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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
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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.
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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
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Frenk etal
redshift slice from CDM sim.
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Extremely large samples w/I 2 deg2
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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
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Subaru1.5x1.5 deg0.7'' res.
Full subaru mosaic
==> 18 bandsfor phot-z
2x106 gal.
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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
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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)
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stuctures from over-densities ==>
Redshift slices :
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adaptive smoothing w/ res. determined by local SNR
Z = 0.3 -- 0.4all SED types
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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.
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Galaxy groups w/ XMM at z > 0.5 : ACS images
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LSS structures from adaptive smoothing~ 30 : massesSED up to 1014Msun sizes up to ~ 10 Mpc
3d cube
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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
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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
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luminous early-type ==> dense core of LSS
COSMOS : environment <==> evolution
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XMM contours shear map
Z = 0.75 cluster
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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
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COSMOS -- lens
smoothing w/ same stretch
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COSMOS ACS I
0.56Z = 0.77 1.34 (?)
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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 !
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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
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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
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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
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http://cosmos.astro.caltech.edu/
http://irsa.ipac.caltech.edu/COSMOS/
COSMOS
Cycle 12 COSMOS Data Release
(also MAST in future)
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XMM
red -- 0.5-2 kev
green -- 2-4.5 kev
blue -- 4.5-10kev
339 sources detected
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GALEX -- UV
Schminovich &Martin etal
1.5 deg200 ks
50,000 UV objw/ mAB< 25
1750-3000Å1300-1750Å
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Early type galaxies only
Z = 0.6 -- 0.7 Z = 0.8 -- 0.9
wavelet ==>
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==> need resolved colors
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Need 2-colors w/ ACS
central 3x3 mosaic has I & g bands
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original g & I adaptively smoothed
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XMM contours shear mapsgalaxy density
Z = 0.75 cluster