We have performed an analysis of the diffuse gamma-ray emission with the Fermi Large Area Telescope (LAT) in the Milky Way halo region, searching for a signal from dark matter annihilation or decay. In the absence of a robust dark matter signal, constraints are presented. We consider both gamma rays produced directly in the dark matter annihilation/decay and produced by inverse Compton scattering of the e+/e- produced in the annihilation/decay. Conservative limits are derived requiring that the dark matter signal does not exceed the observed diffuse gamma-ray emission. A second set of more stringent limits is derived based on modeling the foreground astrophysical diffuse emission using the GALPROP code. Uncertainties in the height of the diffusive cosmic-ray halo, the distribution of the cosmic-ray sources in the Galaxy, the index of the injection cosmic-ray electron spectrum, and the column density of the interstellar gas are taken into account using a profile likelihood formalism, while the parameters governing the cosmic-ray propagation have been derived from fits to local cosmic-ray data. The resulting limits impact the range of particle masses over which dark matter thermal production in the early universe is possible, and challenge the interpretation of the PAMELA/Fermi-LAT cosmic ray anomalies as the annihilation of dark matter. © 2012. The American Astronomical Society. All rights reserved.

Constraints on the galactic halo dark matter from fermi-lat diffuse measurements

Cuoco A.;De Angelis A.;Giglietto N.;
2012

Abstract

We have performed an analysis of the diffuse gamma-ray emission with the Fermi Large Area Telescope (LAT) in the Milky Way halo region, searching for a signal from dark matter annihilation or decay. In the absence of a robust dark matter signal, constraints are presented. We consider both gamma rays produced directly in the dark matter annihilation/decay and produced by inverse Compton scattering of the e+/e- produced in the annihilation/decay. Conservative limits are derived requiring that the dark matter signal does not exceed the observed diffuse gamma-ray emission. A second set of more stringent limits is derived based on modeling the foreground astrophysical diffuse emission using the GALPROP code. Uncertainties in the height of the diffusive cosmic-ray halo, the distribution of the cosmic-ray sources in the Galaxy, the index of the injection cosmic-ray electron spectrum, and the column density of the interstellar gas are taken into account using a profile likelihood formalism, while the parameters governing the cosmic-ray propagation have been derived from fits to local cosmic-ray data. The resulting limits impact the range of particle masses over which dark matter thermal production in the early universe is possible, and challenge the interpretation of the PAMELA/Fermi-LAT cosmic ray anomalies as the annihilation of dark matter. © 2012. The American Astronomical Society. All rights reserved.
THE ASTROPHYSICAL JOURNAL
761
2
91
104
https://arxiv.org/abs/1205.6474
Dark matter; Galaxy: Halo; Gamma rays: Diffuse background; Methods: Statistical
Ackermann M.; Ajello M.; Atwood W.B.; Baldini L.; Barbiellini G.; Bastieri D.; Bechtol K.; Bellazzini R.; Blandford R.D.; Bloom E.D.; Bonamente E.; Borgland A.W.; Bottacini E.; Brandt T.J.; Bregeon J.; Brigida M.; Bruel P.; Buehler R.; Buson S.; Caliandro G.A.; Cameron R.A.; Caraveo P.A.; Casandjian J.M.; Cecchi C.; Charles E.; Chekhtman A.; Chiang J.; Ciprini S.; Claus R.; Cohen-Tanugi J.; Conrad J.; Cuoco A.; Cutini S.; D'Ammando F.; De Angelis A.; De Palma F.; Dermer C.D.; Do Couto E Silva E.; Drell P.S.; Drlica-Wagner A.; Falletti L.; Favuzzi C.; Fegan S.J.; Focke W.B.; Fukazawa Y.; Funk S.; Fusco P.; Gargano F.; Gasparrini D.; Germani S.; Giglietto N.; Giordano F.; Giroletti M.; Glanzman T.; Godfrey G.; Grenier I.A.; Guiriec S.; Gustafsson M.; Hadasch D.; Hayashida M.; Horan D.; Hughes R.E.; Jackson M.S.; Jogler T.; Johannesson G.; Johnson A.S.; Kamae T.; Knodlseder J.; Kuss M.; Lande J.; Latronico L.; Lionetto A.M.; Llena Garde M.; Longo F.; Loparco F.; Lott B.; Lovellette M.N.; Lubrano P.; Mazziotta M.N.; Mcenery J.E.; Mehault J.; Michelson P.F.; Mitthumsiri W.; Mizuno T.; Moiseev A.A.; Monte C.; Monzani M.E.; Morselli A.; Moskalenko I.V.; Murgia S.; Naumann-Godo M.; Norris J.P.; Nuss E.; Ohsugi T.; Orienti M.; Orlando E.; Ormes J.F.; Paneque D.; Panetta J.H.; Pesce-Rollins M.; Pierbattista M.; Piron F.; Pivato G.; Poon H.; Raino S.; Rando R.; Razzano M.; Razzaque S.; Reimer A.; Reimer O.; Romoli C.; Sbarra C.; Scargle J.D.; Sgro C.; Siskind E.J.; Spandre G.; Spinelli P.; Stawarz L.; Strong A.W.; Suson D.J.; Tajima H.; Takahashi H.; Tanaka T.; Thayer J.G.; Thayer J.B.; Tibaldo L.; Tinivella M.; Tosti G.; Troja E.; Usher T.L.; Vandenbroucke J.; Vasileiou V.; Vianello G.; Vitale V.; Waite A.P.; Wallace E.; Wood K.S.; Wood M.; Yang Z.; Zaharijas G.; Zimmer S.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/2318/1830672
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