Peer-Reviewed Journal Details
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Aliu, E,Aune, T,Behera, B,Beilicke, M,Benbow, W,Berger, K,Bird, R,Bouvier, A,Buckley, JH,Bugaev, V,Cerruti, M,Chen, X,Ciupik, L,Connolly, MP,Cui, W,Dumm, J,Dwarkadas, VV,Errando, M,Falcone, A,Federici, S,Feng, Q,Finley, JP,Fleischhack, H,Fortin, P,Fortson, L,Furniss, A,Galante, N,Gillanders, GH,Gotthelf, EV,Griffin, S,Griffiths, ST,Grube, J,Gyuk, G,Hanna, D,Holder, J,Hughes, G,Humensky, TB,Johnson, CA,Kaaret, P,Kargaltsev, O,Kertzman, M,Khassen, Y,Kieda, D,Krennrich, F,Lang, MJ,Madhavan, AS,Maier, G,McArthur, S,McCann, A,Millis, J,Moriarty, P,Mukherjee, R,Nieto, D,de Bhroithe, AO,Ong, RA,Otte, AN,Pandel, D,Park, N,Pohl, M,Popkow, A,Prokoph, H,Quinn, J,Ragan, K,Rajotte, J,Reyes, LC,Reynolds, PT,Richards, GT,Roache, E,Roberts, M,Sembroski, GH,Shahinyan, K,Smith, AW,Staszak, D,Telezhinsky, I
2014
June
Astrophysical Journal
SPATIALLY RESOLVING THE VERY HIGH ENERGY EMISSION FROM MGRO J2019+37 WITH VERITAS
Published
Altmetric: 2WOS: 23 ()
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gamma rays : stars pulsars : individual (PSR J2021+3651) supernovae : individual (CTB 87) GAMMA-RAY EMISSION PULSAR WIND NEBULA GALACTIC PLANE PSR J2021+3651 CYGNUS REGION DISCOVERY MILAGRO STARS HESS ASSOCIATIONS
788
We present very high energy (VHE) imaging of MGRO J2019+37 obtained with the VERITAS observatory. The bright extended (similar to 2 degrees) unidentified Milagro source is located toward the rich star formation region Cygnus-X. MGRO J2019+37 is resolved into two VERITAS sources. The faint, point-like source VER J2016+371 overlaps CTB 87, a filled-center remnant (SNR) with no evidence of a supernova remnant shell at the present time. Its spectrum is well fit in the 0.65-10 TeV energy range by a power-law model with photon index 2.3 +/- 0.4. VER J2019+378 is a bright extended (similar to 1 degrees) source that likely accounts for the bulk of the Milagro emission and is notably coincident with PSR J2021+3651 and the star formation region Sh 2-104. Its spectrum in the range 1-30 TeV is well fit with a power-law model of photon index 1.75 +/- 0.3, among the hardest values measured in the VHE band, comparable to that observed near Vela-X. We explore the unusual spectrum and morphology in the radio and X-ray bands to constrain possible emission mechanisms for this source.
10.1088/0004-637X/788/1/78
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