Infrared luminosities and dust properties of z 2 dust-obscured galaxies

R. S. Bussmann, Arjun Dey, C. Borys, V. Desai, Buell Tomasson Jannuzi, E. Le Floc'H, J. Melbourne, K. Sheth, B. T. Soifer

Research output: Contribution to journalArticle

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Abstract

We present SHARC-II 350 μm imaging of twelve 24 μm bright (F 24 μm > 0.8 mJy) Dust-Obscured Galaxies (DOGs) and Combined Array for Research in Millimeter-wave Astronomy (CARMA) 1 mm imaging of a subset of two DOGs. These objects are selected from the Boötes field of the NOAO Deep Wide-Field Survey. Detections of four DOGs at 350 μm imply infrared (IR) luminosities which are consistent to within a factor of 2 of expectations based on a warm-dust spectral energy distribution (SED) scaled to the observed 24 μm flux density. The 350 μm upper limits for the 8 non-detected DOGs are consistent with both Mrk 231 and M82 (warm-dust SEDs), but exclude cold dust (Arp 220) SEDs. The two DOGs targeted at 1 mm were not detected in our CARMA observations, placing strong constraints on the dust temperature: T dust > 35-60 K. Assuming these dust properties apply to the entire sample, we find dust masses of 3 × 108 M. In comparison to other dusty z 2 galaxy populations such as submillimeter galaxies (SMGs) and other Spitzer-selected high-redshift sources, this sample of DOGs has higher IR luminosities (2 × 1013 L versus 6 × 1012 L for the other galaxy populations) that are driven by warmer dust temperatures (>35-60 K versus 30 K) and lower inferred dust masses (3 × 108 M versus 3 × 109 M ). Wide-field Herschel and Submillimeter Common-User Bolometer Array-2 surveys should be able to detect hundreds of these power-law-dominated DOGs. We use the existing Hubble Space Telescope and Spitzer/InfraRed Array Camera data to estimate stellar masses of these sources and find that the stellar to gas mass ratio may be higher in our 24 μm bright sample of DOGs than in SMGs and other Spitzer-selected sources. Although much larger sample sizes are needed to provide a definitive conclusion, the data are consistent with an evolutionary trend in which the formation of massive galaxies at z 2 involves a submillimeter bright, cold-dust, and star-formation-dominated phase followed by a 24 μm bright, warm-dust and AGN-dominated phase.

Original languageEnglish (US)
Pages (from-to)184-198
Number of pages15
JournalAstrophysical Journal
Volume705
Issue number1
DOIs
StatePublished - 2009
Externally publishedYes

Fingerprint

dust
luminosity
galaxies
astronomy
millimeter waves
bolometers
spectral energy distribution
stellar mass
Hubble Space Telescope
mass ratios
field survey
set theory
star formation
power law
flux density
temperature
cameras

Keywords

  • Galaxies: evolution
  • Galaxies: fundamental parameters
  • Galaxies: high-redshift
  • Submillimeter

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Bussmann, R. S., Dey, A., Borys, C., Desai, V., Jannuzi, B. T., Le Floc'H, E., ... Soifer, B. T. (2009). Infrared luminosities and dust properties of z 2 dust-obscured galaxies. Astrophysical Journal, 705(1), 184-198. https://doi.org/10.1088/0004-637X/705/1/184

Infrared luminosities and dust properties of z 2 dust-obscured galaxies. / Bussmann, R. S.; Dey, Arjun; Borys, C.; Desai, V.; Jannuzi, Buell Tomasson; Le Floc'H, E.; Melbourne, J.; Sheth, K.; Soifer, B. T.

In: Astrophysical Journal, Vol. 705, No. 1, 2009, p. 184-198.

Research output: Contribution to journalArticle

Bussmann, RS, Dey, A, Borys, C, Desai, V, Jannuzi, BT, Le Floc'H, E, Melbourne, J, Sheth, K & Soifer, BT 2009, 'Infrared luminosities and dust properties of z 2 dust-obscured galaxies', Astrophysical Journal, vol. 705, no. 1, pp. 184-198. https://doi.org/10.1088/0004-637X/705/1/184
Bussmann, R. S. ; Dey, Arjun ; Borys, C. ; Desai, V. ; Jannuzi, Buell Tomasson ; Le Floc'H, E. ; Melbourne, J. ; Sheth, K. ; Soifer, B. T. / Infrared luminosities and dust properties of z 2 dust-obscured galaxies. In: Astrophysical Journal. 2009 ; Vol. 705, No. 1. pp. 184-198.
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AU - Dey, Arjun

AU - Borys, C.

AU - Desai, V.

AU - Jannuzi, Buell Tomasson

AU - Le Floc'H, E.

AU - Melbourne, J.

AU - Sheth, K.

AU - Soifer, B. T.

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N2 - We present SHARC-II 350 μm imaging of twelve 24 μm bright (F 24 μm > 0.8 mJy) Dust-Obscured Galaxies (DOGs) and Combined Array for Research in Millimeter-wave Astronomy (CARMA) 1 mm imaging of a subset of two DOGs. These objects are selected from the Boötes field of the NOAO Deep Wide-Field Survey. Detections of four DOGs at 350 μm imply infrared (IR) luminosities which are consistent to within a factor of 2 of expectations based on a warm-dust spectral energy distribution (SED) scaled to the observed 24 μm flux density. The 350 μm upper limits for the 8 non-detected DOGs are consistent with both Mrk 231 and M82 (warm-dust SEDs), but exclude cold dust (Arp 220) SEDs. The two DOGs targeted at 1 mm were not detected in our CARMA observations, placing strong constraints on the dust temperature: T dust > 35-60 K. Assuming these dust properties apply to the entire sample, we find dust masses of 3 × 108 M. In comparison to other dusty z 2 galaxy populations such as submillimeter galaxies (SMGs) and other Spitzer-selected high-redshift sources, this sample of DOGs has higher IR luminosities (2 × 1013 L ⊙ versus 6 × 1012 L ⊙ for the other galaxy populations) that are driven by warmer dust temperatures (>35-60 K versus 30 K) and lower inferred dust masses (3 × 108 M ⊙ versus 3 × 109 M ⊙). Wide-field Herschel and Submillimeter Common-User Bolometer Array-2 surveys should be able to detect hundreds of these power-law-dominated DOGs. We use the existing Hubble Space Telescope and Spitzer/InfraRed Array Camera data to estimate stellar masses of these sources and find that the stellar to gas mass ratio may be higher in our 24 μm bright sample of DOGs than in SMGs and other Spitzer-selected sources. Although much larger sample sizes are needed to provide a definitive conclusion, the data are consistent with an evolutionary trend in which the formation of massive galaxies at z 2 involves a submillimeter bright, cold-dust, and star-formation-dominated phase followed by a 24 μm bright, warm-dust and AGN-dominated phase.

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KW - Galaxies: fundamental parameters

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