NOAO >   Observing Info >   Approved Programs >   2014A-0131

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Proposal Information for 2014A-0131


PI: Emanuele Daddi, CEA Saclay, edaddi@cea.fr
Address: Service d'Astrophysique, Orme des Merisiers, Gif sur Yvette, France 91191, France

CoI: Raphael Gobat, CEA Saclay
CoI: Veronica Strazzullo, CEA Saclay
CoI: Masato Onodera, ETH Zurich
CoI: Mark Dickinson, NOAO
CoI: Francesco Valentino, CEA Saclay
CoI: Mark Sargent, CEA Saclay
CoI: Alvio Renzini, INAF Padova
CoI: Maurilio Pannella, CEA Saclay
CoI: Matthieu Bethermin, CEA Saclay
CoI: Andrea Cimatti, University of Bologna
CoI: Marcella Carollo, ETH Zurich
CoI: Nobuo Arimoto, NAOJ

Title: High-z clusters and 'proto'-clusters. Can you tell the difference ?

Abstract: We propose to perform a deep search for \lya emission in the field of the cluster CL J1449+0856 at z_\rm spec=2. This is the most distant X-ray detected cluster known thus far, a massive system discovered at a redshift very close to the expected main formation epoch of massive cluster galaxies. The core of this cluster is populated by red galaxies, several of which already exhibit an early-type morphology. At the same time, there is clear evidence for strong star formation and AGN activity in the cluster core and in the surroundings. This structure, originally discovered as an overdensity of red Spitzer/IRAC objects, is seemingly very different from well characterized z\gtrsim2 \em protoclusters, identified through overdensities of \lya emitters and could be a later evolutionary stage of the latter. With deep Keck- LRIS narrow-band imaging of this structure we will detect faint \lya emitting galaxies (and possibly \lya blobs and/or diffuse light), allowing for a direct comparison with known \lya selected protoclusters, and a powerful investigation of the dependence of star formation with environment at z=2. A custom narrow-band filter (NB3640) is already available for LRIS that provides a perfect match for these observations. Since our filter is bluer than the [OII]3727 line, we expect no significant contamination from foreground emission line galaxies in our survey.


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