Dust-obscured star formation in intermediate redshift galaxy clusters

Rose A. Finn, Vandana Desai, Gregory Rudnick, Bianca Poggianti, Eric F. Bell, Joannah Hinz, Pascale Jablonka, Bo Milvang-Jensen, John Moustakas, Kenneth Rines, Dennis F Zaritsky

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Abstract

We present Spitzer MIPS 24 μm observations of sixteen 0.4 < z < 0.8 galaxy clusters drawn from the ESO Distant Cluster Survey. This is the first large 24 μm survey of clusters at intermediate redshift. The depth of our imaging corresponds to a total IR luminosity of 8 × 1010 L , just below the luminosity of luminous infrared galaxies (LIRGs), and 6+1-1% of MV < - 19 cluster members show 24 μm emission at or above this level. We compare with a large sample of coeval field galaxies and find that while the fraction of cluster LIRGs lies significantly below that of the field, the IR luminosities of the field and cluster galaxies are consistent. However, the stellar masses of the EDisCS LIRGs are systematically higher than those of the field LIRGs. A comparison with optical data reveals that ∼80% of cluster LIRGs are blue and the remaining 20% lie on the red sequence. Of LIRGs with optical spectra, 88-4-5% show [O II] emission with EW([O II]) > 5 Å, and ∼75% exhibit optical signatures of dusty starbursts. On average, the fraction of cluster LIRGs increases with projected clustercentric radius but remains systematically lower than the field fraction over the area probed (<1.5 × R200). The amount of obscured star formation declines significantly over the 2.4 Gyr interval spanned by the EDisCS sample, and the rate of decline is the same for the cluster and field populations. Our results are consistent with an exponentially declining LIRG fraction, with the decline in the field delayed by ∼1 Gyr relative to the clusters.

Original languageEnglish (US)
Pages (from-to)87-98
Number of pages12
JournalAstrophysical Journal
Volume720
Issue number1
DOIs
StatePublished - Sep 1 2010

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star formation
dust
galaxies
signatures
intervals
radii
rate

Keywords

  • Galaxies: clusters: general
  • Galaxies: evolution

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Dust-obscured star formation in intermediate redshift galaxy clusters. / Finn, Rose A.; Desai, Vandana; Rudnick, Gregory; Poggianti, Bianca; Bell, Eric F.; Hinz, Joannah; Jablonka, Pascale; Milvang-Jensen, Bo; Moustakas, John; Rines, Kenneth; Zaritsky, Dennis F.

In: Astrophysical Journal, Vol. 720, No. 1, 01.09.2010, p. 87-98.

Research output: Contribution to journalArticle

Finn, RA, Desai, V, Rudnick, G, Poggianti, B, Bell, EF, Hinz, J, Jablonka, P, Milvang-Jensen, B, Moustakas, J, Rines, K & Zaritsky, DF 2010, 'Dust-obscured star formation in intermediate redshift galaxy clusters', Astrophysical Journal, vol. 720, no. 1, pp. 87-98. https://doi.org/10.1088/0004-637X/720/1/87
Finn RA, Desai V, Rudnick G, Poggianti B, Bell EF, Hinz J et al. Dust-obscured star formation in intermediate redshift galaxy clusters. Astrophysical Journal. 2010 Sep 1;720(1):87-98. https://doi.org/10.1088/0004-637X/720/1/87
Finn, Rose A. ; Desai, Vandana ; Rudnick, Gregory ; Poggianti, Bianca ; Bell, Eric F. ; Hinz, Joannah ; Jablonka, Pascale ; Milvang-Jensen, Bo ; Moustakas, John ; Rines, Kenneth ; Zaritsky, Dennis F. / Dust-obscured star formation in intermediate redshift galaxy clusters. In: Astrophysical Journal. 2010 ; Vol. 720, No. 1. pp. 87-98.
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AU - Bell, Eric F.

AU - Hinz, Joannah

AU - Jablonka, Pascale

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AU - Rines, Kenneth

AU - Zaritsky, Dennis F

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N2 - We present Spitzer MIPS 24 μm observations of sixteen 0.4 < z < 0.8 galaxy clusters drawn from the ESO Distant Cluster Survey. This is the first large 24 μm survey of clusters at intermediate redshift. The depth of our imaging corresponds to a total IR luminosity of 8 × 1010 L ⊙, just below the luminosity of luminous infrared galaxies (LIRGs), and 6+1-1% of MV < - 19 cluster members show 24 μm emission at or above this level. We compare with a large sample of coeval field galaxies and find that while the fraction of cluster LIRGs lies significantly below that of the field, the IR luminosities of the field and cluster galaxies are consistent. However, the stellar masses of the EDisCS LIRGs are systematically higher than those of the field LIRGs. A comparison with optical data reveals that ∼80% of cluster LIRGs are blue and the remaining 20% lie on the red sequence. Of LIRGs with optical spectra, 88-4-5% show [O II] emission with EW([O II]) > 5 Å, and ∼75% exhibit optical signatures of dusty starbursts. On average, the fraction of cluster LIRGs increases with projected clustercentric radius but remains systematically lower than the field fraction over the area probed (<1.5 × R200). The amount of obscured star formation declines significantly over the 2.4 Gyr interval spanned by the EDisCS sample, and the rate of decline is the same for the cluster and field populations. Our results are consistent with an exponentially declining LIRG fraction, with the decline in the field delayed by ∼1 Gyr relative to the clusters.

AB - We present Spitzer MIPS 24 μm observations of sixteen 0.4 < z < 0.8 galaxy clusters drawn from the ESO Distant Cluster Survey. This is the first large 24 μm survey of clusters at intermediate redshift. The depth of our imaging corresponds to a total IR luminosity of 8 × 1010 L ⊙, just below the luminosity of luminous infrared galaxies (LIRGs), and 6+1-1% of MV < - 19 cluster members show 24 μm emission at or above this level. We compare with a large sample of coeval field galaxies and find that while the fraction of cluster LIRGs lies significantly below that of the field, the IR luminosities of the field and cluster galaxies are consistent. However, the stellar masses of the EDisCS LIRGs are systematically higher than those of the field LIRGs. A comparison with optical data reveals that ∼80% of cluster LIRGs are blue and the remaining 20% lie on the red sequence. Of LIRGs with optical spectra, 88-4-5% show [O II] emission with EW([O II]) > 5 Å, and ∼75% exhibit optical signatures of dusty starbursts. On average, the fraction of cluster LIRGs increases with projected clustercentric radius but remains systematically lower than the field fraction over the area probed (<1.5 × R200). The amount of obscured star formation declines significantly over the 2.4 Gyr interval spanned by the EDisCS sample, and the rate of decline is the same for the cluster and field populations. Our results are consistent with an exponentially declining LIRG fraction, with the decline in the field delayed by ∼1 Gyr relative to the clusters.

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KW - Galaxies: evolution

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