The origin of X-ray emission in the gamma-ray emitting narrow-line Seyfert 1 1H 0323+342

Abstract

<jats:title>ABSTRACT</jats:title> <jats:p>We present the results of X-ray spectral and timing analyses of the closest gamma-ray emitting narrow-line Seyfert 1 (γ-NLS1) galaxy, 1H 0323+342. We use observations from a recent, simultaneous XMM–Newton/NuSTAR campaign. As in radio-quiet NLS1s, the spectrum reveals a soft excess at low energies (≲2 keV) and reflection features such as a broad iron K emission line. We also find evidence of a hard excess at energies above ∼35 keV that is likely a consequence of jet emission. Our analysis shows that relativistic reflection is statistically required, and using a combination of models that includes the reflection model relxill for the broad-band spectrum, we find an inclination of $i=63^{+7}_{-5}$ degrees, which is in tension with much lower values inferred by superluminal motion in radio observations. We also find a flat (q = 2.2 ± 0.3) emissivity profile, implying that there is more reflected flux than usual being emitted from the outer regions of the disc, which in turn suggests a deviation from the thin disc model assumption. We discuss possible reasons for this, such as reflection off of a thick accretion disc geometry.</jats:p>

Jetted Narrow-Line Seyfert 1 Galaxies & Co.: Where Do We Stand?

“…This confirmed also the scaling laws by Heinz and Sunyaev [80], because it was possible to overlap the jet morphologies of the two objects with the proper scaling [156]. Other studies at different wavelengths are [157][158][159][160][161][162][163][164][165][166][167].…”

Jetted Narrow-Line Seyfert 1 Galaxies & Co.: where do we stand?

“…This confirmed also the scaling laws by Heinz and Sunyaev [80], because it was possible to overlap the jet morphologies of the two objects with the proper scaling [156]. Other studies at different wavelengths are [157,158,159,160,161,162,163,164,165,166,167].…”

Generally Applicable Formalism for Modeling the Observable Signatures of Inflows, Outflows, and Moving Coronal Plasma Close to Kerr Black Holes

“…The accretion disks of black holes accreting at super-Eddington rates are expected to be geometrically thick, and the reflection of coronal emission off the funnel walls should lead to observable signatures (e.g. Brightman et al 2019;Thomsen et al 2019;Mundo et al 2020). Along these lines, Kara et al (2016) invoke the Fe Kα emission from a relativistically moving upper accretion disk layer to explain the detection of a blue shifted iron lag from the tidal disruption event Swift J1644+57.…”