Volume 592, August 2016
|Number of page(s)||16|
|Published online||01 August 2016|
A high definition view of the COSMOS Wall at z ~ 0.73 ⋆
1 INAF–Osservatorio Astronomico di Brera, via Brera, 28, 20159 Milano, Italy
2 INAF–IASF Milano, via Bassini 15, 20133, Milano, Italy
3 INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
4 Laboratoire d’Astrophysique de Marseille, CNRS-Université d’Aix-Marseille, 38 rue F. Joliot-Curie, 13388 Marseille, France
5 INAF–IASF Bologna, via P. Gobetti 101, 40129 Bologna, Italy
6 Department of Physics, University of Helsinki, G. Hallstromin katu 2a, 00014 Helsinki, Finland
7 CSST, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA
8 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, 181-8588 Tokyo, Japan
9 Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, 85748 Garching, Germany
10 Institute of Astronomy, ETH Zurich, 8093 Zürich, Switzerland
11 Instituto de Fisica y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Playa Ancha, Valparaíso, Chile
Received: 2 November 2015
Accepted: 2 May 2016
Aims. We present a study of a large filamentary structure at z ~ 0.73 in the field of the COSMOS survey, the so-called COSMOS Wall. This structure encompasses a comprehensive range of environments from a dense cluster and a number of galaxy groups to filaments, less dense regions, and adjacent voids. It thus provides a valuable laboratory for the accurate mapping of environmental effects on galaxy evolution at a look-back time of ~6.5 Gyr, when the Universe was roughly half its present age.
Methods. We performed deep spectroscopic observations with VIMOS at VLT of a K-band selected sample of galaxies in this complex structure, building a sample of galaxies complete in galaxy stellar mass down to a lower limit of log(ℳ∗/ℳ⊙) ~ 9.8, which is significantly deeper than previously available data. Thanks to its location within the COSMOS survey, each galaxy benefits from a wealth of ancillary information: HST-ACS data with I-band exposures down to IAB ~ 28 complemented by extensive multiwavelength ground- and space-based observations spanning the entire electromagnetic spectrum.
Results. In this paper we detail the survey strategy and weighting scheme adopted to account for the biases introduced by the photometric preselection of our targets. We present our galaxy stellar mass and rest-frame magnitudes estimates together with a group catalog obtained with our new data and their member galaxies color/mass distribution.
Conclusions. Owing to our new sample we can perform a detailed, high definition mapping of the complex COSMOS Wall structure. The sharp environmental information, coupled with high quality spectroscopic information and rich ancillary data available in the COSMOS field, enables a detailed study of galaxy properties as a function of local environment in a redshift slice where environmental effects are important, and in a stellar mass range where mass and environment driven effects are both at work.
Key words: galaxies: evolution / galaxies: groups: general / large-scale structure of Universe
© ESO, 2016
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