Cosmology at LAM Cosmology at LAM A deep and wide look in the Universe Jean-Paul Kneib Laboratoire d’Astrophysique de Marseille

Cosmology at LAM  A growing cosmology centre in France (~20 researchers)  Many projects: Observational and Instrumental (for space and ground observatories)  A strong link with particle physicist in Luminy (CPPM+CPT)

People Faculty/Researcher: Jean-Paul Kneib Christophe Adami Stéphane Arnouts Stéphane Basa J.-Gabriel Cuby Jean-Michel Deharveng Olivier Le Fevre Vincent Lebrun Roger Malina Alain Mazure Laurence Tresse Marie Treyer (in Caltech) Anne Ealet Charling Tao PhD students Marie-Helene Aumenier Melanie Filiol Pascale Hibon Eric Jullo Sylvain De Latorre Alexie Leauthaud Baptiste Meneux Postdocs Lidia Tasca Jacob Walcher

Cosmology Themes Cosmology Themes Deep galaxy surveys: a statistical & multi-wavelength approach on galaxy evolution (GALEX, VLT/VIMOS, HST, Spitzer) Supernovae in the SNLS: constrain on the cosmological parameters Gravitational lensing: Dark matter distribution in bounded structures (clusters, groups & galaxies) The first galaxies in the Universe: finding and studying the most distant galaxies (Ly-alpha search, lensing search) Physics of clusters of galaxies: from low to higher z IGM properties: using distant quasars and spectra of Galex sources.

BIG Galaxy Surveys spectra in one shot 2D spectra of a single galaxy Red Blue λ Measuring Spectra with VIMOS (built At LAM) ! Aim to get ~ spectra VLT VIMOS

Deep Galaxy Surveys Deep Galaxy Surveys LAM is involved in many different galaxy surveys aiming at tracing galaxy evolution as a function of time up to z~4 VVDS: The “VIMOS VLT Deep Survey” A I-band magnitude selected survey - shallow I AB <22.5 on 10 sq degrees (on 5 fields): ~ redshifts - deep I AB <24 on 1.2 sq. degree: ~ redshifts

N(z), I AB  24 =0.76 VVDS redshift desert Peaks at z~0.8 High redshift tail to z~5 VVDS redshift desert: due to Å observations VVDS: Redshift distribution VVDS: Redshift distribution

Comparing Observations & Simulations Comparing Observations & Simulations Constraints on galaxy evolution in the Universe 0.7 < z < < z < < z < 0.8 Galaxy densities Courtesie Marinoni Observations Simulations

VVDS: Evolution of galaxy types 2-3x increase with z for early types 5-10x decrease in latest types Spectral types (SED fit to photometry) Early type vs. Latest types LF (2 of 4 types) Zucca et al. astroph/

High redshift galaxies 1.5<z<4.5 2 to 6 times more galaxies at z~3 than previously thought ! BHZGs: A missing link between various populations seen so far ? LBGs, DRGs, SMBGs, BzK… Le Fèvre et al., Nature, in press

COSMOS Survey Features The Largest Contiguous Area observed with Hubble (cycle 12-13) Large Area: 1.4 x 1.4 deg => Cover largest large scale structures (~ Solar Mass) => Rare Objects at high redshift (total of ~ galaxies) High Sensitivity ( I ~27 mag, 10  ) and High Resolution (~0.1”) => Morphology of L * galaxies at z < 2 => Strong and weak lensing (probe of DM) Equatorial Field: 10h +02 => Multi- observations from all telescopes Complementary to other Deep Survey (UDF, GOODS, GEMS, CFHTLS, VVDS, DEEP, SDSS …)

ACS HUBBLE Treasury Data PI:Nick Scoville Caltech 590 orbits: ACS/F814W (~2 sq.deg) + NICMOS-3/ F160W (7% of area) Shown: 477 orbits as of mid May 2005 NICMOS  m -- 24mag ~7% of area ACS I-band 1.4 degree Koekemoer et al Native: 100k x 100k image Drizzled: 165k x 165k => 100 Gb image !!!

Massey et al Cluster at z=0.73 Weak Lensing Mass Map on central 1 sq.degree

R E =1.7” First Strong Lensing Systems in COSMOS R E =3” Faure et al We expect strong lensing systems, Sample comparable in size to other strong lensing surveys!!! Probe mass dsitribution and Cosmology(?)

Faint Sample: (270 hours)  Ground based Color selected to probe high redshift (1.5<z<2.5 tail)  Blue Low Res grism; UBVR+ BzK selection  ~13000 redshifts central area bright catalogue Faint colour- selected catalogue zCOSMOS: VIMOS Redshift survey Bright Sample: (270 hours)  ACS selected: I AB <22.5  Red Med Res grism -> velocity  ~27000 redshifts full area

Other Deep Galaxy Surveys Other Deep Galaxy Surveys CFHT-Legacy survey: Ugriz imaging with Megacam at CFHT - WIDE: cosmic shear motivated - DEEP: galaxy evolution and Supernovae Survey (SNLS) WIRDS: WIRCAM Deep Surveys Aim to cover 3 square degrees in the infrared (J,H,K) with the new WIRCAM camera ZEN: z Equals ~Nine Narrow-band Lyman alpha survey at z~8.8 using infrared cameras

SuperNova Legacy Survey CFHT partly dedicated to SN search, 8m telescopes on alert Observation every month More than 150 SN found Hard to do better from the ground

dataanalysisphysics Supernovae: comological constraints Images Spectra redshift identification Ia magnitude  M,   Hubble

Cluster Lenses  Cluster of Galaxies are powerful lenses:  Cluster mass distribution  Finding high redshift magnified galaxies  Cosmological constraints (cosmography)

First Light with Cluster Lenses  Most distant galaxies and their properties, ACS+NICMOS search on HST  Narrow band searches  Probing re-ionisation Spitzer HST Kneib et al 2004

Future projects NIRSPEC on JWST (galaxy evolution, z>7) DUNE/SNAP (lensing+SN) ECLAIRS (GRB+high-z) Participation on HERSCHELL EMIR on GRANTECAN (high-z) Multi-IFU spectrographs on ELTs (first galaxies and Sne, probing 7<z<18)

Le Next Generation Space Telescope: JWST NIRSPEC Spectrograph (Astrium/LAM)

Wide Field Imager in Space IFU spectrograph slicer visible+IR 3’’x3’’, [ ]  m (LAM) JDEM/SNAP Probe cosmology and dark energy using lensing and SuperNovae, interest for galaxy evolution SNAP and DUNE projects

A unique example a z~6.3 GRBs Detection with TAROT (OHP) Photometric redshift with VLT Redshift with Subaru GRBs are true cosmological probe ! + 25 s +50 s +70 s TAROT

ECLAIRS Horizon 2009 Interface with satellite Camera Gamma of 80°x80° Find gamma-ray burst ~5 keV- 100 keV X-ray/optical telescope to Locate the burst within 1 arcmin Need optical ground based telescope (optical+IR) to produced light curves and measure precise redshift

MOMFIS on OWL  A multi-object, multi-IFU instruments  Probe the 7<z<18 universe: galaxies and SNe  30 IFUs, 20 mas pixel size for a 50 mas resolution, using Slicers (LAM technology)  Similar concepts for TMT (to be tested on 8-10 meters?)  Developpement of OH supression filter/fibers MOMFIS (preliminary study)

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