Bibcode
Sánchez-Portal, M.; Pintos-Castro, I.; Pérez-Martínez, R.; Cepa, J.; Pérez García, A. M.; Domínguez-Sánchez, H.; Bongiovanni, A.; Serra, A. L.; Alfaro, E.; Altieri, B.; Aragón-Salamanca, A.; Balkowski, C.; Biviano, A.; Bremer, M.; Castander, F.; Castañeda, H.; Castro-Rodríguez, N.; Chies-Santos, A. L.; Coia, D.; Diaferio, A.; Duc, P. A.; Ederoclite, A.; Geach, J.; González-Serrano, I.; Haines, C. P.; McBreen, B.; Metcalfe, L.; Oteo, I.; Pérez-Fournón, I.; Poggianti, B.; Polednikova, J.; Ramón-Pérez, M.; Rodríguez-Espinosa, J. M.; Santos, J. S.; Smail, I.; Smith, G. P.; Temporin, S.; Valtchanov, I.
Bibliographical reference
Astronomy and Astrophysics, Volume 578, id.A30, 22 pp.
Advertised on:
6
2015
Journal
Citations
15
Refereed citations
13
Description
The cores of clusters at 0 ≲ z ≲ 1 are dominated by quiescent
early-type galaxies, whereas the field is dominated by star-forming
late-type galaxies. Clusters grow through the accretion of galaxies and
groups from the surrounding field, which implies that galaxy properties,
notably the star formation ability, are altered as they fall into
overdense regions. The critical issues for understanding 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 of the variations in galaxy properties (star
formation, AGN activity, and morphology) as a function of environment in
a representative and well-studied sample of clusters. To address these
questions, the GLACE survey is making a deep panoramic survey of
emission line galaxies (ELG), mapping a set of optical lines ([O ii], [O
iii], Hβ andHα/[N ii] 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), to cover a rest frame velocity range of
several thousand km s-1 centred on the mean cluster redshift,
and scanned for the full TF field of view of an 8 arcmin diameter. Here
we present the first results of the GLACE project, targeting the
Hα/[N ii] lines in the intermediate-redshift cluster ZwCl
0024.0+1652 at z = 0.395. Two pointings have been performed that cover
~2 × rvir. We discuss the specific techniques devised
to process the TF tomography observations in order to generate the
catalogue of cluster Hα emitters, which contains more than 200
sources down to a star formation rate (SFR) ≲1
M⊙/yr. An ancillary broadband catalogue is constructed,
allowing us to discriminate line interlopers by means of colour
diagnostics. The final catalogue contains 174 unique cluster sources.
The AGN population is distinguished using different diagnostics and
found to be ~37% of the ELG population. The median SFR of the
star-forming population is 1.4 M⊙/yr. We studied the
spatial distribution of ELG and confirm the existence of two components
in the redshift space. Finally, we exploited the outstanding spectral
resolution of the TF, attempting to estimate the cluster mass from ELG
dynamics, finding M200 = (4.1 ± 0.2) ×
1014 M⊙ h-1, in agreement with
previous weak-lensing estimates.
Table 5 is available in electronic form at http://www.aanda.org
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