2014ApJ...787...18A

Query : 2014ApJ...787...18A

2014ApJ...787...18A - Astrophys. J., 787, 18 (2014/May-3)

Search for cosmic-ray-induced gamma-ray emission in galaxy clusters.

ACKERMANN M., AJELLO M., ALBERT A., ALLAFORT A., ATWOOD W.B., BALDINI L., BALLET J., BARBIELLINI G., BASTIERI D., BECHTOL K., BELLAZZINI R., BLOOM E.D., BONAMENTE E., BOTTACINI E., BRANDT T.J., BREGEON J., BRIGIDA M., BRUEL P., BUEHLER R., BUSON S., CALIANDRO G.A., CAMERON R.A., CARAVEO P.A., CAVAZZUTI E., CHAVES R.C.G., CHIANG J., CHIARO G., CIPRINI S., CLAUS R., COHEN-TANUGI J., CONRAD J., D'AMMANDO F., DE ANGELIS A., DE PALMA F., DERMER C.D., DIGEL S.W., DRELL P.S., DRLICA-WAGNER A., FAVUZZI C., FRANCKOWIAK A., FUNK S., FUSCO P., GARGANO F., GASPARRINI D., GERMANI S., GIGLIETTO N., GIORDANO F., GIROLETTI M., GODFREY G., GOMEZ-VARGAS G.A., GRENIER I.A., GUIRIEC S., GUSTAFSSON M., HADASCH D., HAYASHIDA M., HEWITT J., HUGHES R.E., JELTEMA T.E., JOHANNESSON G., JOHNSON A.S., KAMAE T., KATAOKA J., KNODLSEDER J., KUSS M., LANDE J., LARSSON S., LATRONICO L., GARDE M.L., LONGO F., LOPARCO F., LOVELLETTE M.N., LUBRANO P., MAYER M., MAZZIOTTA M.N., McENERY J.E., MICHELSON P.F., MITTHUMSIRI W., MIZUNO T., MONZANI M.E., MORSELLI A., MOSKALENKO I.V., MURGIA S., NEMMEN R., NUSS E., OHSUGI T., ORIENTI M., ORLANDO E., ORMES J.F., PERKINS J.S., PESCE-ROLLINS M., PIRON F., PIVATO G., RAINO S., RANDO R., RAZZANO M., RAZZAQUE S., REIMER A., REIMER O., RUAN J., SANCHEZ-CONDE M., SCHULZ A., SGRO C., SISKIND E.J., SPANDRE G., SPINELLI P., STORM E., STRONG A.W., SUSON D.J., TAKAHASHI H., THAYER J.G., THAYER J.B., THOMPSON D.J., TIBALDO L., TINIVELLA M., TORRES D.F., TROJA E., UCHIYAMA Y., USHER T.L., VANDENBROUCKE J., VIANELLO G., VITALE V., WINER B.L., WOOD K.S., ZIMMER S. (The Fermi-LAT Collaboration), PINZKE A. and PFROMMER C.

Abstract (from CDS):

Current theories predict relativistic hadronic particle populations in clusters of galaxies in addition to the already observed relativistic leptons. In these scenarios hadronic interactions give rise to neutral pions which decay into γ rays that are potentially observable with the Large Area Telescope (LAT) on board the Fermi space telescope. We present a joint likelihood analysis searching for spatially extended γ-ray emission at the locations of 50 galaxy clusters in four years of Fermi-LAT data under the assumption of the universal cosmic-ray (CR) model proposed by Pinzke & Pfrommer. We find an excess at a significance of 2.7σ, which upon closer inspection, however, is correlated to individual excess emission toward three galaxy clusters: A400, A1367, and A3112. We discuss these cases in detail and conservatively attribute the emission to unmodeled background systems (for example, radio galaxies within the clusters).Through the combined analysis of 50 clusters, we exclude hadronic injection efficiencies in simple hadronic models above 21% and establish limits on the CR to thermal pressure ratio within the virial radius, R200, to be below 1.25%-1.4% depending on the morphological classification. In addition, we derive new limits on the γ-ray flux from individual clusters in our sample.

Abstract Copyright: ∼

Journal keyword(s): galaxies: clusters: intracluster medium - gamma rays: galaxies: clusters

Simbad objects: 70

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Number of rows : 70
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 ACO 2734 ClG 00 11 21.60 -28 51 16.6           ~ 156 0
2 ACO 85 ClG 00 41 36.21 -09 19 30.4           ~ 974 0
3 ACO 119 ClG 00 56 08.57 -01 12 00.8           ~ 577 2
4 ACO 133 ClG 01 02 41.5 -21 52 53           ~ 391 1
5 ACO 2877 ClG 01 09 49.3 -45 54 02           ~ 160 2
6 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 727 1
7 ACO 400 ClG 02 57 37.4 +06 00 45           ~ 408 3
8 3C 75 PaG 02 57 41.64 +06 01 28.0           ~ 312 1
9 NVSS J025857+055240 BLL 02 58 57.5559833309 +05 52 43.949781063           ~ 29 0
10 IC 310 AGN 03 16 42.9787569912 +41 19 29.615579544   14.3       ~ 311 2
11 ACO 3112 ClG 03 17 52.9 -44 15 06           ~ 329 1
12 ESO 248-6 QSO 03 17 57.67946154 -44 14 17.1632318   14.85   13.16   ~ 85 3
13 ACO 426 ClG 03 19 47.6 +41 30 54           ~ 2508 1
14 NGC 1275 Bla 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 4243 3
15 ACO S 373 ClG 03 38 29.4 -35 27 08           ~ 2029 0
16 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 402 1
17 2MASX J03411752+1523477 BiC 03 41 17.5329189192 +15 23 47.567775336   17.5       ~ 46 1
18 ACO 3158 ClG 03 43 07.5 -53 38 09           ~ 327 0
19 ACO S 405 ClG 03 51 32.8 -82 13 15           ~ 50 0
20 ACO 478 ClG 04 13 24.8 +10 27 52           ~ 522 0
21 NGC 1550 BiC 04 19 37.9450450152 +02 24 35.918168940   14.0       ~ 183 1
22 ClG 0422-09 ClG 04 25 51.02 -08 33 38.5           ~ 97 0
23 ACO 3266 ClG 04 31 26.4 -61 25 17           ~ 447 0
24 ACO 496 ClG 04 33 40.8 -13 14 34           ~ 728 2
25 ACO S 540 ClG 05 40 06.2 -40 50 29           ~ 60 0
26 ACO 548 ClG 05 47 01.7 -25 36 59           B8 209 2
27 ACO 3376 ClG 06 01 25.000 -39 59 51.00           ~ 334 0
28 ACO 3392 ClG 06 27 05.6 -35 29 30           ~ 36 2
29 QSO B0625-354 BLL 06 27 06.7286533392 -35 29 15.363665088   14.93       ~ 206 1
30 ACO 576 ClG 07 21 24.1 +55 44 20           ~ 312 1
31 Z 262-19 BiC 07 40 58.2309667896 +55 25 37.870473828   14.2       ~ 52 1
32 NAME HYA SUPERCL SCG 08 57.9 +03 10           ~ 204 0
33 ACO 754 ClG 09 09 14.8 -09 40 35           ~ 695 1
34 MCG-02-24-007 LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 1077 1
35 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 905 1
36 NAME Leo Cluster ClG 11 30.0 +15 00           ~ 71 0
37 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1127 1
38 NGC 3862 Sy2 11 45 05.00904503 +19 36 22.7409909   14.98 13.97     ~ 646 1
39 M 49 Sy2 12 29 46.8 +08 00 01   13.21 12.17     ~ 2174 2
40 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
41 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
42 ACO 3526 ClG 12 48 49.2 -41 18 17           ~ 1154 2
43 ACO 1644 ClG 12 57 11.6 -17 24 34           ~ 391 1
44 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 5141 2
45 NGC 5044 BiC 13 15 23.9607836592 -16 23 07.547751744   11.9   10.74   ~ 531 0
46 ACO 1795 ClG 13 48 47.4 +26 34 55           ~ 1330 0
47 ACO 2029 ClG 15 10 54.2 +05 44 23           ~ 1020 0
48 ACO 2065 ClG 15 22 22.7 +27 44 20           ~ 398 0
49 ACO 2142 ClG 15 58 26.5 +27 13 52           ~ 825 0
50 ACO 2199 ClG 16 28 34.5 +39 32 26           ~ 1206 1
51 ACO 2244 ClG 17 02 40.33 +34 02 58.7           ~ 301 0
52 ACO 2256 ClG 17 03 37.5 +78 37 23           ~ 928 1
53 ACO 2255 ClG 17 12 56.0 +64 04 06           ~ 605 0
54 ZwCl 1742+3306 ClG 17 44 16.2753 +32 59 55.115           ~ 93 0
55 NAME Fermi Bubbles bub 17 45 -29.0           ~ 525 0
56 MCXC J1958.2-3011 ClG 19 58 14.9 -30 11 13           ~ 14 0
57 1RXS J195815.6-301119 BLL 19 58 14.9123511384 -30 11 11.646174444   17.88   16.16   ~ 61 1
58 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 676 1
59 Z 375-15 BiC 21 13 55.918 +02 33 55.39   15.1       ~ 67 1
60 ACO 3822 ClG 21 54 06.2 -57 50 49           ~ 98 0
61 ACO 3827 ClG 22 01 49.1 -59 57 15           ~ 178 0
62 ACO 3921 ClG 22 49 59.0 -64 25 48           ~ 165 1
63 BAX 349.3187+18.7197 ClG 23 17 11.184 +18 41 48.87           ~ 97 0
64 ACO 2589 ClG 23 24 00.5 +16 49 29           ~ 327 1
65 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 572 0
66 ACO 2634 ClG 23 38 18.4 +27 01 37           ~ 515 2
67 ACT-CL J2344.3-0422 ClG 23 44 15.98 -04 22 24.5           ~ 53 0
68 ACO 2657 ClG 23 44 51.0 +09 08 40           ~ 280 3
69 ACO 4038 ClG 23 47 31.1 -28 12 10           ~ 349 3
70 ACO 4059 ClG 23 57 02.2 -34 45 58           ~ 400 1

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