The Fermi Haze: A Gamma-Ray Counterpart to the Microwave Haze
View/ Open
Published Version
https://doi.org/10.1088/0004-637X/717/2/825Metadata
Show full item recordCitation
Dobler, Gregory, Douglas P. Finkbeiner, Ilias Cholis, Tracy Slatyer, and Neal Weiner. 2010. “The Fermi Haze: A Gamma-Ray Counterpart to the Microwave Haze.” The Astrophysical Journal 717 (2) (June 18): 825–842. doi:10.1088/0004-637x/717/2/825.Abstract
The Fermi Gamma-ray Space Telescope reveals a diffuse inverse Compton (IC) signal in the inner Galaxy with a similar spatial morphology to the microwave haze observed by WMAP, supporting the synchrotron interpretation of the microwave signal. Using spatial templates, we regress out π0 gammas, as well as IC and bremsstrahlung components associated with known soft-synchrotron counterparts. We find a significant gamma-ray excess toward the Galactic center with a spectrum that is significantly harder than other sky components and is most consistent with IC from a hard population of electrons. The morphology and spectrum are consistent with it being the IC counterpart to the electrons which generate the microwave haze seen at WMAP frequencies. In addition, the implied electron spectrum is hard; electrons accelerated in supernova shocks in the disk which then diffuse a few kpc to the haze region would have a softer spectrum. We describe the full-sky Fermi maps used in this analysis and make them available for download.Terms of Use
This article is made available under the terms and conditions applicable to Other Posted Material, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#LAACitable link to this page
http://nrs.harvard.edu/urn-3:HUL.InstRepos:33462895
Collections
- FAS Scholarly Articles [18292]
Contact administrator regarding this item (to report mistakes or request changes)