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Science avec KMOS VLT-2ème génération • Istituto de Astrofisica, Milano, Italy: D. Maccagni (PI), B. Garilli, A. Iovino, G. Bertin, ... LAM, Marseille, France: O. Le Fevre, A. Mazure, B. Millard, L. Tresse, E. Prieto,... Laboratoire d'Astrophysique de l'OMP, Toulouse, France: T. Contini, R. Pello, J.P. Picat, ... IAP: Y. Mellier, ... IRA Bologna, Italy: J. Vettolani, ... ESO, Santiago, Chile: J. G. Cuby, ... IoA, Cambridge, UK: M. Pettini, ... O. De Geneve, Suisse: D. Schaerer, ... University of Durham, UK: J. Allington-Smith, ... UCM: J. Gallego, ... SCIENCE CORE GROUP en cours de constitution .... 24/05/2017 1 IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY Motivation: Scientific Drivers and technical considerations aiming to support the development of a cryogenic multi-object spectrograph for the future 2nd generation of instruments for the VLT ( ~2007/8). after ISAAC : field & wavelength coverage, MOS capability NIRMOS : K band, spectral resolution EMIR : Multi-IFU capability to start science production before NGST to reach maximum efficiency during the early epoch of NGST precursor of future IR instruments for ~20-100 m class telescopes, and a test bench for future Surveys. 24/05/2017 2 IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY Spectral Range 1 – 2.4 m Overall Transmission >70% Field of View 8’x8’ or 10’x10’; 2’x8’(10’) in multi-IFU mode Spectral Resolution 5000 (JH); 3000 (K) Image Quality 0.1 arcsec Sampling 0.11” or 0.15” Multiplexing >60 (MOS); 24 (IFS) KMOS-2 Main Characteristics IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY Telescope 24 steering mirrors Mask Exchange unit 24 Slicer units 24 relay optics MAIN OPTICAL CONCEPTS FOV 8’x8’ 10’x10’ Sampling 0.11” 0.15” Detector 4kx4k 4kx4k R 3000 3000 Multi-IFU FOV 2’x8’ 2’x10’ Individual Field 1’x0.6’ 1’x0.8’ Ind. IFU FOV 1.5”x1.5” 1.8”x1.8” Number of IFUs 24 24 Mirror mode switch Collimator Grating/mirror Exchange mech. Camera Filter wheel detector 24/05/2017 4 Scientific drivers extragalactic astronomy and cosmology IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY Formation and Evolution of galaxies 24/05/2017 + Supernovae at different redshifts IR stellar features in Local Galaxies Clusters of galaxies at very high-z (z S1) AGNs Spectroscopic near-IR follow-up of Wide-field, X and radio surveys 5 IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY ClickKMOS/VLT Science : z > 2 galaxiesto add title IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY ClickKMOS/VLT Science : z > 2 galaxiesto add title IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY The number of galaxies in the field of view of KMOS is ~105 per square degree, or a few thousand in a 10x10 arcmin² field, to K~22 (see Figure 1). At these magnitudes ~10% of galaxies should be at redshifts z>2. McCracken 2002 IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY Pettini et al. (01): ~20 LBGs available NIR spectra with ISAAC/VLT and NIRSPEC/KeckII 13/15 LBGs show e-lines t_exposure~10**4 sec K' (Vega)~ 20.5 - 21.5 Pettini et al. (01) IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY Constraining the formation epoch and the properties of the first sources Cosmological importance: re-ionisation epoch ? Sources (QSO, stars) ? nature of background radiation (UV ionising bg, cosmic IR bg) ? (Bechtold 1994, Miralda-Escude & Ostriker 1990, Haiman & Loeb 1997, Madau et al. 1999, Gnedin 2000, Tumlison & Shull 2000, Steidel et al. 2001, ... etc.) Soon detectable? NGST ground-based (see Haiman & Loeb 1997, Oh 1999, Tumlinson et al. 2001, Bromm et al. 2001, ...) Constraining the formation epoch and the properties of the first sources Key properties of Pop III stars / populations Initial mass function (IMF): Existence of very massive stars: up to ~ 1000 MM ?! (Abel et al. 1998, Uehara et al. 1996, Nakamura & Umemura 1999, 2001, Bromm etal. 1999) bimodal IMF or NO low mass stars ?! (Nakamura & Umemura 1999, 2001, Bromm et al. 1999) Key properties of Pop III stars / populations Nebular continuous emission .... 1 ... dominates the ZAMS spectrum at l 1400 A +Strong HeII lines: HeII l1640, HeII l3203,HeII l4686, ... Stellar SED Schaerer 2001 >> UNIQUE FEATURES OF POPIII STARBURSTS<< Ultra-deep near-IR photometry J-H Photo-z Identification of z>>6 sources H-K ClickKMOS Simulations to add title J 10^7 MM stellar halo Salpeter IMF: 1-500 MM t(exposure)=10^5 sec HeII 1640 H K H band: Detection of Pop III sources with EMIR/GTC and KMOS/VLT Already "hidden" in Ly-alpha surveys ?? (Tumlinson et al. 2001, Malhotra & Rhoads 2001) flux (HeII 1640) SFR=200 Msun/yr (IMF 1-100 Msun) SFR= 5 (IMF 50-500 Msun) redshift Follow-up spectroscopy But: distinction PopIII – QSO ? --> line profiles metal free objects at z <~ 5 expected ? Simulations of primordial galaxy populations FOV 4' * 4' HeII 1640 Oh, Haiman, Rees (2000) Ciardi, Ferrara, Governato, Jenkins (2000) IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY AGN studies: the most important lines IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY Science Goals Field (sq. deg) Evolution of the physical properties of galaxies at z>2 Nobjects Limiting magnitude (or line flux) N x 104 K=21 (spec) K=23 (phot) R~3000 (K) to R~5000 (JH) 0.3 to 2.5 Multi-IFU ~500 to N x 104 e-line ~ n x10-18 erg/s/cm R~3000 (K) to R~5000 (JH) 0.7 to 2.5 Multi-IFU N x 104 K=21 (spec) K=23 (phot) R~3000 (K) to R~5000 (JH) 0.3 to 2.5 - ~100 K=21 (spec) K=23 (phot) R~3000 (K) to R~5000 (JH) 0.3 to 2.5 IFU or multiIFU 1 Constraining the formation epoch and the properties of the first sources 1 LSS at z > 1 1 Clusters of galaxies at very high resdhift (z > 1) 1 R Wavelengt h coverage (m) IFU? Supernovae at different redshifts ~2 to 5 ~1000 K=21 (spec) K=23 (phot) R~3000 (K) to R~5000 (JH) 0.5 to 2.5 - IR stellar and ISM features in local galaxies ~2 to 5 ~100 K=19 (spec) R~5000 1 to 2.5 Multi-IFU Evolution of quasar/AGN 1 1000 K=21 (spec) R~5000 0.3 to 2.5 Multi-IFU Spectroscopic NIR follow-up of wide-field multi-wavelength surveys ~4 N x 104 K=21 (spec) K=23 (phot) R~3000 (K) to R~5000 (JH) 0.3 to 2.5 Multi-IFU Nx1 ~100 K=21 (spec) K=23 (phot) R~5000 0.3 to 2.5 Multi-IFU 24/05/2017 Galactic stellar studies 19