Cosmic Evolution Survey (COSMOS)

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

+ VLT-VIMOS, XMM, Subaru, VLA, Spitzer, Galex, …

• rational for survey • major multi-wavelength components• identification of structures• galaxy evolution vs z and environment

www.astro.caltech.edu/~cosmos/

Data : http://irsa.ipac.caltech.edu/COSMOS/ STScI -- MAST

redshift slice from CDM sim.

Coupled evolution of LSS, galaxies, star formation, AGN w/ Z

90 Mpc

Cosmos

1.4 deg.

2 million gal.

like SDSS atz = 0.5 -- 5

COSMOS -- 38 ==> 80 team members -- US, Japan, Europe and Canada

Telescopes :

Hubble -- very fine & sensitive optical images XMM -- xray imaging Galex -- ultraviolet imaging Spitzer -- Mid IR w/ IRAC

Subaru -- multiple color imaging VeryLargeArray -- radio imaging ESO-VLT & Magellan-- opt. spec. ~ 45,000 gal. NIR -- NOAO, UH88, UKIRT …

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

Richard GriffithsGigi GuzzoGunther HasingerOlivier IlbertChris ImpeyKnud JahnkeJean-Paul KneibKarel NelJeyhan KartaltepeJin KodaAnton KoekemoerLisa KewleyAlexie LeauthaudOlivier LeFevreIngo LehmannSimon LillyCharles LiuRichard MasseyHenry McCrackenYannick MellierSatoshi MiyazakiBahram MobasherTakashi MurayamaColin Norman

COSMOS -- Ludovic Van WaerbekePaolo VettolaniSimon WhiteLin YanMin Yun

Alexandre RefregierAlvio RenziniJason RhodesMike RichDimitra RigopoulouMara SalvatoDave SandersShunji SasakiDave SchminovichEva SchinnererNick ScovilleMarco ScodeggioKartik ShethPatrick ShopbellVernesa SmolcicJason SuraceYoshi TaniguchiJames TaylorDave ThompsonNeil TysonMeg UrryLudovic Van Waerbeke

LSS w/Capak, Finoguenov,Giavalisco, Guzzo,Mobasher, Sanders

Major features :

• large area -- 1.4 x 1.4 deg => cover largest large scale structures • high sensitivity ( I > 28.6 mag AB , 5) => morphology of L* galaxies at z < 2

• sensitivity + area => 2x106 galaxies , unusual objects at higher z

• equatorial => multi- observations from all tel.

Cosmic Evolution Survey

1.4 deg

17 orbits10/31/03

1.4 deg

130 orbits3/31/04

1.4 deg

270 orbits as of 6/15

ACS 270 orbits5/14/04ACS I

-band

Cycle 12

1.4 deg

ACS 477 orbits1/14/05

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

ACS I-band

ACS 590 orbits

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

1.4 deg

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

Cycle 12 & 13

Enormous area and sensitivity ==> large samples of all objects :

!!

ACS source counts

COSMOS Photo-z catalog (Subaru, CFHT, NOAO)

Redshift distribution

Redshift uncertainties

LSS from galaxy overdensities in redshift slices ==>

Test of adaptive smoothing:

~ 50% of gal. w/i structures~ 50% in field

overdensity galaxies

recovered distribution

• recovers all significant structures

• retains power on all scales

• no spurious recoveries

• conserves number counts

All SED types (not just early types)

redshift slices w/ z = 0.1

gal

w/ieach LSS

~ 40 major large-scalestructures at z < 1.2

LSS mass : galaxies w/i each LSS

Prob. of halo mass structures

cosmos

Photometric/luminous mass(DM halo ~ 10+ times larger)

luminous early-type ==> dense core of LSS

XMM-Newton COSMOS

Hasinger etal

X-ray: COSMOS-XMM survey (Hasinger et al.)

Late (spirals and SB)

Early (S0 & E)

higher z ==> later type SED cores of LSS/halos ==> earlier type SED

Z

Galaxy type

see LSS out to highest z !

Ly Alpha emission @ z=5.7 in the COSMOS

narrow band subaru imaging at 8150 Ang.Taniguchi & Ajiki etal

　 58 emission candidates

Survey Volume = 1.5×106 Mpc3

n(LAE) = 3.8×10-5 Mpc-3

Lly alpha > 1042.6 ergs/s

8”

Examples of LAEs @ z=5.7

diffuse

compact chain?

diffuse

COSMOS has gotten to z=5.7 !!!

～ 200Mpc

LSS @ z=5.7 probed by LAEs

COSMOS field : 1.4x1.4 deg near equator RA = 10:00:28.6 DEC = +02:12:21 (near but shifted from VVDS 10 hr field) EB-V = 0.02 mag ! and very uniform

==> rel. sens. only ~20 - 25% worse than very best fields

!! most important : all instruments can see field e.g. VLA, ALMA future TMT/OWL

COSMOS multi-

Selection of LAEsiz-NB816 vs. NB816 ==> 58 candiates

NB816　<　25.1　(5σ)iz　–　NB816　>　0.7　&　3σNot detected in B, V, & r’ [B　>　27.6　V　>　27.1,　&　r’　>　27.1]

　　　　　 58　objects　

Survey　Volume　=　1.5×106　Mpc3

n(LAE)　=　3.8×10-5　Mpc-3

Lly　alpha　>　1042.6　ergs/s

covers vol ~ SDSS at z ~1Lookback 8-10 Gyr

Abell class 2 -4