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|Title:||BUDHIES II: a phase-space view of H I gas stripping and star formation quenching in cluster galaxies||Authors:||Jaffé, Yara L.
Candlish, Graeme N.
POGGIANTI, Bianca Maria
Verheijen, Marc A. W.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||448||Issue:||2||First Page:||1715||Abstract:||We investigate the effect of ram-pressure from the intracluster medium on the stripping of H I gas in galaxies in a massive, relaxed, X-ray bright, galaxy cluster at z = 0.2 from the Blind Ultra Deep H I Environmental Survey (BUDHIES). We use cosmological simulations, and velocity versus position phase-space diagrams to infer the orbital histories of the cluster galaxies. In particular, we embed a simple analytical description of ram-pressure stripping in the simulations to identify the regions in phase-space where galaxies are more likely to have been sufficiently stripped of their H I gas to fall below the detection limit of our survey. We find a striking agreement between the model predictions and the observed location of H I-detected and non-detected blue (late-type) galaxies in phase-space, strongly implying that ram-pressure plays a key role in the gas removal from galaxies, and that this can happen during their first infall into the cluster. However, we also find a significant number of gas-poor, red (early-type) galaxies in the infall region of the cluster that cannot easily be explained with our model of ram-pressure stripping alone. We discuss different possible additional mechanisms that could be at play, including the pre-processing of galaxies in their previous environment. Our results are strengthened by the distribution of galaxy colours (optical and UV) in phase-space, that suggests that after a (gas-rich) field galaxy falls into the cluster, it will lose its gas via ram-pressure stripping, and as it settles into the cluster, its star formation will decay until it is completely quenched. Finally, this work demonstrates the utility of phase-space diagrams to analyse the physical processes driving the evolution of cluster galaxies, in particular H I gas stripping.||Acknowledgments:||YJ gratefully acknowledges support by FONDECYT grant no. 3130476, and thanks Professor Alfonso Aragón-Salamanca, Kyle Oman, Chris Haines, Jacqueline van Gorkom, and Jonathan Hernandez-Fernandez for useful discussions on phase-space analysis and/or the data utilized in this paper. RS acknowledges FONDECYT grant no. 3120135, and gratefully acknowledges Professor Brad Gibson and Professor Alexander Knebe for providing access to the cosmological simulations on which the modelling in this study is based. GC and YKS gratefully acknowledge support by FONDECYT grants no. 3130480 and 3130470, respectively. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/ . The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington.||URI:||http://hdl.handle.net/20.500.12386/23088||URL:||https://academic.oup.com/mnras/article/448/2/1715/1061483||ISSN:||0035-8711||DOI:||10.1093/mnras/stv100||Bibcode ADS:||2015MNRAS.448.1715J||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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