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    An ALMA Multiline Survey of the Interstellar Medium of the Redshift 7.5 Quasar Host Galaxy J1342+0928

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    Novak_2019_ApJ_881_63.pdf
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    Author
    Novak, Mladen
    Bañados, Eduardo cc
    Decarli, Roberto
    Walter, Fabian cc
    Venemans, Bram
    Neeleman, Marcel
    Farina, Emanuele Paolo
    Mazzucchelli, Chiara
    Carilli, Chris
    Fan, Xiaohui
    Rix, Hans–Walter
    Wang, Feige cc
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    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2019-08-13
    Keywords
    cosmology: observations
    galaxies: high-redshift
    galaxies: individual (ULAS J1342+0928)
    galaxies: ISM
    quasars: emission lines
    
    Metadata
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    Publisher
    IOP PUBLISHING LTD
    Citation
    Mladen Novak et al 2019 ApJ 881 63
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    Copyright © 2019. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    We use Atacama Large Millimeter Array observations of the host galaxy of the quasar ULAS J1342+0928 at z = 7.54, to study the dust continuum and far-infrared lines emitted from its interstellar medium (ISM). The Rayleigh-Jeans tail of the dust continuum is well sampled with eight different spectral setups, and from a modified blackbody fit we obtain an emissivity coefficient of beta = 1.85 +/- 0.3. Assuming a standard dust temperature of 47 K we derive a dust mass of M-dust = 0.35 x 10(8) M circle dot and a star formation rate of 150 +/- 30 M circle dot yr(-1). We have >4 sigma detections of the [C II](158) (mu m), [O III](88 mu m), and [N II](205) (mu m) atomic fine structure lines and limits on the [C I](369) mu m, [O I](146) mu m, and [N II](205) (mu m) emission. We also report multiple limits of CO rotational lines with J up >= 7, as well as a tentative 3.3 sigma detection of the stack of four CO lines (J(up) = 11, 10, 8, and 7). We find line deficits that are in agreement with local ultra-luminous infrared galaxies. Comparison of the [N II](205) (mu m) and [C II](158) (mu m) lines indicates that the [C II](158) (mu m) emission arises predominantly from the neutral medium, and we estimate that the photodisassociation regions in J1342+0928 have densities less than or similar to 5 x 10(4) cm(-3). The data suggest that similar to 16% of hydrogen is in ionized form and that the H II regions have high electron densities of n(e) > 180 cm(-3). Our observations favor a low gas-to-dust ratio of <100, and a metallicity of the ISM comparable to the solar value. All the measurements presented here suggest that the host galaxy of J1342+0928 is highly enriched in metal and dust, despite being observed just 680 Myr after the big bang.
    ISSN
    0004-637X
    DOI
    10.3847/1538-4357/ab2beb
    Version
    Final published version
    Sponsors
    ERC Advanced Grant [740246]
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab2beb
    Scopus Count
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    UA Faculty Publications

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