Breaking the rules at $z\simeq$0.45: the rebel case of RBS 1055

Abstract

We report on a long (250 ks) NuSTAR observation of the bright quasar RBS 1055 performed in March 2021, and archival XMM-Newton pointings (185 ks) taken in July 2014. An optical spectrum of the source taken with the Double Spectrograph at the Palomar Observatory, quasi-simultaneous with the NuSTAR observations, is also analyzed. We find that the two-coronae model, in which a warm and hot corona coexist, well reproduces its broad band spectrum, with temperatures kT${}_e=0.12_{-0.03}^{+0.08}$ keV, kT${}_e=30_{-10}^{+40}$ keV and Thomson optical depths $\tau$=30${}_{-10}^{+15}$ and $\tau$=3.0${}_{-1.4}^{+1.0}$ for the former and the latter component, respectively. We confirm the presence of an intense Fe K$\alpha$ emission line (EW=55$\pm$6 eV) and, when a toroidal model is considered for reproducing the Compton reflection, a Compton-thin solution with N${}_{\mathrm{H}}=(3.2_{-0.8}^{+0.9})\times 10^{23}$ cm${}^{-2}$ for the circumnuclear reflector is found. The analysis of the optical spectrum reveals a likely peculiar configuration of our line of sight with respect to the nucleus, and the presence of a broad [O III] component, tracing outflows in the NLR, with a velocity shift $v=$1500$\pm 100$ km s${}^{-1}$, leading to a mass outflow rate ${\dot{M}}_{\mathrm{out}}=25.4\pm 1.5$ M${}_{\odot }$ yr${}^{-1}$ and outflow kinetic power ${\dot{E}}_{\mathrm{kin}}$/L${}_{\mathrm{Bol}}$ $\sim$0.33%. We estimate the BH mass to be in the range 2.8$\times$10${}^8$-1.2$\times$10${}^9$ M${}_{\odot }$, according to different BLR emission lines, with an average value of <$M{}_{\mathrm{BH}}$>=6.5$\times$10${}^8$ M${}_{\odot }$. With an Fe K$\alpha$ which is 3$\sigma$ above the value predicted from the EW-L${}_{2-10\mathrm{keV}}$ relation and an extreme source brightness at 2 keV (a factor 10-15 higher than the one expected from the optical/UV), RBS 1055 confirms to be an outlier in the X-rays, compared to other objects in the same luminosity and redshift range.

arXiv comment11 pages, 10 figures, 4 tables. Accepted for publication in Astronomy & Astrophysics

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