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Titolo:
BeppoSAX observations of Mrk 841 and Mrk 335
Autore:
Bianchi, S; Matt, G; Haardt, F; Maraschi, L; Nicastro, F; Perola, GC; Petrucci, PO; Piro, L;
Indirizzi:
Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy Univ Roma Tre Rome Italy I-00146 , Dipartimento Fis, I-00146 Rome, Italy Univ Insubria, Dipartimento Sci, I-22100 Como, Italy Univ Insubria Como Italy I-22100 , Dipartimento Sci, I-22100 Como, Italy Osserv Astron Brera, I-20121 Milan, Italy Osserv Astron Brera Milan Italy I-20121 tron Brera, I-20121 Milan, Italy Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA Harvard Smithsonian Ctr Astrophys Cambridge MA USA 02138 ge, MA 02138 USA CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy CNR Rome Italy I-00133CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy
Titolo Testata:
ASTRONOMY & ASTROPHYSICS
fascicolo: 1, volume: 376, anno: 2001,
pagine: 77 - 84
SICI:
1432-0746(200109)376:1<77:BOOM8A>2.0.ZU;2-2
Fonte:
ISI
Lingua:
ENG
Soggetto:
ACTIVE GALACTIC NUCLEI; SOFT-X-RAY; SEYFERT-1 GALAXIES; ROSAT; SPECTRA; ULTRAVIOLET; EMISSION; NLS1S; GINGA; BUMP;
Keywords:
galaxies : individual : Mrk 841, Mrk 335; galaxies : Seyfert; X-rays : galaxies;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
32
Recensione:
Indirizzi per estratti:
Indirizzo: Bianchi, S Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy Univ Roma Tre Via Vasca Navale 84 Rome Italy I-00146 me, Italy
Citazione:
S. Bianchi et al., "BeppoSAX observations of Mrk 841 and Mrk 335", ASTRON ASTR, 376(1), 2001, pp. 77-84

Abstract

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 similar to2 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.

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Documento generato il 04/12/20 alle ore 09:51:17