XMM-Newton view of the prototype narrow-line Seyfert 1 galaxy I Zw 1

Details XMM-Newton view of the prototype narrow-line Seyfert 1 galaxy I Zw 1 XMM-Newton view of the prototype narrow-line Seyfert 1 galaxy I Zw 1

2003-12-12

arxiv.org/abs/astro-ph/0312342v1

Astronomy and Astrophysics

Astrophysics

14 pages, uses emulateapj5, submitted to ApJ

Scientific paper

We present results based on an XMM-Newton observation of the prototype narrow-line Seyfert 1 galaxy I Zw 1 performed in June 2002. The 0.6-12 keV spectrum is well described by a steep power-law (Gamma\sim 2.3) and a weak soft blackbody component (kT \sim 200 eV) below 2 kev. The soft X-ray excess emission is featureless and contributes only about 10% to the total X-ray emission in the $0.6-2\kev$ band. There are tentative evidences for an iron iron Kalpha line and an iron K edge, both from high ionized He-like iron. The 0.6-12kev continuum of I Zw 1 can be explained in terms of a blackbody (kT \sim 40eV), thermal comptonization and its reflection off the surface of an ionized accretion disk. We note that characterizing the soft excess copmonent `above a power law continuum' may not be appropriate due to the low energy curvature of a comptonized spectrum. X-ray emission from I Zw 1 was highly variabile during the observation. I Zw 1 showed a large, symmetric X-ray flare during which the X-ray luminosity increased by about 6e43 erg/s in an interval of 2800s only. The X-ray spectral variability was unusual during the flare. In contrast to the general observation of spectral steepening with flux from Seyfert galaxies, there is a clear evidence for hardening of the 0.6-10kev spectrum of I Zw 1 with increasing flux. This hardening is due to a stronger and slightly flatter power-law component at higher flux without any change in the soft X-ray excess component. The large flare, the accompanying spectral flattening, and the steady nature of the soft excess component may be due to an additional flatter power-law component during the flare possibly arising as a result of ejection of electron plasma and the SSC process.

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