Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für extraterrestrische Physik     Collection: Theory & Complex Plasmas     Display Documents



ID: 10744.0, MPI für extraterrestrische Physik / Theory & Complex Plasmas
High resolution soft X-ray spectroscopy of M 87 with the reflection grating spectrometers on XMM-Newton
Authors:Sakelliou, I.; Peterson, J. R.; Tamura, T.; Paerels, F. B. S.; Kaastra, J. S.; Belsole, E.; Böhringer, H.; Branduardi-Raymont, G.; Ferrigno, C.; den Herder, J. W.; Kennea, J.; Mushotzky, R. F.; Vestrand, W. T.; Worrall, D. M.
Language:English
Date of Publication (YYYY-MM-DD):2002-09
Title of Journal:Astronomy & Astrophysics
Journal Abbrev.:Astron. Astrophys.
Volume:391
Issue / Number:3
Start Page:903
End Page:909
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:We present high-resolution X-ray spectroscopic observations of M 87 with the Reflection Grating Spectrometers on XMM-Newton. We detect strong K-shell line emission from N, O, Ne, Mg, some emission from He-like Si, a fully resolved set of Fe L-shell emission spectra, and some emission from C. The angular intensity distributions of the strong emission lines are detectably resolved on scales (15-160)". The gas in the inner arcmin of M 87 has a multi-phase structure, as indicated by the similarity of the emission line profiles of Fe L shell ions with widely separated ionization potentials. The global Fe L spectrum is approximately consistent with an isothermal plasma at kT(e) similar to 1.8 keV, in addition to a component with a temperature distribution appropriate to an isobaric cooling flow, but with a minimum temperature cutoff of kT(min) approximate to 600 eV. The behaviour of this cooling-flow component is qualitatively similar to what is seen in other cooling flow clusters. Finally, we do not find any strong evidence for a spatial variation in abundances due to resonance scattering redistribution in the inner arcminute of the core.
Free Keywords:galaxies : clusters : general; galaxies : clusters : individual : virgo; galaxies : individual : M 87; galaxies : cooling flows; galaxies : abundances; X-rays : galaxies
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für extraterrestrische Physik
External Affiliations:Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W; Midlands, England; Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA; SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands; CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France; Max Planck Inst Extraterr Phys, D-8046 Garching, Germany; Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA; NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA; Los Alamos Natl Lab, Los Alamos, NM 87545 USA; Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England; Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England
Identifiers:ISI:000177590500010
ISSN:0004-6361
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.