Volume 566, June 2014
|Number of page(s)||21|
|Section||Cosmology (including clusters of galaxies)|
|Published online||05 June 2014|
III. Equivalent width measurements, spectral properties, and evolution of local cluster galaxies⋆,⋆⋆,⋆⋆⋆
Sterrenkundig Observatorium Vakgroep Fysica en Sterrenkunde Universiteit
Krijgslaan 281, S9,
2 INAF-Osservatorio Astronomico di Padova, vicolo Osservatorio 5, 35122 Padova, Italy
3 Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland
4 Dipartimento di Astronomia, vicolo Osservatorio 2, 35122 Padova, Italy
5 Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan 1, planta 2, 44001 Teruel, Spain
6 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, VIC 3122 Howthorn, Australia
7 Australian Astronomical Observatory, NSW, 2113 Sydney, Australia
8 Observatories of the Carnegie Institution of Washington, Pasadena CA 91101, USA
9 Niels Bohr Institute, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
10 Specola Vaticana, 00120 Stato Città del Vaticano, Italy
Received: 27 November 2013
Accepted: 13 February 2014
Context. Cluster galaxies are the ideal sites to look at when studying the influence of the environment on the various aspects of the evolution of galaxies, such as the changes in their stellar content and morphological transformations. In the framework of wings, the WIde-field Nearby Galaxy-cluster Survey, we have obtained optical spectra for ~6000 galaxies selected in fields centred on 48 local (0.04 < z < 0.07) X-ray selected clusters to tackle these issues.
Aims. By classifying the spectra based on given spectral lines, we investigate the frequency of the various spectral types as a function of both the clusters’ properties and the galaxies’ characteristics. In this way, using the same classification criteria adopted for studies at higher redshift, we can consistently compare the properties of the local cluster population to those of their more distant counterparts.
Methods. We describe a method that we have developed to automatically measure the equivalent width of spectral lines in a robust way, even in spectra with a non optimal signal-to-noise ratio. This way, we can derive a spectral classification reflecting the stellar content, based on the presence and strength of the [Oii] and Hδ lines.
Results. After a quality check, we are able to measure 4381 of the ~6000 originally observed spectra in the fields of 48 clusters, of which 2744 are spectroscopically confirmed cluster members. The spectral classification is then analysed as a function of galaxies’ luminosity, stellar mass, morphology, local density, and host cluster’s global properties and compared to higher redshift samples (MORPHS and EDisCS). The vast majority of galaxies in the local clusters population are passive objects, being also the most luminous and massive. At a magnitude limit of MV < −18, galaxies in a post-starburst phase represent only ~11% of the cluster population, and this fraction is reduced to ~5% at MV < −19.5, which compares to the 18% at the same magnitude limit for high-z clusters. “Normal” star-forming galaxies (e(c)) are proportionally more common in local clusters.
Conclusions. The relative occurrence of post-starbursts suggests a very similar quenching efficiency in clusters at redshifts in the 0 to ~1 range. Furthermore, more important than the global environment, the local density seems to be the main driver of galaxy evolution in local clusters at least with respect to their stellar populations content.
Key words: galaxies: clusters: general / galaxies: evolution / galaxies: stellar content / methods: data analysis
Based on observations taken at the Anglo Australian Telescope (3.9 m- AAT) and at the William Herschel Telescope (4.2 m-WHT).
Full Table A.1 is available in electronic form at both the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/566/A32 and by querying the wings database at http://web.oapd.inaf.it/wings/new/index.html
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2014
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