Cosmic Evolution Survey (COSMOS) w/ Hubble Telescope

image 2 deg.2 ! 590 orbits in Cy 12-13

VLT-VIMOS, XMM, Subaru, VLA, Galex, …

2 million gal. (z > 0.5) (like SDSS)

• rational for survey • major multi-wavelength components• identification of structures• galaxy evolution vs z and environment• future directions first HST data release

Major features :

• large area -- 9xGEMS => cover largest large scale structures • high sensitivity ( I > 27 mag, 10)

=> morphology of L* galaxies at z < 2

• sensitivity + area

=> 2x106 galaxies , unusual objects at higher z

• equatorial => multi- observations from all tel.

Roberto AbrahamMasaru AjikiJustin AlpertHerve AusselJosh BarnesAndrew BlainDaniela CalzettiPeter CapakJohn CarlstromChris CarilliAndrea CimattiAndrea ComastriMarcella CorolloEmannuel DaddiRichard EllisMartin ElvisAmr El ZantShawn EwaldMike FallAlexis Finoguenov

Alberto FranceschiniMauro GiavaliscoRichard GriffithsGigi GuzzoGunther HasingerChris ImpeyJean-Paul KneibKarel NelJin KodaAnton KoekemoerAlexie LeauthaudOlivier LeFevreIngo LehmannSimon LillyThorsten LiskerCharles LiuRichard MasseyHenry McCrackenYannick MellierSatoshi MiyazakiBahram MobasherTakashi Murayama

Colin NormanAlexandre RefregierAlvio RenziniJason RhodesMike RichDave SandersShunji SasakiDave SchminovichEva SchinnererNick ScovilleMarco ScodeggioKartik ShethPatrick ShopbellJames TaylorDave ThompsonNeil TysonMeg UrryYoshi TaniguchiLudovic Van WaerbekePaolo VettolaniSimon WhiteLin Yan

COSMOS -- team & collaborators

Frenk etal

redshift slice from CDM sim.

Extremely large samples w/I 2 deg2

COSMOS multi-

1.4 deg

270 orbits as of 6/15

ACS 270 orbits5/14/04

NICMOS-31.6 m -- 24mag~7% of area

ACS I-band

Subaru1.5x1.5 deg0.7'' res.

Full subaru mosaic

==> 18 bandsfor phot-z

2x106 gal.

Subaru -- deep multi-color opt. imaging

pi : Y. Taniguchi

• 10n in 04 , 15n in 05

• full 2 deg2 covered to 25-27 mag in 18 bands

==> PHOTO-Z w/ Z ~ 0.03 to 0.1

current photo-z catalog at IAB < 25 ==> 860,000 galaxies

photo-z (Subaru BVRIZ, CFHT U, NOAO K)

==> dz/(1+z) ~ 0.1 , ultimately to ~0.03

Structures/Cluster identification :

• wavelets (Finoguenov)

• adaptive smoothing (Scoville)

both techniques avoid a priori assumptions

w.r.t. shapes and sizes

can select all types of gal. or just early types (easier)

stuctures from over-densities ==>

Redshift slices :

adaptive smoothing w/ res. determined by local SNR

Z = 0.3 -- 0.4all SED types

QuickTime™ and aYUV420 codec decompressor

are needed to see this picture.

Wavelet analysis - Finoguenov etal

most structures show up in XMM diffuse emission ==> clusters

QuickTime™ and aYUV420 codec decompressor

are needed to see this picture.

Galaxy groups w/ XMM at z > 0.5 : ACS images

LSS structures from adaptive smoothing~ 30 : massesSED up to 1014Msun sizes up to ~ 10 Mpc

3d cube

Galaxy/LSS Evolution ==> environmental dependence

Galaxy types : morphology visual classification concentration/assymetry, etc spectral energy distribution (SED from photz)

Environment : defined structures n-th nearest neighbor separation

Capak etal

COSMOS = solid pts

others: Smith etal,Postman etal, Dressler

Elli

pti

cal f

ract

ion

==> at all Z , E’s fraction higher at high density==> evolution earlier at high density

luminous early-type ==> dense core of LSS

COSMOS : environment <==> evolution

XMM contours shear map

Z = 0.75 cluster

Adaptive smoothing :

spatial filtering/smoothing w/ filter width <== local SNR

specify desired local SNR, increase filter width to reach this

• no filtering where SB high ==> retain high res.

• smooth up to 2'' at low SB ==> detect faint, extended gal.

e.g.

applied to picking out large structures

enhance imaging

COSMOS -- lens

smoothing w/ same stretch

COSMOS ACS I

0.56Z = 0.77 1.34 (?)

need for LSS context, large area and multi- ! COSMOS will be a fundamental resource for cosmology

COSMOS major components :

HST (cycle 12 & 13)

Galex deep

VLA (A & C array) Fall 04

Subaru imaging 04/05 (~25 n)

VLT & Magellan spectroscopy

XMM

all underway !

Future : Subaru : COSMOS-18 ==> improved phot-z emission line survey

HST-ACS - g band (to be proposed)

Spitzer IRAC & MIPS (to be proposed)

NOAO, UH88, UKIRT -- deeper J,H, K

COSMOS 6.9 32.3

Lockman 5.0 18.4

Groth Strip 5.2 17.0

CDF-S 5.3 19.4

HDF-N 4.9 16.4

SWIRE-XMM 7.1 31.1

Cosmology Field IR Backgrounds (Mjy/sr)

8m 24m

w/i ~2x of very best fields

COSMOS equatorial ==> instruments N & S

VLA & ALMA

ALMA -- combined w/ VLA + other COSMOS multi-wave surveys

ALMA ==> ISM , far infrared/submm , dynamical masses

w/ subarcsec res.

Equatorial COSMOS field chosen to enable both VLA and ALMA

http://cosmos.astro.caltech.edu/

http://irsa.ipac.caltech.edu/COSMOS/

COSMOS

Cycle 12 COSMOS Data Release

(also MAST in future)

XMM

red -- 0.5-2 kev

green -- 2-4.5 kev

blue -- 4.5-10kev

339 sources detected

GALEX -- UV

Schminovich &Martin etal

1.5 deg200 ks

50,000 UV objw/ mAB< 25

1750-3000Å1300-1750Å

Early type galaxies only

Z = 0.6 -- 0.7 Z = 0.8 -- 0.9

wavelet ==>

==> need resolved colors

Need 2-colors w/ ACS

central 3x3 mosaic has I & g bands

original g & I adaptively smoothed

XMM contours shear mapsgalaxy density

Z = 0.75 cluster