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Author
Venemans, B. P.
Walter, Fabian

Decarli, R.

Bañados, Eduardo

Carilli, Chris L.

Winters, Jan Martin
Schuster, Karl
da Cunha, Elisabete

Fan, Xiaohui

Farina, E. P.

Mazzucchelli, C.

Rix, Hans-Walter

Weiss, Axel

Affiliation
Univ Arizona, Steward ObservIssue Date
2017-12-06
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IOP PUBLISHING LTDCitation
Copious Amounts of Dust and Gas in a z = 7.5 Quasar Host Galaxy 2017, 851 (1):L8 The Astrophysical JournalRights
© 2017. 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 present IRAM/NOEMA and JVLA observations of the quasar J1342+0928 at z = 7.54 and report detections of copious amounts of dust and [C Pi] emission in the interstellar medium (ISM) of its host galaxy. At this redshift, the age of the universe is 690 Myr, about 10% younger than the redshift of the previous quasar record holder. Yet, the ISM of this new quasar host galaxy is significantly enriched by metals, as evidenced by the detection of the [C 158 mu m cooling line and the underlying far-infrared (FIR) dust continuum emission. To the first order, the FIR properties of this quasar host are similar to those found at a slightly lower redshift (z similar to 6), making this source by far the FIR-brightest galaxy known at z greater than or similar to 7.5. The [C Pi]emission is spatially unresolved, with an upper limit on the diameter of 7 kpc. Together with the measured FWHM of the [C Pi]line, this yields a dynamical mass of the host of <1.5 x 10(11) M-circle dot Using standard assumptions about the dust temperature and emissivity, the NOEMA measurements give a dust mass of (0.6-4.3) x 10(8) M-circle dot The brightness of the [C Pi] luminosity, together with the high dust mass, imply active ongoing star formation in the quasar host. Using [C Pi]-SFR scaling relations, we derive star formation rates of 85-545 M-circle dot yr(-1) in the host, consistent with the values derived from the dust continuum. Indeed, an episode of such past high star formation is needed to explain the presence of similar to 10(8) M-circle dot of dust implied by the observations.ISSN
2041-8213Version
Final published versionSponsors
DFG priority program 1573 "The physics of the interstellar medium"; IRAM NOEMA Interferometer [E16AH]; INSU/CNRS (France); MPG (Germany); IGN (Spain)Additional Links
http://stacks.iop.org/2041-8205/851/i=1/a=L8?key=crossref.99d98acf41e5835171b827c83f5b47b7ae974a485f413a2113503eed53cd6c53
10.3847/2041-8213/aa943a