Star formation in the Bullet Cluster. I. the infrared luminosity function and star formation rate

Sun Mi Chung, Anthony H. Gonzalez, Douglas Clowe, Maxim Markevitch, Dennis F Zaritsky

Research output: Contribution to journalArticle

31 Citations (Scopus)

Abstract

The Bullet Cluster is a massive galaxy cluster at z = 0.297 undergoing a major supersonic (Mach 3) merger event. Using data from Spitzer MIPS and the Infrared Array Camera, optical imaging, and optical spectroscopy, we present the global star formation rate (SFR) of this unique cluster. Using a 90% spectroscopically complete sample of 37 star-forming MIPS confirmed cluster members out to R > 1.7 Mpc, and the Rieke et al. relation to convert from 24 μm flux to SFR, we calculate an integrated obscured SFR of 267M yr-1 and a specific SFR of 28M yr-1 per 1014M. The clustermass normalized integrated SFR of the Bullet Cluster is among the highest in a sample of eight other clusters and cluster mergers from the literature. Five LIRGs and one ULIRG contribute 30% and 40% of the total SFR of the cluster, respectively. To investigate the origin of the elevated specific SFR, we compare the infrared luminosity function (IR LF) of the Bullet Cluster to those of Coma (evolved to z = 0.297) and CL1358+62. The Bullet Cluster IR LF exhibits an excess of sources compared to the IR LFs of the other massive clusters. A Schechter function fit of the Bullet Cluster IR LF yields L * = 44.68±0.11 erg s -1, which is ∼0.25 and 0.35 dex brighter than L * of evolved Coma and CL1358+62, respectively. The elevated IR LF of the Bullet Cluster relative to other clusters can be explained if we attribute the "excess" star-forming IR galaxies to a population associated with the infalling group that has not yet been transformed into quiescent galaxies. In this case, the timescale required for quenching star formation in the cluster environment must be longer than the timescale since the group's accretion-a few hundred million years.We suggest that "strangulation" is likely to be an important process in the evolution of star formation in clusters.

Original languageEnglish (US)
Pages (from-to)1536-1549
Number of pages14
JournalAstrophysical Journal
Volume725
Issue number2
DOIs
StatePublished - Dec 20 2010

Fingerprint

star formation rate
star formation
luminosity
merger
timescale
rate
coma
erg
galaxies
spectroscopy
accretion
stars

Keywords

  • Galaxies: clusters: individual (1E0657-56, The Bullet Cluster)
  • Galaxies: evolution
  • Galaxies: luminosity function, mass function
  • Infrared: galaxies

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Star formation in the Bullet Cluster. I. the infrared luminosity function and star formation rate. / Chung, Sun Mi; Gonzalez, Anthony H.; Clowe, Douglas; Markevitch, Maxim; Zaritsky, Dennis F.

In: Astrophysical Journal, Vol. 725, No. 2, 20.12.2010, p. 1536-1549.

Research output: Contribution to journalArticle

Chung, Sun Mi ; Gonzalez, Anthony H. ; Clowe, Douglas ; Markevitch, Maxim ; Zaritsky, Dennis F. / Star formation in the Bullet Cluster. I. the infrared luminosity function and star formation rate. In: Astrophysical Journal. 2010 ; Vol. 725, No. 2. pp. 1536-1549.
@article{7d7e7f0beb8e4c6686c2ac977f6e6e30,
title = "Star formation in the Bullet Cluster. I. the infrared luminosity function and star formation rate",
abstract = "The Bullet Cluster is a massive galaxy cluster at z = 0.297 undergoing a major supersonic (Mach 3) merger event. Using data from Spitzer MIPS and the Infrared Array Camera, optical imaging, and optical spectroscopy, we present the global star formation rate (SFR) of this unique cluster. Using a 90{\%} spectroscopically complete sample of 37 star-forming MIPS confirmed cluster members out to R > 1.7 Mpc, and the Rieke et al. relation to convert from 24 μm flux to SFR, we calculate an integrated obscured SFR of 267M ⊙ yr-1 and a specific SFR of 28M⊙ yr-1 per 1014M⊙. The clustermass normalized integrated SFR of the Bullet Cluster is among the highest in a sample of eight other clusters and cluster mergers from the literature. Five LIRGs and one ULIRG contribute 30{\%} and 40{\%} of the total SFR of the cluster, respectively. To investigate the origin of the elevated specific SFR, we compare the infrared luminosity function (IR LF) of the Bullet Cluster to those of Coma (evolved to z = 0.297) and CL1358+62. The Bullet Cluster IR LF exhibits an excess of sources compared to the IR LFs of the other massive clusters. A Schechter function fit of the Bullet Cluster IR LF yields L * = 44.68±0.11 erg s -1, which is ∼0.25 and 0.35 dex brighter than L * of evolved Coma and CL1358+62, respectively. The elevated IR LF of the Bullet Cluster relative to other clusters can be explained if we attribute the {"}excess{"} star-forming IR galaxies to a population associated with the infalling group that has not yet been transformed into quiescent galaxies. In this case, the timescale required for quenching star formation in the cluster environment must be longer than the timescale since the group's accretion-a few hundred million years.We suggest that {"}strangulation{"} is likely to be an important process in the evolution of star formation in clusters.",
keywords = "Galaxies: clusters: individual (1E0657-56, The Bullet Cluster), Galaxies: evolution, Galaxies: luminosity function, mass function, Infrared: galaxies",
author = "Chung, {Sun Mi} and Gonzalez, {Anthony H.} and Douglas Clowe and Maxim Markevitch and Zaritsky, {Dennis F}",
year = "2010",
month = "12",
day = "20",
doi = "10.1088/0004-637X/725/2/1536",
language = "English (US)",
volume = "725",
pages = "1536--1549",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - Star formation in the Bullet Cluster. I. the infrared luminosity function and star formation rate

AU - Chung, Sun Mi

AU - Gonzalez, Anthony H.

AU - Clowe, Douglas

AU - Markevitch, Maxim

AU - Zaritsky, Dennis F

PY - 2010/12/20

Y1 - 2010/12/20

N2 - The Bullet Cluster is a massive galaxy cluster at z = 0.297 undergoing a major supersonic (Mach 3) merger event. Using data from Spitzer MIPS and the Infrared Array Camera, optical imaging, and optical spectroscopy, we present the global star formation rate (SFR) of this unique cluster. Using a 90% spectroscopically complete sample of 37 star-forming MIPS confirmed cluster members out to R > 1.7 Mpc, and the Rieke et al. relation to convert from 24 μm flux to SFR, we calculate an integrated obscured SFR of 267M ⊙ yr-1 and a specific SFR of 28M⊙ yr-1 per 1014M⊙. The clustermass normalized integrated SFR of the Bullet Cluster is among the highest in a sample of eight other clusters and cluster mergers from the literature. Five LIRGs and one ULIRG contribute 30% and 40% of the total SFR of the cluster, respectively. To investigate the origin of the elevated specific SFR, we compare the infrared luminosity function (IR LF) of the Bullet Cluster to those of Coma (evolved to z = 0.297) and CL1358+62. The Bullet Cluster IR LF exhibits an excess of sources compared to the IR LFs of the other massive clusters. A Schechter function fit of the Bullet Cluster IR LF yields L * = 44.68±0.11 erg s -1, which is ∼0.25 and 0.35 dex brighter than L * of evolved Coma and CL1358+62, respectively. The elevated IR LF of the Bullet Cluster relative to other clusters can be explained if we attribute the "excess" star-forming IR galaxies to a population associated with the infalling group that has not yet been transformed into quiescent galaxies. In this case, the timescale required for quenching star formation in the cluster environment must be longer than the timescale since the group's accretion-a few hundred million years.We suggest that "strangulation" is likely to be an important process in the evolution of star formation in clusters.

AB - The Bullet Cluster is a massive galaxy cluster at z = 0.297 undergoing a major supersonic (Mach 3) merger event. Using data from Spitzer MIPS and the Infrared Array Camera, optical imaging, and optical spectroscopy, we present the global star formation rate (SFR) of this unique cluster. Using a 90% spectroscopically complete sample of 37 star-forming MIPS confirmed cluster members out to R > 1.7 Mpc, and the Rieke et al. relation to convert from 24 μm flux to SFR, we calculate an integrated obscured SFR of 267M ⊙ yr-1 and a specific SFR of 28M⊙ yr-1 per 1014M⊙. The clustermass normalized integrated SFR of the Bullet Cluster is among the highest in a sample of eight other clusters and cluster mergers from the literature. Five LIRGs and one ULIRG contribute 30% and 40% of the total SFR of the cluster, respectively. To investigate the origin of the elevated specific SFR, we compare the infrared luminosity function (IR LF) of the Bullet Cluster to those of Coma (evolved to z = 0.297) and CL1358+62. The Bullet Cluster IR LF exhibits an excess of sources compared to the IR LFs of the other massive clusters. A Schechter function fit of the Bullet Cluster IR LF yields L * = 44.68±0.11 erg s -1, which is ∼0.25 and 0.35 dex brighter than L * of evolved Coma and CL1358+62, respectively. The elevated IR LF of the Bullet Cluster relative to other clusters can be explained if we attribute the "excess" star-forming IR galaxies to a population associated with the infalling group that has not yet been transformed into quiescent galaxies. In this case, the timescale required for quenching star formation in the cluster environment must be longer than the timescale since the group's accretion-a few hundred million years.We suggest that "strangulation" is likely to be an important process in the evolution of star formation in clusters.

KW - Galaxies: clusters: individual (1E0657-56, The Bullet Cluster)

KW - Galaxies: evolution

KW - Galaxies: luminosity function, mass function

KW - Infrared: galaxies

UR - http://www.scopus.com/inward/record.url?scp=78650119806&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=78650119806&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/725/2/1536

DO - 10.1088/0004-637X/725/2/1536

M3 - Article

AN - SCOPUS:78650119806

VL - 725

SP - 1536

EP - 1549

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

ER -