Spectral Energy Distributions of type 2 QSOs: obscured star formation at high redshifts

TL;DR

This study investigates high-redshift type-2 QSOs using mid-infrared and submillimetre data, revealing obscured star formation and AGN activity, and comparing their spectral energy distributions to local ultraluminous galaxies.

Contribution

It provides new multiwavelength observations of high-redshift type-2 QSOs and analyzes their spectral energy distributions to understand star formation and AGN obscuration.

Findings

Some QSOs show evidence of starburst activity in submillimetre emission.

A large fraction of mid-infrared energy likely originates from obscured quasars.

Infrared luminosities exceed 10^12 solar luminosities.

Abstract

We present new mid-infrared and submillimetre observations for a sample of eight high redshift type-2 QSOs located in the Chandra Deep Field South. The sources are X-ray absorbed with luminosities in excess of 10^44 erg/s. Two of the targets have robust detections, S/N > 4, while a further three targets are marginally detected with S/N > =2.5. All sources are detected in multiple mid-infrared bands with the Spitzer Space Telescope. The multiwavelength spectral energy distributions (SEDs) of the type-2 QSOs are compared to those of two local ultraluminous galaxies (Arp220 and IR22491) in order to assess contributions from a star-forming component in various parts of the SED. We suggest that their submillimetre emission is possibly due to a starburst while a large fraction of the mid-infrared energy is likely to originate in the obscured central quasar. Using the mid-infrared and submm observations we derive infrared luminosities which are found to be in excess of L>10^12Lsun. The submillimetre (850micron) to X-ray (2 keV) spectral indices (alpha_SX) span a wide range. About half of the type-2 QSOs have values typical for a Compton-thick AGN with only 1 per cent of the nuclear emission seen through scattering and, the remaining with values typical of submm-bright galaxies. Combining the available observational evidence we outline a possible scenario for the early stages of evolution of these sources.