Star Formation in the Bullet Cluster I: The Infrared Luminosity Function and Star Formation Rate

TL;DR

This study measures the star formation rate in the Bullet Cluster using infrared data, revealing an unusually high SFR and excess star-forming galaxies likely due to ongoing infall and slow quenching processes in the merging cluster.

Contribution

It provides the first detailed infrared luminosity function and star formation rate analysis of the Bullet Cluster, highlighting the impact of cluster mergers on galaxy evolution.

Findings

The Bullet Cluster has a high integrated SFR of 267 solar masses per year.

The IR luminosity function shows an excess of luminous IR galaxies compared to other clusters.

Star formation quenching timescales are longer than the infall timescales, indicating ongoing transformation processes.

Abstract

The Bullet Cluster is a massive galaxy cluster at z=0.297 undergoing a major supersonic (Mach 3) merger event. Using Spitzer 24um images, IRAC data, 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 non-AGN MIPS confirmed cluster members out to R<1.7 Mpc, and the Rieke et al. (2009) relation to convert from 24um flux to SFR, we calculate an integrated obscured SFR of 267 Msolar/yr and a specific star formation rate of 28 Msolar/yr per 10^14 Msolar. The cluster mass 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 ergs/s, 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 have 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.