy has a major impact on the efficiency and type of star formation which occurs therein. Assuming that if a giant molecular cloud (GMC) began with the same molecular abundances throughout, then any changes observed between different clumps within that GMC will be due to its stage of star formation. By studying how these stars form, we will be able to identify how they shape their surrounding environment. To do this, I have studied two contrasting GMCs: G333, (l = 333ᵒ, b = -0.4ᵒ; d ~ 3.6 kpc) and Vela C (l ~ 265ᵒ, b ~ 1.5ᵒ; d ~ 700 pc). For G333, I am enhancing a 3-mm Mopra survey by including pointed ammonia observations targeted towards star forming clumps with the 70-m Tidbinbilla radio telescope. For Vela C, I have surveyed the region in a variety of tracers across the Mopra millimetre bands. By targeting star forming clumps and using the lowest inversion transitions of ammonia, the temperature variations throughout the two clouds can be analysed. By combining the molecular information with archival dust maps from the Spitzer and Herschel space telescopes, the impact of star formation can be determined.

245

BCOOL AUSTRALIA Stephen Marsden

1 , Pascal Petit

2 , Sandra Jeffers

3 , Brad Carter

1 , Carolyn Brown

1 , and the Bcool Collaboration

1. USQ, Toowoomba, QLD, Australia 2. IRAP, Toulouse, France 3. Georg-August-Universitaet, Goettingen, Germany The Bcool project is an international collaboration, with significant Australian involvement, aimed at studying the magnetic activity of low-mass stars from pre-main sequence through to evolved objects. The project has a particular emphasis on the use of spectropolarimetric observations to characterise the magnetic fields of cool stars and improve understanding of the operation of stellar dynamos under a range of conditions. As part of the Bcool project, 167 solar-type stars chosen mainly from planet search databases have been observed using spectropolarimetric observations. From these observations surface magnetic fields have been detected for 67 stars, a vast increase in the number of stars on which magnetism has been detected. In addition, we have mapped the surface magnetic field topology of


over 20 of the stars, with many having multi-epoch observations forming an ongoing search for stellar magnetic cycles akin to the 22 year solar cycle. In this poster we outline some of the main discoveries so far realised from the Bcool solar-type star sample. In addition we discuss a possible enhancement of this project using the planned high-resolution Veloce spectrograph for the AAT.

246

DENSE GAS TOWARDS THE SUPERNOVA REMNANTS RX J1713.7-3946 AND W28 Nigel Maxted

1 , Gavin Rowell

1 , Brent Nicholas

1 , Michael Burton

2 , Yasuo Fukui

3 , Andrew Walsh

4 , Akiko

Kawamura3 , Hirotaka Horachi

3 , Jasmina Lazendic

3 , Hidetoshi Sano

3 , Satoshi Yoshiike

3 , Tatsuya Fukuda

3

1. The University of Adelaide, Adelaide, SA, Australia 2. The University of New South Wales, Sydney, Australia 3. The University of Nagoya, Nagoya, Japan 4. Curtin University, Perth, Australia We study the dense gas towards the young (~1 000yr) supernova remnant, RX J1713.7-3946, and the old (~10 000yr) supernova remnant, W28, using the Mopra radio telescope. Both of these remnants are TeV gamma-ray sources, which suggests local high energy particle populations. It follows that these objects are perfect targets for the study of the origin of cosmic-rays. Gas density inhomogeneities may inhibit the passage of cosmic ray protons and/or provide extra cosmic ray proton target material. These two effects may be energy-dependent, hence may have signatures in gamma-ray observations (spatially and in energy spectra), therefore dense gas studies offer a novel way to test for the hadronic (p-p interactions) scenario and investigate the potential acceleration of cosmic rays in these objects. We present the latest results from our Mopra 7 and 12mm surveys towards RX J1713.7-3946 and W28.

247

DO TILED DISPLAY WALLS IMPROVE FEATURE RECOGNITION IN LARGE ASTRONOMICAL IMAGES? Bernard Meade

1 2 , Christopher Fluke

1

1. Center for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Vic, Australia 2. The University of Melbourne, Vic, Australia A Tiled Display Wall (or TDW) combines many smaller resolution monitors into a single high resolution display. The first large-scale TDW in Australia, the OptIPortal, was launched at The University Of Melbourne in 2008. Astronomy, being such a highly visual science, was thought to be a very suitable candidate for this 98-megapixel display, along with supporting other research activities working with very large images. However, early attempts to engage researchers across all disciplines were largely unsuccessful, due to expensive hardware, unstable software, and complex data preparation processes. Over the last few years, these issues have been addressed and slowly but surely, more research institutions are installing and actually using TDWs. Astronomers, however, are still slow to adopt this technology, preferring to continue with desktop or projected displays. One way of empirically comparing the suitability of displays is through a feature search, where participants are asked to identify specific features of interests within complex images. In this presentation, I will compare results of feature searches within ultra-high resolution astronomical images on three display environments: a typical desktop display, a large format projector display and a Tiled Display Wall. These results will help determine whether ultra-high resolution displays can indeed improve the scientific returns when examining ultra-high resolution astronomical images.

248

TULLY-FISHER RELATIONS WITHOUT GALAXY INCLINATIONS Martin Meyer

1 , Danail Obreschkow

1

1. ICRAR/UWA, Crawley, Wa, Australia The Tully-Fisher relation is a key observational constraint that must be met by any model of galaxy evolution. Linking the baryonic properties of galaxies (via luminosity or mass) to their dark matter content (via rotational velocity) much effort has gone into parametrizing this relation. However, the need for measured galaxy inclinations to convert line-


of-sight velocity measurements into rotational velocities has been a large source of error. In this work, we investigate the use of maximum likelihood techniques to recover the Tully-Fisher relation without the use of galaxy inclinations.

249

HI STACKING CAN BE USED TO MEASURE EDGE-ON ROTATION VELOCITIES FOR USE IN THE TULLY-FISHER RELATION Scott A Meyer

1 , Martin Meyer

1 , Danail Obreschkow

1

1. Physics, ICRAR, Crawley, Western Australia, Australia The Tully-Fisher relation

1 is an empirical relation between the baryonic and dark matter components of spiral

galaxies. In order to reduce or completely exclude the largest source of error in constructing the Tully-Fisher relation, inclination errors, we have investigated stacked HI profile widths, which do not require inclination information. We find a correlation between the width of a stacked HI profile and the maximum rotational velocity of the galaxies used in the stack. We propose that this correlation could be used to construct a Tully-Fisher relation from a set of stacked profiles that mimics the Tully-Fisher relation produced by the input galaxies. We have investigated analytical galaxies, simulated galaxies and the HIPASS data set. We find

1 that HI stacked profiles can be used in place of individual

profiles for use in the Tully-Fisher relation. 1. Tully, R., & Fisher, J. (1977). A new method of determining distances to galaxies. Astronomy & Astrophysics,

54(3), 661.

250

STARS ON THE RUN: ESCAPING FROM STELLAR CLUSTERS Guido Moyano Loyola

1 , Jarrod Hurley

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia It is believed that most stars are born in stellar clusters, which dissolve over time so that the members become part of the disc and halo population of the Galaxy. In the present work we will assume that these young stellar clusters live mainly within the disc of the Galaxy. We have explored four different primordial binary percentages: 0%, 10% and 50%. We have quantified the contribution of these escaping stars to the Galaxy population by analysing their escape velocity and evolutionary stage at the moment of escape. In this way we could analyse the mechanisms that produced these escapers, whether evaporation through weak two-body encounters, energetic close encounters or stellar evolution events, e.g. supernovae. We could also infer that dissolving stellar clusters such as those that we have modeled can populate the Galactic halo with giants stars for which the progenitors were stars of up to 2.4 M⊙. Furthermore, choices made for the velocity kicks of remnants do influence the production of hyper-velocity stars.

251

COLOUR BIMODALITY OF GALAXIES AT HIGH REDSHIFT Themiya Nanayakkara

1

1. CAS, Hawthorn, VIC, Australia One of the main methods that is being used to describe galaxies is their colour morphology. Many studies in the past has focused on low redshift galaxies and has found many interesting results on the dependence of colour of galaxies on environment and mass

1 2 .

With the introduction of many large scale surveys, at present there are many studies which try to identify properties of galaxies at high redshift

6 3 . The study of them is important to try to understand the formation and evolution of

individual galaxies and galaxy clusters. Therefore it is important to try to investigate comparisons between field and cluster galaxies at high redshift and compare them with results from low redshift studies. One of the main impediments for such studies is the lack of galaxy clusters identified at higher redshifts. In 2011 the first results from Z-FOURGE survey revealed a candidate cluster in the COSMOS field around a redshift of two, which possibly is the highest redshift cluster identified so far

5 .


While better resolution redshift data is required to properly establish whether it is a cluster or a group of galaxy overdensities, one of the main aims in my current study is to try identify the colour distribution of the galaxies at the higher redshifts. I am planning to study how the colour bimodality depends on galaxy environment (which itself is defined in many ways

4 ) and/or mass at high redshift and compare results with the SDSS studies done by Baldry et al.

using galaxies around a redshift of two and observed K magnitude cutoff at 24.8. The ultimate goal would be to try to compare results with semi analytic models by Croton and Peng et al. to establish constrains on galaxy evolution for future studies. 1. I. K. Baldry, M. L. Balogh, R. G. Bower, K. Glazebrook, R. C. Nichol, S. P. Bamford, and T. Budavari. Galaxy

bimodality versus stellar mass and environment. , 373:469{483, December 2006. 2. I. K. Baldry, K. Glazebrook, J. Brinkmann, �Z. Ivezi�c, R. H. Lupton, R. C. Nichol, and A. S. Szalay. Quantifying

the Bimodal Color-Magnitude Distribution of Galaxies. , 600:681{694, January 2004. 3. K. Kova�c et al. The Density Field of the 10k zCOSMOS Galaxies. , 708:505{533, January 2010. 4. S. I. Muldrew, D. J. Croton, R. A. Skibba, F. R. Pearce, H. B. Ann, I. K. Baldry, S. Brough, Y.-Y. Choi, C. J.

Conselice, N. B. Cowan, A. Gallazzi, M. E. Gray, R. Gr•utzbauch, I.-H. Li, C. Park, S. V. Pilipenko, B. J. Podgorzec, A. S. G. Robotham, D. J. Wilman, X. Yang, Y. Zhang, and S. Zibetti. Measures of galaxy environment - I. What is 'environment'? , 419:2670{2682, January 2012.

5. L. R. Spitler, I. Labb�e, K. Glazebrook, S. E. Persson, A. Monson, C. Papovich, K.-V. H. Tran, G. B. Poole, R. Quadri, P. van Dokkum, D. D. Kelson, G. G. Kacprzak, P. J. McCarthy, D. Murphy, C. M. S. Straatman, and V. Tilvi. First Results from Z -FOURGE: Discovery of a Candidate Cluster at z = 2.2 in COSMOS. , 748:L21, April 2012.

6. K. E. Whitaker, I. Labb�e, P. G. van Dokkum, G. Brammer, M. Kriek, D. Marchesini, R. F. Quadri, M. Franx, A. Muzzin, R. J. Williams, R. Bezanson, G. D. Illingworth, K.-S. Lee, B. Lundgren, E. J. Nelson, G. Rudnick, T. Tal, and D. A. Wake. The NEWFIRM Mediumband Survey: Photometric Catalogs, Redshifts, and the Bimodal Color Distribution of Galaxies out to z ~ 3. , 735:86, July 2011. 2

252

IS THE FUNDAMENTAL PLANE FUNDAMENTAL? Belinda A Nicholson

1 , Edward N Taylor

1 , Rachel L Webster

1

1. University of Melbourne, Parkville, Vic, Australia The fundamental plane of elliptical galaxies can be transparently understood as a relation between stellar and dynamical mass. Using over 1400 mass-selected (log stellar mass< 10.5) galaxies at redshift less than 0.12 from the Galaxy And Mass Assembly (GAMA) survey, we examine how the stellar-to-dynamical mass ratio varies with stellar mass, (g-i) colour, and Sersic index. We find a weak trend in stellar-to-dynamical mass ratio with colour and a stronger trend with Sersic index. These have significant implications for the reliability of mass estimates, as well as the tilt of the fundamental plane, and therefore for cosmological studies. Our poster explains these implications in more detail.

253

PROPERTIES OF CORONAL RAINS IN THE SUN Robert Nilsson

1 2 , Alina C Donea

2

1. Lulea University of Technology, Lulea, Sweden 2. School of Mathematical Sciences, Monash University, Clayton, VIC, Australia Sometimes, eruptions in the Sun are accompanied by coronal rains. Coronal rain corresponds to cool and dense blob-like material forming in the hot solar coronal environment in timescales of minutes, which subsequently falls down to the surface along loop-like paths. This phenomenon is often observed in chromospheric lines such as Halpha, but can also be observed with the Atmospheric Imaging Assembly (AIA) instrument of the satellite Solar Dynamics Observatory. In this work, we will present spectacular images of coronal rains at various AIA frequencies, and will discuss the complex dynamics of these events at small and large spatial and temporal scales, observed at photospheric, chromospheric and coronal heights. High resolution observations also reveal that prominences are often composed of a myriad of fine threads, outlining a fine-scale structure of the magnetic field and the presence of flows along the threads. Coronal rain is gaining attention from the solar physics community thanks to recently discovered properties such as its deep link to coronal heating and its apparently ubiquitous character in active regions, which will also be discussed here.


254

PULSAR STUDIES WITH THE MURCHISON WIDEFIELD ARRAY (MWA) Samuel S. I. Oronsaye

1 2 , Steven S. J. Tingay

1 2 , Steve S. M. Ord

1 2 , Ramesh N.D.R. Bhat

1 2 , Steven S. Tremblay

1 2

1. CAASTRO, PERTH, WA, AUSTRALIA 2. ICRAR/Curtin University, Bentley, WA, Australia We present the potential capability of the Murchison Widefield Array (MWA) in searching for pulsars and rotating radio transients (RRATs). The MWA, an array of 128 antenna tiles (each tile being a 4x4 dipole array) is a SKA (Square Kilometre Array) precursor which operates within the 80-300 MHz of the electromagnetic spectrum. The flux density of most radio pulsars tend to peak near or within the low frequency range in which the MWA operates. This along with its wide field of view makes the MWA an efficient instrument for conducting pulsar surveys, and we discuss some plausible survey strategies. Pulsar searches with the MWA will be sensitive to slow pulsars and RRATs, while maintaining reasonable sensitivity to millisecond pulsars. We also present some early pulsar detections with the MWA's high time resolution recorder currently under development.

255

THE CLUSTERING OF GAMA GALAXIES: DEPENDENCE ON COLOR, LUMINOSITY, MASS AND REDSHIFT David Palamara

1 , Michael Brown

1

1. MoCA (Monash Centre for Astrophysics), Clayton, VIC, Australia Present galaxy evolution theory has been shaped by the statistical analysis of large-scale galaxy redshift surveys such as the Sloan Digital Sky Survey (SDSS). The 3D distribution of galaxies has influenced our understanding of the underlying Cosmology and dark matter structure of the Universe. How different galaxies trace this underlying structure gives insight into small-scale processes of galaxy formation, such as the merger growth rate and star formation rate (SFR) dependence on environment, etc. While surveys such as SDSS map a wide area, they span a restricted range in look back time and thus limit our ability to trace how these relationships evolve over cosmic time. The Galaxy And Mass Assembly (GAMA) survey

1 , which covers ≈300 deg

2 and has a mean redshift of z≈0.2, provides

an ideal testing ground to push our understanding of how these relationships evolve over a large span of cosmic time. We present the first measures of the 2-point correlation function for GAMA galaxies as a function of color, luminosity, mass and redshift. These measurements will provide the strongest tests of galaxy formation models out to z=0.5 to date. 1. S.P. Driver, P. Norberg, I.K. Baldry, S.P. Bamford, A.M. Hopkins, J. Liske, J. Loveday, J.A. Peacock and the

GAMA Team, 2009, Astronomy & Geophysics, 50, 5.12.

256

GLOBULAR CLUSTER AND STELLAR METALLICITY RADIAL PROFILES IN EARLY-TYPE GALAXIES Nicola Pastorello

1

1. Swinburne University, Hawthorn, VIC, Australia Here I present a chemical study of both globular clusters and stellar component for a range of early-type galaxies. From the joint analysis of the two tracers together it is possible to retrieve new information about galaxy formation. Using the near-IR CaT II absorption lines, we are able to directly probe the metallicity of the galaxy stars and globular clusters. Furthermore, I will show radial metallicity gradients up to several effective radii, reaching regions of the galaxies hardly explored in the past, despite their dramatic importance in revealing the formation history of these objects.


257

THE GAMA VOID GALAXY SAMPLE Samantha Penny

1

1. Monash University, MoCA, Clayton, VIC, Australia Cosmological voids with sizes >10 Mpc are the most under dense regions of the Universe in which to study galaxy evolution, with a galaxy population that is theorised to have assembled its mass via star formation only. Due to their isolation, void galaxies are thought to be pristine, and their evolution is likely governed by internal processes. By examining their properties, we can therefore gain a better understanding of the internal feedback processes that govern low mass galaxy evolution in an environment where galaxy-galaxy interactions are likely uncommon. Using the Galaxy and Mass Assembly (GAMA) dataset, we identify a sample of galaxies residing in cosmological voids to M_g=-18 out to z=0.1, with a population of void dwarf galaxies found at low redshifts (z<0.05). The majority of void galaxies are low mass, blue, star forming irregular or spiral galaxies with colours (g-i) < 0.8. However, a number of red, non star forming galaxies are identified, showing a fraction of void galaxies have undergone processes that have shut off their star formation. By comparing their properties with those of the field, we will establish if these red void galaxies are simply faded disks, or if other processes are responsible for quenching their star formation.

258

THE ROLE OF STELLAR MASS AND ENVIRONMENT FOR CLUSTER BLUE FRACTION, AGN, AND STAR FORMATION Kevin Pimbblet

1 , Peter Jensen

1. Monash University, Clayton, Vic, Australia We present an analysis of the galaxy population of an intermediate X-ray luminosity galaxy cluster, Abell 1691, from SDSS and Galaxy Zoo data to elucidate the relationships between environment and galaxy stellar mass for a variety of observationally important cluster populations that include the Butcher-Oemler blue fraction, the active galactic nucleus (AGN) fraction and spectroscopic classifications of galaxies. We show that there is a mild increase in the AGN fraction with radius from the cluster centre that appears mainly driven by high-mass galaxies [log(stellar mass) > 10.8]. Although the cluster blue fraction follows the same radial trend, it is caused primarily by lower mass galaxies [log(stellar mass) < 10.8]. Significantly, the galaxies that have undergone recent starbursts or are presently starbursting but dust-shrouded [spectroscopic e(a) class galaxies] are also nearly exclusively driven by low-mass galaxies. We therefore suggest that the Butcher-Oemler effect may be a mass-dependent effect. We also examine red and passive spiral galaxies and show that the majority are massive galaxies, much like the rest of the red and spectroscopically passive cluster population. We further demonstrate that the velocity dispersion profiles of low- and high-mass cluster galaxies are different. Taken together, we infer that the duty cycle of high- and low-mass cluster galaxies is markedly different, with a significant departure in star formation and specific star formation rates observed beyond r200.

259

THE HALO MASS FUNCTION & FUTURE GALAXY SURVEYS Chris Power

1 , Steven Murray

1 , Aaron Robotham

1

1. University of Western Australia, Crawley, WA, Australia The dark matter halo mass function is a powerful cosmological probe, allowing us to test our models of dark matter and dark energy. Measuring the halo mass function is one of the key science drivers of future galaxy surveys. We present a new web-application for computing the halo mass function and we discuss optimal survey strategies for constraining dark matter and dark energy.


260

MERCURY, TITAN AND GANYMEDE: NEW THEORETICAL MODELS FOR BULK CHEMICAL COMPOSITION, INTERNAL PHYSICAL STRUCTURE AND ORIGIN WHICH MATCH THE LATEST SPACECRAFT DATA Andrew J. R. Prentice

1

1. School of Mathematical Sciences, Monash University, Clayton, Victoria 3800, Australia The huge bounty of new data about the physical and chemical makeup of Mercury and Titan that has been acquired by the NASA MESSENGER and Cassini-Huygens spacecraft since 2008 and 2004, respectively, coupled with the wealth of new data about Ganymede that was obtained through the Galileo Project between 1996 and 2003, has greatly sharpened our understanding of these 3 remarkably different planet-sized bodies. The only similarity between the three is that they all have roughly the same physical diameter, namely ~ 5000 km. Mercury has an unusually large core of metal, whose mass makes up ~71% of this planet’s mass. It also has an active magnetic dynamo, indicating that the outer portion of the core is molten. Titan is distinct because of its massive atmosphere of N2 and CH4. Since CH4 is being continuously destroyed by solar photolysis, there must be some geophysical mechanism acting within its icy mantle, most likely tidal heating, which serves to bring fresh CH4 to the surface. The mean density of 1.881 g/cm

3 indicates an internal H2O ice mass fraction of ~0.490. Titan has no magnetic field and its shape is slightly oblate,

possibly indicating that Titan first condensed in a solar obit before being captured by the Saturn system (Prentice 1984 Earth, Moon & Planets 30 209; 2006 PASA 23 1). Ganymede does have a large native magnetic field. It is not known if this is dynamo-driven or a frozen-in thermoremanent field. The estimated H2O ice mass fraction is ~0.475. I present a unified set of thermal and structural models for Mercury, Titan and Ganymede which attempt to account for much of the new observational data. These models are based on the author’s modern Laplacian theory of solar system formation, according to which both the planetary system and the regular satellite systems of the gas giant planets condensed from concentric families of orbiting gas rings (Prentice 2006; 2008 LPSC abstract #1945 – see URL). URL for supporting material - http://www.lpi.usra.edu/meetings/lpsc2008/pdf/1945.pdf

261

MULTI-EPOCH VERY LONG BASELINE INTERFEROMETRIC OBSERVATIONS OF THE NUCLEAR STARBURST REGION OF NGC~253: IMPROVED MODELING OF THE SUPERNOVA AND STAR-FORMATION RATES Hayden Rampadarath

1 , Emil Lenc

2 , John S Morgan

1 , Steven J Tingay

1

1. ICRAR, Curtin University, Bentley, WA, Australia 2. Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW, Australia We present the results of multi-epoch observations of the southern starburst galaxy, NGC~253, with the Australian Long Baseline Array (LBA) at 2.3~GHz. Our observations, conducted in 2006, 2007 and 2008 are similar to previous 2.3~GHz LBA observations by Lenc and Tingay (2006) in angular resolution (15~mas), field of view and sensitivity. Eight sources were detected, corresponding to higher frequency VLA detection. Six sources correspond to detections in the previous 2.3 GHz LBA observations, while two are new detections. One supernova remnant, 5.48-43.3, was imaged with the highest resolution in all three epochs, revealing a morphology similar to that of SN~1987A and an upper limit of the expansion speed consistent with, 10,000~km/s. A free-free absorption model was fitted to the spectra of 20 compact sources in NGC~253,incorporating the flux densities from the 2008 epoch. Small differences were found in the spectra and fitted parameters of spectral index and free-free opacity from Lenc and Tingay (2006). These variations are possibly due to the surrounding medium. A value for the upper limit of the supernova rate, 0.29 per yr, was derived for the inner 300~pc of NGC~253 and is consistent with estimates determined from near infrared (NIR) observations of the [FeII] line. The model used to derive this limit was based on the principles Ulvestad & Antonucci (1991) and Lenc and Tingay (2006), and included data from 10 observations over a period of a 20.6 years. Improvements over previous models included better knowledge of the Type~II supernovae peak luminosities at 6~cm, an improved distance estimate and incorporation of time-dependent spectral indices from Type~II supernovae light curves. From the supernova rate we estimate a new upper limit to the star formation rate of SFR(M>5M_solar)<7.1 M_solar/yr , which is consistent with estimates at other wavelengths. 1. Lenc, E. and Tingay, S. J. (2006). AJ, 132:1333–1345 2. Ulvestad, J. S., & Antonucci, R. R. J. 1991, AJ, 102, 875


262

THE RADIO PROPERTIES OF MASS SELECTED IR GALAXIES OUT TO Z=3 Glen Rees

1

1. Macquarie University, Macquarie University, Sydney, NSW, Australia Using the newly observed ZFOURGE NIR photometric survey, we present a preliminary analysis of the radio characteristics of a high-z, stellar mass selected galaxy sample. Further, we attempt to use FIR binned, stacked radio observations to test the evolution of the FIR-Radio correlation out to a redshift of 3.

263

THE FIRST SUPERNOVA DISCOVERED WITH GEMS/GSAOI Stuart Ryder

1 , Seppo Mattila

2 , Erkki Kankare

2

1. Australian Astronomical Observatory, North Ryde, NSW, Australia 2. Tuorla Observatory, Turku, Finland Our search for core-collapse supernovae in Luminous Infrared Galaxies (LIRGs) with adaptive optics on Gemini North has enabled us to place the first empirical constraints on the fraction of supernovae missed by optical surveys. We have commenced a search with the powerful new GeMS/GSAOI facility on Gemini South, and our first epoch images of the LIRG IRAS 18293-3413 already reveal a new supernova not seen in any optical survey. We show preliminary light curve fits which yield information on the supernova's type and line-of-sight extinction.

264

DIRECT IMAGING OF LONG PERIOD RADIAL VELOCITY EXOPLANET SYSTEMS WITH NICI Graeme S. Salter

1 , Chris G. Tinney

1 , Rob Wittenmyer

1 , Hugh R.A. Jones

2 , James S. Jenkins

3 , Simon O'Toole

4

1. UNSW, Kensington Campus, NSW, Australia 2. University of Hertfordshire, Hatfield, UK 3. Universidad de Chile, Santiago, Chile 4. Australian Astronomical Observatory, North Ryde, NSW, Australia We are finally entering an era of exoplanet research where radial velocity and direct imaging parameter spaces are starting to overlap. Radial velocity measurements provide us with a minimum mass for an orbiting companion (the mass as a function of the inclination of the system). By following up these long period radial velocity detections with direct imaging we can determine whether a trend seen is due to an orbiting planet at low inclination of an orbiting brown dwarf at high inclination. In the event of a non-detection we are still able to put a limit on the maximum mass of the orbiting body. The Anglo-Australian Planet Search (AAPS) is one of the longest baseline radial velocity planet searches in existence, amongst its targets are many that show long period trends in the data. I will present our direct imaging survey of these objects with our results to date. ADI Observations have been made using NICI (Near Infrared Coronagraphic Imager) on Gemini South and analysed using an in house, LOCI-like, post processing.

265

THE SUPERMASSIVE BLACK HOLE MASS - SÉRSIC INDEX (AND OTHER) RELATION(S) FOR BULGES AND ELLIPTICAL GALAXIES Giulia Savorgnan

1 , Alister W. Graham

1

1. Swinburne University of Technology, Hawthorn, VIC, Australia Scaling relations between supermassive black hole (SMBH) mass, MBH, and various host spheroid properties are a powerful tool for studying galaxy-(black hole) coevolution. Furthermore, these relations enable us to predict the masses of SMBHs in other galaxies, and to measure the SMBH mass function and quantify the SMBH space density in our local universe. Graham & Driver (2007) presented evidence for a strong correlation between MBH and the central light concentration of the host bulge, quantified by the Sérsic index n. The MBH - n relation might be one of the simplest and strongest black hole mass scaling relations, requiring only uncalibrated galaxy images. However, the recent literature has failed to recover a strong MBH - n relation. Working with the authors of those works, we have successfully recovered the useful MBH - n relation. Moreover, we have explored for potential substructure in the MBH -


n diagram based on galaxy morphology (elliptical or disc) and the nature of the central light profile (Sérsic or core-Sérsic). Future work will focus on accurately modelling the bulge/disc structure of ~80 local galaxies with direct MBH values and a re-investigation of all the black hole mass scaling relations.

266

TYPE IA SUPERNOVA BOLOMETRIC LIGHT CURVES AND EJECTED MASS ESTIMATES FROM THE NEARBY SUPERNOVA FACTORY Richard Scalzo

1 , Greg Aldering

2 , Pierre Antilogus

3 , Cecilia Aragon

2 4 , Stephen Bailey, Charles Baltay

5 , Sebastien

Bongard3 , Clement Buton

6 , Arnaud Canto

3 , Flora Cellier-Holzem

3 , Michael Childress

1 2 7 , Nicolas Chotard

8 ,

Yannick Copin8 , Hannah Fakhouri

2 7 , Emmanuel Gangler

8 , Julien Guy

2 , Eric Hsiao, Matthias Kerschhaggl

6 , Marek

Kowalski6 , Markus Kromer

9 , Peter Nugent

10 , Kerstin Paech

6 , Reynald Pain

3 , Emmanuel Pecontal

11 , Rui Pereira

8 ,

Saul Perlmutter2 7 , David Rabinowitz

5 , Mickael Rigault

8 , Karl Runge, Claire Saunders, Stuart Sim

1 12

, Gerard Smadja

8 , Charling Tao

13 14

, Stefan Taubenberger9 , Rollin Thomas

10 , Benjamin Weaver

15 , Chao Wu

3 16

1. Australian National University, Weston Creek, ACT, Australia 2. Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA 3. LPNHE, Universite Pierre et Marie Curie Paris 6, Paris, France 4. Department of Human Centered Design & Engineering, University of Washington, Seattle, WA, USA 5. Department of Physics, Yale University, New Haven, CT, USA 6. Physikalisches Institut, Universitat Bonn, Bonn, Germany 7. Department of Physics, University of California, Berkeley, Berkeley, CA, USA 8. IPNL, Universite de Lyon, Lyon, France 9. Max-Planck-Institut fur Astrophysik, Garching-bei-Munchen, Germany 10. Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA 11. CRAL, Universite de Lyon, Lyon, France 12. School of Mathematics and Physics, Queen's University Belfast, Belfast, UK 13. Centre de Physique des Particules de Marseille, Marseille, France 14. Tsinghua Center for Astrophysics, Tsinghua University, Beijing, China 15. Center for Cosmology and Particle Physics, New York University, New York, NY, USA 16. National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China We present a sample of normal type Ia supernovae from the Nearby Supernova Factory dataset with spectrophotometry at sufficiently late phases to estimate the ejected mass using the bolometric light curve. We measure

56Ni masses from the peak bolometric luminosity, then compare the luminosity in the

56Co-decay tail to the

expected rate of radioactive energy release from ejecta of a given mass. We infer the ejected mass in a Bayesian context using a semi-analytic model of the ejecta, incorporating constraints from contemporary numerical models as priors on the density structure and distribution of

56Ni throughout the ejecta. We find a strong correlation between

the ejected mass and the light curve decline rate, and consequently the 56

Ni mass, with ejected masses in our data ranging from 0.9–1.4 M⊙. Most fast-declining (SALT2 x1 < −1 or ∆m15,B > 1.2) normal SNe Ia have significantly sub-Chandrasekhar ejected masses in our analysis. At least two progenitor scenarios seem to be necessary to explain our observations.

267

THE RELATIONSHIP BETWEEN LOBE LUMINOSITY AND KINETIC POWER OF AGN JETS Stas Shabala

1 , Leith Godfrey

2

1. University of Tasmania, Hobart, TAS, Australia 2. Curtin University, Perth, WA, Australia Accurate measurement of kinetic power of AGN jets is important to three areas of astrophysics: (1) jet generation mechanisms; (2) studies of jet dynamics; and (3) the role of AGN feedback in galaxy formation and evolution. However, measuring jet power is difficult. The lack of reliable empirical methods has resulted in the widespread use of radio luminosity as a proxy for jet power.We present a new method of measuring jet power in FR-II radio galaxies, based on the observed parameters of jet terminal hotspots. We compare the jet power - lobe luminosity relation derived for our sample with that obtained for FR-I radio galaxies based on X-ray cavity measurements. Somewhat surprisingly, we find approximate agreement between these relations, despite mounting evidence in the literature


favouring vastly differing compositions and energy budgets in these two classes of radio galaxies.We use our hotspot measurements to show that FR-II radiative efficiency is sensitive to radio galaxy size, in agreement with predictions of dynamical models. Any observed jet power - radio luminosity relation is therefore sensitive to sample selection effects. This dependence explains, at least in part, the coincidence of the jet power - lobe luminosity relations for FR-I and FR-II sources. Our findings are important to interpretation of next-generation radio survey data.

268

MEASURING THE ENVIRONMENTS OF PROTO-CLUSTERS IN THE HIGH REDSHIFT UNIVERSE Genevieve Shattow

1

1. Swinburne, Hawthorn, VIC, Australia Environment, specifically overdensity, is a common means of identifying proto-clusters in the high redshift universe, but the resulting measurements are highly dependent on both the scale and method used to define overdensity. This leads to three main questions. First, how does a galaxy's "observed" (projected) overdensity in redshift space compare to its three-dimensional overdensity in real-space? In other words, if I measure a simulated galaxy's environment in a method similar to that of an observer, how similar to its real-space environment will it be? The second question is how stable are these comparisons from a statistical point of view? If I look at the same galaxy from several points of view, will its environment change? And third, how does a galaxy's environment change with time - is there a metric that better predicts a galaxy's future environment?

269

THE CHEMICAL EVOLUTION OF HEAVY ELEMENTS IN GLOBULAR CLUSTERS Luke J. Shingles

1 , Amanda I. Karakas

1 , Raphael Hirschi

2 3

1. Research School of Astronomy and Astrophysics, Australian National University, Weston, ACT, Australia 2. Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele, UK 3. Kavli Institute for the Physics and Mathematics of the Universe, University of Tokyo, Bunkyo, Tokyo, Japan We present preliminary results from a chemical evolution model that tracks the composition of elements heavier than iron in a globular cluster. The heavy elements can be used as tracers of the nucleosynthetic events that defined the formation and evolution of star clusters in the early Universe. In particular, the chemical evolution model focuses on the hypothesis that rapidly-rotating massive stars produced the heavy elements via the slow neutron-capture process and seeded the proto-cluster while the stars we see today were still forming. We compare our model with abundances in M4 and M5, which show very different heavy element patterns even though they have the same metallicity [Fe/H] of -1.2. In these clusters, there are no star-to-star variations in the neutron-capture elements, suggesting that whatever stars produced the heavy elements did not also produce the light elements. We also compare our model to the s-rich and s-poor populations in M22.

270

INTEGRATED PHOTONIC LANTERNS WITH GRATINGS: MINIATURE SPECTRAL FILTERS FOR NEAR-INFRARED SPECTROSCOPY Izabela Spaleniak

1 2 , Nemanja Jovanovic

1 2 3 , Simon Gross

2 4 , Michael Ireland

1 2 3 , Jon Lawrence

1 2 3 , Michael

Withford1 2 4

1. University Research Centre in Astronomy, Astrophysics & Astrophotonics, Macquarie University, Sydney, NSW, Australia

2. MQ Photonics research centre, Macquarie University, Sydney, NSW, Australia 3. Australian Astronomical Observatory, North Ryde, NSW, Australia 4. Centre for Ultrahigh Bandwidth Devices for Optical Systems (CUDOS), Sydney, NSW, Australia Near-infrared observations (0.9-2.5 μm) provide valuable information on a multitude of astronomical objects, but ground-based observations at these wavelengths are typically sky-background dominated due to atmospheric OH emission lines. These can be filtered out using a photonic component known as a fibre Bragg grating. As with most photonic components, fibre Bragg gratings are effective only in single-mode fibres, whereas light delivered by


astronomical telescopes is multimodal in nature. The conversion of multimode light into several single-mode signals can be done using a photonic lantern. However, fibre-based photonic lanterns with fibre Bragg gratings are very complex to make. We are developing an integrated, miniature version of both, in which we use the ultrashort laser direct write technique to fabricate photonic lanterns with gratings in nearly a one-step process. Our first results demonstrate the feasibility of such approach. Our devices have uniform and 5 dB strong gratings reflecting 1545 nm and 1552 nm across all the single-mode waveguides of the photonic lantern. We believe that integrated photonic lanterns can highly improve the quality of astronomical data.

271

A DEBRIS DISK AROUND THE PLANET HOSTING M-STAR GJ 581 SPATIALLY RESOLVED WITH HERSCHEL Elodie Thilliez

1 , Jean-François Lestrade

2 , Mark Wyatt

3 , DEBRIS TEAM

4

1. Swinburne University of Technology, Hawthorn, VIC, Australia 2. LERMA, Observatoire de Paris, Paris, FRANCE 3. Institute of Astronomy, University of Cambridge, Cambridge, UK 4. DEBRIS Team, http://debris.astrosci.ca/ The Key Program DEBRIS (Disc Emission via a Bias-free Reconnaissance in the Infrared/Sub-mm) on the Herschel Space Observatory is an unbiased flux-limited survey to search for dust emission at λ = 100 and 160μm toward the nearest ∼89 stars of each spectral type A, F, G, K, M as evidence of debris disks. As part as the observational program, we have spatially resolved the second debris disk around a M-type star at 70, 100 and 160 μm: GJ 581 which is hosting multiple planets. Contrary to the first M-type star dust disk detected surrounding AU Microscopii (Kalas et al. 2004) extending from 50 to 210 AU, GJ 581 is much older (2-8 Gyr), and X-ray quiet in the ROSAT data. We fit an axisymmetric model of the disk to the three PACS images using a power-law and gaussian densities and found that the best fit model is for a disk extending radially from 25 ± 12 AU to more than 60 AU. Such a cold disk is reminiscent of the Kuiper Belt but it surrounds a low mass star (0.3 M⊙ ) and its fractional dust luminosity Ldust /L∗ of ∼ 10−4 is much higher. This may be explained by the fact that dust cannot be expelled from the system by radiation or wind pressures because of the low luminosity and low X-ray luminosity of GJ 581. Hosting at least 4 known planets of low masses and orbiting within 0.3 AU from the star, we suggest that the correlation between low-mass planets and debris disks recently found for G-type stars also applies to M-type stars.

272

ADVENTURES IN THE MICROLENSING CLOUD: ERESEARCH TOOLS FOR ZOOMING INTO THE HEART OF QUASARS Georgios Vernardos

1 , Christopher J Fluke

1

1. Swinburne University of Technology, Hawthorn, Vic, Australia Cosmological gravitational microlensing is an established technique for exploring the structure of the inner parts of a quasar, especially the accretion disk and the central supermassive black hole. Results from studies on ~20 of the ~90 known lensed systems indicate the presence of a thin disk (Eigenbrod et al.2008, Blackburne et al. 2011, Mediavilla et al.2011), although this is not always the case (Floyd et al. 2009, Morgan et al. 2010). Upcoming all-sky synoptic surveys are expected to discover, and monitor regularly, thousands of new microlensed systems. The GPU-Enabled, High-Resolution cosmological MicroLensing parameter survey (GERLUMPH) can be thought of as a theoretical counterpart of an all-sky survey, which explores the microlensing parameter space in preparation for these new discoveries. GERLUMPH's high resolution magnification maps, the basic tool for cosmological microlensing, allow for statistical studies of accretion disk models and comparisons to observations. I will discuss the first GERLUMPH data release of 3060 magnification maps produced using gSTAR, the GPU-Supercomputer for Theoretical Astrophysics Research, and the publicly available eResearch tools which aim to simplify their use.


273

HIGH SPATIAL RESOLUTION OBSERVATIONS OF WATER MASERS IN HOPS Andrew Walsh

1

1. Curtin University, Bentley, WA, Australia I will present results of observations with the Australia Telescope Compact Array towards water masers that were previously observed with by HOPS (the H2O southern Galactic Plane Survey). The ATCA observations can pinpoint the masers with arcsecond accuracy, allowing a more reliable association of the masers with astrophysical sources such as young stellar objects and evolved stars. The morphology of the maser sites can also help us understand the origins of the maser emission.

274

EXPLORING THE URSA MAJOR REGION Kathrin Wolfinger

1

1. Swinburne, Hawthorn, VIC, Australia The Ursa Major region is an ideal target to study the effect of environment on the evolution of gas-rich galaxies as it is nearby and most of the known members are late-type galaxies that are rich in neutral hydrogen (HI). I investigate 480 deg

2 and a heliocentric velocity range from 300-1900 km/s using data from the HI Jodrell All Sky Survey (HIJASS). The

surveyed region includes the Ursa Major cluster (17.1 Mpc3 ), the Canes Venatici groups (4.1 Mpc

1 ) and the less dense

filament connecting the Ursa Major and Virgo cluster (16.7 Mpc2 ).

In this talk I will present an overview of the region: (i) the peak-flux limited catalogue containing 166 HI sources, 10 of which are first time detections in HI including a candidate galaxy/tidal tail/HI stream, (ii) intriguing objects such as HIJASS detections with HI extensions/plumes and (iii) candidate regions for galaxy-galaxy interactions

4 . Furthermore I

will show preliminary results from my studies regarding substructures in the region and their dynamics to investigate if Ursa Major is an unevolved and newly forming cluster in the context of hierarchical structure formation. 1. Karachentsev I. D. et al., 2003, A&A, 398, 467 2. Mei S. et al., 2007, ApJ, 655, 144 3. Tully R. B. et al., 2008, ApJ, 686, 1523 4. Wolfinger K. et al., 2013, MNRAS, 428, 1790

275

THE PHYSICAL CONDITIONS OF THE LUPUS MOLECULAR CLOUDS Graeme F Wong

1 , Nick F. N. Tothill

1 , James Green

2 , Miroslav Filipovic

1 , Shinji Horiuchi

3

1. University of Western Sydney, Penrith, NSW, Australia 2. CSIRO, Sydney 3. CDSCC, Canberra Lupus Molecular Cloud complex, about 150 pc away in the Gould Belt, is one of the closest star-forming regions to us. We present the preliminary results of ammonia inversion transition lines (1,1 and 2,2) from observation data obtained with the Tidbinbilla 70m radio telescope in Lupus I and III regions. These results will allow us to estimate the kinetic temperature of the clouds and characterise the conditions occurring within the region.

276

GIANTS IN VELA: THE HIGH ENERGY TAIL OF VELA'S PULSED RADIO EMISSION Tim Young

1 , Michael Burton

1 , Aidan Hotan

1. University of New South Wales, Sydney, NSW, Australia In a detailed single pulse study of the Vela pulsar, we focus on the energy spectrum of the individual pulses. The large and comprehensive nature of the data collected, involving over 3 million individual pulses, gives the study an unprecedented degree of statistical significance. In devising new methods and metrics with which to analyse the data, we notice a pronounced high energy tail with individual events in excess of 10

3 Jy of peak flux (or a brightness

temperature of the order 1030

K), and systematic changes in pulse morphology at different energy levels. The data also


suggests possible variability in the emission statistics on timescales of days, which may imply that the pulsar magnetosphere is more dynamic than previously thought.

277

PHOTOMETRIC REDSHIFTS: TEMPLATE-BASED VS. EMPIRICAL Christian Wolf

1

1. Australian National University, Canberra, ACT, Australia Photometric redshifts have been with us for two thirds of a century, although they have become scientifically useful only in the last ~15 years. But what drives their precision and reliability and is the state-of-the-art good enough for the surveys of the future? We present some photo-z theory, present a bias-free, empirical KDE approach, discuss their application in large surveys such as RCS2 or DES, requirements for the future and where the OzDES-deep survey could help.


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ATTENDEE LIST Brett Addison University of New South Wales, NSW [email protected]

Shaila Akhter UNSW School of Physics, NSW [email protected]

Mohammad Ali Nawaz ANU, ACT [email protected]

Rebecca Allen Swinburne University, VIC [email protected]

James Allison University of Sydney, NSW [email protected]

Paul Angel University of Melbourne, Vic [email protected]

Michael Ashley University of New South Wales, NSW [email protected]

Carlos Bacigalupo Macquarie University, NSW [email protected]

Matthew Bailes Swinburne University of Technology, Vic [email protected]

Lewis Ball CSIRO, NSW [email protected]

Julie Banfield CSIRO Astronomy and Space Science, NSW [email protected]

Michele Bannister NRC - Herzberg, Canada [email protected]

Amanda Bauer AAO, NSW [email protected]

Daniel Bayliss ANU, ACT [email protected]

Richard Beare Monash Centre for Astrophysics, VIC [email protected]

Georgios Bekiaris Swinburne University of Technology, VIC [email protected]

Martin Bell Sydney University, NSW [email protected]

Maksym Bernyk Swinburne University of Technology, VIC [email protected]

Ramesh Bhat ICRAR, Curtin University, WA [email protected]

Antonio Bibiano Swinburne University, VIC [email protected]

Sarah Bird Tuorla Observatory, University of Turku, Finland [email protected]

Christina Blom Swinburne University, VIC [email protected]

Douglas Bock CSIRO, NSW [email protected]

Nicolas Bonne MoCA, Monash University, VIC [email protected]

Kimberly Bott University of New South Wales, NSW [email protected]

Brian Boyle DIICCSRTE, ACT [email protected]

Mita Brierley Astronomy Australia Ltd, VIC [email protected]

Tui Britton Macquarie University, NSW [email protected]

Kate Brooks CSIRO, NSW [email protected]

Michael Brown Monash University, VIC [email protected]

Sarah Bruzzese ICRAR/UWA, WA [email protected]

Julia Bryant University of Sydney, NSW [email protected]

Craig Burnett University of Melbourne, VIC [email protected]

Donna Burton University of Southern Queensland, NSW [email protected]

Paul Cally Monash University, VIC [email protected]

Russell Cannon AAO, NSW [email protected]

Brad Carter USQ, QLD [email protected]

Andrew Casey RSAA, ANU, ACT [email protected]

Barbara Catinella Swinburne University of Technology, VIC [email protected]

Pierluigi Cerulo Swinburne University of Technology, VIC [email protected]

Michael Childress Australian National University, ACT [email protected]

Kate Chow CSIRO, NSW [email protected]

Patrick Clearwater The University of Melboune, Vic [email protected]

Jordan Collier University of Western Sydney, NSW [email protected]

Jeff Cooke Swinburne University, VIC [email protected]

Joanna Corby University of New South Wales, NSW [email protected]

Camila Correa University of Melbourne, VIC [email protected]

Luca Cortese Swinburne University of Technology, VIC [email protected]

Warrick Couch Swinburne University, VIC [email protected]

David Coward University of Western Australia, WA [email protected]

Roland Crocker ANU, ACT [email protected]

Darren Croton Swinburne University of Technology, VIC [email protected]

Gary Da Costa Australian National University, ACT [email protected]

Ashkbiz Danehkar Macquarie University, NSW [email protected]


Taissa Danilovich Chalmers University of Technology, Sweden [email protected]

Rebecca Davies RSAA, ANU, ACT [email protected]

Joanne Dawson University of Tasmania, TAS [email protected]

Catherine de Burgh-Day The University of Melbourne, VIC [email protected]

Phoebe de Wilt University of Adelaide, SA [email protected]

Helga Denes Swinburne University of Technology, VIC [email protected]

Philip Diamond SKA Organisation, United Kingdom [email protected]

Tim Dolley MoCA, VIC [email protected]

Valentina D'Orazi Macquarie University, NSW [email protected]

Dimitri Douchin Macquarie University / Universite Montpellier 2, NSW [email protected]

Danica Draskovic Macquarie University, NSW [email protected]

Marc Duldig University of Tasmania, Tas [email protected]

Vincent Dumont UNSW School of Physics, NSW [email protected]

Mark Durre Swinburne University of Technology, VIC [email protected]

Jamie Farnes SifA, NSW [email protected]

Sean Farrell The University of Sydney, NSW [email protected]

Tobias Feger Macquarie University, NSW [email protected]

Michael Fitzgerald Macquarie University, NSW [email protected]

Christopher Fluke Swinburne University of Technology, VIC [email protected]

Bi-Qing For ICRAR/UWA, WA [email protected]

Amelia Fraser-McKelvie Monash University, VIC [email protected]

Bryan Gaensler The University of Sydney, NSW [email protected]

Duncan Galloway Monash University, VIC [email protected]

Karl Glazebrook Swinburne University, VIC [email protected]

Gregory Goldstein Univ Western Sydney, NSW [email protected]

Ioannis Gonidakis CSIRO, NSW [email protected]

Andy Green Australian Astronomical Observatory, NSW [email protected]

Anne Green University of Sydney, NSW [email protected]

James Green CSIRO Astronomy and Space Science, NSW [email protected]

Claire Elise Green UNSW School of Physics, NSW [email protected]

Duane Hamacher University of New South Wales, NSW [email protected]

Elise Hampton RSAA, ANU, ACT [email protected]

Paul Hancock University of Sydney, NSW [email protected]

Lisa Harvey-Smith CSIRO, NSW [email protected]

Alexander Heger Monash University, VIC [email protected]

Tracey Hill Joint ALMA Observatory, Chile [email protected]

Alex Hill CSIRO Astronomy & Space Science, NSW [email protected]

Tanya Hill Museum Victoria, VIC [email protected]

Andrew Hopkins Australian Astronomical Observatory, NSW [email protected]

Laura Hoppmann ICRAR/UWA, WA [email protected]

Jonathan Horner UNSW School of Physics, NSW [email protected]

Aidan Hotan CSIRO, NSW [email protected]

Eric Howell University Western Australia, WA [email protected]

Louise Howes Australian National University, ACT [email protected]

Richard Hunstead Sydney Institute for Astronomy, NSW [email protected]

Natasha Hurley-Walker Curtin Institute of Radio Astronomy, WA [email protected]

Minh Huynh University of Western Australia, WA [email protected]

Roberto Iaconi Macquarie University, NSW [email protected]

Michael Ireland Australian Astronomical Observatory, NSW [email protected]

James Jackson Boston University, United States [email protected]

Andrew Jacob Sydney Observatory, NSW [email protected]

Akila Jeeson-Daniel University of Melbourne, Vic [email protected]

Heath Jones Monash University, VIC [email protected]

Christopher Jordan University of Tasmania, TAS [email protected]

Shahab Joudaki Swinburne University, VIC [email protected]

Glenn Kacprzak Swinburne University of Technology, VIC [email protected]


Amanda Karakas Australian National University, ACT [email protected]

Sreeja Kartha Swinburne University, VIC [email protected]

Antonios Katsianis University of Melbourne, VIC [email protected]

Champlain Kenyi University of NSW,Sydney, NSW [email protected]

Markus Kissler-Patig Gemini Observatory, United States [email protected]

Dane Kleiner Monash University, VIC [email protected]

Jun Koda Swinburne University of Technology, VIC [email protected]

Iraklis Konstantopoulos Australian Astronomical Observatory, NSW [email protected]

Kyler Kuehn AAO, NSW [email protected]

Nathanael Lampe Monash University, VIC [email protected]

Paul Lasky University of Melbourne, VIC [email protected]

Emil Lenc University of Sydney, NSW [email protected]

Sarah Leslie Research School of Astronomy and Astrophysics, ACT [email protected]

Karen Lewis Tokyo Institute of Technology, Japan [email protected]

Jack Line University of Melbourne, VIC [email protected]

Chuanwu Liu The University of Melbourne, VIC [email protected]

Nick Lomb Sydney Observatory, VIC [email protected]

John Lopez UNSW School of Physics, NSW [email protected]

Vicki Lowe University of New South Wales, CSIRO Astronomy and Space Science, NSW [email protected]

Maria Lugaro Monash University, VIC [email protected]

Katherine Mack University of Melbourne, VIC [email protected]

Damien Macpherson ICRAR, WA [email protected]

Sarah Maddison Swinburne University, VIC [email protected]

Stephen Marsden USQ, QLD [email protected]

Sarah Martell Australian Astronomical Observatory, NSW [email protected]

Nigel Maxted The University of Adelaide, SA [email protected]

Mark McAuley Astronomy Australia Ltd, VIC [email protected]

Naomi McClure-Griffiths CSIRO Astronomy & Space Science, NSW [email protected]

Benjamin McKinley Australian National University, ACT [email protected]

Bernard Meade Swinburne University of Technology, Vic [email protected]

Scott Meyer ICRAR, WA [email protected]

Matthew Middleton University of Amsterdam, Netherlands [email protected]

Jeremy Mould Swinburne, VIC [email protected]

Guido Moyano Loyola Swinburne University of Technology, VIC [email protected]

Michael Murphy Swinburne University of Technology, VIC [email protected]

Simon Mutch The University of Melbourne, VIC [email protected]

Themiya Nanayakkara CAS, VIC [email protected]

Colin Navin Macquarie University, NSW [email protected]

Daniel Neri-Larios The University of Melbourne, Vic [email protected]

Belinda Nicholson University of Melbourne, Vic [email protected]

Robert Nilsson Monash University and Lulea University of Technology, Sweden, VIC [email protected]

John O'Byrne Sydney Institute for Astronomy, The University of Sydney, NSW [email protected]

Paola Oliva-Altamirano Swinburne University of Technology, VIC [email protected]

Daniela Opitz UNSW School of Physics, NSW [email protected]

Samuel Oronsaye ICRAR/Curtin University, WA [email protected]

Christopher Owen Australian National University, ACT [email protected]

Sinem Ozbilgen University of Melbourne, VIC [email protected]

David Palamara MoCA (Monash Centre for Astrophysics), VIC [email protected]

Jaehong Park The University of Melbourne, VIC [email protected]

Quentin Parker Macquarie University/AAO, NSW [email protected]

Nicola Pastorello Swinburne University, VIC [email protected]

Francesco Pignatale Swinburne University of Technology, Vic [email protected]

Kevin Pimbblet Monash University, Vic [email protected]

Christophe Pinte UMI-FCA Santiago, Chile [email protected]

Gregory Poole University of Melbourne, VIC [email protected]


Benjamin Pope Sydney Institute for Astronomy, NSW [email protected]

Chris Power University of Western Australia, WA [email protected]

Shakya Premachandra Monash University, VIC [email protected]

Andrew Prentice Monash University, VIC [email protected]

Peter Quinn International Centre for Radio Astronomy Research (ICRAR), WA [email protected]

Hayden Rampadarath ICRAR, Curtin University, WA [email protected]

Jill Rathborne CSIRO Astronomy and Space Science, NSW [email protected]

Glen Rees Macquarie University, NSW [email protected]

Nastaran Rezaee University of Melbourne, VIC [email protected]

Luciano Rezzolla Max-Planck Institute for Gravitational Physics, [email protected]

Jennifer Riding University of Melbourne, VIC [email protected]

Aaron Rizzuto Macquarie University, NSW [email protected]

Peter Robertson University of Melbourne, VIC [email protected]

Gavin Rowell University of Adelaide, SA [email protected]

Emma Ryan-Weber Swinburne University, VIC [email protected]

Stuart Ryder Australian Astronomical Observatory, NSW [email protected]

Giulia Savorgnan Swinburne University of Technology, VIC [email protected]

Richard Scalzo Australian National University, ACT [email protected]

Antony Schinckel CSIRO, NSW [email protected]

Sarah Schon University of Melbourne, VIC [email protected]

Nicholas Scott Swinburne University of Technology, VIC [email protected]

Paul Scott-Taylor University of WA, WA [email protected]

Katrina Sealey Australian Astronomical Observatory, NSW [email protected]

Stas Shabala University of Tasmania, TAS [email protected]

Genevieve Shattow Swinburne, VIC [email protected]

Luke Shingles Australian National University, ACT [email protected]

Doug Simons CFHT, United States [email protected]

Roberto Soria Curtin University, WA [email protected]

Izabela Spaleniak Macquarie University, NSW [email protected]

Lee Spitler Australian Astronomical Observatory / Macquarie University, NSW [email protected]

Jan Staff Macquarie University, NSW [email protected]

Lister Staveley-Smith University of Western Australia, WA [email protected]

Sarah Sweet University of Queensland, Qld [email protected]

Anant Tanna UNSW School of Physics, NSW [email protected]

Edoardo Tescari University of Melbourne, VIC [email protected]

Steven Tingay Curtin University, WA [email protected]

Luis Alberto Torres CAS Swinburne, VIC [email protected]

Michele Trenti University of Cambridge, United Kingdom [email protected]

Cathryn Trott Curtin University, WA [email protected]

Syed Uddin CAS, Swinburne, VIC [email protected]

Christopher Usher Swinburne University of Technology, VIC [email protected]

Georgios Vernardos Swinburne University of Technology, VIC [email protected]

Andrew Walsh Curtin University, WA [email protected]

Randall Wayth Curtin University, WA [email protected]

Rachel Webster University of Melbourne, VIC [email protected]

Christian Wolf ANU, ACT [email protected]

Kathrin Wolfinger Swinburne, VIC [email protected]

Graeme Wong University of Western Sydney, NSW [email protected]

Hauke Worpel MoCA, VIC [email protected]

Duncan Wright UNSW, NSW [email protected]

Angus Wright ICRAR/UWA, WA [email protected]

Stuart Wyithe University of Melbourne, Vic [email protected]

Tim Young University of New South Wales, NSW [email protected]

Fang Yuan Australian National University, ACT [email protected]


INDEX OF ABSTRACT AUTHORS (by abstract number) Addison, B 80 Adermann, E 201 Akhter, S 202 Aldering, G 266 Ali Nawaz, M 203 Allen, R 204 Allison, J.R 56 Alves-Brito, A 63 Andre, P 48 Angelou, G 215 Antilogus, P 266 Appleton, P.N 75 Aragon, C 266 Arzoumanian, D 48 Ashley, M.C 52 Asplund, M 228 ATLAS Team 3 Atteia, J 37 Bailes, M 100 Bailey, J 81,237 Bailey, S 266 Baltay, C 266 Banfield, J 3, 213 Bannister, M 8 Barnes, D 16 Basa, S 37 Bayliss, D 78 Bcool Collaboration 245 Beare, R 205 Bekiaris, G 206 Bekki, K 19 Bell, M 25 Benjamin, R.A 227 Bento, J 219 Bhat, R.N 254 Bicknell, G 203 Bird, S 207 Blake, C 43 Blom, C 20 Boer, M 37 Bongard, S 266 Bonne, N.J 77 Bott, K 81 Boyle, B 31 Bragaglia, A 215 Breen, S 53 Briggs, F 15 Briley, M.M 73 Britton, T 208 Brooks, G 11 Brough, S 6 Brown, C 245 Brown, M 77, 84, 98, 205,

209, 255 Bruzzese, S 210 Bryant, J 2 Builders List, M 15 Burton, D.M 60 Burton, M 52, 246,276 Buton, C 266 Cally, P 59 Calrberg, R 42 Canto, A 266

Cappellari, M 74 Carretta, E 215 Carretti, E 53 Carter, B 60, 245 Casares, J 93 Casassus, S 82 Casey, A 63 Caswell, J 50,53 Catarina, U 47 Catinella, B 12 Cellier-Holzem, F 266 Cerulo, P 211 Childress, M 46, 266 Chotard, N 266 Chow, K.E 212 Churchill, C.W 85 Cluver, M.E 75 Colless, M 41 Collier, J.D 213 Cooke, J 42 Copin, Y 266 Cornelisse, R 93 Correa, C 214 Cortese, L 5 Cotton, D.V 237 Couch, W 6,211 Coward, D 37 Crawford, E 223 Crocker, R 39 Crossett, J.P 76 Croton, D 17 Cunningham, M 53,244 Curran, J.R 54 Cutini, S 37 D'Elia, V 37 D'Orazi, V 215 Da Costa, G 21,63 Danehkar, A 216 Danilovich, T 58 Davies, R 69,74 Davis, T 43 Dawson, J 53 de Wilt, P 95 DEBRIS TEAM 271 DeMarco, o 217 Denes, H 19,55 Diamond, P 32,64 Diaz, G 42 Dickey, J 53 Didelon, P 48 Dolley, T 84 Donea, A.C 253 Dopita, M.A 69 Dopital, M.A 241 Douchin, D 217 Drinkwater, M.J 19 Duffau, S 73 Duffy, A 214 Durre, M 218 Ellingsen, S 53,235 Ellis, R 42 Eric, P 47 Fakhouri, H 266

Farrell, S 91,201 Feain, I 15 Feger, T 219 Filipovic, M 213,223,275 Fitzgerald, M.T 220 Floyd, D 68 Fluke, C 16,247,272 Flynn, C 207 For, B 221 Foster, C 222 Foster, J 231 Fraser-McKelvie, A 68 Frebel, A 63 Freeman, K 63 Freudling, W 4 Fukuda, T 246 Fukui, Y 246 Funk, S 225 Gaensler, B 15,91,226 Gal-Yam, A 42 Galloway, D.K 93,94 Gangler, E 266 Gendre, B 37 Gibson, B.K 242 Gibson, S 53 Glazebrook, K 204 Godfrey, L 267 Goldstein, G 223 Gomez, J 53 Gonidakis, I 64 Goodwin, M 224 Graham, A.W 74,265 Gratton, R 215 Grebel, E.K 73 Green, A 13,201 Green, J 50,53,275 Grise, F 92 Gross, S 270 Guy, J 266 Haines, C 68 Hamacher, D 66,208 Hampton, E 225 Hancock, P.J 226 Harris, W.E 207 Harvey-Smith, L 30,50 Heger, A 36 Hennebelle, P 53 Hill, A.S 227 Hill, T 48 Hirschi, R 269 HITRUN TEAM 100 Hopkins, A 103,230 Hoppmann, L 4 Horachi, H 246 Horiuchi, S 275 Horner, J 10 Horns, D 225 Horst, C 42 Hotan, A 276 Houghton, R 74 Howell, E 37 Howes, L.M 228 Hsiao, E 266


Hunstead, R.W 229 Hurley, J 250 Hurley-Walker, N 27 Huynh, M 230 Ida, S 79 Imai, H 53 Ireland, M 51,65,219,270 Jackson, J 231 Jacob, A 232,233 Jacobson, H 63 Jarrett, T.H 75,213 Jean-Francois, G 47 Jeeson-Daniel, A 234 Jeffers, S 245 Jenkins, J.S 264 Jensen, P 258 Johnson, A 43 Johnston, H.M 229 Jones, C 53 Jones, D.H 238 Jones, H 41,76,264 Jones, P 53 Jordan, C.H 235 Jovanovic, N 270 Justtanont, K 58 Kacprzak, G 85,204 Kankare, E 263 Karakas, A 62,63,269 Kartha, S 236 Katsianis, A 89 Kawamura, A 246 Kedziora-Chudczer, L 81, 237 Keller, S 63,228 Kemball, A 64 Kenyi, C 237 Kerschhaggl, M 266 Kewley, L.J 69,241 Kilborn, V 19 Kimball, A 213 Kissler-Patig, M 61 Kleiner, D 238 Klotz, A 37 Kobayashi, C 38 Koda, J 43 Konstantopoulos, I 7 Koribalski, B 238 Kowalski, M 266 Krishnan, V 53 Kromer, M 266 Kuehn, K 102 Kulesa, C.A 52 Kummerfeld, J.K 54 Lange, R 239 Lasky, P 240 Lawrence, J 270 Lazendic, J 246 Lenc, E 28,230,261 Leslie, S.K 241 Lestrade, J 271 Lewis, K.M 79,242 Lidman, C 6,211 Liffman, K 11 Lineweaver, C 35 Lister Staveley-Smith, L 4 Lo, K 91 Lo, N 53

Lockman, F.J 227 Lonsdale, C.J 213 Lopez, J.A 243 Lowe, V 53,235,244 Lucatello, S 215 Lugaro, M 242 Maddison, S 11,49,82 Magoulas, C 41 Mao, M 230 Mao, S 50,227 Marsden, S 60,245 Marsh, T 93 Martell, S.L 73 Mattila, S 263 Maxted, N 246 McClure-Griffiths, N 50,53, 54, 227 McKinley, B 15 Meade, B 247 Menard, F 47,49 Meurer, G 19 Meyer, M 248,249 Meyer, S.A 249 Middelberg, E 230 Milone, A.P 73 Morgan, J.S 261 Moss, V.A 54 Motch, C 92 Motte, F 48 Mould, J 41,218 Moyano Loyola, G 250 Murphy, T 54,91,226 Murray, S 259 Mutch, S.J 97 MWA EoR Collaboration 24 Nanayakkara, T 251 Nicholas, B 246 Nicholson, B.A 252 Nielsen, N.M 85 Nilsson, R 253 Norris, R 213, 230 Nugent, P 266 O'Toole, S 264 Obreschkow, D 248,249 Ogle, P 75 Oliva-Altamirano, P 6 Olofsson, H 58 Omori, Y 42 Ord, S.S 254 Oronsaye, S.S 254 Paech, K 266 Pain, R 266 Pakull, M.W 92 Palamara, D 255 Park, J 44 Parker, Q 83,216 Pastorello, N 256 Pecontal, E 266 Penny, S 18,257 Pereira, R 266 Perlmutter, S 266 Petit, P 245 Pietrzynski, G 92 Pignatale, F 11 Pilkington, K 242 Pimbblet, K 68,74,76,

205,238, 258

Pinte, C 47 Piro, L 37 Pisano, D 54 Podsiadlowski, P 38 Poole, G 45 Pope, B 70 Power, C 96,259 Premachandra, S.S 93 Prentice, A.J 260 Price, D.J 94 Purcell, C 53 Rabinowitz, D 266 Rampadarath, H 261 Randall, K 230 Rasmussen, J 75 Rathborne, J 231 Rees, G 262 Reeves, S 14 Rezzolla, L 40 Rich, J.A 69,241 Rigault, M 266 Rizzuto, A.C 51 Robishaw, T 50 Robotham, A 259 Rowell, G 95,225,246 Runge, K 266 Russell, T.D 90 Ryan-Weber, E 42 Ryder, S 263 Sadler, E 14, 56 Salter, G.S 264 Sano, H 246 Sarah, M 47 Sato, B 79 Saunders, C 266 Savorgnan, G 265 Scalzo, R 38,266 Schaefer, A.L 229 Schimidt, B.P 38 Schinckel, A 29 Schlaufman, K 63 Schnitzeler, D.H 213 Scott, N 74 Scrimgeour, M 43 Shabala, S 67,68,267 Shattow, G 268 Shingles, L.J 269 Sim, S 38,266 Simons, D 104 Smadja, G 266 Smith, G.H 73 Soria, R 92 Spaleniak, I 270 Spitler, L 86,204 Springob, C 41,43 Staff, J.E 57 Staveley-Smith, L 34 Steeghs, D 93 Stevenson, T 232, 233 Storey, J.W 52 Stott, J.P 76 Stratta, G 37 Sullivan, M 42 Survey, T 72 Sweet, S.M 19 Tao, C 266


Taubenberger, S 266 Taylor, E 6,252 Tescari, E 88,89 Thilliez, E 271 Thomas, R 266 Tingay, S 22,254,261 Tinney, C 9,65,80,264 Tothill, N 223,275 Tremblay, S.S 254 Trenti, M 87 Trott, C 26 Ubach, C 49 Uchiyama, Y 225 Usher, C 72 Valtonen, M 207

Vernardos, G 272 Voronkov, M 235 Wagner, A 203 Wagner, S 225 Walsh, A 53,235,246,273 Wayth, R 23 Weaver, B 266 Webster, R 1,24,252 Whitaker, S 231 Windhorst, R.A 101 Wisnioski, E 99 Withford, M 270 Wittenmyer, R 9,10,264 Wolf, C 277 Wolfinger, K 274

Wong, G.F 275 Worpel, H 94 Wright, C 49,82 Wright, D 9,80 Wu, C 266 Wyatt, M 271 Wyithe, J 89 Wyithe, S 33,71,214 Yong, D 63 Yoshiike, S 246 Young, T 276 Yu, Q 63 Yuan, F 38

astronomical society of australia annual scientific meeting

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