THE FERMI HAZE: A GAMMA-RAY COUNTERPART TO THE MICROWAVE HAZE

By Gregory Dobler, Douglas P. Finkbeiner, I. Cholis, T. Slatyer, N. Weiner. 2009

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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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/074f3d584c8c49b97fadf23aa5e255ff4e412051

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Citations in the corpus

Dark Matter Searches with Astroparticle Data (2011, methodology): “Similarly, analysis of Fermi -LAT data has led to claims of a corresponding gamma-ray haze, described as the high-energy counterpart to the WMAP haze (Dobler et al., 2010) and produced by IC scattering of electrons and positions on the ISRF.”
Galactic Searches for Dark Matter (2012, methodology): “erized, an interesting morphological structure has come to light in recent analysis of the data. After subtracting out templates for the neutral pion, inverse Compton, and 74 bremsstrahlung emission, Dobler et al. (2010) rst reported a detection of the \Fermi Haze," which extends 50above and be”
THE SPECTRUM AND MORPHOLOGY OF THE FERMI BUBBLES (2014, background): “…Salam International Center for Theoretical Physics, Strada Costiera 11, Trieste 34151 - Italy Gamma-ray lobes, called the Fermi bubbles, were discovered (Dobler et al. 2010; Su et al. 2010; Su & Finkbeiner 2012) in a search for a gamma-ray counterpart to the Wilkinson Microwave Anisotropy Probe…”
Background model systematics for the Fermi GeV excess (2014, background): “Moreover, the analysis of gamma-ray data has led to the discovery of the Fermi bubbles [23, 24], which are believed to be the inverse Compton scattering (ICS) counterpart [23] of the WMAP haze [25, 26], recently observed also with Planck [27].”
COrE (Cosmic Origins Explorer) A White Paper (2011, background): “The existence of an anomalous microwave “haze” (in the WMAP data) coinciding with gamma-ray bubbles (in the Fermi-LAT data) centered around the GC has been largely debated and remains a controversial issue ([213, 158].”
WIMP dark matter candidates and searches—current status and future prospects (2017, background): “Interesting features were identified in the spectrum of γrays originating from regions around the GC in the WMAP data [341] (so-called WMAP haze), Fermi-LAT data [342, 343] (Fermi bubbles) and Planck data [344] (Planck haze), with a possible common origin.”
THE SPECTRUM OF ISOTROPIC DIFFUSE GAMMA-RAY EMISSION BETWEEN 100 MeV AND 820 GeV (2014, background): “Dobler et al. (2010) and Su et al. (2010) have noted the existence of large-scale structures of residual diffuse γ-ray emission above and below the Galactic center region that became well known as the ‘Fermi Bubbles’.”
THE FERMI BUBBLES. I. POSSIBLE EVIDENCE FOR RECENT AGN JET ACTIVITY IN THE GALAXY (2011, methodology): “For the latter, gamma rays can be produced by the inverse Compton (IC) scattering of CR electrons with the interstellar radiation field (ISRF) and the cosmic microwave background (CMB; Dobler et al. 2010, Su et al. 2010).”
GIANT GAMMA-RAY BUBBLES FROM FERMI-LAT: ACTIVE GALACTIC NUCLEUS ACTIVITY OR BIPOLAR GALACTIC WIND? (2010, methodology): “As in Dobler et al. (2010), we construct maps of front-converting and back-converting events separately, smooth to a common PSF, and then combine them.”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS (2012, background): “One interesting possibility characterizes the haze as a separate hard spectrum synchrotron component associated with the Gammaray bubbles (Planck Collaboration IX 2012; Dobler et al. 2010).”
Cool outflows in galaxies and their implications (2020, background): “Long before the Fermi discovery of two giant ∼ 12-kpc 1-100 GeV γ-ray emitting bubbles extending ∼ 55◦ on either side of the Galactic center (Fig. 9a; Su et al. 2010; Dobler et al. 2010; Ackermann et al. 2014) and the earlier discovery of a microwave “haze” in the data from the Wilkinson Microwave A”
A Tentative Gamma-Ray Line from Dark Matter Annihilation at the Fermi Large Area Telescope (2012, unknown): “[68]).”
The physics of galactic winds driven by active galactic nuclei (2012, background): “Fermi9 also recently detected bubbles of a similar scale in our Galaxy, clearly originating from the Galactic Center (Dobler et al. 2010; Su et al. 2010).”