2010ApJ...723.1082A

Query : 2010ApJ...723.1082A

2010ApJ...723.1082A - Astrophys. J., 723, 1082-1096 (2010/November-2)

Fermi large area telescope constraints on the gamma-ray opacity of the universe.

ABDO A.A., ACKERMANN M., AJELLO M., ALLAFORT A., ATWOOD W.B., BALDINI L., BALLET J., BARBIELLINI G., BARING M.G., BASTIERI D., BAUGHMAN B.M., BECHTOL K., BELLAZZINI R., BERENJI B., BHAT P.N., BLANDFORD R.D., BLOOM E.D., BONAMENTE E., BORGLAND A.W., BOUVIER A., BRANDT T.J., BREGEON J., BREZ A., BRIGGS M.S., BRIGIDA M., BRUEL P., BUEHLER R., BURNETT T.H., BUSON S., CALIANDRO G.A., CAMERON R.A., CARAVEO P.A., CARRIGAN S., CASANDJIAN J.M., CAVAZZUTI E., CECCHI C., CELIK O., CHARLES E., CHEKHTMAN A., CHEN A.W., CHEUNG C.C., CHIANG J., CIPRINI S., CLAUS R., COHEN-TANUGI J., CONNAUGHTON V., CONRAD J., COSTAMANTE L., DERMER C.D., DE ANGELIS A., DE PALMA F., DIGEL S.W., DINGUS B.L., DO COUTO E SILVA E., DRELL P.S., DUBOIS R., FAVUZZI C., FEGAN S.J., FINKE J., FORTIN P., FUKAZAWA Y., FUNK S., FUSCO P., GARGANO F., GASPARRINI D., GEHRELS N., GERMANI S., GIGLIETTO N., GILMORE R.C., GIOMMI P., GIORDANO F., GIROLETTI M., GLANZMAN T., GODFREY G., GRANOT J., GREINER J., GRENIER I.A., GROVE J.E., GUIRIEC S., GUSTAFSSON M., HADASCH D., HAYASHIDA M., HAYS E., HORAN D., HUGHES R.E., JOHANNESSON G., JOHNSON A.S., JOHNSON R.P., JOHNSON W.N., KAMAE T., KATAGIRI H., KATAOKA J., KNODLSEDER J., KOCEVSKI D., KUSS M., LANDE J., LATRONICO L., LEE S.-H., GARDE M.L., LONGO F., LOPARCO F., LOTT B., LOVELLETTE M.N., LUBRANO P., MAKEEV A., MAZZIOTTA M.N., McCONVILLE W., McENERY J.E., McGLYNN S., MEHAULT J., MESZAROS P., MICHELSON P.F., MIZUNO T., MOISEEV A.A., MONTE C., MONZANI M.E., MORETTI E., MORSELLI A., MOSKALENKO I.V., MURGIA S., NAKAMORI T., NAUMANN-GODO M., NOLAN P.L., NORRIS J.P., NUSS E., OHNO M., OHSUGI T., OKUMURA A., OMODEI N., ORLANDO E., ORMES J.F., OZAKI M., PANEQUE D., PANETTA J.H., PARENT D., PELASSA V., PEPE M., PESCE-ROLLINS M., PIRON F., PORTER T.A., PRIMACK J.R., RAINO S., RANDO R., RAZZANO M., RAZZAQUE S., REIMER A., REIMER O., REYES L.C., RIPKEN J., RITZ S., ROMANI R.W., ROTH M., SADROZINSKI H.F.-W., SANCHEZ D., SANDER A., SCARGLE J.D., SCHALK T.L., SGRO C., SHAW M.S., SISKIND E.J., SMITH P.D., SPANDRE G., SPINELLI P., STECKER F.W., STRICKMAN M.S., SUSON D.J., TAJIMA H., TAKAHASHI H., TAKAHASHI T., TANAKA T., THAYER J.B., THAYER J.G., THOMPSON D.J., TIBALDO L., TORRES D.F., TOSTI G., TRAMACERE A., UCHIYAMA Y., USHER T.L., VANDENBROUCKE J., VASILEIOU V., VILCHEZ N., VITALE V., VON KIENLIN A., WAITE A.P., WANG P., WILSON-HODGE C., WINER B.L., WOOD K.S., YAMAZAKI R., YANG Z., YLINEN T. and ZIEGLER M.

Abstract (from CDS):

The extragalactic background light (EBL) includes photons with wavelengths from ultraviolet to infrared, which are effective at attenuating gamma rays with energy above ∼10 GeV during propagation from sources at cosmological distances. This results in a redshift- and energy-dependent attenuation of the γ-ray flux of extragalactic sources such as blazars and gamma-ray bursts (GRBs). The Large Area Telescope on board Fermi detects a sample of γ-ray blazars with redshift up to z ∼ 3, and GRBs with redshift up to z ∼ 4.3. Using photons above 10 GeV collected by Fermi over more than one year of observations for these sources, we investigate the effect of γ-ray flux attenuation by the EBL. We place upper limits on the γ-ray opacity of the universe at various energies and redshifts and compare this with predictions from well-known EBL models. We find that an EBL intensity in the optical-ultraviolet wavelengths as great as predicted by the "baseline" model of Stecker et al. can be ruled out with high confidence.

Abstract Copyright: ∼

Journal keyword(s): diffuse radiation - dust, extinction - gamma rays: general

Simbad objects: 18

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Number of rows : 18
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 QSO B0227-369 Bla 02 29 28.44905708 -36 43 56.8223412     19.0 20.4   ~ 113 1
2 RX J0232.8+2017 BLL 02 32 48.6148874688 +20 17 17.486717388     18.00 13.96   ~ 387 1
3 NGC 1316 rG 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1491 1
4 QSO B0347-121 BLL 03 49 23.1862105584 -11 59 27.366035532   18.74 18.2 17.46   ~ 245 1
5 GRB 080916C gB 07 59 23.24 -56 38 16.8           ~ 386 0
6 QSO B0805-077 Bla 08 08 15.53603763 -07 51 09.8865298     19.80 16.71   ~ 291 1
7 Fermi bn090423330 gB 09 55 33.19 +18 08 57.7           ~ 392 0
8 SDSS J101241.37+243923.4 Bla 10 12 41.3779909824 +24 39 23.394747816   19.77 19.58 19.4   ~ 82 1
9 QSO J1016+0513 Bla 10 16 03.13647602 +05 13 02.3413146   20.26 19.83 20   ~ 162 1
10 QSO B1144-3755 BLL 11 47 01.37071212 -38 12 11.0235229   19.03 16.2 16.72   ~ 320 1
11 3C 279 Bla 12 56 11.16657958 -05 47 21.5251510   18.01 17.75 15.87   ~ 3205 2
12 PG 1424+240 BLL 14 27 00.3917926224 +23 48 00.037510776 14.52 14.34 14.95 14.5   ~ 420 1
13 QSO B1502+1041 Bla 15 04 24.97978391 +10 29 39.1985309   18.97 18.56 18.94   ~ 634 1
14 QSO J1512-0906 Bla 15 12 50.53293048 -09 05 59.8297908   16.74 16.54     ~ 1409 1
15 PG 1553+113 BLL 15 55 43.0440048528 +11 11 24.365649948 14.91 14.72 14.57 13.99   ~ 672 1
16 Fermi bn090902462 gB 17 39 45.26 +27 19 28.1           ~ 440 0
17 Fermi bn090510016 G 22 14 12.6230 -26 34 58.550           ~ 548 0
18 Fermi bn090926181 gB 23 33 36.18 -66 19 25.9           ~ 339 0

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