"The extended gamma-ray source MGRO J1908+06, discovered by the Milagro air shower detector in 2007, has. been observed for ∼4 years by the ARGO-YBJ experiment at TeV energies, with a statistical significance of 6.2. standard deviations. The peak of the signal is found at a position consistent with the pulsar PSR J1907+0602.. Parameterizing the source shape with a two-dimensional Gauss function, we estimate an extension of σext = 0. ◦ 49 ±. 0. ◦ 22, which is consistent with a previous measurement by the Cherenkov Array H.E.S.S. The observed energy. spectrum is dN\/dE = 6.1 ± 1.4 × 10−13 (E\/4 TeV)−2.54±0.36 photons cm−2 s−1 TeV−1, in the energy range of. ∼1–20 TeV. The measured gamma-ray flux is consistent with the results of the Milagro detector, but is ∼2–3 times. larger than the flux previously derived by H.E.S.S. at energies of a few TeV. The continuity of the Milagro and. ARGO-YBJ observations and the stable excess rate observed by ARGO-YBJ and recorded in four years of data. support the identification of MGRO J1908+06 as the steady powerful TeV pulsar wind nebula of PSR J1907+0602,. with an integrated luminosity over 1 TeV ∼ 1.8 times the luminosity of the Crab Nebula."

B. Bartoli1, 2, P. Bernardini3, 4, X. J. Bi5, C. Bleve3, et al. (2012). OBSERVATION OF THE TeV GAMMA-RAY SOURCE MGRO J1908+06 WITH ARGO-YBJ. THE ASTROPHYSICAL JOURNAL, 760(2), 610-615 [10.1088/0004-637X/760/2/110].

OBSERVATION OF THE TeV GAMMA-RAY SOURCE MGRO J1908+06 WITH ARGO-YBJ

MARI, Stefano Maria;P. Montini8;F. Ruggieri8;
2012

Abstract

"The extended gamma-ray source MGRO J1908+06, discovered by the Milagro air shower detector in 2007, has. been observed for ∼4 years by the ARGO-YBJ experiment at TeV energies, with a statistical significance of 6.2. standard deviations. The peak of the signal is found at a position consistent with the pulsar PSR J1907+0602.. Parameterizing the source shape with a two-dimensional Gauss function, we estimate an extension of σext = 0. ◦ 49 ±. 0. ◦ 22, which is consistent with a previous measurement by the Cherenkov Array H.E.S.S. The observed energy. spectrum is dN\/dE = 6.1 ± 1.4 × 10−13 (E\/4 TeV)−2.54±0.36 photons cm−2 s−1 TeV−1, in the energy range of. ∼1–20 TeV. The measured gamma-ray flux is consistent with the results of the Milagro detector, but is ∼2–3 times. larger than the flux previously derived by H.E.S.S. at energies of a few TeV. The continuity of the Milagro and. ARGO-YBJ observations and the stable excess rate observed by ARGO-YBJ and recorded in four years of data. support the identification of MGRO J1908+06 as the steady powerful TeV pulsar wind nebula of PSR J1907+0602,. with an integrated luminosity over 1 TeV ∼ 1.8 times the luminosity of the Crab Nebula."
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11590/278774
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