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Title: Star-Forming Brightest Cluster Galaxies at 0.25 < z < 1.25: A Transitioning Fuel Supply

Abstract

In this paper, we present a multiwavelength study of the 90 brightest cluster galaxies (BCGs) in a sample of galaxy clusters selected via the Sunyaev Zel'dovich effect by the South Pole Telescope, utilizing data from various ground- and space-based facilities. We infer the star-formation rate (SFR) for the BCG in each cluster—based on the UV and IR continuum luminosity, as well as the [O ii]λλ3726,3729 emission line luminosity in cases where spectroscopy is available—and find seven systems with SFR > 100 M⊙ yr-1. We find that the BCG SFR exceeds 10 M⊙ yr-1 in 31 of 90 (34%) cases at 0.25 < z < 1.25, compared to ~1%–5% at z ~ 0 from the literature. At z ≳ 1, this fraction increases to $${92}_{-31}^{+6}$$%, implying a steady decrease in the BCG SFR over the past ~9 Gyr. At low-z, we find that the specific SFR in BCGs is declining more slowly with time than for field or cluster galaxies, which is most likely due to the replenishing fuel from the cooling ICM in relaxed, cool core clusters. At z ≳ 0.6, the correlation between the cluster central entropy and BCG star formation—which is well established at z ~ 0—is not present. Instead, we find that the most star-forming BCGs at high-z are found in the cores of dynamically unrelaxed clusters. We use data from the Hubble Space Telescope to investigate the rest-frame near-UV morphology of a subsample of the most star-forming BCGs, and find complex, highly asymmetric UV morphologies on scales as large as ~50–60 kpc. Finally, the high fraction of star-forming BCGs hosted in unrelaxed, non-cool core clusters at early times suggests that the dominant mode of fueling star formation in BCGs may have recently transitioned from galaxy–galaxy interactions to ICM cooling.

Authors:
 [1];  [2];  [3];  [4];  [5];  [6];  [1];  [7];  [8];  [9];  [10];  [11];  [12];  [13];  [14];  [15];  [16];  [1];  [17];  [18] more »;  [11];  [5];  [19];  [6];  [20];  [21] « less
+ Show Author Affiliations
  1. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States). Kavli Inst. for Astrophysics and Space Research
  2. Univ. of Hawaii, Honolulu, HI (United States). Inst. for Astronomy (IFA)
  3. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States); Harvard Univ., Cambridge, MA (United States). Dept. of Physics
  4. Stanford Univ., CA (United States). Kavli Inst. for Particle Astrophysics and Cosmology; Stanford Univ., CA (United States). Dept. of Physics; SLAC National Accelerator Lab., Menlo Park, CA (United States)
  5. Argelander-Inst. for Astronomy, Bonn (Germany)
  6. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  7. Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Univ. of Chicago, IL (United States). Kavli Inst. for Cosmological Physics; Univ. of Chicago, IL (United States). Dept. of Astronomy and Astrophysics
  8. Univ. of Chicago, IL (United States). Kavli Inst. for Cosmological Physics; Argonne National Lab. (ANL), Argonne, IL (United States); Univ. of Chicago, IL (United States). Dept. of Physics
  9. Univ. of Missouri, Kansas City, MO (United States). Dept. of Physics and Astronomy
  10. Univ. of Chicago, IL (United States). Kavli Inst. for Cosmological Physics; Univ. of Chicago, IL (United States). Dept. of Astronomy and Astrophysics; Argonne National Lab. (ANL), Argonne, IL (United States); Univ. of Chicago, IL (United States). Dept. of Physics; Univ. of Chicago, IL (United States). Enrico Fermi Inst.
  11. Ludwig Maximilian Univ., Munich (Germany). Dept. of Physics
  12. Ludwig Maximilian Univ., Munich (Germany). Dept. of Physics; Excellence Cluster Universe, Garching (Germany)
  13. Univ. of Florida, Gainesville, FL (United States). Dept. of Astronomy
  14. Univ. of Montreal, Quebec (Canada). Dept. of Physics
  15. Univ. of California, Berkeley, CA (United States). Dept. of Physics
  16. Univ. of Arizona, Tucson, AZ (United States). Steward Observatory
  17. Univ. of Melbourne (Australia). School of Physics
  18. Case Western Reserve Univ., Cleveland, OH (United States). Physics Dept. Center for Education and Research in Cosmology and Astrophysics
  19. Univ. of California, Davis, CA (United States). Dept. of Physics
  20. Univ. of Illinois, Urbana, IL (United States). Dept. of Astronomy. Dept. of Physics
  21. Cerro Tololo Inter-American Observatory (CTIO), La Serena (Chile)
Publication Date:
Research Org.:
Argonne National Laboratory (ANL), Argonne, IL (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); SLAC National Accelerator Lab. (SLAC), Menlo Park, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP); National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); Natural Sciences and Engineering Research Council of Canada (NSERC); Australian Research Council
OSTI Identifier:
1271012
Alternate Identifier(s):
OSTI ID: 1254644
Report Number(s):
FERMILAB-PUB-16-174-AE-E
Journal ID: ISSN 1538-4357; 1445061
Grant/Contract Number:  
AC02-06CH11357
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 817; Journal Issue: 2; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; galaxies: clusters: intracluster medium; galaxies: elliptical and lenticular, cD; galaxies: starburst; X-rays: galaxies: clusters

Citation Formats

McDonald, M., Stalder, B., Bayliss, M., Allen, S. W., Applegate, D. E., Ashby, M. L. N., Bautz, M., Benson, B. A., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chiu, I., Desai, S., Gonzalez, A. H., Hlavacek-Larrondo, J., Holzapfel, W. L., Marrone, D. P., Miller, E. D., Reichardt, C. L., Saliwanchik, B. R., Saro, A., Schrabback, T., Stanford, S. A., Stark, A. A., Vieira, J. D., and Zenteno, A. Star-Forming Brightest Cluster Galaxies at 0.25 < z < 1.25: A Transitioning Fuel Supply. United States: N. p., 2016. Web. doi:10.3847/0004-637X/817/2/86.
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McDonald, M., Stalder, B., Bayliss, M., Allen, S. W., Applegate, D. E., Ashby, M. L. N., Bautz, M., Benson, B. A., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chiu, I., Desai, S., Gonzalez, A. H., Hlavacek-Larrondo, J., Holzapfel, W. L., Marrone, D. P., Miller, E. D., Reichardt, C. L., Saliwanchik, B. R., Saro, A., Schrabback, T., Stanford, S. A., Stark, A. A., Vieira, J. D., & Zenteno, A. Star-Forming Brightest Cluster Galaxies at 0.25 < z < 1.25: A Transitioning Fuel Supply. United States. https://doi.org/10.3847/0004-637X/817/2/86
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McDonald, M., Stalder, B., Bayliss, M., Allen, S. W., Applegate, D. E., Ashby, M. L. N., Bautz, M., Benson, B. A., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chiu, I., Desai, S., Gonzalez, A. H., Hlavacek-Larrondo, J., Holzapfel, W. L., Marrone, D. P., Miller, E. D., Reichardt, C. L., Saliwanchik, B. R., Saro, A., Schrabback, T., Stanford, S. A., Stark, A. A., Vieira, J. D., and Zenteno, A. Fri . "Star-Forming Brightest Cluster Galaxies at 0.25 < z < 1.25: A Transitioning Fuel Supply". United States. https://doi.org/10.3847/0004-637X/817/2/86. https://www.osti.gov/servlets/purl/1271012.
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@article{osti_1271012,
title = {Star-Forming Brightest Cluster Galaxies at 0.25 < z < 1.25: A Transitioning Fuel Supply},
author = {McDonald, M. and Stalder, B. and Bayliss, M. and Allen, S. W. and Applegate, D. E. and Ashby, M. L. N. and Bautz, M. and Benson, B. A. and Bleem, L. E. and Brodwin, M. and Carlstrom, J. E. and Chiu, I. and Desai, S. and Gonzalez, A. H. and Hlavacek-Larrondo, J. and Holzapfel, W. L. and Marrone, D. P. and Miller, E. D. and Reichardt, C. L. and Saliwanchik, B. R. and Saro, A. and Schrabback, T. and Stanford, S. A. and Stark, A. A. and Vieira, J. D. and Zenteno, A.},
abstractNote = {In this paper, we present a multiwavelength study of the 90 brightest cluster galaxies (BCGs) in a sample of galaxy clusters selected via the Sunyaev Zel'dovich effect by the South Pole Telescope, utilizing data from various ground- and space-based facilities. We infer the star-formation rate (SFR) for the BCG in each cluster—based on the UV and IR continuum luminosity, as well as the [O ii]λλ3726,3729 emission line luminosity in cases where spectroscopy is available—and find seven systems with SFR > 100 M⊙ yr-1. We find that the BCG SFR exceeds 10 M⊙ yr-1 in 31 of 90 (34%) cases at 0.25 < z < 1.25, compared to ~1%–5% at z ~ 0 from the literature. At z ≳ 1, this fraction increases to ${92}_{-31}^{+6}$%, implying a steady decrease in the BCG SFR over the past ~9 Gyr. At low-z, we find that the specific SFR in BCGs is declining more slowly with time than for field or cluster galaxies, which is most likely due to the replenishing fuel from the cooling ICM in relaxed, cool core clusters. At z ≳ 0.6, the correlation between the cluster central entropy and BCG star formation—which is well established at z ~ 0—is not present. Instead, we find that the most star-forming BCGs at high-z are found in the cores of dynamically unrelaxed clusters. We use data from the Hubble Space Telescope to investigate the rest-frame near-UV morphology of a subsample of the most star-forming BCGs, and find complex, highly asymmetric UV morphologies on scales as large as ~50–60 kpc. Finally, the high fraction of star-forming BCGs hosted in unrelaxed, non-cool core clusters at early times suggests that the dominant mode of fueling star formation in BCGs may have recently transitioned from galaxy–galaxy interactions to ICM cooling.},
doi = {10.3847/0004-637X/817/2/86},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 817,
place = {United States},
year = {Fri Jan 22 00:00:00 EST 2016},
month = {Fri Jan 22 00:00:00 EST 2016}
}
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