1 / 28

intrinsically deepest + widest survey of high - z universe

The HST Frontier Fields Program. www.stsci.edu/hst/campaigns/frontier-fields. intrinsically deepest + widest survey of high - z universe (sneak peak at JWST ’ s universe with Hubble now). PI/Co-PI: Matt Mountain, Jennifer Lotz

jamar
Download Presentation

intrinsically deepest + widest survey of high - z universe

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The HST Frontier Fields Program www.stsci.edu/hst/campaigns/frontier-fields intrinsically deepest + widest survey of high-zuniverse (sneak peak at JWST’s universe with Hubble now) PI/Co-PI:Matt Mountain, Jennifer Lotz Implementation Technical Lead: Science Data Products Lead Norman GroginAnton Koekemoer + STScI Frontier Fields Implementation Team: http://www.stsci.edu/hst/campaigns/frontier-fields/Contact David S. Adler, Jay Anderson, Roberto J. Avila, Elizabeth Barker, Dan Coe, Scott Fleming, Andrew S. Fruchter, Shireen Gonzaga, Derek Hammer, Bryan Hilbert, Ian Jordan, Harish Khandrika, Janice Lee, Karen Levay, Ray Lucas, Jennifer Mack, John MacKenty, Sara Ogaz, Massimo Robberto, Patricia Royle, Linda Smith, Josh Sokol, Denise C. Taylor, Alan Welty, Bill Workman

  2. how to do better than Hubble Ultra Deep Field (before JWST)? ACS (optical) = 537 orbits WFC3 (IR) = 253 orbits = 790 orbits of HST 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.

  3. Matt: how to do better than Hubble Ultra Deep Field (before JWST)? 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 James Bullock (Chair, UCI), Mark Dickinson (NOAO), Steve Finkelstein (UT), Adriano Fontana ( INAF, Rome), Ann Hornschemier Cardiff (GSFC), Jennifer Lotz (STScI), PriyaNatarajan (Yale), Alexandra Pope (UMass), Brant Robertson (Arizona), Brian Siana (UC-Riverside), Jason Tumlinson (STScI), Michael Wood-Vasey (U Pitt)

  4. 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 astrophysicson 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

  5. HST Frontier Fields: Science Goals • 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?)

  6. STScI Core Implementation Team PI/Co-PI - Matt Mountain, 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: Jennifer Mack, Roberto Avila, Jay Anderson, Elizabeth Barker, Andy Fruchter, Shireen Gonzaga, Derek Hammer, Bryan Hilbert, Harish Khandrika, Ray Lucas, 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, PriyamvadaNatarajan, Johan Richard, AdiZitrin 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

  7. 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, AdiZitrin, 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

  8. The HST Frontier Fields Clusters Abell 2744 MACSJ0416.1-2403 MACSJ0717.5+3745 MACSJ1149.5+2223. Abell370 Abell S1063

  9. The HST Frontier Fields Clusters (aka Abell S1063) 5/6 clusters observable from Mauna Kea; 5/6 cluster observable with ALMA

  10. 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

  11. 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 Cluster Blank Field WFC3/IR ACS

  12. HST Prime and Parallel Observations Abell 2744 MACSJ0416.1-2403 MACSJ0717.5+3745 Abell 370 Abell S1063 MACSJ1149.5+2223. many fields have bright stars Gemini GEMS AO K-band of MACS0416.1-2403 planned

  13. HST Frontier Fields Schedule Abell S1063 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

  14. Data and High-Level Science Products • Raw, calibrated exposures: available immediate from archive • Cumulative full-depth HST mosaics: • release cumulative-depth v0.5 mosaics throughout epoch • 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)

  15. Astrometry: ~milliarcsecond accuracy (Astrometric tests by Jennifer Mack & Roberto Avila; currently workingwith V. Platais and ACS team for even further improvements)

  16. Calibration: New Challenges & Solutions • ACS dark current: • Dark reference files don’t fully capture all the features • Solution: selfcal (J. Anderson): use the actual data to improve dark • WFC3/IR time-variable sky background: • Changing background during multi-accum is problematic for standard calwf3 up-the-ramp slope fitting • Solutions: correct for time-variable component and rerun calwf3, or treat multi-accums as a single exposure • Persistence “bad actors”: • Bright spatial scanning obs can leave very bad persistence • Solution: improved HST scheduling (for all programs)

  17. ACS Self-cal (see talk by Jay Anderson) Default calacs (no selfcal) calacs after selfcal

  18. WFC3/IR Time-variable sky (see talk by Hilbert/Robberto/Lucas) Before correction After correction

  19. MAST / Archive Frontier Fields Data Page http://archive.stsci.edu/prepds/frontier • Deliver v0.5 mosaicson a weekly basis • cumulative-depthstacks of all datato date • Deliver v1.0 mosaicsat end of each epoch

  20. Example MAST Interactive Displays

  21. HST Frontier Fields Lensing Maps • www.stsci.edu/hst/campaigns/frontier-fields/Frontier-Fields-Lensing-Map-Seminar 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

  22. Mosaics Released to Date: Abell 2744 • Epoch 1: • - v0.5 releases: • Oct - Nov 2013 • - v1.0 release 17 Dec 2013 • Epoch 2: • - v0.5 releases: • May - Jul 2013 • - v1.0 release 23 Jul 2014 • Fields: • - main cluster • - parallel field “hffpar” • - other surrounding fields

  23. Mosaics Released to Date: MACS J0416-2403 • Epoch 1: • - v0.5 releases: • January 2013 • - v1.0 release 28 Feb 2014 • Epoch 2: • - v0.5 release: • 9 Aug 2014 • - more v0.5 releases as • this epoch proceeds • - epoch ends in Sep 2014

  24. 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 are public as soon as possible: • STScIprovides high-level science data products, including calibrated, full-depth drizzled mosaics on a fast-turnaround regular 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 • A wide range of HST GO programs related to FF selected so far: • SN followup; WFC3/UV; WFC3/IR grism, archival 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

More Related