Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Almeida, U. Barres de; Bazer‐Bachi, A. R.; Becherini, Y.; Behera, B.; Benbow, W.; Bernlöhr, K.; Boisson, C.; Bochow, A.; Borrel, V.; Braun, I.; Brion, E.; Brucker, J.; Brun, P.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Carrigan, S.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L.‐M.; Clapson, A. C.; Coignet, G.; Dalton, M.; Daniel, M. K.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati‐Ataï, A.; Domainko, W.; Drury, L. O’c.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Farnier, C.; Feinstein, F.; Fiaßon, A.; Förster, A.; Fontaine, G.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gérard, L.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Hauser, D.; Hauser, M.; Heinz, Sebastian; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Holleran, M.; Hoppe, S.; Horns, D.; Jachołkowska, A.; Jager, O. C. de; Jung, I.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kendziorra, E.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Keogh, D.; Komin, Nu.; Kosack, K.; Lamanna, G.; Lenain, J.‐P.; Löhse, T.; Marandon, V.; Martin, Jean‐Michel; Martineau‐Huynh, O.; Marcowith, A.; Maurin, D.; McComb, T. J. L.; Medina, M. C.; Moderski, R.; Moulin, Emmanuel; Naumann-Godó, M.; Naurois, M. de; Nedbal, D.; Nekrassov, D.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J.‐F.; Wilhelmi, E. de Oña; Orford, K. J.; Ostrowski, M.; Panter, M.; Arribas, M. Paz; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raubenheimer, B. C.; Raue, M.; Rayner, S. M.; Renaud, M.; Reimer, O.; Rieger, F.; Ripken, J.; Rob, L.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schröder, R.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Skilton, J. L.; Sol, H.; Spangler, D.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Superina, G.; Tam, P. H. T.; Tavernet, J.‐P.; Terrier, R.; Tibolla, O.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Venter, L.; Vialle, J. P.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Wagner, S. J.; Ward, M. J.; Zdziarski, A. A.; Zech, A.

doi:10.1051/0004-6361/200811357

Cited by 67 publications

(48 citation statements)

References 26 publications

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“…The data were consistent both with a point source and with an extended source of diameter <2.6°. The Cherenkov telescope HESS confirmed the discovery with the detection of the extended .source HESS J1908+063 (Aharonian et al, 2009) at energies above 300 GeV, positionally consistent with the MILAGRO source. The extension of the source, evaluated assuming a symmetrical twodimensional Gaussian shape, was <Text=0.34°^Q,,j.…”

Section: Mgroj1908+06supporting

confidence: 64%

Gamma ray sources observation with the ARGO-YBJ detector

Vernetto¹

2011

Astrophys. Space Sci. Trans.

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"In this paper we report on the observations of. TeV gamma ray sources performed by the air shower detector. ARGO-YBJ. The objects studied in this work are. the blazar Markarian 421 and the extended galactic source. MGROJ1908+06, monitored during 2 years of operation.. Mrk421 has been detected by ARGO-YBJ with a statistical. significance of 11 standard deviations. The observed. TeV emission was highly variable, showing large enhancements. of the flux during active periods. The study of the. spectral behaviour during flares revealed a positive correlation. of the hardness with the flux, as already reported in the. past by the Whipple telescope, suggesting that this is a long. term property of the source.. ARGO-YBJ observed a strong correlation between TeV. gamma rays and the X-ray flux measured by RXTM\/ASM. and SWIFT\/BAT during the whole period, with a time lag. compatible with zero, supporting the one-zone SSC model to. describe the emission mechanism.. MGROJ1908+06 has been detected by ARGO-YBJ with. 5 standard deviation of significance. From our data. the source appears extended and the measured extension is. ext=0.48+0.26. −0.28, in agreement with a previous HESS observation.. The average flux is in marginal agreement with that. reported by MILAGRO, but significantly higher than that obtained. by HESS, suggesting a possible flux variability.

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Section: Mgroj1908+06supporting

confidence: 64%

Gamma ray sources observation with the ARGO-YBJ detector

Vernetto¹

2011

Astrophys. Space Sci. Trans.

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“…Abdo et al (2010) found that this pulsar (yellow cross in Figure 6) lies in the extended emission seen also with the High Energy Stereoscopic System (HESS; Aharonian et al 2009) and the Very Energetic Radiation Imaging Telescope Array System (VERITAS; Ward 2008). They noted, however, that the association with G40.5-0.5 seems very unlikely as it would require an extremely high transverse velocity and should have resulted in a bow-shock shaped nebula near the pulsar which was not evident in their Chandra X-ray observations.…”

Section: Psr J1907+0631mentioning

confidence: 93%

Timing of 29 Pulsars Discovered in the Palfa Survey

Lyne¹,

Stappers²,

Bogdanov³

et al. 2017

ApJ

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“…[16,20,21], and the ARGO-YBJ experiment [22]. This source has been detected also by ACTs, like HESS [23], which finds a spectrum with no evidence of a cut-off for energies < 20 TeV. The HESS detector reports a flux systematically lower than the Milagro and ARGO-YBJ data.…”

Section: Mgro J1908+06mentioning

confidence: 95%

Prospects for detecting galactic sources of cosmic neutrinos with IceCube: An update

Halzen

Kheirandish

Niro

2017

Astroparticle Physics

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Air-Cherenkov telescopes have mapped the Galactic plane at TeV energies. Here we evaluate the prospects for detecting the neutrino emission from sources in the Galactic plane assuming that the highest energy photons originate from the decay of pions, which yields a straightforward prediction for the neutrino flux from the decay of the associated production of charged pions. Four promising sources are identified based on having a large flux and a flat spectrum. We subsequently evaluate the probability of their identification above the atmospheric neutrino background in IceCube data as a function of time. We show that observing them over the twenty-year lifetime of the instrumentation is likely, and that some should be observable at the 3 σ level with six years of data. In the absence of positive results, we derive constraints on the spectral index and cut-off energy of the sources, assuming a hadronic acceleration mechanism.

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Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Cited by 67 publications

References 26 publications

Gamma ray sources observation with the ARGO-YBJ detector

Gamma ray sources observation with the ARGO-YBJ detector

Timing of 29 Pulsars Discovered in the Palfa Survey

Prospects for detecting galactic sources of cosmic neutrinos with IceCube: An update

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