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Deep spectroscopic redshift surveys are a central tool to modern Astrophysics

Deep spectroscopic redshift surveys are a central tool to modern Astrophysics. Understand galaxy formation and evolution. Measure Cosmology parameters. Understand LSS formation and evolution. Deep redshift surveys (z>0.3) have shaped our current understanding: CFRS (1995)

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Deep spectroscopic redshift surveys are a central tool to modern Astrophysics

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  1. Deepspectroscopic redshift surveys are a central tool to modern Astrophysics Understandgalaxy formation and evolution MeasureCosmologyparameters Understand LSS formation and evolution • 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 600z 50000 z

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

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

  5. Survey selectionfunction: a keyelement • 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. VIMOS VLT Deep Survey • R~230, 5500-9300Å • ~50000 spectra 50+ paperspublishedso far

  7. Total VVDS N(z), 17.5≤IAB≤24.75

  8. Basic counts Magnitude selectionis more completethancolor selection

  9. VVDS has completesamples in other bands

  10. Serendipitous power in VVDS VVDS target Slits: 1”x5-20” Serendipitous Lya @ 1216Å Target spectrum  Photometrically invisible Lya emitter DO IT ON WIDE !!! • 1200 slits, 3.3 arcmin2, 3500-9500Å, 65000s • 8000 slits, 22.2 arcmin2, 5500-9500 AA, 16000s 200 LAEs identified 2<z<6.5 (Cassata et al., in prep.)

  11. VVDS: enablesfollow-ups merger MASSIV perturbed • Select galaxies from a large and unbiasedsamplebefore to study the physics of galaxyassembly perturbed disc SINFONI obs. of VVDS galaxies 1<z<2 Epinat et al., arXiv:0903.1216 (today)

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

  13. VVDS Highlights All works are great ! Attempt to look at the keypapers, per citation Some flops, strangely: Population census z~3, Nature, 2005 (33) LD, 2007 (30) - VVDS-SWIRE clustering, 2007 (3)

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