Astron. Astrophys. 342, L41-L44 (1999)

Letter to the Editor

BeppoSAX uncovers the hidden Seyfert 1 nucleus in the Seyfert 2 galaxy NGC 2110

G. Malaguti ¹, L. Bassani ¹, M. Cappi ¹, A. Comastri ², G. Di Cocco ¹, A.C. Fabian ³, G.G.C. Palumbo ⁴, T. Maccacaro ⁵, R. Maiolino ⁶, P. Blanco ⁷, M. Dadina ⁸, D. Dal Fiume ¹, F. Frontera ¹ and M. Trifoglio <sup>1

1</sup> ITESRE/CNR, via Piero Gobetti 101, I-40129 Bologna, Italy
² Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy
³ Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK
⁴ Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, I-40127 Bologna, Italy
⁵ Osservatorio Astronomico di Brera, via Brera 28, I-20121 Milano, Italy
⁶ Osservatorio Astrofisico di Arcetri, L.E.Fermi 5, I-50125 Firenze, Italy
⁷ UCSD/CASS, 9500 Gilman Drive, Code 0111, La Jolla, CA, USA
⁸ BeppoSAX SDC, ASI, via Corcolle 19, I-00131 Roma, Italy

Received 19 November 1998 / Accepted 11 January 1999

Abstract

The Seyfert 2 galaxy NGC 2110 has been observed with BeppoSAX between 0.5 and 150 keV. The high energy instrument onboard, PDS, has succeeded in measuring for the first time the spectrum of this source in the 13-150 keV range. The PDS spectrum, having a photon index is fully compatible with that expected from a Seyfert 1 nucleus. In the framework of unified models, the harder () 2-10 keV spectrum is well explained assuming the presence of a complex partial + total absorber (cm^-225% +cm^-2100%). The high column density of this complex absorber is consistent both with the FeK line strength and with the detection of an absorption edge at keV in the power-law spectrum.

Key words: X-rays: galaxies galaxies: Seyfert  galaxies: individual: NGC 2110

Send offprint requests to: G. Malaguti (malaguti@tesre.bo.cnr.it)

SIMBAD Objects

Contents

• 1. Introduction
• 2. Observation and data reduction
• 3. Spectral analysis
  • 3.1. The 0.5-10 keV spectrum
  • 3.2. The Seyfert 1 nucleus in the PDS spectrum
  • 3.3. The broad-band 0.5-150 keV spectrum
• 4. Discussion and conclusions
• Acknowledgements
• References

© European Southern Observatory (ESO) 1999

Online publication: February 23, 1999
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