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Journal Article

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

MPS-Authors

Novak,  Mladen
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bañados,  Eduardo
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Decarli,  Roberto
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Walter,  Fabian
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Venemans,  Bram
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Neeleman,  Marcel
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Farina,  Emanuele Paolo
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mazzucchelli,  Chiara
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Carilli,  Chris
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fan,  Xiaohui
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rix,  Hans─Walter
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wang,  Feige
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019ApJ...881...63N
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Citation

Novak, M., Bañados, E., Decarli, R., Walter, F., Venemans, B., Neeleman, M., et al. (2019). An ALMA Multiline Survey of the Interstellar Medium of the Redshift 7.5 Quasar Host Galaxy J1342+0928. The Astrophysical Journal, 881.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D038-1
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 β = 1.85 ± 0.3. Assuming a standard dust temperature of 47 K we derive a dust mass of M dust = 0.35 × 108 M ☉ and a star formation rate of 150+/- 30 {M}ȯ {yr}}-1. We have >4σ detections of the {[{{C}}{{II}}]}158μ {{m}}, {[{{O}}{{III}}]}88μ {{m}}, and {[{{N}}{{II}}]}205μ {{m}} atomic fine structure lines and limits on the {[{{C}}{{I}}]}369μ {{m}}, {[{{O}}{{I}}]}146μ {{m}}, and {[{{N}}{{II}}]}205μ {{m}} emission. We also report multiple limits of CO rotational lines with J up ≥ 7, as well as a tentative 3.3σ 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}}]}205μ {{m}} and {[{{C}}{{II}}]}158μ {{m}} lines indicates that the {[{{C}}{{II}}]}158μ {{m}} emission arises predominantly from the neutral medium, and we estimate that the photodisassociation regions in J1342+0928 have densities ≲5 × 104 cm−3. The data suggest that ∼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.