EDP Sciences
Free access
Volume 406, Number 1, July IV 2003
Page(s) 105 - 109
Section Galactic structure and dynamics
DOI http://dx.doi.org/10.1051/0004-6361:20030743

A&A 406, 105-109 (2003)
DOI: 10.1051/0004-6361:20030743

A BeppoSAX observation of MKN6

A. Malizia1, L. Bassani1, M. Capalbi2, A. C. Fabian3, F. Fiore4 and F. Nicastro5

1  IASF/CNR, via Piero Gobetti 101, 40129 Bologna, Italy
2  ASI Science Data Center, c/o ESA-ESRIN, Via Galileo Galilei, 00044 Frascati, Italy
3  Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, USA
4  INAF, Osservatorio Astronomico di Roma, Via dell'Osservatorio, 00044 Monteporzio Catone, Italy
5  Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA

(Received 4 March 2003 / Accepted 16 May 2003)

We have used the BeppoSAX satellite to study the broad band (0.5-100 keV) X-ray spectrum of the Seyfert 1.5 galaxy MKN6. The source is characterized by a power law of $\Gamma =1.7 ^{+0.08}_{-0.07}$ and there is no strong evidence for either a reflection bump or a high energy cut-off. We have detected a narrow iron line at 6.4 keV (rest frame) with an equivalent width of 98 +33-35 eV. MKN6 also exhibits strong and complex absorption. At least two components ( $N_{\rm H_{1}} =1.34 ^{+0.4}_{-0.4} \times 10 ^{22}$ cm -2 and $N_{\rm H_{2}} =4.18 ^{+2.2}_{-1.3} \times 10 ^{22}$ cm -2) are present and they both partially cover the source with covering fractions of ~90% and ~50% respectively. Comparison with a previous ASCA observation indicates that in both absorbing columns the  $N_{\rm H}$ is variable over a 2 year timescale, while the covering fractions are constant over the same amount of time. The state of each absorber is cold or mildly photoionized. The Broad Line Region (BLR) is suggested as the possible location for this complex absorption.

Key words: X-rays: galaxies -- galaxies: Seyfert  -- galaxies: individual: MKN6

Offprint request: A. Malizia, malizia@bo.iasf.cnr.it

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© ESO 2003