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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7108
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dc.contributor.authorDeger, Sinan-
dc.contributor.authorRudnick, Gregory-
dc.contributor.authorKelkar, Kshitija-
dc.date.accessioned2018-12-25T18:39:12Z-
dc.date.available2018-12-25T18:39:12Z-
dc.date.issued2018-12-10-
dc.identifier.citationAstrophysical Journal, 2018, Vol. 869, p6en_US
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357-(Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7108-
dc.descriptionOpen Accessen_US
dc.description.abstractWe study the fraction of tidal interactions and mergers (TIMs) with well-identified observability timescales (f TIM) in group, cluster, and accompanying field galaxies and its dependence on redshift (z), cluster velocity dispersion (σ), and environment analyzing Hubble Space Telescope/ACS images and catalogs from the ESO Distant Cluster Survey. Our sample consists of 11 clusters, seven groups, and accompanying field galaxies at 0.4 ≤ z ≤ 0.8. We derive f TIM using both a visual classification of galaxy morphologies and an automated method, the G − M 20 method. We calibrate this method using the visual classifications that were performed on a subset of our sample. We find marginal evidence for a trend between f TIM and z, in that higher z values correspond to higher f TIM. However, we also cannot rule out the null hypothesis of no correlation at higher than 68% confidence. No trend is present between f TIM and σ. We find that f TIM shows suggestive peaks in groups, and tentatively in clusters at R > 0.5 × R 200, implying that f TIM gets boosted in these intermediate-density environments. However, our analysis of the local densities of our cluster sample does not reveal a trend between f TIM and density, except for a potential enhancement at the very highest densities. We also perform an analysis of projected radius–velocity phase space for our cluster members. Our results reveal that TIM and undisturbed galaxies only have a 6% probability of having been drawn from the same parent population in their velocity distribution and 37% in radii, in agreement with the modest differences obtained in f TIM at the clusters.en_US
dc.language.isoenen_US
dc.publisherIOP Sciences for The American Astronomical Societyen_US
dc.relation.urihttp://adsabs.harvard.edu/abs/2018ApJ...869....6Den_US
dc.relation.urihttps://arxiv.org/abs/1810.01430en_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/aaeb87en_US
dc.rights2018, The American Astronomical Societyen_US
dc.subjectclustersen_US
dc.subjectgeneral–galaxiesen_US
dc.subjectevolution–galaxiesen_US
dc.subjectgroupsen_US
dc.subjectinteractionsen_US
dc.titleTidal Interactions and Mergers in Intermediate Redshift EDisCS Clustersen_US
dc.typeArticleen_US
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