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|Title:||The Grism Lens-Amplified Survey from Space (GLASS). V. Extent and Spatial Distribution of Star Formation in z ~ 0.5 Cluster Galaxies||Authors:||Vulcani, Benedetta
Schmidt, Kasper B.
POGGIANTI, Bianca Maria
Brammer, Gabriel B.
von der Linden, Anja
|Issue Date:||2015||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||814||Issue:||2||First Page:||161||Abstract:||We present the first study of the spatial distribution of star formation in z ̃ 0.5 cluster galaxies. The analysis is based on data taken with the Wide Field Camera 3 as part of the Grism Lens-Amplified Survey from Space (GLASS). We illustrate the methodology by focusing on two clusters (MACS 0717.5+3745 and MACS 1423.8+2404) with different morphologies (one relaxed and one merging) and use foreground and background galaxies as a field control sample. The cluster+field sample consists of 42 galaxies with stellar masses in the range 108-1011 M☉ and star formation rates in the range 1-20 M☉ yr-1. Both in clusters and in the field, Hα is more extended than the rest-frame UV continuum in 60% of the cases, consistent with diffuse star formation and inside-out growth. In ̃20% of the cases, the Hα emission appears more extended in cluster galaxies than in the field, pointing perhaps to ionized gas being stripped and/or star formation being enhanced at large radii. The peak of the Hα emission and that of the continuum are offset by less than 1 kpc. We investigate trends with the hot gas density as traced by the X-ray emission, and with the surface mass density as inferred from gravitational lens models, and find no conclusive results. The diversity of morphologies and sizes observed in Hα illustrates the complexity of the environmental processes that regulate star formation. Upcoming analysis of the full GLASS data set will increase our sample size by almost an order of magnitude, verifying and strengthening the inference from this initial data set.||Acknowledgments:||Support for GLASS ( HST -GO-13459) was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. We are very grateful to the staff of the Space Telescope for their assistance in planning, scheduling, and executing the observations. B.V. acknowledges the support from the World Premier International Research Center Initiative (WPI), MEXT, Japan, and the Kakenhi Grant-in-Aid for Young Scientists (B)(26870140) from the Japan Society for the Promotion of Science (JSPS). We thank the referee for useful comments that helped us to strengthen our results.||URI:||http://hdl.handle.net/20.500.12386/29656||URL:||https://iopscience.iop.org/article/10.1088/0004-637X/814/2/161||ISSN:||0004-637X||DOI:||10.1088/0004-637X/814/2/161||Bibcode ADS:||2015ApJ...814..161V||Fulltext:||restricted|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Jan 16, 2021
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