GLACE survey: OSIRIS/GTC tuneable filter Hα imaging of the rich galaxy cluster ZwCl 0024.0+1652 at z = 0.395

I. Survey presentation, TF data reduction techniques, and catalogue^⋆

¹ European Space Astronomy Centre (ESAC)/ESA, PO Box 78, 28690 Villanueva de la Canada, Madrid, Spain
e-mail: miguel.sanchez@sciops.esa.int
² ISDEFE, Beatriz de Bobadilla 3, 28040 Madrid, Spain
³ Instituto de Astrofísica de Canarias, 38205, La Laguna, 38701, La Laguna, Tenerife, Spain
⁴ Universidad de La Laguna, 38207 Tenerife, Spain
⁵ Instituto de Astrofísica de Andalucía, CSIC, 18080 Granada, Spain
⁶ School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD, UK
⁷ GEPI, Observatoire de Paris & CNRS, 92195 Meudon, France
⁸ Centro de Astrobiología, INTA-CSIC, 28850 Torrejón de Ardoz, Madrid, Spain
⁹ INAF, Osservatorio Astronomico di Trieste, 34143 Trieste, Italy
¹⁰ Department of Physics, University of Bristol, Bristol, BS8 1TH, UK
¹¹ Institut de Ciències de l’Espai (CSIC), 08193 Barcelona, Spain
¹² Instituto Polictécnico Nacional, 07738 México D.F., México
¹³ Laboratoire AIM Saclay, CEA/IRFU, CNRS/INSU, Université Paris Diderot, 75014 Paris, France
¹⁴ Department of Physics, McGill University, Montreal, H3A 2T8, Quebec, Canada
¹⁵ Instituto de Física de Cantabria, CSIC-Univ. de Cantabria, 39005 Santander, Spain
¹⁶ Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Correo Central, Casilla 36-D, Correo Central, Santiago, Chile
¹⁷ University College, Belfield, Dublin Bristol, BS8 1 TH, Ireland
¹⁸ INAF, Osservatorio Astronomico di Padova, 35122 Padova, Italy
¹⁹ Institute for Computational Cosmology, Durham University, Durham DH1 3LE, UK
²⁰ Institute of Astro- and Particle Physics, University of Innsbruck, 6020 Innsbruck, Austria
²¹ Centro de Estudios de Física del Cosmos de Aragón, 44001 Teruel, Spain
²² Dipartimento di Fisica, Università degli Studi di Milano, 20133 Milano, Italy
²³ Dipartimento di Fisica, Università di Torino, 10125 Torino, Italy
²⁴ Istituto Nazionale di Fisica Nucleare (INFN), sezione di Torino, 10125 Torino, Italy
²⁵ Departamento de Astronomia, Instituto de Astronomia, Geofísica e Ciências Atmosféricas da USP, 1226 São Paulo, Brazil
²⁶ Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK
²⁷ European Southern Observatory, 85748 Garching, Germany
²⁸ INAF-Osservatorio Astrofisico di Arcetri, 50125 Florence, Italy
²⁹ Departamento de Astrofísica, Facultad de CC. Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain

Received: 6 January 2015
Accepted: 10 February 2015

Abstract

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 × r_vir. 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.