EDP Sciences
Free Access
Issue
A&A
Volume 411, Number 2, November IV 2003
Page(s) 77 - 82
Section Galactic structure and dynamics
DOI https://doi.org/10.1051/0004-6361:20031466
Published online 17 November 2003


A&A 411, 77-82 (2003)
DOI: 10.1051/0004-6361:20031466

Research Note

BeppoSAX observations of Seyfert 1s in the Piccinotti sample

I. poorly studied sources
A. Quadrelli, A. Malizia, L. Bassani and G. Malaguti

IASF/CNR, via Piero Gobetti 101, 40129 Bologna, Italy
(Received 16 June 2003 / Accepted 15 September 2003 )

Abstract
In this work we present the first of two papers devoted to the study of the X-ray spectral characteristics of Seyfert 1 galaxies in the Piccinotti sample. In particular we analyse here the BeppoSAX broad band (0.1-100 keV) data of 4 objects which, despite their X-ray brightness, have been historically poorly studied due to their late identification with an AGN; these are H0111-149 (MKN 1152), H0235-525 (ESO 198-G24), H0557-385 (IRAS F05563-3820) and H1846-786 (IRAS F18389-7834). We have assumed for all the sources a baseline model which includes a power law with an exponential cut-off plus a reflection component and an iron K $_\alpha$ line; we have also searched for the presence of intrinsic absorption and/or a soft excess component. Our analysis indicates the presence of complex absorption in two objects (H0557-385 and H0111-149) best described by a combination of two uniform absorbers, one cold and one warm. Only in one source, H0557-385, a soft excess component has been measured. The primary continuum is best described by a canonical power law ( $\Gamma=1.7{-}2$) with a high energy cut-off in the range 40-130 keV. A cold reflection component is likely present in all sources with values ranging from less than 0.6 to higher than 2. In 3 out of 4 objects we find a cold iron line having equivalent width typical of Seyfert 1s (100-200 eV).


Key words: X-rays: galaxies -- galaxies: Seyfert -- galaxies: general

Offprint request: A. Quadrelli, quadrelli@bo.iasf.cnr.it

SIMBAD Objects



© ESO 2003

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