2013ApJ...770...93A

Query : 2013ApJ...770...93A

2013ApJ...770...93A - Astrophys. J., 770, 93 (2013/June-3)

Discovery of TeV gamma-ray emission toward supernova remnant SNR G78.2+2.1.

ALIU E., ARCHAMBAULT S., ARLEN T., AUNE T., BEILICKE M., BENBOW W., BIRD R., BOUVIER A., BRADBURY S.M., BUCKLEY J.H., BUGAEV V., BYRUM K., CANNON A., CESARINI A., CIUPIK L., COLLINS-HUGHES E., CONNOLLY M.P., CUI W., DICKHERBER R., DUKE C., DUMM J., DWARKADAS V.V., ERRANDO M., FALCONE A., FEDERICI S., FENG Q., FINLEY J.P., FINNEGAN G., FORTSON L., FURNISS A., GALANTE N., GALL D., GILLANDERS G.H., GODAMBE S., GOTTHELF E.V., GRIFFIN S., GRUBE J., GYUK G., HANNA D., HOLDER J., HUAN H., HUGHES G., HUMENSKY T.B., KAARET P., KARLSSON N., KERTZMAN M., KHASSEN Y., KIEDA D., KRAWCZYNSKI H., KRENNRICH F., LANG M.J., LEE K., MADHAVAN A.S., MAIER G., MAJUMDAR P., McARTHUR S., McCANN A., MILLIS J., MORIARTY P., MUKHERJEE R., NELSON T., O'FAOLAIN DE BHROITHE A., ONG R.A., ORR M., OTTE A.N., PANDEL D., PARK N., PERKINS J.S., POHL M., POPKOW A., PROKOPH H., QUINN J., RAGAN K., REYES L.C., REYNOLDS P.T., ROACHE E., ROSE H.J., RUPPEL J., SAXON D.B., SCHROEDTER M., SEMBROSKI G.H., SENTURK G.D., SKOLE C., TELEZHINSKY I., TESIC G., THEILING M., THIBADEAU S., TSURUSAKI K., TYLER J., VARLOTTA A., VASSILIEV V.V., VINCENT S., WAKELY S.P., WARD J.E., WEEKES T.C., WEINSTEIN A., WEISGARBER T., WELSING R., WILLIAMS D.A. and ZITZER B.

Abstract (from CDS):

We report the discovery of an unidentified, extended source of very-high-energy gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hr of data taken by the VERITAS gamma-ray observatory in 2009. These data confirm the preliminary indications of gamma-ray emission previously seen in a two-year (2007-2009) blind survey of the Cygnus region by VERITAS. VER J2019+407, which is detected at a post-trials significance of 7.5 standard deviations in the 2009 data, is localized to the northwestern rim of the remnant in a region of enhanced radio and X-ray emission. It has an intrinsic extent of 0°.23 ±0°.03 stat0°.02sys+0°.04 and its spectrum is well-characterized by a differential power law (dN/dE = N0x(E/TeV)–Γ) with a photon index of Γ = 2.37±0.14stat± 0.20sys and a flux normalization of N0= 1.5 ± 0.2stat± 0.4sysx10–12 photon.TeV–1/cm2/s. This yields an integral flux of 5.2±0.8stat± 1.4sysx10–12 photon/cm2/s above 320 GeV, corresponding to 3.7% of the Crab Nebula flux. We consider the relationship of the TeV gamma-ray emission with the GeV gamma-ray emission seen from SNR G78.2+2.1 as well as that seen from a nearby cocoon of freshly accelerated cosmic rays. Multiple scenarios are considered as possible origins for the TeV gamma-ray emission, including hadronic particle acceleration at the SNR shock.

Abstract Copyright: ∼

Journal keyword(s): acceleration of particles - cosmic rays - gamma rays: general - ISM: supernova remnants

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 M 1 SNR 05 34 30.9 +22 00 53           ~ 6192 1
2 NAME Vela Jr SN BL? 08 52.0 -46 20           ~ 474 2
3 ESO 134-11 HII 14 40 29 -62 38.7           ~ 565 1
4 HESS J1702-420 gam 17 02 44.0 -42 00 57           ~ 42 0
5 PSR J1702-4128 Psr 17 02 52.52 -41 28 48.2           ~ 65 0
6 * P Cyg s*b 20 17 47.2019733389 +38 01 58.549132671 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1176 1
7 HD 193322 ** 20 18 06.98820 +40 43 55.5001 5.17 5.94 5.84 5.69 5.68 O9IV(n)+B1.5V 278 0
8 ARGO J2021+4038 gam 20 19 00.0 +40 42 00           ~ 32 1
9 NAME gam Cyg SNR BL? 20 20 17.100 +40 26 09.00           ~ 229 2
10 GRO J2019+40 gam 20 21.5 +40 26           ~ 129 1
11 PSR J2021+4026 Psr 20 21 30.496 +40 26 53.56           ~ 275 2
12 * gam Cyg V* 20 22 13.7018357 +40 15 24.044963 3.44 2.90 2.23 1.74 1.40 F8Ib 583 0
13 * 40 Cyg PM* 20 27 34.2590464440 +38 26 25.262381940 5.74 5.68 5.62     A3V 96 0
14 NAME Cyg Complex reg 20 32 +45.0           ~ 601 0
15 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 943 0

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