The Grism Lens-Amplified Survey from Space (GLASS). VIII. The Influence of the Cluster Properties on Hα Emitter Galaxies at 0.3 < z < 0.7

Journal
Date Issued
2017
Author(s)
•
Treu, Tommaso
•
•
Schmidt, Kasper B.
•
Dressler, Alan
•
Morshita, Takahiro
•
•
Malkan, Matthew
•
Hoag, Austin
•
Bradač, Marusa
•
Abramson, Louis
•
Trenti, Michele
•
•
von der Linden, Anja
•
Morris, Glenn
•
Wang, Xin
DOI
Abstract
Exploiting the data of the Grism Lens-Amplified Survey from Space (GLASS), we characterize the spatial distribution of star formation in 76 highly active star-forming galaxies in 10 clusters at 0.3< z< 0.7. All of these galaxies are likely restricted to first infall. In a companion paper, we contrast the properties of field and cluster galaxies, whereas here we correlate the properties of Hα emitters to a number of tracers of the cluster environment to investigate its role in driving galaxy transformations. Hα emitters are found in the clusters out to 0.5 virial radii, the maximum radius covered by GLASS. The peak of the Hα emission is offset with respect to the peak of the UV continuum. We decompose these offsets into a radial and a tangential component. The radial component points away from the cluster center in 60% of the cases, with 95% confidence. The decompositions agree with cosmological simulations; that is, the Hα emission offset correlates with galaxy velocity and ram-pressure stripping signatures. Trends between Hα emitter properties and surface mass density distributions and X-ray emissions emerge only for unrelaxed clusters. The lack of strong correlations with the global environment does not allow us to identify a unique environmental effect originating from the cluster center. In contrast, correlations between Hα morphology and local number density emerge. We conclude that local effects, uncorrelated to the cluster-centric radius, play a more important role in shaping galaxy properties.
Volume
837
Issue
2
Start page
126
Uri
Url
Issn Identifier
0004-637X
Ads BibCode
2017ApJ...837..126V
Rights
open.access
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