"A Spectroscopically Confirmed Excess of 24 μm Sources in a Super Galax" by Kim-Vy H. Tran, Amelie Saintonge et al.

Chemistry and Physics Faculty Articles

Title

A Spectroscopically Confirmed Excess of 24 μm Sources in a Super Galaxy Group at z=0.37: Enhanced Dusty Star Formation Relative to the Cluster and Field Environment

Authors

Kim-Vy H. Tran, Texas A&M University; University of Zürich
Amelie Saintonge, University of Zürich
John Moustakas, University of California - San Diego
Lei Bai, University of Arizona; Observatories of the Carnegie Institution of Washington
Anthony H. Gonzalez, University of Florida
Bradford P. Holden, University of California, Santa Cruz
Dennis Zaritsky, University of Arizona
Stefan Kautsch, University of FloridaFollow

Document Type

Article

Publication Date

10-15-2009

Publication Title

The Astrophysical Journal

Keywords

Galaxies: clusters: general, Galaxies: clusters: individual (SG1120-1202), Galaxies: evolution, Galaxies: luminosity function, Mass function, Galaxies: starburst, Infrared: galaxies

ISSN

0004-637X

Volume

705

Issue/No.

First Page

809

Last Page

820

Abstract

To trace how dust-obscured star formation varies with environment, we compare the fraction of 24 μm sources in a super galaxy group to the field and a rich galaxy cluster at z ~ 0.35. We draw on multi-wavelength observations that combine Hubble, Chandra, and Spitzer imaging with extensive optical spectroscopy (>1800 redshifts) to isolate galaxies in each environment and thus ensure a uniform analysis. We focus on the four galaxy groups (σ_1D = 303-580 km s^–1) in supergroup 1120-12 that will merge to form a galaxy cluster comparable in mass to Coma. We find that (1) the fraction of supergroup galaxies with SFR_IR ≥ 3 M _☉ yr^–1 is 4 times higher than in the cluster (32% ± 5% versus 7% ± 2%); (2) the supergroup's infrared luminosity function confirms that it has a higher density of IR members compared to the cluster and includes bright IR sources (log(L _IR)[erg s^–1] >45) not found in galaxy clusters at z 0.35; and (3) there is a strong trend of decreasing 24 μm fraction with increasing galaxy density, i.e., an infrared-density relation, not observed in the cluster. These dramatic differences are surprising because the early-type fraction in the supergroup is already as high as in clusters, i.e., the timescales for morphological transformation cannot be strongly coupled to when the star formation is completely quenched. The supergroup has a significant fraction (~17%) of luminous, low-mass (10.0 < log(M _*)[M _☉] < 10.6), SFR_IR ≥ 3 M _☉ yr^–1 members that are outside the group cores (R _proj ≥ 0.5 Mpc); once their star formation is quenched, most will evolve into faint red galaxies. Our analysis indicates that the supergroup's 24 μm population also differs from that in the field: (1) despite the supergroup having twice the fraction of E/S0s as the field, the fraction of SFR_IR ≥ 3 M _☉ yr^–1 galaxies is comparable in both environments, and (2) the supergroup's IR luminosity function has a higher L*_IR than that previously measured for the field.

Comments

Additional Comments

Swiss National Science Foundation grant # PP002-110576; NASA-06-GALEX06-0030; Spitzer G05-AR-50443; NASA Spitzer JPL subcontract #s: 1255094, 1256318; NASA HST G0-10499; JPL/Caltech SST GO-20683; Chandra GO2-3183X3

NSUWorks Citation

Tran, K. H., Saintonge, A., Moustakas, J., Bai, L., Gonzalez, A. H., Holden, B. P., Zaritsky, D., & Kautsch, S. (2009). A Spectroscopically Confirmed Excess of 24 μm Sources in a Super Galaxy Group at z=0.37: Enhanced Dusty Star Formation Relative to the Cluster and Field Environment. The Astrophysical Journal, 705, (1), 809 - 820. https://doi.org/10.1088/0004-637X/705/1/809. Retrieved from https://nsuworks.nova.edu/cnso_chemphys_facarticles/109

DOI

10.1088/0004-637X/705/1/809

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