Bibcode
Sánchez-Portal, M.; Pintos-Castro, I.; Pérez-Martínez, R.; Cepa, J.; Pérez García, A. M.; Bongiovanni, A.; GLACE Team
Referencia bibliográfica
Highlights of Spanish Astrophysics VIII, Proceedings of the XI Scientific Meeting of the Spanish Astronomical Society held on September 8-12, 2014, in Teruel, Spain, ISBN 978-84-606-8760-3. A. J. Cenarro, F. Figueras, C. Hernández-Monteagudo, J. Trujillo Bueno, and L. Valdivielso (eds.), p. 381-381
Advertised on:
5
2015
Número de citas
0
Número de citas referidas
0
Descripción
Cluster cores are dominated by quiescent early-type galaxies, whereas
the field is dominated by star-forming late-type galaxies. Galaxy
properties, notably the star formation ability, are altered as they fall
into overdense regions. The critical issues to understand this evolution
are how the truncation of star formation is connected to the
morphological transformation and what physical mechanism is responsible
for these changes.The GaLAxy Cluster Evolution Survey (GLACE) is
conducting a thorough study on the variation of galaxy properties (star
formation, AGN activity and morphology) as a function of environment in
a representative and uniquely well-studied sample of clusters. GLACE is
a deep panoramic survey of emission line galaxies (ELG), mapping a set
of optical lines (oii, oiii, Hβ and Hanii\ when possible) in
several galaxy clusters at z ˜ 0.40, 0.63 and 0.86. Using the
Tunable Filters (TF) of the OSIRIS instrument at the 10.4 m GTC
telescope, the GLACE survey applies the technique of TF tomography: for
each line, a set of images are taken through the OSIRIS TF, each image
tuned at a different wavelength (equally spaced), so that a rest frame
velocity range of several thousands km s^{-1} centred at the mean
cluster redshift is scanned for the full TF field of view of 8 arcmin in
diameter. Here we present results on the Hanii\ mapping of the
intermediate redshift cluster ZwCl 0024.0+1652 at z= 0.395. Two
pointings, covering ˜ 2 × r_{vir} have been performed. The
ELG sample contains 174 unique cluster sources down to a star formation
rate (SFR) ≲ 1 M_{⊙} yr^{-1}.