Absorption spectrum of the quasar HS1603+3820*
I. Observations and data analysis
ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany e-mail: email@example.com
2 Faculty of Physics, University of Białystok, Lipowa 41, 15424 Białystok, Poland e-mail: firstname.lastname@example.org
3 Steward Observatory, University of Arizona, Tucson, AZ 85721, USA e-mail: email@example.com
4 Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA e-mail: firstname.lastname@example.org
5 Copernicus Astronomical Center, Bartycka 18, 00716 Warszawa, Poland e-mail: bcz,email@example.com
Accepted: 27 September 2007
Context.We present multi-wavelength observations of the bright quasar HS1603+3820: the optical data taken with the MMT and Keck telescopes, with the 40–50 km s-1 resolution, and X-ray data taken by the Chandra X-ray Observatory satellite.
Aims.The optical spectra contain a very large number of absorption lines from numerous heavy elements. Our goal is to analyze these features to obtain constraints on the properties of associated absorbers, to be used in modeling of the quasar intrinsic flux and properties of the clouds.
Methods.We have determined the properties – column densities and redshifts – of the individual components. We derived the X-ray properties of HS1603+3820 and the optical-to-X-ray slope index .
Results.We found of 1.70, which is at the high end of the typical range for a radio quiet quasar. We found 49 individual heavy element absorption clouds, which can be grouped into eleven distinct systems. Absorbers from the associated system, which likely is the one spatially closest to the quasar, show large to column density ratio, reaching ~20.
Conclusions.Intrinsic X-ray properties of the quasar are typical. Determination of column densities of ions (including hydrogen) gives a strong foundation for modeling of the quasar ionising flux.
Key words: quasars: absorption lines / quasars: individual: HS1603+3820
Based on the observations collected at the MMT, which is a joint facility of the Smithsonian Institution and the University of Arizona. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
© ESO, 2007