The GeV-TeV Galactic gamma-ray diffuse emission

Abstract

Context. The Galactic γ-ray diffuse emission is currently observed in the GeV-TeV energy range with unprecedented accuracy by the Fermi satellite. Understanding this component is crucial because it provides a background to many different signals, such as extragalactic sources or annihilating dark matter. It is timely to reinvestigate how it is calculated and to assess the various uncertainties that are likely to affect the accuracy of the predictions. Aims. The Galactic γ-ray diffuse emission is mostly produced above a few GeV by the interactions of cosmic ray primaries impinging on the interstellar material. The theoretical error on that component is derived by exploring various potential sources of uncertainty. Particular attention is paid to cosmic ray propagation. Nuclear cross sections, the proton and helium fluxes at the Earth's position, the Galactic radial profile of supernova remnants, and the hydrogen distribution can also severely affect the signal. Methods. The propagation of cosmic ray species throughout the Galaxy is described in the framework of a semi-analytic two-zone diffusion/convection model. The γ-ray flux is reliably and quickly determined. This allows conversion of the constraints set by the boron-to-carbon data into a theoretical uncertainty on the diffuse emission. New deconvolutions of the HI and CO sky maps are also used to get the hydrogen distribution within the Galaxy. Results. The thickness of the cosmic ray diffusive halo is found to have a significant effect on the Galactic γ-ray diffuse emission, while the interplay between diffusion and convection has little influence on the signal. The uncertainties related to nuclear cross sections and to the primary cosmic ray fluxes at the Earth are significant. The radial distribution of supernova remnants along the Galactic plane turns out to be a key ingredient. As expected, the predictions are extremely sensitive to the spatial distribution of hydrogen within the Milky Way. Conclusions. Most of the sources of uncertainty are likely to be reduced in the near future. The stress should be put (i) on better determination of the thickness of the cosmic ray diffusive halo; and (ii) on refined observations of the radial profile of supernova remnants.

Sensitivity projections for dark matter searches with the Fermi large area telescope

“…This is compatible with, and in some cases somewhat better than, estimates of the uncertainties of the modeling procedures (that are closer to 20 to 30% for the local emissions alone, see Ref. [63]). However, as mentioned above, large-scale residuals associated with specific structures and source populations do exist, and in some parts of the sky and for some energy ranges the observed Galactic diffuse emission can exceed the modeling predictions by 100% or more.…”

Dusty star-forming galaxies at high redshift

“…Within the Milky Way and Local Group (aside from the Small Magallenic Cloud [SMC]), the conversion factor appears to display a remarkably narrow range of X CO ≈ 2 − 4 × 10 20 cm −2 /K km s −1 (or α CO ≈ 3 − 6 M pc −2 (K km s −1 ) −1 Bloemen et al, 1986;Solomon et al, 1987;Blitz et al, 2007;Delahaye et al, 2011;Leroy et al, 2011;Donovan Meyer et al, 2012b,a). The independent H 2 mass measurements in these observations come from virial mass measurements, dust to gas ratio assumptions (or measurements), and γ-ray observations.…”

LOCAL H i EMISSIVITY MEASURED WITHFERMI-LAT AND IMPLICATIONS FOR COSMIC-RAY SPECTRA

“…The EGRET apparent excess not confirmed by Fermi (Abdo et al 2009a) was of likely instrumental origin (Stecker et al 2008). Delahaye et al (2011) compared those emissivities with predictions from various proton and Helium local interstellar spectra (LIS) and a γ-ray production cross-section of Huang et al (2007). They found good agreement with the LAT measurements but neglected the contribution from electrons.…”