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 language | English (US) |
|---|---|
| Pages (from-to) | 1536-1549 |
| Number of pages | 14 |
| Journal | Astrophysical Journal |
| Volume | 725 |
| Issue number | 2 |
| DOIs | |
| State | Published - Dec 20 2010 |
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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 journal › Article
}
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 -