SEARCHING FOR DARK MATTER ANNIHILATION IN RECENTLY DISCOVERED MILKY WAY SATELLITES WITH FERMI-LAT

被引:433
作者
Albert, A. [1 ]
Anderson, B. [2 ,3 ]
Bechtol, K. [4 ,5 ]
Drlica-Wagner, A. [6 ]
Meyer, M. [2 ,3 ]
Sanchez-Conde, M. [2 ,3 ]
Strigari, L. [7 ,8 ]
Wood, M. [1 ]
Abbott, T. M. C. [9 ]
Abdalla, F. B. [10 ,11 ]
Benoit-Levy, A. [10 ,12 ,13 ]
Bernstein, G. M. [14 ]
Bernstein, R. A. [15 ]
Bertin, E. [12 ,13 ]
Brooks, D. [10 ]
Burke, D. L. [16 ,17 ]
Rosell, A. Carnero [18 ,19 ]
Kind, M. Carrasco [20 ,21 ]
Carretero, J. [22 ,23 ]
Crocce, M. [22 ]
Cunha, C. E. [16 ]
D'Andrea, C. B. [24 ,25 ]
da Costa, L. N. [19 ]
Desai, S. [26 ,27 ]
Diehl, H. T. [6 ]
Dietrich, J. P. [26 ,27 ]
Doel, P. [10 ]
Eifler, T. F. [14 ,28 ]
Evrard, A. E. [29 ,30 ]
Fausti Neto, A. [18 ]
Finley, D. A. [6 ]
Flaugher, B. [6 ]
Fosalba, P. [22 ]
Frieman, J. [6 ,31 ]
Gerdes, D. W.
Goldstein, D. A. [32 ,33 ]
Gruen, D. [16 ,17 ]
Gruendl, R. A. [20 ,21 ]
Honscheid, K. [34 ,35 ]
James, D. J. [9 ]
Kent, S. [6 ]
Kuehn, K. [36 ]
Kuropatkin, N. [6 ]
Lahav, O. [10 ]
Li, T. S. [7 ,8 ]
Maia, M. A. G. [18 ,19 ]
March, M.
Marshall, J. L. [7 ,8 ]
Martini, P. [34 ,37 ]
Miller, C. J. [29 ,30 ]
机构
[1] Los Alamos Natl Lab, Los Alamos, NM 87545 USA
[2] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden
[3] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden
[4] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA
[5] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA
[6] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA
[7] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA
[8] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA
[9] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, Casilla 603, La Serena, Chile
[10] UCL, Dept Phys & Astron, London WC1E 6BT, England
[11] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa
[12] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France
[13] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France
[14] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA
[15] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA
[16] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA
[17] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA
[18] Lab Interinst eAstron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil
[19] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil
[20] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA
[21] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA
[22] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain
[23] Barcelona Inst Sci & Technol, Inst Fisica Altes Energies, Campus UAB, E-08193 Barcelona, Spain
[24] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England
[25] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England
[26] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany
[27] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany
[28] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA
[29] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA
[30] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA
[31] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
[32] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA
[33] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA
[34] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA
[35] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA
[36] Australian Astron Observ, N Ryde, NSW 2113, Australia
[37] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA
[38] Inst Catalana Rec & Estud Avancats, E-08010 Barcelona, Spain
[39] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England
[40] CIEMAT, Madrid, Spain
[41] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil
[42] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA
[43] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA
基金
美国国家科学基金会; 英国科学技术设施理事会;
关键词
dark matter; galaxies: dwarf; gamma rays: galaxies; LARGE-AREA TELESCOPE; DWARF SPHEROIDAL GALAXIES; GAMMA-RAY EMISSION; ALL-SKY SURVEY; GLOBULAR-CLUSTER; TRIANGULUM II; RETICULUM; HYDRA II; FAINT; KINEMATICS;
D O I
10.3847/1538-4357/834/2/110
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We search for excess gamma-ray emission coincident with the positions of confirmed and candidate Milky Way satellite galaxies using six years of data from the Fermi Large Area Telescope (LAT). Our sample of 45 stellar systems includes 28 kinematically confirmed dark-matter-dominated dwarf spheroidal galaxies (dSphs) and 17 recently discovered systems that have photometric characteristics consistent with the population of known dSphs. For each of these targets, the relative predicted gamma-ray flux due to dark matter annihilation is taken from kinematic analysis if available, and estimated from a distance-based scaling relation otherwise, assuming that the stellar systems are DM-dominated dSphs. LAT data coincident with four of the newly discovered targets show a slight preference (each similar to 2 sigma local) for gamma-ray emission in excess of the background. However, the ensemble of derived gamma-ray flux upper limits for individual targets is consistent with the expectation from analyzing random blank-sky regions, and a combined analysis of the population of stellar systems yields no globally significant excess (global significance < 1 sigma). Our analysis has increased sensitivity compared to the analysis of 15 confirmed dSphs by Ackermann et al. The observed constraints on the DM annihilation cross section are statistically consistent with the background expectation, improving by a factor of similar to 2 for large DM masses (m(DM, b<(b)over bar>) greater than or similar to 1 TeV and m(DM, tau+tau-) greater than or similar to 70 GeV) and weakening by a factor of similar to 1.5 at lower masses relative to previously observed limits.
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