THE GRISM LENS-AMPLIFIED SURVEY FROM SPACE (GLASS). VII. THE DIVERSITY OF THE DISTRIBUTION OF STAR FORMATION IN CLUSTER AND FIELD GALAXIES AT 0.3 ≤ z ≤ 0.7

• Published in: The Astrophysical journal Vol. 833; no. 2; pp. 178 - 200
• Main Authors: Vulcani, Benedetta, Treu, Tommaso, Schmidt, Kasper B., Morishita, Takahiro, Dressler, Alan, Poggianti, Bianca M., Abramson, Louis, Brada, Marusa, Brammer, Gabriel B., Hoag, Austin, Malkan, Matthew, Pentericci, Laura, Trenti, Michele
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 20.12.2016; IOP Publishing
• Subjects: Astrophysics; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASYMMETRY; Deposition; Emitters; GALACTIC EVOLUTION; GALAXIES; galaxies: clusters: general; galaxies: evolution; galaxies: formation; galaxies: general; galaxies: star formation; GALAXY CLUSTERS; Galaxy distribution; Glass; INTERACTIONS; MASS; Morphology; Polls & surveys; RED SHIFT; SPACE; Spatial analysis; SPATIAL DISTRIBUTION; SPECTROSCOPY; Star & galaxy formation; Star clusters; Star formation; Star formation rate; STARS; Stars & galaxies; Stellar mass; STRIPPING
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/833/2/178

ABSTRACT Exploiting the slitless spectroscopy taken as part of the Grism Lens-Amplified Survey from Space (GLASS), we present an extended analysis of the spatial distribution of star formation in 76 galaxies in 10 clusters at . We use 85 foreground and background galaxies in the same redshift range as a field sample. The samples are well matched in stellar mass (108−1011 ) and star formation rate (0.5-50 ). We visually classify galaxies in terms of broad band morphology, H morphology, and likely physical process acting on the galaxy. Most H emitters have a spiral morphology (41% 8% in clusters, 51% 8% in the field), followed by mergers/interactions (28% 8%, 31% 7%, respectively) and early-type galaxies (remarkably as high as 29% 8% in clusters and 15% 6% in the field). A diversity of H morphologies is detected, suggesting a diversity of physical processes. In clusters, 30% 8% of the galaxies present a regular morphology, mostly consistent with star formation diffused uniformly across the stellar population (mostly in the disk component, when present). The second most common morphology (28% 8%) is asymmetric/jellyfish, consistent with ram-pressure stripping or other non-gravitational processes in 18% 8% of the cases. Ram-pressure stripping appears significantly less prominent in the field (2% 2%), where the most common morphology/mechanism appears to be consistent with minor gas-rich mergers or clump accretion. This work demonstrates that while environment-specific mechanisms affect galaxy evolution at this redshift, they are diverse and their effects are subtle. A full understanding of this complexity requires larger samples and detailed and spatially resolved physical models.