CaltechAUTHORS
Published December 2020 | Version Accepted Version + Published
Journal Article Open

Hα star formation main sequence in cluster and field galaxies at z ∼ 1.6

Creators

  • 1. ROR icon Andrés Bello University
  • 2. ROR icon University of California, Riverside
  • 3. ROR icon York University
  • 4. ROR icon European Space Astronomy Centre
  • 5. ROR icon University of Concepción
  • 6. ROR icon University of Waterloo
  • 7. ROR icon University of Kansas
  • 8. ROR icon University of California, Irvine
  • 9. ROR icon Lawrence Berkeley National Laboratory
  • 10. ROR icon University of California, Berkeley
  • 11. ROR icon Australian National University
  • 12. ROR icon Arizona State University
  • 13. ROR icon University of Montreal
  • 14. ROR icon Infrared Processing and Analysis Center
  • 15. ROR icon European Southern Observatory

Abstract

We calculate Hα-based star formation rates and determine the star formation rate–stellar mass relation for members of three Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS) clusters at z ∼ 1.6 and serendipitously identified field galaxies at similar redshifts to the clusters. We find similar star formation rates in cluster and field galaxies throughout our range of stellar masses. The results are comparable to those seen in other clusters at similar redshifts, and consistent with our previous photometric evidence for little quenching activity in clusters. One possible explanation for our results is that galaxies in our z ∼ 1.6 clusters have been accreted too recently to show signs of environmental quenching. It is also possible that the clusters are not yet dynamically mature enough to produce important environmental quenching effects shown to be important at low redshift, such as ram-pressure stripping or harassment.

Additional Information

© 2020 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 2020 September 15. Received 2020 September 14; in original form 2020 August 31. Published: 30 September 2020. This research uses observations obtained with MegaPrime/MegaCam, a joint project of the Canada-France-Hawaii Telescope (CFHT) and Comisariat a l'Énergie Atomique et aux Énergies Alternatives (CEA)/Dapnia, 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 (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This project also uses observations taken at the European Southern Observatory (ESO) Paranal Observatory (ESO programs 085.A-0166, 085.A-0613, 086.A-0398, 087.A-0145, 087.A-0483, 088.A-0639, 089.A-0125, and 091.A-0478), Las Campanas Observatory in Chile, the Keck Telescopes in Hawaii, and the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Our research team recognizes support from the following grants: Universidad Andres Bello internal research project DI-12-19/R (JN), Basal Center for Astrophysics and Associated Technologies (CATA) grant AFB-170002 (RD), and Atacama Large Millimeter Array - Comisión Nacional de Investigación en Ciencia y Tecnología (ALMA-CONICYT) grant no 31180051 (PC). This work was supported in part by National Science Foundation (NSF) grants AST-1517863, AST-1518257, and AST-1815475. Additional support was provided by the National Aeronautics and NASA through grants GO-15294 and AR-14289 from the Space Telescope Science Institute (STSCI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support is acknowledged from a European Space Agency (ESA) research fellowship (LJO) and by grant number 80NSSC17K0019 issued through the NASA Astrophysics Data Analysis Program (ADAP). Data Availability: The near-IR spectroscopy used in this paper is available to the public on the Keck Observatory Archive (KOA) Data Access Service: https://koa.ipac.caltech.edu/cgi-bin/KOA/nph-KOAlogin. Information about the nights of observation is available in the Appendix. To request access to other data, please ask the authors.

Attached Files

Published - staa2872.pdf

Accepted Version - 2009.07861.pdf

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2009.07861.pdf

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Additional details

Identifiers

Eprint ID
107453
Resolver ID
CaltechAUTHORS:20210113-105407239

Related works

Describes
https://arxiv.org/abs/2009.07861 (URL)
https://koa.ipac.caltech.edu/cgi-bin/KOA/nph-KOAlogin (URL)

Funding

NASA/JPL/Caltech
Universidad Andres Bello
DI-12-19/R
BASAL-CATA
AFB-170002
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)
31180051
NSF
AST-1517863
NSF
AST-1518257
NSF
AST-1815475
NASA
GO-15294
NASA
AR-14289
NASA
NAS 5-26555
European Space Agency (ESA)
NASA
80NSSC17K0019

Dates

Created
2021-01-13
Created from EPrint's datestamp field
Updated
2021-11-16
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
Infrared Processing and Analysis Center (IPAC)