High resolution soft X-ray spectroscopy of M 87 with the reflection grating spectrometers on XMM-Newton

I Sakelliou, G Peterson, T Tamura, FBS Paerels, JS Kaastra, E Belsole, H Bohringer, G Branduardi-Raymont, C Ferrigno, JW den Herder, J Kennea, RF Mushotzky, WT Vestrand, DM Worrall

Research output: Contribution to journalArticle (Academic Journal)peer-review

Abstract

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.

Original languageEnglish
Pages (from-to)903-909
Number of pages7
JournalAstronomy and Astrophysics
Volume391
Issue number3
DOIs
Publication statusPublished - Sep 2002

Keywords

  • galaxies : clusters : general
  • galaxies : clusters : individual : virgo
  • galaxies : individual : M 87
  • galaxies : cooling flows
  • galaxies : abundances
  • X-rays : galaxies
  • EARLY-TYPE GALAXIES
  • COOLING FLOWS
  • ELLIPTIC GALAXIES
  • VIRGO CLUSTER
  • HOT GAS
  • M87
  • HALO
  • ABUNDANCES
  • METALLICITY
  • MULTIPHASE

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