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Discovery of Warm Gas in the Virgo Cluster

Published online by Cambridge University Press:  12 April 2016

R. Lieu ,
J.P.D. Mittaz ,
S. Bowyer ,
J.H.M.M. Schmitt  and
J. Lewis
R. Lieu
Affiliation:
Center for EUV Astrophysics, 2150 Kittredge Street, University of California, Berkeley, CA 94720-5030, USA
J.P.D. Mittaz
Affiliation:
Milliard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
S. Bowyer
Affiliation:
Center for EUV Astrophysics, 2150 Kittredge Street, University of California, Berkeley, CA 94720-5030, USA
J.H.M.M. Schmitt
Affiliation:
Center for EUV Astrophysics, 2150 Kittredge Street, University of California, Berkeley, CA 94720-5030, USA Max Planck Institut für Extraterrestrische Physik, W-8046 Garching-bei-München, Germany
J. Lewis
Affiliation:
Center for EUV Astrophysics, 2150 Kittredge Street, University of California, Berkeley, CA 94720-5030, USA

Abstract

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During the EUVE sky survey of the Virgo region, a central source positionally coincident with the X-ray emitting galaxy M87, and a surrounding halo of extended emission, were detected in the 0.065–0.248 keV band. A detailed comparison of these data with the ROSAT PSPC data of M87 revealed an excess flux at energies < 0.4 keV within the central 30’ radius which cannot be associated with the well-known cluster gas at X-ray temperatures (kT ≥ a few keV). Instead, it is necessary to introduce a second gas component, of temperature T ~ 5 × 106K (kT ~ 0.1 keV). The resulting two-component model (warm + hot) can account for all the data. The origin and stability of the warm component, with a temperature near the peak of the thermal plasma cooling curve, is unclear. Both the temperature and spatial extent argue against cooling flow as the primary process responsible for its production. Other mechanisms, such as a galactic wind and heating by galaxy motions, must be considered.

Type
II. Extragalactic Sources in the EUV
Information
International Astronomical Union Colloquium , Volume 152: Astrophysics in the Extreme Ultraviolet , 1996 , pp. 37 - 43
Copyright
Copyright © Kluwer 1996

References

Axford, W.I. 1981, 17th International Cosmic Ray Conference, 12, 155 Google Scholar
Böhringer, H., Briel, U.G., Schwarz, R.A., Voges, W., Hartner, G. & Trümper, J. 1994, Nature, 368, 828 Google Scholar
Fabricant, D. & Gorenstein, P. 1983, ApJ, 267, 535 Google Scholar
Forman, W. Jones, C. & Defaccio, M. 1985, ESO Workshop on the Virgo Cluster of Galaxies, ed. Richter, O.-G. & Binggeli, B., ESO Conf. Proc. No. 20, ESO, Garching, 323 Google Scholar
Mewe, R., Gronenschild, E.H.B.M. & Van Den, Oord 1985, A&AS, 62, 197 Google Scholar
Mewe, R., Lemen, J.R. & Van Den Oord, G.H.J. 1986, A&AS, 65, 511 Google Scholar
Sarazin, C.L. 1986, Rev. Mod. Phys., 58, 1 Google Scholar
Snowden, S. et al. 1995, ApJ, submittedGoogle Scholar
Stark, A.A., Gammie, C.F., Wilson, R.W., Bally, J., Linke, R.A., Heiles, C. & Hurwitz, M. 1992, ApJS, 79, 77 Google Scholar
Stewart, G.C., canizares, C.R., Fabian, A.C. & Nulsen, P.E.J. 1984, ApJ, 278, 536 CrossRefGoogle Scholar
White, D.A., Fabian, A.C., Johnstone, R.M., Mushotzky, R.F. & Arnaud, K.A. 1991, MNRAS, 252, 72 Google Scholar