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Cambridge University Press (CUP), Proceedings of the International Astronomical Union, S275(6), p. 145-149, 2010

DOI: 10.1017/s1743921310015838

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The far-infrared view of M87 as seen by the Herschel Space Observatory

Journal article published in 2010 by M. Clemens, M. Clemens M. Xilouris E. M. Fritz J. Cotton W. D. Davies J. I. Bendo G. J. Bianchi S. Cortese L. De Looze I. Pohlen M. Verstappen J. Böhringer H. Bomans D. J. Boselli A. Corbelli E. Dariush A. Di Serego Alighieri S. Fadda D. Garcia-Appadoo D. A. Gavazzi G Baes ORCID, E. M. Xilouris, J. Fritz, W. D. Cotton, J. I. Davies, G. J. Bendo, S. Bianchi ORCID, L. Cortese, I. De Looze, M. Pohlen, J. Verstappen, H. Böhringer, D. J. Bomans, A. Boselli and other authors.
This paper was not found in any repository, but could be made available legally by the author.
This paper was not found in any repository, but could be made available legally by the author.

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Abstract

AbstractThe origin of the far-infrared emission from the nearby radio galaxy M87 remains a matter of debate. Some studies find evidence of a far-infrared excess due to thermal dust emission, whereas others propose that the far-infrared emission can be explained by synchrotron emission without the need for an additional dust emission component. We observed M87 with PACS and SPIRE as part of the Herschel Virgo Cluster Survey (HeViCS). We compare the new Herschel data with a synchrotron model based on infrared, submm and radio data to investigate the origin of the far-infrared emission. We find that both the integrated SED and the Herschel surface brightness maps are adequately explained by synchrotron emission. At odds with previous claims, we find no evidence of a diffuse dust component in M87.

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