Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..587..416h&link_type=abstract
GAMMA 2001: Gamma-Ray Astrophysics 2001. AIP Conference Proceedings, Volume 587, pp. 416-421 (2001).
Astronomy and Astrophysics
Astrophysics
Galaxy Clusters, X-Ray Sources, X-Ray Bursts, Gamma-Ray Sources, Gamma-Ray Bursts
Scientific paper
Galaxy clusters appear to have a hard X-ray component based on recent SAX observations. The emission is best fit by a powerlaw and is likely non-thermal in origin. For the Coma cluster, the non-thermal emission is 10% of the thermal component in the 2-10 keV range and dominates above 25 keV. Thus it should be the dominant component in the soft gamma-ray regime. The spectral index is not well constrained by the current X-ray data but appears to be flatter than predicted by the standard Synchrotron-inverse Compton model for both Coma and A2256. INTEGRAL will be able to measure the spectral index of Coma, for example, to 20% and provide an important constraint on emission models. INTEGRAL observations should also reduce possible systematic errors associated with these early detections. The SAX observations challenge the standard model for non-thermal emission since some NT clusters have radio halos (Coma, A2256), others do not (A2199). Alternative emission processes have been suggested to explain the lack of radio halo emission in these clusters. Future missions such as GLAST will provide an important constraint on models of cluster formation and evolution as traced by cosmic-rays. .
Chiang James
Henriksen Mark
No associations
LandOfFree
The soft γ-ray spectrum of galaxy clusters does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The soft γ-ray spectrum of galaxy clusters, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The soft γ-ray spectrum of galaxy clusters will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1101828