the hst frontier fields program · acs - wfc3/ir in parallel; do 180-degree swap ~6 months later...

The HST Frontier Fields Program, Anton Koekemoer (STScI), STUC, 17 Oct 2013

intrinsically deepest and widest survey

of high-redshift universe (sneak peak at JWST’s universe

with Hubble now)

The HST Frontier Fields program www.stsci.edu/hst/campaigns/frontier-fields

PI: Matt Mountain

Co-PI: Jennifer Lotz Science Data Products Lead: Anton Koekemoer Implementation Technical Lead: Norman Grogin

Lensing Map Models Coordinator: Dan Coe +

STScI Frontier Fields Implementation Team


ACS (optical) = 537 orbits WFC3 (IR) = 253 orbits

= 790 orbits of HST

how to do better than Hubble Ultra Deep Field (before JWST)?

HST Ultra Deep Field: Main ACS and WFC3 programs led by Beckwith et al., Illingworth et al., Ellis et al., Teplitz et al.; final mosaics include data from programs led by Giavalisco et al., Faber, Ferguson et al., Perlmutter et al., Riess et al.

Matt: how to do better than Hubble Ultra Deep Field (before JWST)?

James Bullock (Chair, UCI), Mark Dickinson (NOAO), Steve Finkelstein (UT), Adriano Fontana ( INAF, Rome), Ann Hornschemier Cardiff (GSFC), Jennifer Lotz (STScI), Priya Natarajan (Yale), Alexandra Pope (UMass), Brant Robertson (Arizona), Brian Siana (UC-Riverside), Jason Tumlinson (STScI), Michael Wood-Vasey (U Pitt)

HDFI SWG: use Hubble + nature’s telescopes x 6 (strong lensing clusters) ⇒ Go intrinsically deeper than HUDF ⇒ Go wider than HUDF+parallels 6 Lensed Fields + 6 parallel “Blank Fields” = New Parameter Space



HST Frontier Fields: Science Goals

HDFI SWG: •  probe galaxies 10-100x intrinsically fainter than any seen before (especially at z~5-10) •  characterize the stellar populations of high-redshift galaxies intrinsically faint enough to be the early progenitors of the Milky Way •  enable astrophysics on highly-magnified galaxies at z>8 (spatially resolved sizes and internal structures, follow-up spectroscopy) •  perform statistical studies of z>5 star-forming galaxies, including sizes and structures


Community: •  get detailed maps of dark matter in clusters; test DM substructure predictions •  use 100s of multiple lensed images as independent probe of distance, DE •  deep and high-spatial resolution studies of z~1-4 galaxies, including UV escape fraction, sub-kpc structures and star-formation •  study distant transients (SNe, AGN); possibility of using time delays of multiplied images transients as cosmology probe •  counting z~10 galaxies as a test of DM ( rule out Warm Dark Matter?)

HST Frontier Fields: Science Goals


STScI Core Implementation Team PI - Matt Mountain Lead, Co-PI - Jennifer Lotz Implementation Technical Lead - Norman Grogin Team: Denise Taylor, Patricia Royle, David Adler, Ian Jordan, Alan Welty, Bill Workman Science Data Products Lead - Anton Koekemoer Team: Roberto Avila, Jay Anderson, Elizabeth Barker, Andy Fruchter, Shireen Gonzaga, Derek Hammer, Bryan Hilbert, Ray Lucas, Jennifer Mack, Sara Ogaz, Massimo Robberto, Josh Sokol Lensing Map Coordinator - Dan Coe Team: Elizabeth Barker, Scott Fleming, Anton Koekemoer, Karen Levay, Lou Strolger Web/Blog Master - Elizabeth Barker Instrument Team Liasons - John MacKenty, Norman Grogin, Linda Smith, Janice Lee STScI Science Advisors - Larry Bradley, Stefano Casertano, Harry Ferguson, Helmut Jenkner, Jason Tumlinson External Science Advisors - James Bullock, Mark Dickinson, Priyamvada Natarajan, Johan Richard, Adi Zitrin Program Advisory Council - Neill Reid, Ken Sembach, Bob Williams OPO/Citizen Science team - Carol Christian, Brandon Lawton, Alex Viana, Tony Darnell, Hussein Jirdeh, Max Mutchler, Ray Villard, Donna Weaver Spitzer Implementation Team - Peter Capak, Jason Surace, Lisa Storrie-Lombardi Admin Support - Ana-Maria Valenzuela

HST Frontier Fields Implementation Team


HST Frontier Fields: Clusters Initial list of ~16 clusters provided by HDFI SWG based solely on lensing properties; additional suggestions and feedback solicited from the community Selection Criteria - Strongest Lensers (# z~10 galaxies magnified to H=27 within WFC3/IR FOV) based on lensing models by Johan Richard, Adi Zitrin, analyzed by Dan Coe - Observable with HST, Spitzer, JWST checked HST guide star availability, ~30 day position angle hold, Spitzer bright stars/schedule, checked against JWST proto-type scheduler - Low zodiacal background and Galactic extinction - Blank field locations selected avoid bright stars, cluster structures - Observable with ALMA, Mauna Kea - Existing ancillary data (shallow HST, MIPS 24 micron, Herschel, IRAC, Chandra, SZ .. ) - Suitability for deep radio observations


The HST Frontier Fields Clusters Abell 2744 MACSJ0416.1-2403 MACSJ0717.5+3745

MACSJ1149.5+2223. Abell370 Abell S1063


The HST Frontier Fields Clusters

5/6 clusters observable from Mauna Kea; 5/6 cluster observable with ALMA

(aka Abell S1063)


6 strong-lensing clusters + 6 adjacent parallel fields

140 HST DD orbits per pointing ACS/ WFC3-IR in parallel

~29th ABmag in 7 bands 2 clusters per year x 3 years

→ 840 total orbits

1000 hours Spitzer DD time for

~26th ABmag in IRAC 3.6, 4.5 μm

WFC3/IR

ACS

Cluster

Blank Field


HST Prime and Parallel Observations Abell 2744 MACSJ0416.1-2403 MACSJ0717.5+3745

MACSJ1149.5+2223. Abell 370 Abell S1063

many fields have bright stars Gemini GEMS AO K-band of MACS0416.1-2403 planned


HST Frontier Fields: Filters and Depth ACS - WFC3/IR in parallel; do 180-degree swap ~6 months later Imaging in 7 bands to AB~28.7 (5σ point source, 0.4” diameter ap), 140 orbits per field ⇒ 840 orbits for 6 fields ACS: (70 orbits per position) F435W: 18 orbits, 28.8 ABmag F606W: 10 28.8 F814W: 42 29.1 WFC3/IR: (70 orbits per position) F105W: 24 orbits, 28.9 ABmag F125W: 12 28.6 F140W: 10 28.6 F160W: 24 28.7 deep multi-band imaging needed to identify z~3-12 galaxies via Lyman break


HST Frontier Fields Schedule

first HST Frontier Fields DD observations this fall first Spitzer Frontier Fields DD observations in September decision on Cycle 23 observations expected in Dec. 2014

Abell S1063


Data and High-Level Science Products

•  Raw, calibrated exposures: available immediate from archive •  Cumulative full-depth HST mosaics:

•  plan to release weekly cumulative-depth v0.5 mosaics •  release full-depth, best-calibration v1.0 end of each epoch •  incorporate all other existing images for each filter •  registered onto a common pixel grid •  astrometric alignment onto SDSS, 2MASS, previous CLASH

astrometry •  Most up-to-date processing and calibration:

•  Drizzlepac: Astrodrizzle, Tweakreg, and related software •  ACS self-calibration (Anderson et al. algorithms) •  Improved WFC3/IR data (persistence masking, variable sky)


HST Frontier Fields: Data Pipeline Team

•  Anton Koekemoer (FF Science Data Products Pipeline lead) •  Jennifer Mack (RIAB coordination, testing lead) •  Roberto Avila, Derek Hammer (devel. & testing for astrodrizzle, tweakreg)

•  Sara Ogaz (software devel. & testing for calacs/ selfcal)

•  Jay Anderson (ACS selfcal algorithm development)

•  Bryan Hilbert, Elizabeth Barker (WFC3/IR reprocessing, persistence)

•  Massimo Robberto (calwf3 improvements for time-variable sky background) •  Ray Lucas (additional ACS inspection, satellite trail masking) •  Josh Sokol, Shireen Gonzaga (phase II tracking)


ACS Self-cal (Jay Anderson)


ACS Self-cal: typical improvement


MAST / Archive Frontier Fields Data Page http://archive.stsci.edu/prepds/frontier

•  Propagate v0.5 mosaics��on a weekly basis

•  cumulative-depth��stacks of all data��to date

•  Propagate v1.0 mosaics��at end of each epoch


Example MAST Interactive Displays


HST Frontier Fields Lensing Maps

lensing models are key to interpreting luminosities of background galaxies

5 groups have made preliminary magnification maps for FF before 1st observations

100s of arcs expected in FF data ⇒ tighter constraints on lensing models

www.stsci.edu/hst/campaigns/frontier-fields/Frontier-Fields-Lensing-Map-Seminar


Milestones Completed Fall 2012: HDFI SWG presented a unanimous recommendation

Winter 2012: Frontier Fields announced in Cycle 21 call for proposals

Community input solicited on cluster selection, filter choice, general input via email exploder, website, and AAS flyer.

All six clusters selected and announced

WFC3/IR F140W filter added to parallel field observations

Blank field positions announced Spring 2013: ~35 Frontier Fields related proposal received for HST Cycle 21;

3 GO program and 7 archival/theory programs selected.

Public lensing map-makers selected through separate call Summer 2013: PhaseIIs submitted for first 4 fields

Data Pipeline testing: astrodrizzle, tweakreg, + self-calibration

Chandra GO programs awarded

Lensing maps delivered Fall 2013: First Spitzer observations of Abell 2744 obtained 9/14/2013

Frontier Fields ‘readiness review‘ 9/20/2013

Abell 2744 Lensing Map release by MAST/HLSP with interactive tool

First HST Frontier Field observations - visit 1 of MACS0717 10/17/2013 - epoch 1 Abell 2744 10/23/2013 – 12/11/2013


Upcoming Milestones October 2013: Abell 2744 observations begin February 2014: MACSJ0416 observations begin March 2014: HST Cycle 22 proposal deadline July 2014: Abell 2744 HST observations complete August 2014: Spitzer observations of 1st 4 clusters complete September 2014: MACSJ0416 HST observations complete

MACSJ0717 HST observations begin October 2014: MACSJ1149 HST observations begin November 2014: Decision on last 2 clusters needed December 2014: HST Cycle 23 call for proposals released April 2015: MACSJ0717 HST observations complete June 2015: MACSJ1149 HST observations complete


HST Frontier Fields: a legacy for the community

Continual updates are provided at the main HST Frontier Fields website: http://www.stsci.edu/hst/campaigns/frontier-fields

All raw HST DD data will be public as soon as possible: STScI is provide high-level science data products, including calibrated, full-depth drizzled mosaics on ~ weekly basis. All HST High-Level Science Products are available via MAST / Archive:

http://archive.stsci.edu/prepds/frontier Lensing maps by multiple group/methods are being made available to pubic via MAST/Archive before HST FF observing campaign Spitzer DD time for deep IRAC 3.6, 4.5 micron imaging (5σ ~26.5, 26.0 ABmag) SSC will provide calibrated, reduced IRAC images. 10 HST programs related to FF selected in HST Cycle 21 TAC Rodney: SN followup; Siana: WFC3/UV; Treu: WFC3/IR grism (non-proprietary) + 7 archival programs ( theory, lensing, asteroids ... ) 5/6 fields observable with ALMA, 5/6 observable with Mauna Kea, 4/6 have MIPS 24micron, 4/6 suitable for deep radio all are observable with JWST and selected for low IR background

the hst frontier fields program · acs - wfc3/ir in parallel; do 180-degree swap ~6 months later...

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