THE<i>FERMI</i>-LAT HIGH-LATITUDE SURVEY: SOURCE COUNT DISTRIBUTIONS AND THE ORIGIN OF THE EXTRAGALACTIC DIFFUSE BACKGROUND

Abdo, A. A.; Ackermann, M.; Ajello, M.; Antolini, E.; Baldini, Luca; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, Pascal; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; Angelis, A. De; Palma, F. de; Silva, E. Do Couto E; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Knödlseder, J.; Kuss, M.; Landé, J.; Latronico, L.; Lee, S.-H.; Lemoine‐Goumard, M.; Garde, M. Llena; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, Masanori; Paneque, D.; Panetta, J.; Parent, D.; Pelassa, V.; Pepé, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Ritz, S.; Rochester, Lynn; Rodriguez, A. Y.; Romani, Roger W.; Roth, M.; Sadrozinski, H. F-W.; Sander, A.; Parkinson, P. M. Saz; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, Jean-Luc; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, Takaaki; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.

doi:10.1088/0004-637x/720/1/435

Cited by 193 publications

(319 citation statements)

References 45 publications

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“…Since the contribution from star forming galaxies is quite uncertain and since the fiducial model we use lies closer to the upper value of this contribution, we explore below the effects that a lower contribution has in our results (see section IV C). If the observed count distribution of blazars is extrapolated to zero flux then their contribution to the total observed signal between 0.1 GeV and 100 GeV is ∼ 23(±9)% (including statistical and systematic uncertainties) [34]. As we mentioned before, this percentage drops to ∼ 16(±9)% when only sources down to the minimum flux are considered.…”

Section: A Observationsmentioning

confidence: 73%

“…They all give approximately the correct relic density. Observations from soft X-rays to gamma-rays are marked with red to violet, following approximately a rainbow color pattern: red symbols [46], red arrows (Chandra, [33]), orange symbols (INTEGRAL, [47]), yellow symbols (SWIFT BAT, [32]), yellow arrows [48], green area (SMM, [49]), light blue (COMPTEL, [50]), blue (EGRET, [51]), violet (Fermi-LAT, [52]), violet arrows [34,35]. The points with error bars are absolute measurements with 2σ or 1σ errors.…”

Section: Extragalactic Cdmabmentioning

confidence: 99%

“…Its total specific intensity in this energy range (i.e. its integrated flux between these energies) down to the minimum detected source flux is ∼ 16% of the derived value for the cosmic gamma-ray background [34]. We use the energy spectrum given by these authors (see their Table 6 and Fig.…”

Section: A Observationsmentioning

confidence: 99%

“…5 we have assumed a minimal contribution from unresolved substructures. Blazars are assumed to contribute by a fixed amount (16%) in the energy range measured by Fermi [34].…”

Section: Benchmark Models Fitting the Cosmic Ray Excessesmentioning

confidence: 99%

“…This has been partially confirmed by accounting for the radiation of known sources and by estimating the contribution of an expected population of sources yet to be observed. This combined set of observations and expectations puts strong constraints on the contribution of dark matter annihilation, being specially stringent in the soft-X-ray regime where ∼ 90% of the emission comes from Xray point sources, mostly Active Galactic Nuclei (AGN) [33], and on the gamma-ray regime where blazars and star-forming galaxies are expected to contribute significantly to the background radiation, at the level of ∼ 70% [34,35].…”

Section: Introductionmentioning

confidence: 99%

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Cosmic X-ray and gamma-ray background from dark matter annihilation

et al. 2011

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The extragalactic background light (EBL) observed at multiple wavelengths is a promising tool to probe the nature of dark matter. This radiation might contain a significant contribution from gamma-rays produced promptly by dark matter particle annihilation in the many halos and subhalos within our past-light cone. Additionally, the electrons and positrons produced in the annihilation give energy to the cosmic microwave photons to populate the EBL with X-rays and gamma-rays.To study these signals, we create full-sky maps of the expected radiation from both of these contributions using the high-resolution Millennium-II simulation of cosmic structure formation. Our method also accounts for a possible enhancement of the annihilation rate by a Sommerfeld mechanism due to a Yukawa interaction between the dark matter particles prior to annihilation. We use upper limits on the contributions of unknown sources to the EBL to constrain the intrinsic properties of dark matter using a model-independent approach that can be employed as a template to test different particle physics models. These upper limits are based on observational measurements spanning eight orders of magnitude in energy (from soft X-rays measured by the CHANDRA satellite to gamma-rays measured by the Fermi satellite), and on expectations for the contributions from non-blazar active galactic nuclei, blazars and star forming galaxies. To exemplify this approach, we analyze a set of benchmark Sommerfeld-enhanced models that give the correct abundance of dark matter, satisfy constraints from the cosmic microwave background, and fit the cosmic ray spectra measured by PAMELA and Fermi without any contribution from local substructure. We find that these models are in conflict with the EBL constraints unless the contribution of unresolved substructure is small and the dark matter annihilation signal dominates the EBL. We conclude that provided the collisionless cold dark matter paradigm is accurate, even for conservative estimates of the contribution from unresolved substructure and astrophysical backgrounds, the EBL is at least as sensitive a probe of these types of scenarios as the cosmic microwave background. More generally, our results disfavor an explanation of the positron excess measured by the PAMELA satellite based only on dark matter annihilation in the smooth Galactic dark matter halo.PACS numbers: 95.35.+d,95.85.Nv,95.85.Pw

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Section: A Observationsmentioning

confidence: 73%

Section: Extragalactic Cdmabmentioning

confidence: 99%

Section: A Observationsmentioning

confidence: 99%

“…5 we have assumed a minimal contribution from unresolved substructures. Blazars are assumed to contribute by a fixed amount (16%) in the energy range measured by Fermi [34].…”

Section: Benchmark Models Fitting the Cosmic Ray Excessesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Cosmic X-ray and gamma-ray background from dark matter annihilation

et al. 2011

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GeV Gamma-Ray Emission from Normal and Starburst Galaxies

Knödlseder

2013

Cosmic Rays in Star-Forming Environments

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With the launch of the Fermi satellite and the advent of modern air-Cherenkov telescopes such as H.E.S.S. and VERITAS, star-forming galaxies have become a new class of gamma-ray sources that extend the study of cosmic-ray physics from the Milky Way to external galaxies. So far, 8 star-forming galaxies have been observed at GeV energies (SMC, LMC, Milky Way, M 31, M 82, NGC 253, NGC 1068, and NGC 4945) while 2 have been seen at TeV energies (M 82, NGC 253). In this paper, I review the observational status of the GeV observation of these galaxies, and I summarize the conclusions that have been drawn from these observations on cosmic-ray physics in normal and starburst galaxies.

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Consequences of Supernovae

Branch

Wheeler

2017

Astronomy and Astrophysics Library

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THEFERMI-LAT HIGH-LATITUDE SURVEY: SOURCE COUNT DISTRIBUTIONS AND THE ORIGIN OF THE EXTRAGALACTIC DIFFUSE BACKGROUND

Cited by 193 publications

References 45 publications

Cosmic X-ray and gamma-ray background from dark matter annihilation

Cosmic X-ray and gamma-ray background from dark matter annihilation

GeV Gamma-Ray Emission from Normal and Starburst Galaxies

Consequences of Supernovae

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