involved LAM people :

1
PI Chris Martin (Caltech) LAM coI Bruno
Milliard, José Donas
GALEX DEEP SURVEYS and GOYA
involved LAM people Stéphane Arnouts (UV-NIR
photometry LF/LD, UV SFR ...) José Donas
(UV FOCA/GALEX photo clusters ...) Bruno
Milliard (UV FOCA/GALEX instr/
photospectro envt ...) Laurence Tresse
(opticalNIR spectro LF/LD, H? SFR ...) Marie
Treyer (UV FOCA/GALEX spectral
diagnostics ...)
2
GALEX DEEP SURVEYS and GOYA

• Recent GALEX results
• (First papers in ApJ Letters , 2005, vol 619)
• Evolution of the FUV-LF(FUV)
• Evolution of spectro-photmetrical types
• Evolution of the SFR (uncorr - dust corr)
• UVLG galaxies morphology of a sub-sample
  0.5ltZlt0.8
• GALEX-GOYA combined science
• H? follow-up of GALEX sources at zlt1.5

GALEX-VVDS
3

• One of the main goal of GALEX
• Evolution of the SFR density up to z1.5
• GALEX fills the gap between FOCA (zlt0.2) and
  LBGs (z3)
• where most of the SFR evolution is seen
• Pilot Study with
• DEEP GALEX observations (DIS)
• DEEP optical spectro-photometry ( spectra up to
  IABlt24)

(PI O. Le Fèvre , G. Vettolani)
4
GALEX-02hr field
Used area ?????
FUVNUV color image
5
Redshift distribution
with secure redshifts
Unique OC lt 2 Ocs full sample
6
-1b- FUV Luminosity Functions with 1000 Zspec
(Arnouts et al. 2005)
FUVabs from NUV mag LF estimation ALF tool
(Ilbert et al., 2004)
Local GALEX LF (Wyder et al., 2005 Treyer et
al., 2005)
Strong evolution from 0ltzlt1.2 (GALEX)
Zphot from HDF NS
Trend continues to z3 (HDF)
7
-1c- Evolution of the FUV Luminosity Function
Arnouts et al (2005)
Possible evolution in slope ?
Significant evolution 0 lt z lt 1 ?M 2
mag (or x6 in L) 1 lt z lt 3 ?M
1 mag
8
-2- Galaxy Type classification with Zspec
(Arnouts et al., 2005)
Kinney et al, 1996
(NUV-R) correlates SF history (B-I) as a crude
proxy for galaxy type
Poggianti et al 1997
Type fraction vs Z
Increase of the unobscured SB class from z0 to
1 (also true for the volume corrected
fractions)
Apply to the Zphot sample
9
-3- Evolution of FUV Luminosity
DensitySchiminovich et al. (2005)
LD using ALF tool
(1z)3.5
(1z)2.5
(1z)1.5
(1z)2.5 luminosity density evolution since
z1 Continued slow evolution 1ltzlt3
10
-3a- Dust attenuation correctionSchiminovich et
al. (2005)
Using UV slope ? AFUV f(?)
FWHM(?)1.4 ?(?)0.4
(Meurer et al.,1999Kong et al., 2004)
Full sample ? consistent with - local FUV
sample (Treyer et al., 2005) - high-z sample
(Adelberger, 2000)
11
-3b- Local Dust attenuation correctionBuat et
al. (2005)
Using GALEX NUV selected local sample with
IRAS (60?m)
log Fdust/FFUV
-1 0
1 2
(FUV-NUV)

• UV selected galaxies exhibit a lower dust
  attenuation law
• than those from Starbursts

Mean ANUV 1.1
12
-3c- Evolution of the SFR Density uncorrected
and dust-corrected (hatched region)
Uncorrected SFRD
(1z)2.5
0ltzlt1.5 ?2.5 1.2ltzlt3 ?0.5
Corrected SFRD
Meas ltAFUVgt1.8 Min AFUV1.0 (local UV sample
Buat et al. 2005)
13
-4- GALEX Find Rare Objects UVLGs
Local Measurement GALEX-SDSS (Heckman et al,
2005)
Lyman Break Galaxies at z0?
14
-4b- UVLGs at intermediate Z
0.55ltzlt0.8 COSMOS (M. Zamojski D.
Schiminovich)
Luminosity density (for Lgt0.2 L(z3))
Large
Compact

• Locus slightly higher than LBGs
• LBG-like galaxies shows dramatic evolution
  (1z)5
• UVLGs produce a significant fraction of LD at z
  1 (25)

15
GALEX and GOYA

• GALEX selected sample at 0.7ltzlt1.5
• Optical NIR spectroscopy
• Comparing the SFR estimators LUV , LOII , H?
• Dust attenuation from Balmer lines
• Kinematics from emission lines
• SFR/attenuation vs b-parameter , stellar mass,
  envt ...
• First priority sample UVLG galaxies
• GALEX NUV dropouts at 2ltzlt2.8
• NIR spectroscopy
• OII (J band) and H? (K band)