Large-amplitude rapid X-ray variability in the narrow-line Seyfert 1 galaxy PG 1404$+$226

TL;DR

This study analyzes a long XMM-Newton observation of the Seyfert galaxy PG 1404+226, revealing rapid, large-amplitude X-ray variability and exploring the origin of the soft X-ray excess through spectral modeling.

Contribution

It provides the first detailed analysis of rapid X-ray variability in PG 1404+226, supporting a lamppost geometry for the corona and modeling the soft excess with disk Comptonization and relativistic reflection.

Findings

Detected a factor of 7 variability in 10 ks.

Soft X-ray excess described by disk Comptonization and relativistic reflection models.

X-ray rms spectrum indicates variable primary emission and less variable soft excess.

Abstract

We present the first results from a detailed analysis of a new, long ($\sim100$ ks) XMM-Newton observation of the narrow-line Seyfert 1 galaxy PG 1404$+$226 which showed a large-amplitude, rapid X-ray variability by a factor of $\sim7$ in $\sim10$ ks with an exponential rise and a sharp fall in the count rate. We investigate the origin of the soft X-ray excess emission and rapid X-ray variability in the source through time-resolved spectroscopy and fractional root-mean-squared (rms) spectral modeling. The strong soft X-ray excess below 1 keV observed both in the time-averaged and time-resolved spectra is described by the intrinsic disk Comptonization model as well as the relativistic reflection model where the emission is intensive merely in the inner regions ($r_{\rm in}<1.7 r_{\rm g}$) of an ionized accretion disk. We detected no significant UV variability while the soft X-ray excess flux varies together with the primary power-law emission (as $F_{{\rm primary}}\propto F_{{\rm excess}}^{1.54}$), although with a smaller amplitude, as expected in the reflection scenario. The observed X-ray fractional rms spectrum is approximately constant with a drop at $\sim0.6$ keV and is described by a non-variable emission line component with the observed energy of $\sim0.6$ keV and two variable spectral components: a more variable primary power-law emission and a less variable soft excess emission. Our results suggest the `lamppost geometry' for the primary X-ray emitting hot corona which illuminates the innermost accretion disk due to strong gravity and gives rise to the soft X-ray excess emission.