EGRET Observations of the Diffuse Gamma‐Ray Emission from the Galactic Plane

Hunter, S. D.; Bertsch, D. L.; Catelli, J. R.; Dame, T. M.; Digel, S. W.; Dingus, B. L.; Esposito, J. A.; Fichtel, C. E.; Hartman, R. C.; Kanbach, G.; Kniffen, D. A.; Lin, Y. C.; Mayer‐Hasselwander, H. A.; Michelson, P. F.; Montigny, C. von; Mukherjee, R.; Nolan, P. L.; Schneid, E. J.; Sreekumar, P.; Thaddeus, P.; Thompson, D. J.

doi:10.1086/304012

Cited by 696 publications

(627 citation statements)

References 63 publications

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“…9 We note, however, that this calculation is approximate as the modeling of the various components that make the diffuse mid-latitude gamma-ray spectrum is still very much an active area of research. In constructing our custom astrophysical models we started with a model (galdef 50p 599278) that was designed to fit the EGRET measurement [87] of the diffuse mid-latitude gammas (see e.g., [88]), which is now known to be in tension with the more recent FERMI-LAT measurements [9,10]. In addition, the work [89] has also presented a more accurate parameterization of the gamma spectra arising from the decays of spallatively-produced π 0 's, which is not yet incorporated into the latest public version of GALPROP.…”

Section: Jhep01(2011)064mentioning

confidence: 99%

“…Also shown is the spectrum for the benchmark model (red curve). We display for comparison the EGRET [87] and FERMI [9] data, as well as preliminary FERMI data presented in [10]. Figure 10: The propagated DM positron flux (scaled by E 2 ) from a representative pMSSM model for each of our 524 astrophysical models (grey curves).…”

Section: Jhep01(2011)064mentioning

confidence: 99%

“…The DM signal is calculated using the DarkSUSY default NFW halo profile. Data shown are published data from EGRET [87] and FERMI [9], as well as the preliminary FERMI data presented in [10].…”

Section: Jhep01(2011)064mentioning

confidence: 99%

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Cosmic ray anomalies from the MSSM?

Cotta

Conley

Gainer

et al. 2011

J. High Energ. Phys.

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Abstract:The recent positron excess in cosmic rays (CR) observed by the PAMELA satellite may be a signal for dark matter (DM) annihilation. When these measurements are combined with those from FERMI on the total (e + + e − ) flux and from PAMELA itself on thep/p ratio, these and other results are difficult to reconcile with traditional models of DM, including the conventional mSUGRA version of Supersymmetry even if boosts as large as 10 3−4 are allowed. In this paper, we combine the results of a previously obtained scan over a more general 19-parameter subspace of the MSSM with a corresponding scan over astrophysical parameters that describe the propagation of CR. We then ascertain whether or not a good fit to this CR data can be obtained with relatively small boost factors while simultaneously satisfying the additional constraints arising from gamma ray data. We find that a specific subclass of MSSM models where the LSP is mostly pure bino and annihilates almost exclusively into τ pairs comes very close to satisfying these requirements. The lightestτ in this set of models is found to be relatively close in mass to the LSP and is in some cases the nLSP. These models lead to a significant improvement in the overall fit to the data by an amount ∆χ 2 ∼ 1/dof in comparison to the best fit without Supersymmetry while employing boosts ∼ 100. The implications of these models for future experiments are discussed.

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Section: Jhep01(2011)064mentioning

confidence: 99%

Section: Jhep01(2011)064mentioning

confidence: 99%

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Cosmic ray anomalies from the MSSM?

Cotta

Conley

Gainer

et al. 2011

J. High Energ. Phys.

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“…10. Note that X CO is lower than the Galactic value of 1.6 × 10 20 cm −2 (K km s −1 ) −1 (Hunter et al 1997) at all positions and for all methods. We find that X CO varies across the disk of M 82 by about a factor of 5 if one considers the LTE solutions (X CO = 2.1 − 10.8 × 10 19 cm −2 (K km s −1 ) −1 ) and by a factor of 8-9 for the LVG and LVG P F solutions (X CO = 1.3 − 11.5 × 10 19 cm −2 (K km s −1 ) −1 and X CO = 1.5 − 12.2 × 10 19 cm −2 (K km s −1 ) −1 ) .…”

Section: Conversion From I(co) To N (H 2 ) and Total Massmentioning

confidence: 79%

The Effect of Violent Star Formation on the State of the Molecular Gas in M 82

Weiß

Neininger

Hüttemeister

et al. 2001

The Evolution of Galaxies

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Abstract. We present the results of a high angular resolution, multi-transition analysis of the molecular gas in M 82. The analysis is based on the two lowest transitions of 12 CO and the ground transition of the rare isotopes 13 CO and C 18 O measured with the PdBI, the BIMA array and the IRAM 30m telescope. In order to address the question of how the intrinsic molecular cloud properties are influenced by massive star formation we have carried out radiative transfer calculations based on the observed CO line ratios. The calculations suggest that the kinetic temperature of the molecular gas is high in regions with strong star formation and drops towards the outer molecular lobes with less ongoing star formation. The location of the highest kinetic temperature is coincident with that of the mid infrared (MIR) peaks which trace emission from hot dust. The hot gas is associated with low H 2 densities while the cold gas in the outer molecular lobes has high H 2 densities. We find that CO intensities do not trace H 2 column densities well. Most of the molecular gas is distributed in a double-lobed distribution which surrounds the starburst. A detailed analysis of the conversion factor from CO intensity to H 2 column density shows that X CO depends on the excitation conditions. We find X CO ∼ T −1 kin n(H 2 ) 1/2 , as expected for virialized clouds.

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“…This minimum level of diffuse emission should be completed with the addition of the expected γ-rays from the ICS contribution off the Galactic radiation field. The γ-ray diffuse emission is well studied at GeV energies (Hunter et al 1997;Ackermann et al 2012). With the large dataset accumulated with observation by the H.E.S.S.…”

Section: Implication For Diffuse Emissionmentioning

confidence: 99%

On the possible correlation of Galactic very-high energy source locations and enhancements of the surface density in the Galactic plane

Pedaletti

Wilhelmi

Torres

2014

A&A

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Aims. The association of very-high energy sources with regions of the sky rich in dust and gas has been noticed in the study of individual very-high energy (VHE; E > ∼ 100 GeV) sources. However, the statistical significance of this correlation for the whole population of TeV detections has not been assessed yet. Here, we present a study of the association of VHE sources in the central Galactic region with positions of enhanced material content. Methods. We obtain estimates of the material content through two classical tracers: dust emission and intensity of the 12 CO(1 → 0) line. We make use of the recently released all-sky maps of astrophysical foregrounds of the Planck Collaboration, and of an extensive existing CO mapping of the Galactic sky. To test the correlation, we construct randomized samples of VHE source positions starting from the inner Galactic plane survey sources detected by the High Energy Stereoscopic System (H.E.S.S.) array. Results. We find hints of a positive correlation between positions of VHE sources and regions rich in molecular material, which reaches the 3.9σ level in the best of cases. The latter confidence is however decreased if variations in the selection criteria are considered, which lead us to conclude that a positive correlation cannot be firmly established yet. Forthcoming VHE facilities will be needed to firmly establish the correlation.

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EGRET Observations of the Diffuse Gamma‐Ray Emission from the Galactic Plane

Cited by 696 publications

References 63 publications

Cosmic ray anomalies from the MSSM?

Cosmic ray anomalies from the MSSM?

The Effect of Violent Star Formation on the State of the Molecular Gas in M 82

On the possible correlation of Galactic very-high energy source locations and enhancements of the surface density in the Galactic plane

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