RT Journal Article
T1 Magic observations of the unidentified gamma-ray source TEV J2032+4130
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Fonseca González, Mª Victoria
A1 López Moya, Marcos
A1 Miranda Pantoja, José Miguel
A1 Nieto, Daniel
AB We observed the first known very high energy (VHE) gamma-ray-emitting unidentified source, TeV J2032 + 4130, for 94 hr with the MAGIC telescope. The source was detected with a significance of 5.6 sigma. The flux, position, and angular extension are compatible with the previous ones measured by the HEGRA telescope system 5 years ago. The integral flux amounts to (4.5 +/- 0.3(stat)+/- 0.35(sys)) x 10 (- 13) photons cm(-2) s(-1) above 1 TeV. The source energy spectrum, obtained with the lowest energy threshold to date, is compatible with a single power law with a hard photon index of Gamma= - 2.0 +/- 0.3(stat)+/- 0.2(sys).Miranda Pantka
PB IOP Publishing
SN 2041-8205
YR 2008
FD 2008-03-01
LK https://hdl.handle.net/20.500.14352/50883
UL https://hdl.handle.net/20.500.14352/50883
LA eng
NO Abdo, A. A., et al. 2007, ApJ, 658, L33.Aharonian, F. A., et al. 2002, A&A, 393, L37———. 2005, A&A, 431, 197———. 2006, A&A, 460, 743.Albert, J., et al. 2006a, Science, 312, 1771———. 2006b, ApJ, 637, L41———. 2006c, ApJ, 638, L101———. 2006d, ApJ, 643, L53———. 2007a, Astropart. Phys., submitted (astro-ph/0702475)———. 2007b, Astropart. Phys., submitted (arXiv:0709.3719)———. 2008, ApJ, in press (arXiv:0705.3244).Amenomori, M., et al. 2006, Science, 314, 439.Anchordoqui, L. A., et al. 2007, Phys. Rev. D, 75, 063001.Bednarek, W. 2003, MNRAS, 345, 847.Bosch-Ramon, V., Aharonian, F., Paredes, J. M. 2005, A&A, 432, 609.Bretz, T., Wagner, W. 2003, in Proc. 28th Int. Cosmic Ray Conf. (Tsukuba), 2947.Butt, Y., et al. 2003, ApJ, 597, 494———. 2006, ApJ, 643, 238.Cortina, J., et al. 2005, in Proc. 29th Int. Cosmic Ray Conf. (Pune), 5, 359.Domingo-Santamaría, E., Torres, D. F. 2006, A&A, 448, 613.Domingo-Santamaría, E., et al. 2005, in Proc. 29th Int. Cosmic Ray Conf. (Pune), 5, 363.Fegan, D. J. 1997, J. Phys. G, 23, 1013.Hillas, A. M. 1985, in Proc. 19th Int. Cosmic Ray Conf. (La Jolla), 3, 445.Horns, D., et al. 2007, A&A, 469, L17.Konopelko, A., et al. 2007, ApJ, 658, 1062.Lang, M. J., et al. 2004, A&A, 423, 415.Martí, J., et al. 2006, A&A, 451, 1037———. 2007, A&A, 472, 557.Mukherjee, R., et al. 2003, ApJ, 589, 487.Paredes, J. M., et al. 2007, ApJ, 654, L135.Rolke, W. A., López, A. M., Conrad, J. 2005, Nucl. Instrum. Methods Phys. Res., A551, 493.Tikhonov, A. N., Arsenin, V. Ja. 1979, in Numerical Methods for the Solution of Ill-posed Problems (Moscow: Nauka).Torres, D. F., Domingo-Santamaría E., Romero, G. E. 2004, ApJ, 601, L75.
NO © The American Astronomical Society. We thank the IAC for the excellent working conditions at the ORM. The support of the German BMBF and MPG, the Italian INFN, the Spanish CICYT, the ETH Research Grant TH 34/04 3, and the Polish MNiI Grant 1P03D01028 is gratefully acknowledged.
NO German BMBF
NO German MPG
NO Italian INFN
NO Spanish CICYT
NO ETH Research Grant
NO Polish MNiI Grant
DS Docta Complutense
RD 4 may 2024