CaltechAUTHORS
  A Caltech Library Service

The Relation between Cool Cluster Cores and Herschel-detected Star Formation in Brightest Cluster Galaxies

Rawle, T. D. and Edge, A. C. and Egami, E. and Rex, M. and Smith, G. P. and Altieri, B. and Fiedler, A. and Haines, C. P. and Pereira, M. J. and Pérez-González, P. G. and Portouw, J. and Valtchanov, I. and Walth, G. and van der Werf, P. P. and Zemcov, M. (2012) The Relation between Cool Cluster Cores and Herschel-detected Star Formation in Brightest Cluster Galaxies. Astrophysical Journal, 747 (1). Art. No. 29. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20120328-081918889

[img]
Preview
PDF - Published Version
See Usage Policy.

1598Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20120328-081918889

Abstract

We present far-infrared (FIR) analysis of 68 brightest cluster galaxies (BCGs) at 0.08 < z < 1.0. Deriving total infrared luminosities directly from Spitzer and Herschel photometry spanning the peak of the dust component (24-500 μm), we calculate the obscured star formation rate (SFR).22^(+6.2)_(–5.3)% of the BCGs are detected in the far-infrared, with SFR = 1-150 M_☉ yr^(–1). The infrared luminosity is highly correlated with cluster X-ray gas cooling times for cool-core clusters (gas cooling time <1 Gyr), strongly suggesting that the star formation in these BCGs is influenced by the cluster-scale cooling process. The occurrence of the molecular gas tracing Hα emission is also correlated with obscured star formation. For all but the most luminous BCGs(L_(TIR) > 2 × 10^(11) L_☉), only a small (≾0.4 mag) reddening correction is required for SFR(Hα) to agree with SFR_(FIR). The relatively low Hα extinction (dust obscuration), compared to values reported for the general star-forming population, lends further weight to an alternate (external) origin for the cold gas. Finally, we use a stacking analysis of non-cool-core clusters to show that the majority of the fuel for star formation in the FIR-bright BCGs is unlikely to originate from normal stellar mass loss.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/747/1/29DOIArticle
http://iopscience.iop.org/0004-637X/747/1/29/PublisherArticle
ORCID:
AuthorORCID
Valtchanov, I.0000-0001-9930-7886
van der Werf, P. P.0000-0001-5434-5942
Zemcov, M.0000-0001-8253-1451
Additional Information:© 2012 American Astronomical Society. Received 2011 November 18; accepted 2012 January 3; published 2012 February 10. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is partially based on observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We also thank the HSC and NHSC consortia for support with data reduction. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. G.P.S. acknowledges support from the Royal Society.
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
NSFUNSPECIFIED
Royal SocietyUNSPECIFIED
Subject Keywords: galaxies: clusters: general; galaxies: elliptical and lenticular, cD; galaxies: star formation; infrared: galaxies
Record Number:CaltechAUTHORS:20120328-081918889
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20120328-081918889
Official Citation:The Relation between Cool Cluster Cores and Herschel-detected Star Formation in Brightest Cluster Galaxies T. D. Rawle et al. 2012 ApJ 747 29
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:29872
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:28 Mar 2012 15:54
Last Modified:27 Mar 2019 22:06

Repository Staff Only: item control page