The Extreme Ultraviolet Spectrum of the Kinetically Dominated Quasar 3C 270.1

TL;DR

This paper presents the first EUV spectrum of the kinetically dominated quasar 3C 270.1, revealing a steep EUV continuum consistent with known correlations and clarifying its classification regarding broad absorption lines.

Contribution

It provides the first EUV spectrum of a kinetically dominated quasar and examines its spectral features to clarify its BAL quasar status.

Findings

EUV continuum of 3C 270.1 is very steep with $eta_{EUV} \\sim 2.98$

The EUV deficit correlates with the ratio of jet power to bolometric luminosity

3C 270.1 has no broad absorption lines in multiple epochs

Abstract

Only a handful of quasars have been identified as kinetically dominated, their long term time averaged jet power, $\overline{Q}$, exceeds the bolometric thermal emission, $L_{bol}$, associated with the accretion flow. This letter presents the first extreme ultraviolet (EUV) spectrum of a kinetically dominated quasar, 3C 270.1. The EUV continuum flux density of 3C 270.1 is very steep, $F_{\nu} \sim \nu^{-\alpha_{EUV}}$, $\alpha_{EUV} =2.98\pm 0.15$. This value is consistent with the correlation of $\overline{Q}/L_{bol}$ and $\alpha_{EUV}$ found in previous studies of the EUV continuum of quasars, the EUV deficit of radio loud quasars. Curiously, although ultraviolet broad absorption line (BAL) troughs in quasar spectra are anti-correlated with $\overline{Q}$, 3C 270.1 has been considered a BAL quasar based on an SDSS spectrum. This claim is examined in terms of the EUV spectrum of OVI 1and the highest resolution CIV spectrum in the archival data and the SDSS spectrum. First, from [OIII]4959,5007 (IR) observations and the UV spectral lines, it is concluded that the correct redshift for 3C 270.1 is 1.5266. It is then found that the standard measure of broad absorption, BALnicity = 0, for MgII 2800, CIV 1549 and OVI 1032 in all epochs.