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Stéphane ArnoutsDavid SchiminovichOlivier Ilbert and VVDS and GALEX teams
THE GALEX-VVDS DEEP SURVEYS :
Evolution of the Far UV luminosity Function and Density (+ SFR) up to z=1.5
PI : Chris Martin (Caltech)
PI : O. LeFèvre (Marseille) G. Vettolani (Bologna)
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One of the principal goal of GALEX
•Evolution of the SFR density up to z=1.5
•UV sensitive measurement of the ongoing Star Formation Used to derive SFRD: locally (z<0.2 , FOCA) at high-z (z>2.5, in optical band)
• GALEX fills the gap where most of the SFR evolution is seen
Required
•DEEP and WIDE GALEX observations
•DEEP and WIDE optical spectro-photometry observations
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Outline of the talk :
•Results from a PILOT STUDY done in the 2hr field : GALEX Deep obervations VVDS Deep spectroscopy and photometry
• Spectroscopic sample : Evolution of the FUV LF and LD Implication in the SFR history
• Morphology of a sub-sample of UV luminous galaxies
•Recent Photo-z analyses : Combined dataset : VVDS+CFHTLS+SWIRE
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AAS 72.07 - DS Jan 11, 2005
Texp = 52765 sec
FUV+NUV color image
GALEX-02hr field
Used area :
<E(B-V)>=0.027
Field of View
1.2 degrees
Bands FUV 1350-1750 ANUV 1750-2800 A[simultaneous]
Angular resolution
4.5” FWHM
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GALEX Galaxy Number counts
NUV < 24.5.Completenesscorrection withHST counts (Gardner et al. 2000)
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Spectroscopic Area : 0.46 deg2
The 2hr field combined dataset
VVDS : BVRI (JK) VVDS : spectroscopy IAB=24
ANDCFHTLS : ugriz
SWIRE : 3.6 to 8m
+24m
(section photo-z)
GALEX
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Jan 11, 2005AAS 72.07 - DS
NUV band5” PSF
GALEX - OPTICAL matches
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Jan 11, 2005AAS 72.07 - DS
GALEX - OPTICAL matches B band1” PSF
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GALEX - OPTICAL matches
Counterparts searched in a distance = 4’’ : ast = 0.7’’
PSF=5’’ but good astrometry
•ALL UV sources have an optical counterparts
•NUV<24.5 ~50% have a single optical counterparts
•NUV<24.5 ~35% have two optical counterparts
•NUV<24.5 ~15% have more than two optical counterparts
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GALEX - OPTICAL matches
•Preliminary Analysis : UV sources matched with the closest OC which is in 90% cases the brightest one
•Impact of the blends based on : -1 : expected colors from single match -2 : apportion the UV flux among the multiple OCs using Sutherland & Sanders (1992) method
<UV flux> overestimated by 0.25 mag for 2 OCs0.50 mag for multiple OCs
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GALEX with VVDS spectroscopy
~1100 Zspec19.5<NUV<24.5
~15% UV sample
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Color distribution
Spectro : Good samplingof UV sources.
Saturation : 95% at z<0.2 (SDSS)
IAB>24 : only 4%
Saturation in I
Limit spectro
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Redshift distribution
LF
Unique OC
<= 2 Ocs
full sample
with secure redshifts
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FUV Luminosity Function with ~1000 Z-spectro
(Arnouts, Schiminovich, Ilbert et al. 2005)
Strong evolutionfrom 0<z<1.2 (GALEX)
FUVabs from NUV mag
LF estimators :Vmax, C+, SWML, STYusing ALF tool (Ilbert et al., 2004)
Weight to account for :1. Spectroscopic strategy 2. NUV counts completeness
Local GALEX LF(Wyder et al., 2005)
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FUV Luminosity Function at higher z (Arnouts, Schiminovich, Ilbert et al. 2005)
Trend continues to z=3 (HDF)
Zphot from HDF N+S (Arnouts et al., 1999 & 2002)
z to be FUV rest-frame :
1.75<Z<2.25 with F450<27
2.40<Z<3.40 with F606<27
1700A LF @z=3(Steidel et al., 1999)
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Evolution of the FUV Luminosity Function Arnouts, Schiminovich, Ilbert et al (2005)
Possible evolution in slope
Significant evolution 0 < z < 1 : M*= 2 mag (or x6 in L*)1 < z < 3 : M*= 1 mag
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Evolution of FUV Luminosity DensitySchiminovich, Ilbert, Arnouts et al. (2005)
LD using ALF tool(1+z)2.5
Integration of STY fit up to L=0
Sum of (L).L.dLUsing Vmax LF
(1+z)2.5 luminositydensity evolutionsince z~1
Continued slowevolution 1<z<3
GALEX AIS-MIS : Wyder et al
GALEX DIS : This work
HDF : Arnouts et al (99, 02)
Steidel et al (1999)
(1+z)1.5
(1+z)3.5
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UV Luminous Galaxies (UVLGs)(DS, Ilbert, Arnouts et al)
(1+z)2.5
Luminosity density ofUV luminous: L>0.2 L*(z=3)
•“LBG-like” galaxies shows dramatic evolution: (1+z)5
• Steeper than QSO LD evolution (Boyle + Madau et al)
• UVLGs produce a significant fraction of LD at z = 1 (25%)
Total
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AAS 72.07 - DS Jan 11, 2005
Sizes of extreme UV-luminous galaxies
LFUV,bol > 2x1010 Msol
SFR 5-50 Msol/yr
Local : u-band r1/2 (circles)
Compact galaxies may be LBG analogs with high SFR/area and SFR/<SFR>
Large
Compact
(Slide courtesy of D.S.)Local Measurement: GALEX-SDSS (Heckman, Hoopes et al, 2005)
0.55<z<0.8 : COSMOS M. Zamojski & D. Schiminovich V-band r1/2 (squares)
r1/2 consistent with local sample & Locus slightly higher than for LBGs
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AAS 72.07 - DS Jan 11, 2005
Large UV Luminous Galaxies (UVLGs) r50~10 kpc 0.55<z<0.8
(Slide courtesy of D.S.)
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AAS 72.07 - DS Jan 11, 2005
Compact UV Luminous Galaxies (UVLGs) r50~2.5 kpc 0.55<z<0.8
(Slide courtesy of D.S.)
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(Meurer et al.,1999Kong et al., 2004)
Dust attenuation correctionSchiminovich, Ilbert, Arnouts et al. (2005)
Using UV slope: AFUV = f()
Full sample consistent with- local FUV sample (Treyer et al., 2005)
- high-z sample (Adelberger, 2000)
FWHM()=1.4()=0.4
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Uncorrected SFR vs. Z
NUV <24.5 NUV <26 (UDIS)
Conv. LFUV to SFR (Kennicutt, 1998)
No dependence ofdust attenuation AFUV
with SFRuncor
L*(z)As a consequence
Schiminovich, Ilbert, Arnouts et al. (2005)
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Corrected SFR vs. Z
Conv. LFUV to SFR (Kennicutt, 1998)+ AFUV (Meurer et al., 1999)
Paucity of low AFUV
galaxies with
high SFRcor
- Large scatter in the
measured AFUV - Dust attenuation law
NUV=24.5AFUV
4.0
2.5
1.5 0.5 0.
M99 relation may overestimate AFUV for star-forming galaxies
Schiminovich, Ilbert, Arnouts et al. (2005)
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Evolution of the SFR Density uncorrected and dust-corrected (hatched region)
(1+z)2.5
Wilson et al (2002)
Lilly et al (1996)
Sullivan et al (2000)
Brinchmann
Tresse and MaddoxPerez-GonzalezGronwall
Uncorrected SFRD
Meas <AFUV>=1.8Min AFUV=1.0(local UV sample Buat et al. 2005)
Corrected SFRD
0<z<1.5 : =2.51.2<z<3 : =0.5
Consistent withH measurements
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Z photometric Area : 0.65 deg2
VVDS : (U)BVRI (JK)Photometry used :
VVDS : (U)BVRI(JK)CFHTLS : ugrizSWIRE : 3.6 +4.5m
GALEX
Photometric Reshifts in F02 field works by Ilbert , Arnouts, Budavari et al
Classification in Galaxy/Star/QSO
FUV LF with photo-zfor a large sample
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Photometric Reshifts of UV galaxies in F02 field
Secure Zspec : 949
Colors : galaxy typesFilled circles : 1 OCOpen triangles : n OCs
No systematic 0<z<1.2Small scatter : =0.04
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VVDS : (U)BVRI (JK)
Photometric Reshifts of UV galaxies in F02 field
All Zspec : 1127
Colors : galaxy typesFilled circles : 1 OCOpen triangles : n OCs
No systematic 0<z<1.2Small scatter : =0.05Small number of outliers
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VVDS : (U)BVRI (JK)
Color-color checks vs classification
(NUV-B) vs (B-I)
Star/galaxy separation
Galaxies below the line
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VVDS : (U)BVRI (JK)
Color-color checks vs classification
(FUV-NUV) vs (B-I)
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VVDS : (U)BVRI (JK)
Color-color checks vs classification
(B-I) vs (3.6-4.5)
Same QSOs and Stars regionsfor spec. and phot.
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VVDS : (U)BVRI (JK)
Galaxy Redshift distribution
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FUV Luminosity Function with ~6000 Z-photo
At z=1: no constraint on slopeConsistent with =-1.6
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FUV Luminosity Function Zspec vs Zphot
Consistent with LF(spec)
•Smaller errorbars
•At 0.2<z<0.4 : constraint on M*
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FUV Luminosity Function Zspec vs Zphot
No evolution in 0<z<0.8
Consistent M*(z) evolution
Fixed
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Galaxy “Type” classification with Zspec (Arnouts, Schiminovich, Ilbert et al., 2005)
Poggianti et al 1997
Apply to the Zphot sample
Kinney et al;, 1996- Small number of galaxiesredder than Sb
-Degeneracy between old syst. and dusty SB
(NUV-R) correlated with SFRcurrent/ <SFR>past (Salim et al. 2005) : Galaxy SF history
(B-I) correlates with (NUV-R) : (B-I) as a crude proxy for galaxy type
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Galaxy “Type” classification with Zphot
Type fraction vs Z
(FUV<22, z<0.2) Increase of the unobscuredSB class from z=0 to 1
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Galaxy “Type” LF with Zphot
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Galaxy “Type” LF with Zphot
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Galaxy “Type” LF with Zphot
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Galaxy “Type” LF with Zphot
Similar evolution for the two reddest classesStronger evolution of the SB class wrt red ones
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Galaxy “Type” LF with Zphot
(z)~constant per type
2 Red classes : -0.9< <-1.2
SB class : -1.5< <-1.8
Modest luminosity evolutionof SB class wrt reddest classes
Number density evolution of the SB class
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Conclusion
GALEX-VVDS PILOT STUDY •Global evolution of the FUV light of galaxies in 0<z<1.5 and LFs per type: strong increase in density of SB class •Constraint on the evolution of the SFRD (uncorr.,corr.) •A new class of UVLG at 0.5<z<1 (LBG analogs) in easy reach for optical follow-up
NEAR FUTUR•GALEX-VVDS-SWIRE : nice combined science
(zphot, dust law, SFR vs Mass, AGN evolution,...) •More deep field and a few deeper ( lower SFR sensitivity)•SF sites vs LSS (UV / optical-IR cross-correlation)
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Conclusion
GALEX-VVDS PILOT STUDY •Global evolution of the FUV light of galaxies in 0<z<1.5 and LFs per type: strong increase in density of SB class •Constraint on the evolution of the SFRD (uncorr.,corr.) •A new class of UVLG at 0.5<z<1 (LBG analogs) in easy reach for optical follow-up
NEAR FUTUR•GALEX-VVDS-SWIRE : nice combined science
(zphot, dust law, SFR vs Mass, AGN evolution,...) •More deep field and a few deeper ( lower SFR sensitivity)•SF sites vs LSS (UV / optical-IR cross-correlation)