X-rays from the radio-quiet quasar PG 1407+265: relativistic jet or accretion disc emission?

Details X-rays from the radio-quiet quasar PG 1407+265: relativistic jet or accretion disc emission? X-rays from the radio-quiet quasar PG 1407+265: relativistic jet or accretion disc emission?

2005-10-25

arxiv.org/abs/astro-ph/0510703v2

Mon.Not.Roy.Astron.Soc.365:960-968,2006

Astronomy and Astrophysics

Astrophysics

9 pages, 8 figures. Accepted for publication in MNRAS. Correction made to reported aox value. No changes in conclusions

Scientific paper

10.1111/j.1365-2966.2005.09780.x

We present two XMM-Newton observations of the luminous (L_x > 10^46 erg/s), radio-quiet quasar, PG 1407+265, separated by eleven months. The data indicate two distinct states: a highly variable, bright state (first epoch); and a quiescent, low-flux one (second epoch). During the low-flux state the spectrum is consistent with a single, unabsorbed power law. However, during the brighter state a highly variable, steep component is statistically required. Contemporaneous UV data from the Optical Monitor allow an estimate of the optical-to-X-ray spectral index (alpha_ox), which appears typical of radio-quiet quasars during the low-flux state, but extremely flat during the high-flux state. The XMM-Newton data can be described as originating from a combination of jet and accretion disc processes, in which the (relativistic) X-ray jet only works intermittently. The scenario could help describe some of the complexities seen in the broadband spectral energy distribution of PG 1407+265, such as weak high-ionisation emission lines, strong Fe II, unbeamed continuum, and the weak radio emission relative to the optical.

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