ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) XMM-Newton: the next decade, May 2016

Netherlands Institute for Radio Astronomy

Synergy with new radio facilities: from LOFAR to SKA

Raffaella Morganti

ASTRON (NL) and Kapteyn Institute (Groningen)

Friday, 13 May 16

New generation radio telescopes

Major new capabilities of radio telescopes:

★ large field of view

★ broad instantaneous band

★ fast response

Commensality of the observations ➜ allow a variety of different science using one pointing

New possibilities for the science ➜ but huge datasets and need for pipelines

Availability of ancillary data very important! Coordination with other facilities/telescopes essential for success

Many sq deg in one pointing! with high spatial resolution

HI over large redshift, spectral properties, magnetism

Transient events

Friday, 13 May 16

New Radio Facilities Frequencies Surveys? Status

LOFAR North 40 - 200 MHz Yes Operational Cycle 6

Apertif-WSRT North 1.15 - 1.7 GHz Yes Close to completion Commissioning

MWA South 74 - 230 MHz Yes Operational

ASKAP South 0.7 - 1.8 GHz Yes Close to completion Commissioning

MeerKAT South 00.6 – 1.0 GHz 1.0 – 1.7 GHz

Large areas, famous fields

Close to completion Commissioning

Square Kilometre Array - SKA

HI

HI

HI

Friday, 13 May 16

Some new (low spatial resolution) surveys

Frequencies

Resolution

Web site References

MSSS: Multifrequency Snapshot Sky Survey (MSSS)- LOFAR

150 MHz http://vo.astron.nl/ Heald et al. 2015

http://arxiv.org/abs/1509.01257

GLEAM: The GaLactic and Extragalactic All-sky MWA survey

150MHz

2.5arcmin

http://mwatelescope.org/astronomers/public-data-release

http://arxiv.org/abs/1505.06041Wayth, et al. 2015

TGSS - GMRT 150MHz

~25 arcsec

http://tgssadr.strw.leidenuniv.nl/doku.php http://arxiv.org/abs/1603.04368

Intema et al. 2016

Observations often taken in different epochs to enable also search for transients

Friday, 13 May 16

The LOw Frequency ARray

• Transients Key Science Project ➜ PIs: Rob Fender, Ben Stappers, Ralph Wijers

• Imaging surveys Key Science Project ➜ PI: Huub Rottgering

• Unique because:

38 stations in NL spread over ~100 km 12 international stations

➜ high spatial resolution (arcsec to subarcsec) at low freq (~40-200 MHz) and large field of view

High Band Antenna Low Band Antenna

Friday, 13 May 16

LOFAR imaging SURVEYS• PI: Huub Rottgering (Leiden)

co-I: Miley, Brugger, Brunetti, Best, Morganti, Jackson, White, Jarvis, Conway, Chyzy, Barthel, Lehnert

• Goals @ 150MHz: all northern sky, 8h per pointing, 5” images with 100 µJy/beam noise

• Entering production mode (leading the data reduction: Tim Shimwell, Leiden)

➜ where are we now? relatively easy to reach 20” HBA (@150MHz), major progress on the pipeline to reach higher resolutions; LBA (~60MHz) more difficult (calibration issues)

• synergy with (slow)transients ➜ more than one observation per pointing in different epochs

Friday, 13 May 16

Example of the Boötes field at 150MHz with 5” resolution

Williams et al. MNRAS 2016 astro-ph/1605.01531

One pointing: 6546 sources detected over

an area of 19deg2

~4 d

egre

es

Some of the famous fields first targets for LOFAR

A number of famous fields done: Lockman Hole (Mahony et al.), HETDEX (Shimwell et al.), XMM-LSS (Best et al.), Herschel-ATLAS (Hardcastle et al.) etc.

Friday, 13 May 16

Energetics of radio galaxies: combining X-ray and low-frequencies spectral information

X-ray providing an indipendent way to derive the magnetic field strength (for IC process)

➜ need constraints for spectrum at low frequencies (seeds electrons)

radio obs

synchrotron

IC-CMB

X-ray obs

SSC3C452

3C223N

Harwood et al. 2016 MNRAS arXiv:1603.04438

The total lobe energy density is greater than previous estimates

LOFAR @ 150MHz

Characterise the entire radio galaxy/starburst population (not only the most powerful radio galaxies!)

Morganti, Hardcastle, Rottgering et al. Friday, 13 May 16

Clusters and cluster relics

Duy Hoang et al. in prep

Abell 2034, Shimwell et al. 2016 astro-ph/1603.06591

Searching for new clusters and cluster relics

Brugger, Brunetti, Rottgering et al. Friday, 13 May 16

LOFAR transients (http://www.transientskp.org/)

•in imaging ➜ slow transients, fast transients (still to come)

• AARTFAAC (will send real-time alert, PI: Ralph Wijers )

Amsterdam—ASTRON Radio Transients Facility and Analysis Centre

http://www.aartfaac.org all sky monitor at low spatial resolution

•in time-domain ➜ e.g. pulsars

•Transients Key Science project ➜ PI Rob Fender, Ben Stappers, Ralph Wijersall time-variable astronomical radio sources, including pulsars, gamma-ray bursts, fast radio bursts, X-ray binaries, radio supernovae, flare stars, exo-planets.

Including a Multi-Messenger Follow-Up Working Group

soon we will be able to trigger from radio transients and accurate locate their positions

Friday, 13 May 16

AARTFAAC&–&a&real,-me&sky&monitor&

Credit:&Mark&Kuiack&Prasad&et&al.&(2014),&Cendes&et&al.&(in&prep)&

PI Ralph Wijers

Friday, 13 May 16

The$first$low$frequency$transient$(LOFAR$NCP)$

0h1h2hRight Ascension (J2000)

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2011-12-24 04:18:05

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2011-12-24 04:33:05

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2011-12-24 04:48:05

23h

Right Ascension (J2000)

+86°10'

20'

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Stewart$et$al.$(2015)$Frequency$57$MHz$DuraIon$~4$minutes$

Friday, 13 May 16

• Fast transients: responsive telescope needed

• No movable parts, MWA already fast response but low spatial resolution, LOFAR not so fast yet (day?) preparing for real time alert!

GRB, FRB, GW Explore a range of different timescales for triggered transient searches with LOFAR

from Antonia Rowlinson

Friday, 13 May 16

Kaplan,'Rowlinson'et'al.'(2015)'

0 200 400 600 800 1000 1200 1400 1600 1800Time Since GRB (s)

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•  26'seconds'aFer'GRB'•  10'seconds'aFer'VOEvent'•  RedshiF'>'0.7'

60 70 80 90 100 110 120 130 140 150Frequency (MHz)

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Observa(ons  started  26s  a.er  the  GRB  occurred  (10s  a.er  the  alert  was  received)

A  telescope  with  no  moving  parts    no  slew  =me  limita=ons

Kaplan,  Rowlinson  et  al.  (2015)

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GRB, FRB, GW

Antonia Rowlinson et al. Friday, 13 May 16

X-ray dim, un-pulsed

X-ray bright, pulsed

Radio bright

Pulsar magnetospheric mode switchingHermsen et al. 2013, Science

Radio dim

“B-Mode”

“Q-Mode”

Discovery of correlated radio/X-ray mode switching

XMM+LOFAR+GMRT

Indicating global changes to the conditions in the magnetosphereFriday, 13 May 16

➜

Possibilities at GHz frequencies ‣ New instruments: Apertif (NL), ASKAP (Aus), Meerkat (SA)

‣ Apertif (FoV~8 sqdeg, PIs: T. Oosterloo, M. Verheijen) complementary to LOFAR for continuum and for transients

‣ Search for HI

Apertif system @ WSRT z = 0.44 HI

Allison et al. (2015; arXiv:1503.01265)

example from ASKAP

Friday, 13 May 16

traced by X-ray ➜ winds from accretion disks (Tombesi et al., Pounds et al., see Cappi talk tomorrow)

traced on larger scale by HI absorption?

➜ large HI absorption surveys may provide targets of outflows for X-ray follow-up

Case of Mrk231 Tom

bes

i et

al. 2

012

Morganti et al. 2016

AGN-driven outflows Feruglio et al. 2015

21cm HI absorption

~1300 km/s

Friday, 13 May 16

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Square Kilometre Array (SKA1)

• combines all capabilities (and more) of the pathfinders with extra sensitivity

• ongoing preparatory negotiation for Intergovernmental Organisation

How will the time allocation work? Key Science Projects and based on the contribution of the countries

SKA low - WAustralia

SKA high - South Africa

http://pos.sissa.it/cgi-bin/reader/conf.cgi?confid=215Advancing Astrophysics with the Square Kilometre Array

Friday, 13 May 16

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Conclusions

•SKA 1 is coming: more opportunities, involvement in the preparation of the surveys is welcome!

• Many new possibilities with the present/upcoming radio facilities• New large surveys in continuum and line• Transients ➜ in the future we will have a “two-ways” synergy

•A better coordination between radio and X-ray (and in particular XMM) observations may result in larger and less biased samples of interesting objects and provide an important synergy valuable to both communities

Friday, 13 May 16