EDP Sciences
Free Access
Volume 376, Number 1, September II 2001
Page(s) 77 - 84
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361:20010971
Published online 15 September 2001

A&A 376, 77-84 (2001)
DOI: 10.1051/0004-6361:20010971

BeppoSAX observations of Mrk 841 and Mrk 335

S. Bianchi1, G. Matt1, F. Haardt2, L. Maraschi3, F. Nicastro4, G. C. Perola1, P. O. Petrucci3 and L. Piro5

1  Dipartimento di Fisica, Università degli Studi "Roma Tre", Via della Vasca Navale 84, 00146 Roma, Italy
2  Dipartimento di Scienze, Università dell'Insubria, Via Lucini 3, 22100 Como, Italy
3  Osservatorio Astronomico di Brera, Via Brera 28, 20121 Milano, Italy
4  Harvard-Smithsonian Center for Astrophysics, 60 Garden st., Cambridge, MA 02138, USA
5  Istituto di Astrofisica Spaziale, C.N.R., Via Fosso del Cavaliere, 00133 Roma, Italy

(Received 30 January 2001 / Accepted 4 July 2001 )

We present and discuss BeppoSAX observations of Mrk 841 and Mrk 335, two Seyfert 1 galaxies in which previous observations have established the presence of soft excesses. We confirm the soft excess in both sources, even if for Mrk 841 a warm absorber provides a fit almost as good as the one with a true excess. As far as the hard X-ray continuum is concerned, a Comptonization model provides a fit as good as a power law and a physically sound solution for Mrk 841. For Mrk 335, the Comptonization model gives a result which is somewhat better on statistical ground, but rather problematic on physical ground. The most interesting results regard the reprocessing components. For Mrk 841 we find a very large reflection continuum but an almost normal iron line equivalent width even if, within the errors, a solution in which both components are a factor ~2 larger than expected for an accretion disc is still marginally acceptable. If this is the case, an anisotropy of the primary emission seems the best explanation. On the contrary, in Mrk 335 we find a very large iron line EW but a reflection component not accordingly large. In this case, the best solution seems to be in terms of reflection from an ionized disc.

Key words: galaxies: individual: Mrk 841, Mrk 335 -- galaxies: Seyfert -- X-rays: galaxies

Offprint request: S. Bianchi, bianchi@fis.uniroma3.it

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