DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1

E Aliu; S Archambault; T Arlen; T Aune; M Beilicke; J. H Buckley; V Bugaev; R Dickherber; W Benbow; R Bird; A Cannon; E Collins-Hughes; A Bouvier; S. M Bradbury; K Byrum; A Cesarini; M. P Connolly; L Ciupik; W Cui; C Duke; P Kaaret

doi:10.1088/0004-637X/770/2/93

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DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1

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DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1

E Aliu, S Archambault, T Arlen, T Aune, M Beilicke, J. H Buckley, V Bugaev, R Dickherber, W Benbow, R Bird, …

The Astrophysical journal, Vol.770(2), 93

06/20/2013

DOI: 10.1088/0004-637X/770/2/93

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Abstract

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 Degree-Sign .23 {+-} 0. Degree-Sign 03{sub stat-0 Degree-Sign .02sys}{sup +0 Degree-Sign .04} and its spectrum is well-characterized by a differential power law (dN/dE = N{sub 0} Multiplication-Sign (E/TeV){sup -{Gamma}}) with a photon index of {Gamma} = 2.37 {+-} 0.14{sub stat} {+-} 0.20{sub sys} and a flux normalization of N{sub 0} = 1.5 {+-} 0.2{sub stat} {+-} 0.4{sub sys} Multiplication-Sign 10{sup -12} photon TeV{sup -1} cm{sup -2} s{sup -1}. This yields an integral flux of 5.2 {+-} 0.8{sub stat} {+-} 1.4{sub sys} Multiplication-Sign 10{sup -12} photon cm{sup -2} s{sup -1} 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.

ACCELERATION

ASTROPHYSICS, COSMOLOGY AND ASTRONOMY

COSMIC RADIATION

CRAB NEBULA

GAMMA RADIATION

GEV RANGE

HADRONS

PARTICLES

PHOTONS

SPECTRA

TEV RANGE

X RADIATION

Details

Title: Subtitle: DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1
Creators: E Aliu - Columbia University
S Archambault - McGill University
T Arlen - University of California, Los Angeles
T Aune - University of California, Los Angeles
M Beilicke - Washington University in St. Louis
J. H Buckley - Washington University in St. Louis
V Bugaev - Washington University in St. Louis
R Dickherber - Washington University in St. Louis
W Benbow - Harvard University
R Bird - University College Dublin
A Cannon - University College Dublin
E Collins-Hughes - University College Dublin
A Bouvier - University of California, Santa Cruz
S. M Bradbury - University of Leeds
K Byrum - Argonne National Laboratory
A Cesarini - Ollscoil na Gaillimhe – University of Galway
M. P Connolly - Ollscoil na Gaillimhe – University of Galway
L Ciupik - Adler Planetarium
W Cui - Purdue University West Lafayette
C Duke - Grinnell College
P Kaaret - University of Iowa, Physics and Astronomy
Resource Type: Journal article
Publication Details: The Astrophysical journal, Vol.770(2), 93
DOI: 10.1088/0004-637X/770/2/93
ISSN: 0004-637X
eISSN: 1538-4357
Publisher: Institute of Physics (IOP)
Language: English
Date published: 06/20/2013
Academic Unit: Physics and Astronomy
Record Identifier: 9984199824402771

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