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VLT 2ème génération

VLT 2ème génération. MUSE et KMOS PNC Octobre 2002. MUSE. Lyon, Marseille Cambridge, Oxford, Durham Leiden, Zürich, Postdam A 3D deep field to study the progenitors of normal nearby galaxies up to z=7 Detailed studies of nearby normal, starburst and interacting galaxies

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VLT 2ème génération

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  1. VLT 2ème génération MUSE et KMOS PNC Octobre 2002

  2. MUSE • Lyon, Marseille • Cambridge, Oxford, Durham • Leiden, Zürich, Postdam A 3D deep field to study the progenitors of normal nearby galaxiesup to z=7 Detailed studies of nearby normal, starburst and interacting galaxies Massive spectroscopy of resolved stellar populations

  3. Science Requirements • Improve by several magnitudes the detection limit • Spectroscopic follow-up of HDF • Ly-break galaxies up to I~27-28 • Get spatially resolved spectroscopic information • Internal physics of galaxies up to z~3 • Detect high z galaxies (z>5) • Search for objects that are not detectable in broad band imaging surveys • Lya emitters (z<7)

  4. Recherche actuelle des émetteurs Lyalpha • Filtres étroits, grand champ, domaine étroit de z • 2 10-17 erg/cm2/s • Longue fente: très petit champ, grand domaine en z • 1-3 Lya émetteur par arcmin² • Prédictions à 5 10-19 erg/cm2/s • Redshift range Number arcmin-2 • 4.5-7 83 • 3.5-7 225 • 2.5-7 506

  5. Caractéristiques Champ 1’ x 1’ Résolution spatiale MCAO Sampling 0.2 arcsec Résolution spectrale 1000 à 2000 Domaine spectral 0.5 à 1 micron 24 éléments de 2k x 4k Profondeur R ~ 28 90 000 pixels spatiaux 2048 éléments spectraux  184 millions de pixels (VIMOS, 3.5 millions)

  6. Volume de données 1 image = 0.7 Gb 1 nuit = 100 Gb Un champ profond sera fait en 10 nuits L’instrument est prévu pour arriver en 2009-2010 Avec JWST et ALMA Très complémentaires

  7. KMOS 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, ... Instrument NIR cryogénique

  8. KMOS: caractéristiques Spectral Range 1 – 2.4 m 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) Détecteurs 4k x 4k

  9. KMOS Drivers scientifiques •  Formation et Evolution des galaxies • Supernovae à differents redshifts • IR stellaire dans les galaxies locales • Amas de galaxies à grand-z (z ~ 1) • AGNs • Follow-up spectro NIR des surveys grand champ radio, X, etc..

  10. KMOS IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY ClickKMOS/VLT Science : z > 2 galaxiesto add title

  11. KMOS IMAGING MULTI-SLIT SPECTROSCOPY INTEGRAL FIELD SPECTROSCOPY

  12. Etat actuel Aujourd’hui seulement 20 LBG ont été observés spectroscopiquement 13-15 ont des raies d’émission (Pettini et al 2001) T(int) = 10 000 sec NIR ISAAC/VLT NIRSPEC/KECK Les premiers objets (IMF?) +raies HeII fortes:HeII l1640, HeII l3203, HeII l4686, ... Schaerer 2001

  13. KMOS1 PI: R. Bender (USM) et MPE-Garching Reiner Hofman (MPE) Ray Sharples, Durham Edinburg, Oxford, Bristol KMOS2 KMOS1

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