Star Formation and ISM Properties in the Host Galaxies of Three Far-infrared Luminous Quasars at z ∼ 6

Release time:2023-03-22 Hits:

Impact Factor:5.8

DOI number:10.3847/1538-4357/ab133d

Journal:The Astrophysical Journal

Abstract:We present Karl G. Jansky Very Large Array observations of the CO (2−1) line emission toward three far-infrared luminous quasars at z ∼ 6: SDSS J231038.88+185519.7 and SDSS J012958.51−003539.7 with ∼0farcs6 resolution and SDSS J205406.42−000514.8 with ∼2farcs1 resolution. All three sources are detected in the CO (2−1) line emission—one source is marginally resolved, and the other two appear as point sources. Measurements of the CO (2−1) line emission allow us to calculate the molecular gas mass even without a CO excitation model. The inferred molecular gas masses are (0.8–4.3) × 1010 M⊙. The widths and redshifts derived from the CO (2−1) line are consistent with previous CO (6−5) and [C ii] measurements. We also report continuum measurements using Herschel for SDSS J231038.88+185519.7 and SDSS J012958.51−003539.7, and for SDSS J231038.88+185519.7 data obtained at ∼140 and ∼300 GHz using the Atacama Large Millimeter/submillimeter Array. In the case of SDSS J231038.88+185519.7, we present a detailed analysis of the spectral energy distribution and derive the dust temperature (∼40 K), the dust mass (∼109 M⊙), the far-infrared luminosity (8–1000 μm; ∼1013 L⊙), and the star formation rate (2400–2700 M⊙ yr−1). Finally, an analysis of the photodissociation regions associated with the three high-redshift quasars indicates that the interstellar medium in these sources has similar properties to local starburst galaxies.

Co-author:Ran Wang, Chris L. Carilli, Jeff Wagg, Fabian Walter, Jianan Li, Xiaohui Fan, Linhua Jiang, Dominik A. Riechers, Frank Bertoldi, Michael A. Strauss, Pierre Cox, Alain Omont, and Karl M. Menten

First Author:Yali Shao

Volume:876

Issue:2

Page Number:99

Translation or Not:no

Date of Publication:2019-05-08

Included Journals:SCI

Links to published journals:https://iopscience.iop.org/article/10.3847/1538-4357/ab133d