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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];  [8];  [10];  [11];  [12];  [13];  [14];  [15];  [1];  [16];  [17] more »;  [10];  [5];  [18];  [6];  [19];  [20] « less
  1. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
  2. Univ. of Hawaii, Honolulu, HI (United States)
  3. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States); Harvard Univ., Cambridge, MA (United States)
  4. Stanford Univ., Stanford, CA (United States); SLAC National Accelerator Lab., Menlo Park, CA (United States)
  5. Argelander-Institut fur Astronomie, 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, Chicago, IL (United States)
  8. Univ. of Chicago, Chicago, IL (United States); Argonne National Lab. (ANL), Argonne, IL (United States)
  9. Univ. of Missouri, Kansas City, MO (United States)
  10. Ludwig Maximilian Univ., Munchen (Germany)
  11. Ludwig Maximilian Univ., Munchen (Germany); Excellence Cluster Universe, Garching (Germany)
  12. Univ. of Florida, Gainesville, FL (United States)
  13. Univ. of Montreal, Quebec (Canada)
  14. Univ. of California, Berkeley, CA (United States)
  15. Univ. of Arizona, Tucson, AZ (United States)
  16. Univ. of Melbourne, Parkville (Australia)
  17. Case Western Reserve Univ., Cleveland, OH (United States)
  18. Univ. of California, Davis, CA (United States)
  19. Univ. of Illinois, Urbana, IL (United States)
  20. Cerro Tololo Inter-American Observator, La Serena (Chile)
Publication Date:
Research Org.:
Argonne National Lab. (ANL), Argonne, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); SLAC National Accelerator Lab. (SLAC), Menlo Park, CA (United States)
Sponsoring Org.:
National Aeronautic and Space Administration (NASA); National Science Foundation (NSF); Natural Sciences and Engineering Research Council of Canada (NSERC); Australian Research Council; USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
OSTI Identifier:
1271012
Alternate Identifier(s):
OSTI ID: 1254644
Report Number(s):
FERMILAB-PUB-16-174-AE-E
Journal ID: ISSN 1538-4357; 127626
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.
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. doi:10.3847/0004-637X/817/2/86.
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. doi:10.3847/0004-637X/817/2/86. https://www.osti.gov/servlets/purl/1271012.
@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 = {2016},
month = {1}
}

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Thermal Instability with Anisotropic Thermal Conduction and Adiabatic Cosmic Rays: Implications for cold Filaments in Galaxy Clusters
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SUZAKU OBSERVATIONS OF THE TYPE 2 QSO IN THE CENTRAL GALAXY OF THE PHOENIX CLUSTER
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Thermal conduction and reduced cooling flows in galaxy clusters
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COOLING TIME, FREEFALL TIME, AND PRECIPITATION IN THE CORES OF ACCEPT GALAXY CLUSTERS
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Regulation of star formation in giant galaxies by precipitation, feedback and conduction
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Star Formation in High-Redshift Cluster Ellipticals
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    Works referencing / citing this record:

    Cooling flow solutions for the circumgalactic medium
    journal, July 2019

    • Stern, Jonathan; Fielding, Drummond; Faucher-Giguère, Claude-André
    • Monthly Notices of the Royal Astronomical Society, Vol. 488, Issue 2
    • DOI: 10.1093/mnras/stz1859