CANDELS C osmic A ssembly N ear-infrared D eep E xtragalactic L egacy S urvey Co-PIs: Sandra Faber University of California Santa Cruz Harry Ferguson Space Telescope Science Institute

CANDELS C osmic A ssembly N ear-infrared D eep E xtragalactic L egacy S urvey CANDELS Team: 100 scientists 12 countries Major nodes: UCSC, STScI, ROE, NOAO, UCI, UMich, MPIA,…

What WFC3-IR can do

But the WFC3 diffraction limit is 2-3 times softer than ACS

Existing space and ground Photometry gains

New WFC3

Exposure Strategy “Wedding cake” strategy: three layers of J+H WIDE: 2 orbit depth over ~0.2 sq deg DEEP: 8 orbit depth over ~0.04 sq deg UDFs: orbit depth over ~0.004 sq deg

Highlights  Imaging data for 250,000 galaxies from z =  WFC3 bridges the Balmer break out to z ~ 2.5  WFC3 cuts through dust  Spitzer Extended Deep Survey, SEDS: IRAC 26 AB (5  ); means stellar masses measured to ~3  10 9 M  to z ~ 7  Overlapping ACS parallels: panchromatic imaging from V  H; new ACS imaging in UDS, deeper/multicolor ACS imaging in COSMOS and EGS..... photoz’s!  UV in GOODS-N: 100 orbits of F275W, F336W  Every pointing observed at least twice:  Search for variable AGN  First search for SNe beyond z ~ 1.5

ERS: 9 WFC3 pointings to J+H depth of 4 orbits Deep vs. ERS: 5 times more galaxies, 0.6 mag deeper Wide vs. ERS: 8 times more galaxies, 0.6 mag shallower Deep: 30 WFC3 pointings to J+H depth of 8 orbits Wide: 162 WFC3 pointings to J+H depth of 2 orbits Wide + Deep will be the prime finding fields for first JWST spectroscopy Survey comparisons

COSMOS: 10 h 00 m +2 deg EGS: 14 h 18 m +53 deg UDS/UKIDSS/SXDS: 2 h 18 m -5 deg Three WIDE Fields

ACS parallel array WFC3-IR primary array SEDS/IRAC region WFC3-IR: 2 orbits of J+H, at two different epochs for SNe discovery ACS parallels: 4 orbits of V+I, provides low-z SNe rejection WIDE FILTERS AND EXPOSURE TIMES:

GOODS-N: 12 h 37 m +62 deg Two DEEP Fields GOODS-S: 03 h 30 m -28 deg

ERS2 Deep region “Skirt” region GOODS-S strategy

WFC3 array 1 orbit GOODS-S strategy

ACS parallel array WFC3 array 1 orbit GOODS-S strategy

≥ 2 orbits ACS parallel array GOODS-S strategy

GOODS-S exposure maps J and H-band Y-band Deep region WFC3-IR: 4 orbits each of Y, J, H, 10 different epochs for SNe discovery ACS parallels: minimum 14 orbits F814W for secure high-z identifications DEEP FILTERS AND EXPOSURE TIMES:

GOODS-S exposure maps F814W, I-band: needed to identify high-z galaxies Deep region Goal: ≥ 28,000 s in Deep region

GOODS-S exposure maps F814W, I-band: needed to identify high-z galaxies Deep region Goal: minimum 28,000 sec PLUS:… * New ACS mosaic in UDS, plus V added to I in COSMOS * Follow-up of 8 high-z SNe using 9-orbit grism exposures and 10 orbits of J+H for light curves * Approx 4-orbits each of F275W and F336W in GOODS-N Deep using dayside CVZ * One orbit coverage of each Deep region using F850LP for variability * Extra V wherever possible

Point source limits 5-  AB mag 5-  AB mag Wide Plus existing ACS Deep >29 >30 29Incl existing ACS UDF Incl existing ACS Stellar z~2 M 1500, z~7 Wide 10 9 M  ~ -20 Deep 4  10 8 M  ~ -19 UDF 1.4  10 8 M  ~ -18 sq degtilesY J HV I z Wide /3 4/34/3 8/3 -- Plus existing ACS Deep >3 >14 5Incl existing ACS UDF0.0043~40 ~40 ~ Incl existing ACS Area# WFC3Exposure, orbitsEff. Exposure, orbits 10 9 M  Magnitude and mass limits

Observing schedule

 Orbit Totals:  GOODS fields: 483  EGS: 90  UDS: 88  COSMOS: 88  SNe Follow-up: 152  Test orbit: 1  Total: 902 orbits  Phase II Program IDs  GOODS-S:  EGS:  UDS:  SNe:  Public website:  Summary  Data releases:  V0.5: builds summed multi-drizzled images as images come in using existing instrumental and astrometric calibrations. Available within days.  V1.0: improved versions of V0.5 images based on all data, additional quality control, and improved calibrations. Available within 3 months after last field data are obtained.  V2.0: archival version. One year after last data.  Value-added data products:  Re-reduced existing ACS images multi-drizzled with new data  Serving all public ancillary data

Supernovae prospects

Dark energy differences

Supernovae evolution HST lifetime Supernovae prospects

New WFC3 z   candidates Yan et al. 2010

Importance of SEDS/IRAC

At z  ,  candidate galaxies in Deep

60 objects here At z  ,  candidate galaxies in Deep

At z  ,  candidate galaxies in Wide 100 objects here 50 objects here

Merger signatures at z   Courtesy J. Lotz

radii Sersic n axial ratio Gini M 20 Useful limit: H ~ 24 AB mag in Wide survey. This is 2 x 10 9 M  at z ~ 2. Structural parameters at z   Simulated data

Galaxy radii vs. color at z   Courtesy M. Mozena Blue- cloud galaxies Half light radius in kpc

   Simulation by Naab et al (small points)  UMass measurements at z=0, z=0.4 and z=2 Courtesy of M. Giavalisco RADII OF EARLY-TYPE (PASSIVE) GALAXIES

Sersic indices at z   Red galaxies Blue galaxies WFC3 regime Sersic index Courtesy M. Mozena

Fireworks ERS2 Catalog z spec = 2.431log(mass) = Fireworks UDF Catalog z spec = 1.998log(mass) = ViH 3” ViH Old stars?

With dust (absorption and scattering) z = 2.33 log(mass) = Hydro-ART Simulations (Ceverino et al. 2010) ViH 3” ViH Raw, no dust Old stars

Guo et al. in prep. z-bandH-bandz-HH-bandz-bandz-H PSF-matched color maps

Simulated “lookback slices” Back in time

Theoretical completeness Two SAMs compared: mass completeness in Wide CANDELS theory group: Darren Croton, Romeel Dave, Aaron Dutton, Avishai Dekel, Joel Primack, Rachel Somerville, Risa Wechsler, and their collaborators… Bernyk, Croton et al. Somerville et al.

GOODS-S exposure maps