Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South^⋆

¹ INAF/IRA, Istituto di Radioastronomia, Via Piero Gobetti 101, 40129 Bologna, Italy
e-mail: quirino.damato2@unibo.it
² Dipartimento di Fisica e Astronomia dell’Università degli Studi di Bologna, Via P. Gobetti 93/2, 40129 Bologna, Italy
³ INAF/OAS, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via P. Gobetti 93/3, 40129 Bologna, Italy
⁴ INAF, Istituto di Radioastronomia – Italian Alma Regional Center (ARC), Via Piero Gobetti 101, 40129 Bologna, Italy
⁵ European Southern Observatory, Karl-Schwarzschild-Str 2, 85748 Garching bei München, Germany
⁶ Instituto de Astrofísica and Centro de Astroingenieria, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile
⁷ Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, 100012 Beijing, PR China
⁸ Instituto de Radioastronomía y Astrofisíca, UNAM, Campus Morelia, AP 3-72, 58089 Morelia, Mexico
⁹ INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
¹⁰ SISSA, Via Bonomea 265, 34136 Trieste, Italy
¹¹ Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
¹² Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA
¹³ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

Received: 25 June 2019
Accepted: 16 March 2020

Abstract

Context. Obscured active galactic nuclei (AGN) represent a significant fraction of the entire AGN population, especially at high redshift (∼70% at z = 3 − 5). They are often characterized by the presence of large gas and dust reservoirs that are thought to sustain and possibly obscure vigorous star formation processes that make these objects shine at FIR and submillimeter wavelengths. Studying the physical properties of obscured AGN and their host galaxies is crucial to shedding light on the early stages of a massive system lifetime.

Aims. We aim to investigate the contribution of the interstellar medium (ISM) to the obscuration of quasars in a sample of distant highly star forming galaxies and to unveil their morphological and kinematics properties.

Methods. We exploit Atacama Large Millimeter/submillimeter Array Cycle 4 observations of the continuum (∼2.1 mm) and high-J CO emission of a sample of six X-ray selected, FIR detected galaxies hosting an obscured AGN at z_spec >  2.5 in the 7 Ms Chandra Deep Field-South. We measured the masses and sizes of the dust and molecular gas by fitting the images, visibilities, and spectra, and we derived the gas density and column density on the basis of a uniform sphere geometry. Finally, we compared the measured column densities with those derived from the Chandra X-ray spectra.

Results. We detected both the continuum and line emission for three sources for which we measured both the flux density and size. For the undetected sources, we derived an upper limit on the flux density from the root mean square of the images. We found that the detected galaxies are rich in gas and dust (molecular gas mass in the range < 0.5–2.7 × 10¹⁰ M_⊙ for α_CO = 0.8 and up to ∼2 × 10¹¹ M_⊙ for α_CO = 6.5, and dust mass < 0.9–4.9 × 10⁸ M_⊙) and generally compact (gas major axis 2.1–3.0 kpc, dust major axis 1.4–2.7 kpc). The column densities associated with the ISM are on the order of 10^{23 − 24} cm⁻², which is comparable with those derived from the X-ray spectra. For the detected sources we also derived dynamical masses in the range 0.8–3.7 × 10¹⁰ M_⊙.

Conclusions. We conclude that the ISM of high redshift galaxies can substantially contribute to nuclear obscuration up to the Compton-thick (> 10²⁴ cm⁻²) regime. In addition, we found that all the detected sources show a velocity gradient reminding one rotating system, even though two of them show peculiar features in their morphology that can be associated with a chaotic, possibly merging, structure.