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Published January 2019 | Published + Accepted Version
Journal Article Open

Searching for environmental effects on galaxy kinematics in groups and clusters at z ∼ 1 from the ORELSE survey


We present an investigation of the dependence of galaxy kinematics on the environment for a sample of 94 star-forming galaxies at z ∼ 0.9 from the ORELSE survey. ORELSE is a large photometric and spectroscopic campaign dedicated to mapping out and characterizing galaxy properties across a full range of environments in 15 fields containing large-scale structures (LSSs) in a redshift range of 0.6 < z < 1.3. We constrained the rotation velocity for our kinematic sample in an ORELSE field, containing the SC1604 supercluster, by fitting high-resolution semi-analytical models to the data. We constructed the stellar-mass/B-band Tully–Fisher relation and found no dependence of the intrinsic scatter on both local and global environment. Moreover, we compared the stellar-to-dynamical mass ratio (M*/M_(dyn)) of SC1604 galaxies to those residing in less dense local environment by leveraging data from the HR-COSMOS sample. We found that, at fixed stellar mass, SC1604 galaxies have ∼30 per cent smaller dynamical masses on average. By comparing the distributions of the galaxy parameters that define M_(dyn) (i.e., circular velocity and the characteristic radius r_(2.2)) between SC1604 and HR-COSMOS, we found that smaller dynamical masses are mostly caused by smaller r_(2.2) for SC1604 galaxies. We also observed that SC1604 galaxies in general show ∼20 per cent lower stellar specific angular momentum (j*) with respect to the HR-COSMOS sample. Adopting literature estimates for (1) the excess rate of galaxy–galaxy mergers in intermediate/high-density environments and (2) the average amount of j* loss per merger event, we investigated the possibility that galaxy mergers are mainly responsible for the loss of angular momentum in higher density environments.

Additional Information

© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2018 October 21. Received 2018 October 12; in original form 2018 July 12. Published: 25 October 2018. We thank Olga Cucciati for helping with the 3D rendering. This material is based upon work supported by the National Science Foundation under Grant No. 1411943 and the National Aeronautics and Space Administration under NASA Grant Number NNX15AK92G. A portion of this work made use of the Peloton computing cluster operated by the Division of Mathematical and Physical Sciences at the University of California, Davis. This study is based, in part, on data collected at the Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. This work is based, in part, on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. UKIRT is supported by NASA and operated under an agreement among the University of Hawaii, the University of Arizona, and Lockheed Martin Advanced Technology Center; operations are enabled through the cooperation of the East Asian Observatory. When the data reported here were acquired, UKIRT was operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K. This study is also based, in part, on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, and the Canada-France-Hawaii Telescope which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawai'i. The spectroscopic observations used in this work were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We wish to thank the indigenous Hawaiian community for allowing us to be guests on their sacred mountain, a privilege, without which, this work would not have been possible. We are most fortunate to be able to conduct observations from this site.

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Accepted Version - 1807.04763.pdf


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August 19, 2023
October 20, 2023