Herschel detection of dust emission from UV-luminous star-forming galaxies at 3.3 ≲ z ≲ 4.3

Kyoung Soo Lee, Stacey Alberts, David Atlee, Arjun Dey, Alexandra Pope, Buell Tomasson Jannuzi, Naveen Reddy, Michael J I Brown

Research output: Contribution to journalArticle

33 Citations (Scopus)

Abstract

We report the Herschel/SPIRE detection of dust emission arising from UV-luminous (L ≳ L*) star-forming galaxies at 3.3 ≲ z ≲ 4.3. Our sample of 1913 Lyman break galaxy (LBG) candidates is selected over an area of 5.3deg2 in the Boötes field of the NOAO Deep Wide-Field Survey. This is one of the largest samples of UV-luminous galaxies at this epoch and enables an investigation of the bright end of the galaxy luminosity function. We divide our sample into three luminosity bins and stack the Herschel/SPIRE data to measure the average spectral energy distribution (SED) of LBGs at far-infrared (FIR) wavelengths. We find that these galaxies have average IR luminosities of (3-5) × 1011 L and 60%-70% of their star formation obscured by dust. The FIR SEDs peak at λrest ≳ 100 μm suggesting dust temperatures (Td = 27-30 K) significantly colder than that of local galaxies of comparable IR luminosities. The observed IR-to-UV luminosity ratio (IRX ≡ L IR/L UV) is low (3-4) compared with that observed for z 2 LBGs (IRX z 2 7.1 ± 1.1). The correlation between the slope of the UV continuum and IRX for galaxies in the two lower luminosity bins suggests dust properties similar to those of local starburst galaxies. However, the galaxies in the highest luminosity bin appear to deviate from the local relation, suggesting that their dust properties may differ from those of their lower-luminosity and low-redshift counterparts. We speculate that the most UV-luminous galaxies at this epoch are being observed in a short-lived and young evolutionary phase.

Original languageEnglish (US)
Article numberL31
JournalAstrophysical Journal Letters
Volume758
Issue number2
DOIs
StatePublished - Oct 20 2012

Fingerprint

dust
galaxies
luminosity
stars
time measurement
detection
starburst galaxies
field survey
spectral energy distribution
star formation
wavelength
slopes
continuums
energy
wavelengths
temperature

Keywords

  • dust, extinction
  • galaxies: high
  • infrared: galaxies
  • redshift

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Herschel detection of dust emission from UV-luminous star-forming galaxies at 3.3 ≲ z ≲ 4.3. / Lee, Kyoung Soo; Alberts, Stacey; Atlee, David; Dey, Arjun; Pope, Alexandra; Jannuzi, Buell Tomasson; Reddy, Naveen; Brown, Michael J I.

In: Astrophysical Journal Letters, Vol. 758, No. 2, L31, 20.10.2012.

Research output: Contribution to journalArticle

Lee, Kyoung Soo ; Alberts, Stacey ; Atlee, David ; Dey, Arjun ; Pope, Alexandra ; Jannuzi, Buell Tomasson ; Reddy, Naveen ; Brown, Michael J I. / Herschel detection of dust emission from UV-luminous star-forming galaxies at 3.3 ≲ z ≲ 4.3. In: Astrophysical Journal Letters. 2012 ; Vol. 758, No. 2.
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abstract = "We report the Herschel/SPIRE detection of dust emission arising from UV-luminous (L ≳ L*) star-forming galaxies at 3.3 ≲ z ≲ 4.3. Our sample of 1913 Lyman break galaxy (LBG) candidates is selected over an area of 5.3deg2 in the Bo{\"o}tes field of the NOAO Deep Wide-Field Survey. This is one of the largest samples of UV-luminous galaxies at this epoch and enables an investigation of the bright end of the galaxy luminosity function. We divide our sample into three luminosity bins and stack the Herschel/SPIRE data to measure the average spectral energy distribution (SED) of LBGs at far-infrared (FIR) wavelengths. We find that these galaxies have average IR luminosities of (3-5) × 1011 L and 60{\%}-70{\%} of their star formation obscured by dust. The FIR SEDs peak at λrest ≳ 100 μm suggesting dust temperatures (Td = 27-30 K) significantly colder than that of local galaxies of comparable IR luminosities. The observed IR-to-UV luminosity ratio (IRX ≡ L IR/L UV) is low (3-4) compared with that observed for z 2 LBGs (IRX z 2 7.1 ± 1.1). The correlation between the slope of the UV continuum and IRX for galaxies in the two lower luminosity bins suggests dust properties similar to those of local starburst galaxies. However, the galaxies in the highest luminosity bin appear to deviate from the local relation, suggesting that their dust properties may differ from those of their lower-luminosity and low-redshift counterparts. We speculate that the most UV-luminous galaxies at this epoch are being observed in a short-lived and young evolutionary phase.",
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AU - Pope, Alexandra

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AB - We report the Herschel/SPIRE detection of dust emission arising from UV-luminous (L ≳ L*) star-forming galaxies at 3.3 ≲ z ≲ 4.3. Our sample of 1913 Lyman break galaxy (LBG) candidates is selected over an area of 5.3deg2 in the Boötes field of the NOAO Deep Wide-Field Survey. This is one of the largest samples of UV-luminous galaxies at this epoch and enables an investigation of the bright end of the galaxy luminosity function. We divide our sample into three luminosity bins and stack the Herschel/SPIRE data to measure the average spectral energy distribution (SED) of LBGs at far-infrared (FIR) wavelengths. We find that these galaxies have average IR luminosities of (3-5) × 1011 L and 60%-70% of their star formation obscured by dust. The FIR SEDs peak at λrest ≳ 100 μm suggesting dust temperatures (Td = 27-30 K) significantly colder than that of local galaxies of comparable IR luminosities. The observed IR-to-UV luminosity ratio (IRX ≡ L IR/L UV) is low (3-4) compared with that observed for z 2 LBGs (IRX z 2 7.1 ± 1.1). The correlation between the slope of the UV continuum and IRX for galaxies in the two lower luminosity bins suggests dust properties similar to those of local starburst galaxies. However, the galaxies in the highest luminosity bin appear to deviate from the local relation, suggesting that their dust properties may differ from those of their lower-luminosity and low-redshift counterparts. We speculate that the most UV-luminous galaxies at this epoch are being observed in a short-lived and young evolutionary phase.

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KW - infrared: galaxies

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