We report the observation of TeV gamma-rays from the Cygnus region using the ARGO-YBJ data collected from 2007 November to 2011 August. Several TeV sources are located in this region including the two bright extended MGRO J2019+37 and MGRO J2031+41. According to the Milagro data set, at 20 TeV MGRO J2019+37 is the most significant source apart from the Crab Nebula. No signal from MGRO J2019+37 is detected by the ARGO-YBJ experiment, and the derived flux upper limits at the 90% confidence level for all the events above 600 GeV with medium energy of 3 TeV are lower than the Milagro flux, implying that the source might be variable and hard to be identified as a pulsar wind nebula. The only statistically significant (6.4 standard deviations) gamma-ray signal is found from MGRO J2031+41, with a flux consistent with the measurement by Milagro.

OBSERVATION OF TeV GAMMA RAYS FROM THE CYGNUS REGION WITH THE ARGO-YBJ EXPERIMENT / Bartoli, Bruno; Bernardini, P.; X. J., Bi; Bleve, C.; Bolognino, I.; Branchini, P.; Budano, A.; A. K. C., ; Camarri, P.; Cao, Z.; Cardarelli, R.; Catalanotti, Sergio; Cattaneo, C.; Chen, S. Z.; Chen, T. L.; Chen, Y.; Creti, P.; Cui, S. W.; Dai, B. Z.; Staiti, G. D.; Danzengluobu, ; Dattoli, M.; Mitri, I. D.; D'ETTORRE PIAZZOLI, Benedetto; DI GIROLAMO, Tristano; Ding, X. H.; Sciascio, G. D.; Feng, C. F.; Feng, Z. Y.; Feng, Z. Y.; Galeazzi, F.; Giroletti, E.; Gou, Q. B.; Guo, Y. Q.; H. H., He; H. B., Hu; H. B., Hu; Huang, Q.; Iacovacci, Michele; Iuppa, R.; James, I.; Jia, H. Y.; Labaciren, ; H. J., Li; J. Y., Li; X. X., Li; Liguori, G.; Liu, C.; Liu, C. Q.; Liu, J.; Liu, M. Y.; Lu, H.; L. L., Ma; X. H., Ma; Mancarella, G.; Mari, S. M.; Marsella, G.; Martello, D.; Mastroianni, S.; Montini, P.; Ning, C. C.; Pagliaro, A.; Panareo, M.; Panico, B.; Perrone, L.; Pistilli, P.; Ruggieri, F.; Salvini, P.; Santonico, R.; Shen, P. R.; Sheng, X. D.; Shi, F.; Stanescu, C.; Surdo, A.; Tan, Y. H.; Vallania, P.; Vernetto, S.; Vigorito, C.; Wang, B.; Wang, H.; C. Y., Wu; H. R., Wu; Xu, B.; Xue, L.; Yang, Q. Y.; Yang, X. C.; Yao, Z. G.; Yuan, A. F.; Zha, M.; Zhang, H. M.; Zhang, J. L.; Zhang, J. L.; Zhang, L.; Zhang, P.; Zhang, X. Y.; Zhang, Y.; Zhao, J.; Zhaxiciren, Zhaxisangzhu; Zhou, X. X.; Zhu, F. R.; Zhu, Q. Q.; Zizzi, G.. - 745:L22(2012), pp. 1-5. [10.1088/2041-8205/745/2/L22]

OBSERVATION OF TeV GAMMA RAYS FROM THE CYGNUS REGION WITH THE ARGO-YBJ EXPERIMENT

BARTOLI, BRUNO;CATALANOTTI, SERGIO;D'ETTORRE PIAZZOLI, BENEDETTO;DI GIROLAMO, TRISTANO;IACOVACCI, MICHELE;B. Panico;
2012

Abstract

We report the observation of TeV gamma-rays from the Cygnus region using the ARGO-YBJ data collected from 2007 November to 2011 August. Several TeV sources are located in this region including the two bright extended MGRO J2019+37 and MGRO J2031+41. According to the Milagro data set, at 20 TeV MGRO J2019+37 is the most significant source apart from the Crab Nebula. No signal from MGRO J2019+37 is detected by the ARGO-YBJ experiment, and the derived flux upper limits at the 90% confidence level for all the events above 600 GeV with medium energy of 3 TeV are lower than the Milagro flux, implying that the source might be variable and hard to be identified as a pulsar wind nebula. The only statistically significant (6.4 standard deviations) gamma-ray signal is found from MGRO J2031+41, with a flux consistent with the measurement by Milagro.
2012
OBSERVATION OF TeV GAMMA RAYS FROM THE CYGNUS REGION WITH THE ARGO-YBJ EXPERIMENT / Bartoli, Bruno; Bernardini, P.; X. J., Bi; Bleve, C.; Bolognino, I.; Branchini, P.; Budano, A.; A. K. C., ; Camarri, P.; Cao, Z.; Cardarelli, R.; Catalanotti, Sergio; Cattaneo, C.; Chen, S. Z.; Chen, T. L.; Chen, Y.; Creti, P.; Cui, S. W.; Dai, B. Z.; Staiti, G. D.; Danzengluobu, ; Dattoli, M.; Mitri, I. D.; D'ETTORRE PIAZZOLI, Benedetto; DI GIROLAMO, Tristano; Ding, X. H.; Sciascio, G. D.; Feng, C. F.; Feng, Z. Y.; Feng, Z. Y.; Galeazzi, F.; Giroletti, E.; Gou, Q. B.; Guo, Y. Q.; H. H., He; H. B., Hu; H. B., Hu; Huang, Q.; Iacovacci, Michele; Iuppa, R.; James, I.; Jia, H. Y.; Labaciren, ; H. J., Li; J. Y., Li; X. X., Li; Liguori, G.; Liu, C.; Liu, C. Q.; Liu, J.; Liu, M. Y.; Lu, H.; L. L., Ma; X. H., Ma; Mancarella, G.; Mari, S. M.; Marsella, G.; Martello, D.; Mastroianni, S.; Montini, P.; Ning, C. C.; Pagliaro, A.; Panareo, M.; Panico, B.; Perrone, L.; Pistilli, P.; Ruggieri, F.; Salvini, P.; Santonico, R.; Shen, P. R.; Sheng, X. D.; Shi, F.; Stanescu, C.; Surdo, A.; Tan, Y. H.; Vallania, P.; Vernetto, S.; Vigorito, C.; Wang, B.; Wang, H.; C. Y., Wu; H. R., Wu; Xu, B.; Xue, L.; Yang, Q. Y.; Yang, X. C.; Yao, Z. G.; Yuan, A. F.; Zha, M.; Zhang, H. M.; Zhang, J. L.; Zhang, J. L.; Zhang, L.; Zhang, P.; Zhang, X. Y.; Zhang, Y.; Zhao, J.; Zhaxiciren, Zhaxisangzhu; Zhou, X. X.; Zhu, F. R.; Zhu, Q. Q.; Zizzi, G.. - 745:L22(2012), pp. 1-5. [10.1088/2041-8205/745/2/L22]
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11588/468600
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