MAGIC DISCOVERY OF VERY HIGH ENERGY EMISSION FROM THE FSRQ PKS 1222+21

被引：287

作者：

Aleksic, J. ^{[1
]}

Antonelli, L. A. ^{[2
]}

Antoranz, P. ^{[3
,4
]}

Backes, M. ^{[5
]}

Barrio, J. A. ^{[6
]}

Bastieri, D. ^{[7
,8
]}

Becerra Gonzalez, J. ^{[9
,19
]}

Bednarek, W. ^{[10
]}

Berdyugin, A. ^{[11
]}

Berger, K. ^{[9
,19
]}

Bernardini, E. ^{[12
]}

Biland, A. ^{[13
]}

Blanch, O. ^{[1
]}

Bock, R. K. ^{[14
]}

Boller, A. ^{[13
]}

Bonnoli, G. ^{[2
]}

Tridon, D. Borla ^{[14
]}

Braun, I. ^{[13
]}

Bretz, T. ^{[15
]}

Canellas, A. ^{[16
]}

Carmona, E. ^{[14
]}

Carosi, A. ^{[2
]}

Colin, P. ^{[14
]}

Colombo, E. ^{[9
]}

Contreras, J. L. ^{[6
]}

Cortina, J. ^{[1
]}

Cossio, L. ^{[17
,18
]}

Covino, S. ^{[2
]}

Dazzi, F. ^{[17
,18
]}

De Angelis, A. ^{[17
,18
]}

De Cea del Pozo, E. ^{[20
]}

De Lotto, B. ^{[17
,18
]}

Delgado Mendez, C. ^{[9
]}

Diago Ortega, A. ^{[9
,19
]}

Doert, M. ^{[5
]}

Dominguez, A. ^{[21
]}

Prester, D. Dominis ^{[22
,23
]}

Dorner, D. ^{[13
]}

Doro, M. ^{[24
]}

Elsaesser, D. ^{[15
]}

Ferenc, D. ^{[22
,23
]}

Fonseca, M. V. ^{[6
]}

Font, L. ^{[24
]}

Fruck, C. ^{[14
]}

Garcia Lopez, R. J. ^{[9
,19
]}

Garczarczyk, M. ^{[9
]}

Garrido, D. ^{[24
]}

Giavitto, G. ^{[1
]}

Godinovic, N. ^{[22
,23
]}

Hadasch, D. ^{[20
]}

机构：

[1] IFAE, E-08193 Bellaterra, Spain

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

[3] Univ Siena, Dipartimento Fis, I-53100 Siena, Italy

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

[5] Tech Univ Dortmund, Fak Phys, D-44221 Dortmund, Germany

[6] Univ Complutense, Grp Fis Atlas Energias, E-28040 Madrid, Spain

[7] Univ Padua, Dipartimento Fis, I-35131 Padua, Italy

[8] INFN, I-35131 Padua, Italy

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

[10] Univ Lodz, Div Expt Phys, PL-90236 Lodz, Poland

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

[12] DESY, D-15738 Zeuthen, Germany

[13] ETH, CH-8093 Zurich, Switzerland

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

[15] Univ Wurzburg, Fak Phys & Astron, D-97074 Wurzburg, Germany

[16] Univ Barcelona, Fac Fis, ICC IEEC, E-08028 Barcelona, Spain

[17] Univ Udine, Dipartimento Fis Sperimentale, I-33100 Udine, Italy

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

[19] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[20] IEEC CSIC, Inst Ciencies Espai, E-08193 Bellaterra, Spain

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

[22] Univ Rijeka, Inst R Boskovic, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia

[23] Univ Split, HR-10000 Zagreb, Croatia

[24] Univ Autonoma Barcelona, Fac Fis, E-08193 Bellaterra, Spain

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

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

[27] INFN, I-34143 Trieste, Italy

[28] Univ Insubria, Dipartimento Fis & Matemat, I-22100 Como, Italy

[29] Univ Pisa, Dipartimento Fis, I-56126 Pisa, Italy

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

[31] ICREA, E-08010 Barcelona, Spain

[32] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan

[33] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 730卷 / 01期

基金：

瑞典研究理事会; 芬兰科学院;

关键词：

cosmic background radiation; galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (PKS 1222+21); EXTRAGALACTIC BACKGROUND LIGHT; GAMMA-RAY ABSORPTION; RELATIVISTIC JETS; UPPER LIMITS; BLAZARS; RADIATION; SPECTRA; CONSTRAINTS;

D O I：

10.1088/2041-8205/730/1/L8

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Very high energy (VHE) gamma-ray emission from the flat spectrum radio quasar (FSRQ) PKS 1222+ 21 (4C 21.35, z = 0.432) was detected with the MAGIC Cherenkov telescopes during a short observation (similar to 0.5 hr) performed on 2010 June 17. The MAGIC detection coincides with high-energy MeV/ GeV gamma-ray activity measured by the Large Area Telescope (LAT) on board the Fermi satellite. The VHE spectrum measured by MAGIC extends from about 70 GeV up to at least 400 GeV and can be well described by a power-law dN/dE proportional to E-Gamma with a photon index Gamma = 3.75 +/- 0.27(stat) +/- 0.2(syst). The averaged integral flux above 100 GeV is (4.6 +/- 0.5) x 10(-10) cm(-2) s(-1) (similar to 1 Crab Nebula flux). The VHE flux measured by MAGIC varies significantly within the 30 minute exposure implying a flux doubling time of about 10 minutes. The VHE and MeV/GeV spectra, corrected for the absorption by the extragalactic background light (EBL), can be described by a single power law with photon index 2.72 +/- 0.34 between 3 GeV and 400 GeV, and is consistent with emission belonging to a single component in the jet. The absence of a spectral cutoff constrains the gamma-ray emission region to lie outside the broad-line region, which would otherwise absorb the VHE gamma-rays. Together with the detected fast variability, this challenges present emission models from jets in FSRQs. Moreover, the combined Fermi/LAT and MAGIC spectral data yield constraints on the density of the EBL in the UV-optical to near-infrared range that are compatible with recent models.

引用

页数：6

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