EDP Sciences
Free Access
Volume 408, Number 3, September IV 2003
Page(s) 921 - 928
Section Galactic structure and dynamics
DOI https://doi.org/10.1051/0004-6361:20031021

A&A 408, 921-928 (2003)
DOI: 10.1051/0004-6361:20031021

Chandra LETGS and XMM-Newton observations of NGC 4593

K. C. Steenbrugge1, J. S. Kaastra1, A. J. Blustin2, G. Branduardi-Raymont2, M. Sako3, E. Behar4, S. M. Kahn5, F. B. S. Paerels5 and R. Walter6

1  SRON National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
2  Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking Surrey RH5 6NT, UK
3  Theoretical Astrophysics and Space Radiation Laboratory, California Institute of Technology, MC 130-133, Pasadena, CA 91125, USA
4  Physics Department, Technion 32000, Israel
5  Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA
6  University of Geneva, Geneva, Switzerland

(Received 21 January 2003 / Accepted 24 June 2003)

In this paper, we analyze spectra of the Seyfert 1 galaxy NGC 4593 obtained with the Chandra Low Energy Transmission Grating Spectrometer (LETGS), the Reflection Grating Spectrometer (RGS) and the European Photon Imaging Camera's (EPIC) onboard of XMM-Newton. The two observations were separated by ~7 months. In the LETGS spectrum we detect a highly ionized warm absorber corresponding to an ionization state of $400\times 10 ^{-9}$ W m, visible as a depression at 10-18 Å. This depression is formed by multiple weak Fe and Ne lines. A much smaller column density was found for the lowly ionized warm absorber, corresponding to $\xi = 3 \times 10 ^{-9}$ W m. However, an intermediate ionization warm absorber is not detected. For the RGS data the ionization state is hard to constrain. The EPIC results show a narrow Fe K $\alpha$ line.

Key words: galaxies: active -- galaxies: Seyfert -- galaxies: individual: NGC 4593 -- X-rays: galaxies -- techniques: spectroscopic

Offprint request: K. C. Steenbrugge, K.C.Steenbrugge@sron.nl

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