PERIODIC VERY HIGH ENERGY γ-RAY EMISSION FROM LS I+61°303 OBSERVED WITH THE MAGIC TELESCOPE

被引：70

作者：

Albert, J. ^{[1
]}

Aliu, E. ^{[2
]}

Anderhub, H. ^{[3
]}

Antonelli, L. A. ^{[4
]}

Antoranz, P. ^{[5
]}

Backes, M. ^{[6
]}

Baixeras, C. ^{[7
]}

Barrio, J. A. ^{[5
]}

Bartko, H. ^{[8
]}

Bastieri, D. ^{[9
,10
]}

Becker, J. K. ^{[6
]}

Bednarek, W. ^{[11
]}

Berger, K. ^{[1
]}

Bernardini, E. ^{[12
]}

Bigongiari, C. ^{[9
,10
]}

Biland, A. ^{[3
]}

Bock, R. K. ^{[8
,9
,10
]}

Bonnoli, G. ^{[13
,14
]}

Bordas, P. ^{[15
]}

Bosch-Ramon, V. ^{[15
]}

Bretz, T. ^{[1
]}

Britvitch, I. ^{[3
]}

Camara, M. ^{[5
]}

Carmona, E. ^{[8
]}

Chilingarian, A. ^{[16
]}

Commichau, S. ^{[3
]}

Contreras, J. L. ^{[5
]}

Cortina, J. ^{[2
]}

Costado, M. T. ^{[17
,18
]}

Covino, S. ^{[4
]}

Curtef, V. ^{[6
]}

Dazzi, F. ^{[9
,10
]}

De Angelis, A. ^{[19
,20
]}

De Cea del Pozo, E. ^{[21
]}

De Los Reyes, R. ^{[5
]}

De Lotto, B. ^{[19
,20
]}

De Maria, M. ^{[19
,20
]}

De Sabata, F.

Mendez, C. Delgado ^{[19
,20
]}

Dominguez, A. ^{[17
]}

Dorner, D. ^{[22
]}

Doro, M. ^{[9
,10
]}

Errando, M. ^{[2
]}

Fagiolini, M. ^{[13
,14
]}

Ferenc, D. ^{[23
]}

Fernandez, E. ^{[2
]}

Firpo, R. ^{[2
]}

Fonseca, M. V. ^{[5
]}

Font, L. ^{[7
]}

Galante, N. ^{[8
]}

机构：

[1] Univ Wurzburg, D-97074 Wurzburg, Germany

[2] IFAE, E-08193 Bellaterra, Spain

[3] ETH, CH-8093 Zurich, Switzerland

[4] INAF Natl Inst Astrophys, I-00136 Rome, Italy

[5] Univ Complutense, E-28040 Madrid, Spain

[6] Tech Univ, D-44221 Dortmund, Germany

[7] Univ Autonoma Barcelona, E-08193 Barcelona, Spain

[8] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[9] Univ Padua, I-35131 Padua, Italy

[10] Ist Nazl Fis Nucl, I-35131 Padua, Italy

[11] Univ Lodz, PL-90236 Lodz, Poland

[12] DESY Deutsch Elektr Synchrotron, D-15738 Zeuthen, Germany

[13] Univ Siena, I-53100 Siena, Italy

[14] INFN Pisa, I-53100 Siena, Italy

[15] Univ Barcelona, ICC IEEC, E-08028 Barcelona, Spain

[16] Yerevan Phys Inst, AM-375036 Yerevan, Armenia

[17] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain

[18] Univ La Laguna, Depto Astrofis, E-38206 Tenerife, Spain

[19] Univ Udine, I-33100 Udine, Italy

[20] INFN Trieste, I-33100 Udine, Italy

[21] Inst Ciencies Espai IEEC CSIC, E-08193 Barcelona, Spain

[22] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[23] Univ Calif Davis, Davis, CA 95616 USA

[24] Turku Univ, Tuorla Observ, FI-21500 Piikkio, Finland

[25] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria

[26] Humboldt Univ, D-12489 Berlin, Germany

[27] INAF Osservatorio Astron, I-34143 Trieste, Italy

[28] Ist Nazl Fis Nucl, I-34143 Trieste, Italy

[29] ICREA, E-08010 Barcelona, Spain

[30] Univ Pisa, I-56126 Pisa, Italy

[31] Ist Nazl Fis Nucl, I-56126 Pisa, Italy

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 693卷 / 01期

关键词：

gamma rays: observations; stars: individual (LS I+61 degrees 303); X-rays: binaries; SOURCE 2CG 135+01; X-RAY; H-ALPHA; MICROQUASAR LS-I+61-303; SPACED DATA; LSI+61-DEGREES-303; BINARY; RADIO; LS-I-+61-303;

D O I：

10.1088/0004-637X/693/1/303

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The MAGIC collaboration has recently reported the discovery of gamma-ray emission from the binary system LS I +61 degrees 303 in the TeV energy region. Here we present new observational results on this source in the energy range between 300 GeV and 3 TeV. In total, 112 hr of data were taken between 2006 September and December covering four orbital cycles of this object. This large amount of data allowed us to produce an integral flux light curve covering for the first time all orbital phases of LS I +61 degrees 303. In addition, we also obtained a differential energy spectrum for two orbital phase bins covering the phase range 0.5 < phi < 0.6 and 0.6 < phi < 0.7. The photon index in the two phase bins is consistent within the errors with an average index Gamma = 2.6 +/- 0.2(stat) +/- 0.2(sys). LS I +61 degrees 303 was found to be variable at TeV energies on timescales of days. These new MAGIC measurements allowed us to search for intranight variability of the very high energy emission; however, no evidence for flux variability on timescales down to 30 min was found. To test for possible periodic structures in the light curve, we apply the formalism developed by Lomb and Scargle to the LS I +61 degrees 303 data taken in 2005 and 2006. We found the LS I +61 degrees 303 data set to be periodic with a period of (26.8 +/- 0.2) days (with a post-trial chance probability of 10(-7)), close to the orbital period.

引用

页码：303 / 310

页数：8

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