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Title:
An X-ray absorption analysis of the high-velocity system in NGC 1275
Authors:
Gillmon, K.; Sanders, J. S.; Fabian, A. C.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA; Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0389, USA), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 348, Issue 1, pp. 159-164. (MNRAS Homepage)
Publication Date:
02/2004
Origin:
MNRAS
MNRAS Keywords:
galaxies: clusters: individual: Abell 426, galaxies: individual: NGC 1275, galaxies: interactions, X-rays: galaxies
DOI:
10.1111/j.1365-2966.2004.07336.x
Bibliographic Code:
2004MNRAS.348..159G

Abstract

We present an X-ray absorption analysis of the high-velocity system (HVS) in NGC 1275 using results from a deep 200-ks Chandra observation. We are able to describe the morphology of the HVS in more detail than ever before. We present a Hubble Space Telescope image for comparison, and note close correspondence between the deepest X-ray absorption and the optical absorption. A column density map of the HVS shows an average column density NH of 1 × 1021 cm-2 with a range from ~5 × 1020 to 5 × 1021 cm-2. From the NH map we calculate a total mass for the absorbing gas in the HVS of (1.32 +/- 0.05) × 109 Msolar at solar abundance. 75 per cent of the absorbing mass is contained in the four regions of deepest absorption. We examine temperature maps produced by spectral fitting and find no direct evidence for shocked gas in the HVS. Using deprojection methods and the depth of the observed absorption, we are able to put a lower limit on the distance of the HVS from the nucleus of 57 kpc, showing that the HVS is quite separate from the body of NGC 1275.

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