1. 1 Deep spectroscopic redshift surveys are a central tool to modern Astrophysics Deep redshift surveys (z>0.3) have shaped our current understanding:  CFRS (1995)  LBG surveys (Steidel et al. 1996+)  DEEP/DEEP2 (2005+)  VVDS (2005+) Compare high redshift to low redshift spectroscopic surveys Knowledge of the sources: physical informations available Redshift information with ~100km/s accuracy enables to look for 3D distribution A basis for robust selection for detailed follow-ups Important serendipitous capabilities Understand galaxy formation and evolution Understand LSS formation and evolution Measure Cosmology parameters 600z 50000 z

2. 2 Deep spectroscopic surveys at ESO and elsewhere Deep spectroscopic surveys at ESO and elsewhere 10-15 years ago: CFHT-MOS, EFOSC, EMMI, OPTOPUS/MEFOS,  CFRS, 600z, z~1  ESP, 3000z, z~0.3 VVDS/VIMOS: created a new expertise in Europe Now at the VLT, several spectroscopic surveys covering up to z~6  VIMOS: VVDS (50000z, up to z=5), zCOSMOS (25000z, up to z=3), GOODS (7000z), UDF (5000z), VIPERS (100,000z, z~1)  FORS2: GMASS, UDF  FLAMES/GIRAFFE, SINFONI: follow-ups

3. 3 VIMOS -VLT-UT3 A highly efficient high redshift machine in operations since 2002 on the VLT

4. 4 Multi-slit mode Low res. High res.

5. 5 Survey selection function: a key element Survey selection function: a key element  VVDS is magnitude limited, I-band (CFRS like)  Probes to UV as z increase: a bias “easy” to work with  Enables a complete census of the population probed  Only other survey today with this selection: zCOSMOS  Most other surveys are color + magnitude/flux (+shape) selected  LBG, BM/BX, BzK, EROs  LAE, H , …

6. 6 VIMOS VLT Deep Survey VIMOS VLT Deep Survey R~230, 5500-9300Å ~50000 spectra ~50000 spectra 50+ papers published so far

7. Total VVDS N(z), 17.5≤IAB≤24.75 7

8. Basic counts 8 Magnitude selection is more complete than color selection

9. VVDS has complete samples in other bands 9

10. 10 Serendipitous power in VVDS Serendipitous power in VVDS Slits: 1”x5-20” VVDS target Photometrically invisible Lya emitter Target spectrum Serendipitous Lya @ 1216Å 1200 slits, 3.3 arcmin 2, 3500-9500Å, 65000s 8000 slits, 22.2 arcmin 2, 5500-9500 AA, 16000s 200 LAEs identified 2<z<6.5 (Cassata et al., in prep.) DO IT ON WIDE !!!

11. 11 VVDS: enables follow-ups VVDS: enables follow-ups Select galaxies from a large and unbiased sample before to study the physics of galaxy assembly SINFONI obs. of VVDS galaxies 1<z<2 Epinat et al., arXiv:0903.1216 (today)arXiv:0903.1216 merger perturbed disc MASSIV

12. VVDS prepared/prepares the future z-surveys VVDS heritage  zCOSMOS  VIPERS New generation VIMOS surveys  z>3 survey, proposed New generation facilities, multi-slit  JWST  EELT  EUCLID 12

13. VVDS Highlights PaperYearCitationRate Survey epoch 120051702.8 CDFS20041612.2 Galex-VVDS20051422.4 Photoz20071382.9 LF global2005921.5 Galex LF2005891.0 LF type2006741.4 MF2007662.2 VLA2003580.9 Growth rate2008543.0 Color-density2006541.3 Mass assembly2007511.7 Clustering per type2006451.3 Bias2005390.8 All works are great ! Attempt to look at the key papers, per citation Some flops, strangely: - Population census z~3, Nature, 2005 (33) - LD, 2007 (30) - - VVDS-SWIRE clustering, 2007 (3) 13