# The HELLAS2XMM survey. X. The bolometric output of luminous obscured quasars: The Spitzer perspective

## TL;DR

This study estimates the spectral energy distributions and physical parameters of high X-ray-to-optical obscured quasars, revealing their bolometric luminosities, black hole masses, and low accretion rates using Spitzer infrared data.

## Contribution

It provides the first detailed SED modeling and black hole parameter estimates for a sample of luminous obscured quasars at z>0.9 using Spitzer observations.

## Key findings

- Bolometric luminosities range from 10^45 to 10^47 erg/s.
- Median bolometric correction is approximately 25.
- Black hole masses are between 0.2 and 2.5 billion solar masses.

## Abstract

Aims: We aim at estimating the spectral energy distributions (SEDs) and the physical parameters related to the black holes harbored in eight high X-ray-to-optical (F_X/F_R>10) obscured quasars at z>0.9 selected in the 2--10 keV band from the HELLAS2XMM survey. Methods: We use IRAC and MIPS 24 micron observations, along with optical and Ks-band photometry, to obtain the SEDs of the sources. The observed SEDs are modeled using a combination of an elliptical template and torus emission (using the phenomenological templates of Silva et al. 2004) for six sources associated with passive galaxies; for two point-like sources, the empirical SEDs of red quasars are adopted. The bolometric luminosities and the M_BH-L_K relation are used to provide an estimate of the masses and Eddington ratios of the black holes residing in these AGN. Results: All of our sources are detected in the IRAC and MIPS (at 24 micron) bands. The SED modeling described above is in good agreement with the observed near- and mid-infrared data. The derived bolometric luminosities are in the range ~10^45-10^47 erg s^-1, and the median 2--10 keV bolometric correction is ~25, consistent with the widely adopted value derived by Elvis et al. (1994). For the objects with elliptical-like profiles in the K_s band, we derive high stellar masses (0.8-6.2)X10^11 Mo, black hole masses in the range (0.2-2.5)X10^9 Mo, and Eddington ratios L/L_Edd<0.1, suggesting a low-accretion phase.