Stéphane Arnouts David Schiminovich Olivier 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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Stéphane Arnouts David Schiminovich Olivier Ilbert and VVDS and GALEX teams
PI : Chris Martin (Caltech). PI : O. LeFèvre (Marseille) G. Vettolani (Bologna). THE GALEX-VVDS DEEP SURVEYS : Evolution of the Far UV luminosity Function and Density (+ SFR) up to z=1.5. Stéphane Arnouts David Schiminovich Olivier Ilbert and VVDS and GALEX teams. - PowerPoint PPT Presentation
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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)
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
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
NUV < 24.5.Completenesscorrection withHST counts (Gardner et al. 2000)
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
Jan 11, 2005AAS 72.07 - DS
NUV band5” PSF
GALEX - OPTICAL matches
Jan 11, 2005AAS 72.07 - DS
GALEX - OPTICAL matches B band1” PSF
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
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
No systematic 0<z<1.2Small scatter : =0.05Small number of outliers
VVDS : (U)BVRI (JK)
Color-color checks vs classification
(NUV-B) vs (B-I)
Star/galaxy separation
Galaxies below the line
VVDS : (U)BVRI (JK)
Color-color checks vs classification
(FUV-NUV) vs (B-I)
VVDS : (U)BVRI (JK)
Color-color checks vs classification
(B-I) vs (3.6-4.5)
Same QSOs and Stars regionsfor spec. and phot.
VVDS : (U)BVRI (JK)
Galaxy Redshift distribution
FUV Luminosity Function with ~6000 Z-photo
At z=1: no constraint on slopeConsistent with =-1.6
FUV Luminosity Function Zspec vs Zphot
Consistent with LF(spec)
•Smaller errorbars
•At 0.2<z<0.4 : constraint on M*
FUV Luminosity Function Zspec vs Zphot
No evolution in 0<z<0.8
Consistent M*(z) evolution
Fixed
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
Galaxy “Type” classification with Zphot
Type fraction vs Z
(FUV<22, z<0.2) Increase of the unobscuredSB class from z=0 to 1
Galaxy “Type” LF with Zphot
Galaxy “Type” LF with Zphot
Galaxy “Type” LF with Zphot
Galaxy “Type” LF with Zphot
Similar evolution for the two reddest classesStronger evolution of the SB class wrt red ones
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
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)
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)