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Big Three Dragons: A z=7.15 Lyman-break galaxy detected in [Oiii] 88 mu m, [Cii] 158 mu m, and dust continuum with ALMA
Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan;Osaka Sangyo Univ, Fac Design Technol, Dept Environm Sci & Technol, 3-1-1 Nagaito, Daito, Osaka 5748530, Japan;Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
Osaka Sangyo Univ, Fac Design Technol, Dept Environm Sci & Technol, 3-1-1 Nagaito, Daito, Osaka 5748530, Japan.
Osaka Sangyo Univ, Fac Design Technol, Dept Environm Sci & Technol, 3-1-1 Nagaito, Daito, Osaka 5748530, Japan;Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan.
Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan.
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2019 (English)In: Publications of the Astronomical Society of Japan, ISSN 0004-6264, E-ISSN 2053-051X, Vol. 71, no 4, article id 71Article in journal (Refereed) Published
Abstract [en]

We present new ALMA observations and physical properties of a Lyman break galaxy at z = 7.15. Our target, B14-65666, has a bright ultra-violet (UV) absolute magnitude, M-UV approximate to -22.4, and has been spectroscopically identified in Ly alpha with a small rest-frame equivalent width of approximate to 4 angstrom. A previous Hubble Space TElescope (HST) image has shown that the target is composed of two spatially separated clumps in the rest-frame UV. With ALMA, we have newly detected spatially resolved [Oiii] 88 mu m, [Cii] 158 mu m, and their underlying dust continuum emission. In the whole system of B14-65666, the [Oiii] and [Cii] lines have consistent redshifts of 7.1520 +/- 0.0003, and the [Oiii] luminosity, (34.4 +/- 4.1)x 10(8)L(circle dot), is about three times higher than the [Cii] luminosity, (11.0 +/- 1.4) x 10(8)L(circle dot). With our two continuum flux densities, the dust temperature is constrained to be T-d approximate to 50-60K under the assumption of a dust emissivity index of beta(d) = 2.0-1.5, leading to a large total infrared luminosity of L-TIR approximate to 1 x 10(12)L(circle dot). Owing to our high spatial resolution data, we show that the [Oiii] and [Cii] emission can be spatially decomposed into two clumps associated with the two rest-frame UV clumps whose spectra are kinematically separated by approximate to 200kms(-1). We also find these two clumps have comparable UV, infrared, [Oiii], and [Cii] luminosities. Based on these results, we argue that B14-65666 is a starburst galaxy induced by a major merger. The merger interpretation is also supported by the large specific star formation rate (defined as the star formation rate per unit stellar mass), sSFR Gyr(-1), inferred from our SED fitting. Probably, a strong UV radiation field caused by intense star formation contributes to its high dust temperature and the [Oiii]-to-[Cii] luminosity ratio.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS , 2019. Vol. 71, no 4, article id 71
Keywords [en]
galaxies: formation, galaxies: high-redshift, galaxies: ISM
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-393832DOI: 10.1093/pasj/psz049ISI: 000482425000005OAI: oai:DiVA.org:uu-393832DiVA, id: diva2:1356160
Funder
Knut and Alice Wallenberg FoundationAvailable from: 2019-10-01 Created: 2019-10-01 Last updated: 2019-10-01Bibliographically approved

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Zackrisson, Erik

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