An ALMA Multiline Survey of the Interstellar Medium of the Redshift 7.5 Quasar Host Galaxy J1342+0928
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Author
Novak, MladenBañados, Eduardo

Decarli, Roberto
Walter, Fabian

Venemans, Bram
Neeleman, Marcel
Farina, Emanuele Paolo
Mazzucchelli, Chiara
Carilli, Chris
Fan, Xiaohui
Rix, Hans–Walter
Wang, Feige

Affiliation
Univ Arizona, Steward ObservIssue Date
2019-08-13Keywords
cosmology: observationsgalaxies: high-redshift
galaxies: individual (ULAS J1342+0928)
galaxies: ISM
quasars: emission lines
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IOP PUBLISHING LTDCitation
Mladen Novak et al 2019 ApJ 881 63Journal
ASTROPHYSICAL JOURNALRights
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
0004-637XVersion
Final published versionSponsors
ERC Advanced Grant [740246]ae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/ab2beb