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Astron. Astrophys. 335, 161-172 (1998)


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High-energy gamma-ray emission from the Galactic Center

H.A. , Mayer-Hasselwander 1, D.L. , Bertsch 2, B.L. , Dingus 3, A. , Eckart 1, J.A. , Esposito 2, 10, R. , Genzel 1, R.C. , Hartman 2, S.D. , Hunter 2, G. , Kanbach 1, D.A. , Kniffen 4, Y.C. , Lin 5, P.F. , Michelson 5, A. , Mücke 1, C. , von , Montigny 6, R. , Mukherjee 7, P.L. , Nolan 5, M. , Pohl 8, O. , Reimer 1, E.J. , Schneid 9, P. , Sreekumar 2, 10, D.J. and Thompson 2

1 Max-Planck-Institut für Extraterrestrische Physik, D-85748 Garching, Germany
2 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
3 University of Utah, Salt Lake City, Utah, USA
4 Department of Physics and Astronomy, Hampden-Sydney College, Hampden-Sydney, VA 23943, USA
5 W.W. Hansen Experimental Physics Laboratory and Department of Physics, Stanford University, Stanford, CA 94305, USA
6 Landessternwarte Königstuhl, D-69117 Heidelberg, Germany
7 Barnard College & Columbia University, Columbia Astrophysics Lab, New York, NY 10027, USA
8 Danish Space Research Institute, DK-2100 Copenhagen O, Denmark
9 Northrop Grumman Corporation, Bethpage, NY 11714, USA
10 USRA Research Associate

Received 24 September 1997 / Accepted 24 March 1998

Abstract

The EGRET instrument on the Compton Gamma-Ray Observatory has observed the Galactic Center (GC) region with good coverage at a number of epochs. A strong excess of emission is observed, peaking at energies [FORMULA] MeV in an error circle of 0.2 degree radius including the position [FORMULA] and [FORMULA]. The close coincidence of this excess with the GC direction and the fact that it is the strongest emission maximum within 15 degrees from the GC is taken as compelling evidence for the source's location in the GC region. The history of the emission intensity, observed over 5 years, leaves room for possible time variation; however, it does not provide evidence. The angular extent of the excess appears only marginally compatible with the signature expected for a single compact object. The emission therefore may stem from one or more compact objects or may originate from diffuse interactions within 85 pc from the center of the Galaxy at 8.5 kpc distance. The spatial distribution of the emission does not correlate with the details of the CO-line surveys. Thus, in spite of the existence of a strong emission peak, earlier conclusions based on an apparent `gamma-ray deficit', postulating the masses of the `wide-line' clouds in the GC area to be an order of magnitude lower than indicated by naive CO interpretation, are supported. However, the total gas mass in the Nuclear Bulge (NB) derived from the gamma-ray emission is found to be in agreement with the mass which in recent studies has been derived from molecular-line and FIR surveys. The [FORMULA] -ray emission spectrum is peculiar and different from the spectrum of the large-scale galactic diffuse emission. A diffuse emission scenario requires an enhanced and peculiar Cosmic Ray (CR) spectrum as suggested for the electrons in the `Radio Arc'. A compact sources model hints at an origin in pulsars. While the spectrum suggests middle-aged pulsars like Vela, too many are required to produce the observed flux. The only detected very young pulsar, the Crab pulsar, has an incompatible spectrum. However, it is not proven that the Crab spectrum is characteristic for all young pulsars: thus, a single or a few very young pulsars (at the GC not detectable in radio emission), provided their gamma-ray emission is larger than that of the Crab pulsar by a factor of 13, are likely candidates. Alternatively, more exotic scenarios, related to the postulated central black hole or dark matter (neutralino) annihilation, may be invoked.

Key words: ISM: clouds – ISM: general – Galaxy: center – gamma rays: observations

Send offprint requests to: HRM@MPE.MPG.DE

© European Southern Observatory (ESO) 1998

Online publication: June 12, 1998

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