野田浩司

Koji Noda

基本情報

所属: 千葉大学国際高等研究基幹准教授

J-GLOBAL ID: 201801008139951033
researchmap会員ID: B000306963

研究分野

自然科学一般 / 素粒子、原子核、宇宙線、宇宙物理にする実験 /

受賞

2022年2月

日本学術振興会賞日本学術振興会

論文

153

The variability patterns of the TeV blazar PG 1553+113 from a decade of MAGIC and multi-band observations

Abe, H., Abe, S., Abhir, J., Acciari, V.~A., Agudo, I., Aniello, T., Ansoldi, S., Antonelli, L.~A., Arbet Engels, A., Arcaro, C., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., Barres de Almeida, U., Batković, I., Baxter, J., Becerra González, J., Bernardini, E., Bernete, J., Berti, A., Besenrieder, J., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Burelli, I., Busetto, G., Campoy-Ordaz, A., Carosi, A., Carosi, R., Carretero-Castrillo, M., Castro-Tirado, A.~J., Chai, Y., Cifuentes, A., Cikota, S., Colombo, E., Contreras, J.~L., Cortina, J., Covino, S., D'Amico, G., D'Elia, V., da Vela, P., Dazzi, F., de Angelis, A., de Lotto, B., Del Popolo, A., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., di Pierro, F., di Venere, L., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Emery, G., Escudero, J., Fariña, L., Fattorini, A., Foffano, L., Font, L., Fukami, S., Fukazawa, Y., Garćıa López, R.~J., Gasparyan, S., Gaug, M., Giesbrecht Paiva, J.~G., Giglietto, N., Giordano, F., Gliwny, P., Grau, R., Green, J.~G., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hovatta, T., Hrupec, D., Hütten, M., Imazawa, R., Inada, T., Iotov, R., Ishio, K., Jiménez Mart́ınez, I., Jormanainen, J., Kerszberg, D., Kluge, G.~W., Kobayashi, Y., Kouch, P.~M., Kubo, H., Kushida, J., Láinez Lezáun, M., Lamastra, A., Leone, F., Lindfors, E., Liodakis, I., Lombardi, S., Longo, F., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Machado de Oliveira Fraga, B., Majumdar, P., Makariev, M., Maneva, G., Mang, N., Manganaro, M., Mannheim, K., Mariotti, M., Mart́ınez, M., Mart́ınez-Chicharro, M., Mas-Aguilar, A., Mazin, D., Menchiari, S., Mender, S., Miceli, D., Miener, T., Miranda, J.~M., Mirzoyan, R., Molero González, M., Molina, E., Mondal, H.~A., Moralejo, A., Morcuende, D., Nakamori, T., Nanci, C., Neustroev, V., Nigro, C., Nikolić, L., Nilsson, K., Nishijima, K., Ekoume, T. Njoh, Noda, K., Nozaki, S., Ohtani, Y., Okumura, A., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J.~M., Pavlović, D., Persic, M., Pihet, M., Pirola, G., Podobnik, F., Prada Moroni, P.~G., Prandini, E., Principe, G., Priyadarshi, C., Rhode, W., Ribó, M., Rico, J., Righi, C., Sahakyan, N., Saito, T., Satalecka, K., Saturni, F.~G., Schleicher, B., Schmidt, K., Schmuckermaier, F., Schubert, J.~L., Schweizer, T., Sciaccaluga, A., Sitarek, J., Spolon, A., Stamerra, A., Strišković, J., Strom, D., Suda, Y., Suutarinen, S., Tajima, H., Takeishi, R., Tavecchio, F., Temnikov, P., Terauchi, K., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Ventura, S., Verguilov, V., Viale, I., Vigorito, C.~F., Vitale, V., Walter, R., Wunderlich, C., Yamamoto, T., Jermak, H., Steele, I.~A., Smith, P.~S., Blinov, D., Raiteri, C.~M., Villata, M., Mirzaqulov, D.~O., Kurtanidze, S.~O., Carosati, D., Savchenko, S.~S., Acosta-Pulido, J.~A., Borman, G.~A., Bozhilov, V., Carnerero, M.~I., Chigladze, R.~A., Damljanovic, G., Ehgamberdiev, S.~A., Feige, M., Grishina, T.~S., Gupta, A.~C., Hagen-Thorn, V.~A., Ibryamov, S., Ivanidze, R.~Z., Jorstad, S.~G., Kania, J., Kimeridze, G.~N., Kopatskaya, E.~N., Kopp, M., Kunkel, L., Kurtanidze, O.~M., Larionov, V.~M., Larionova, E.~G., Larionova, L.~V., Lorey, C., Marchini, A., Marscher, A.~P., Minev, M., Morozova, D.~A., Nikolashvili, M.~G., Ovcharov, E., Reinhart, D., Sadun, A.~C., Scherbantin, A., Schneider, L., Semkov, E., Sigua, L.~A., Steineke, R., Troitskaya, Yu V., Troitskiy, I.~S., Valcheva, A., Vasilyev, A.~A., Vince, O., Zaharieva, E., Zottmann, N., Kiehlmann, S., Readhead, A., Max-Moerbeck, W., Reeves, R.~A., Sandrinelli, A., Fallah Ramazani, V., Giroletti, M., Righini, S., Marchili, N., Patricelli, B., Ghirlanda, G., Lico, R., MAGIC Collaboration

\mnras 529(4) 3894-3911 2024年3月

PG 1553 + 113 is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band. The source is also a very high energy (VHE; >100 GeV) gamma-ray emitter. To better understand its properties and identify the underlying physical processes driving its variability, the MAGIC Collaboration initiated a multiyear, multiwavelength monitoring campaign in 2015 involving the OVRO 40-m and Medicina radio telescopes, REM, KVA, and the MAGIC telescopes, Swift and Fermi satellites, and the WEBT network. The analysis presented in this paper uses data until 2017 and focuses on the characterization of the variability. The gamma-ray data show a (hint of a) periodic signal compatible with literature, but the X-ray and VHE gamma-ray data do not show statistical evidence for a periodic signal. In other bands, the data are compatible with the gamma-ray period, but with a relatively high p-value. The complex connection between the low- and high-energy emission and the non-monochromatic modulation and changes in flux suggests that a simple one-zone model is unable to explain all the variability. Instead, a model including a periodic component along with multiple emission zones is required.
Multi-year characterisation of the broad-band emission from the intermittent extreme BL Lac 1ES 2344+514

MAGIC Collaboration, Abe, H., Abe, S., Acciari, V.~A., Agudo, I., Aniello, T., Ansoldi, S., Antonelli, L.~A., Arbet Engels, A., Arcaro, C., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., Barres de Almeida, U., Batković, I., Baxter, J., Becerra González, J., Bernardini, E., Bernete, J., Berti, A., Besenrieder, J., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Burelli, I., Busetto, G., Campoy-Ordaz, A., Carosi, A., Carosi, R., Carretero-Castrillo, M., Castro-Tirado, A.~J., Chai, Y., Cifuentes, A., Cikota, S., Colombo, E., Contreras, J.~L., Cortina, J., Covino, S., D'Amico, G., D'Ammando, F., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Del Popolo, A., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., Di Pierro, F., Di Venere, L., Dominis Prester, D., Dorner, D., Doro, M., Elsaesser, D., Emery, G., Escudero, J., Fariña, L., Fattorini, A., Foffano, L., Font, L., Fukami, S., Fukazawa, Y., Garćıa López, R.~J., Gasparyan, S., Gaug, M., Giesbrecht Paiva, J.~G., Giglietto, N., Giordano, F., Gliwny, P., Grau, R., Green, J.~G., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hrupec, D., Hütten, M., Imazawa, R., Inada, T., Iotov, R., Ishio, K., Jiménez Mart́ınez, I., Jormanainen, J., Kerszberg, D., Kluge, G.~W., Kobayashi, Y., Kouch, P.~M., Kubo, H., Kushida, J., Láinez Lezáun, M., Lamastra, A., Leone, F., Lindfors, E., Linhoff, L., Lombardi, S., Longo, F., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Machado de Oliveira Fraga, B., Majumdar, P., Makariev, M., Maneva, G., Mang, N., Manganaro, M., Mariotti, M., Mart́ınez, M., Mart́ınez-Chicharro, M., Mas-Aguilar, A., Mazin, D., Menchiari, S., Mender, S., Miceli, D., Miener, T., Miranda, J.~M., Mirzoyan, R., Molero González, M., Molina, E., Mondal, H.~A., Moralejo, A., Morcuende, D., Nakamori, T., Nanci, C., Neustroev, V., Nigro, C., Nikolić, L., Nishijima, K., Njoh Ekoume, T., Noda, K., Nozaki, S., Ohtani, Y., Okumura, A., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J.~M., Pavlović, D., Persic, M., Pihet, M., Pirola, G., Podobnik, F., Prada Moroni, P.~G., Prandini, E., Principe, G., Priyadarshi, C., Rhode, W., Ribó, M., Rico, J., Righi, C., Sahakyan, N., Saito, T., Satalecka, K., Saturni, F.~G., Schleicher, B., Schmidt, K., Schmuckermaier, F., Schubert, J.~L., Schweizer, T., Sciaccaluga, A., Sitarek, J., Spolon, A., Stamerra, A., Strišković, J., Strom, D., Suda, Y., Tajima, H., Takeishi, R., Tavecchio, F., Temnikov, P., Terauchi, K., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Ventura, S., Verguilov, V., Viale, I., Vigorito, C.~F., Vitale, V., Walter, R., Wunderlich, C., Yamamoto, T., Multi-wavelength Collaborators, Perri, M., Verrecchia, F., Leto, C., Das, S., Chatterjee, R., Raiteri, C.~M., Villata, M., Semkov, E., Ibryamov, S., Bachev, R., Strigachev, A., Damljanovic, G., Vince, O., Jovanovic, M.~D., Stojanovic, M., Larionov, V.~M., Grishina, T.~S., Kopatskaya, E.~N., Larionova, E.~G., Morozova, D.~A., Savchenko, S.~S., Troitskiy, I.~S., Troitskaya, Y.~V., Vasilyev, A.~A., Chen, W.~P., Hou, W.~J., Lin, C.~S., Tsai, A., Jorstad, S.~G., Weaver, Z.~R., Acosta-Pulido, J.~A., Carnerero, M.~I., Carosati, D., Kurtanidze, S.~O., Kurtanidze, O.~M., Jordan, B., Ivanidze, R.~Z., Gazeas, K., Vrontaki, K., Hovatta, T., Liodakis, I., Readhead, A.~C.~S., Kiehlmann, S., Zheng, W., Filippenko, A.~V., Fallah Ramazani, V.

åp 682 2024年2月

Aims. The BL Lac 1ES 2344+514 is known for temporary extreme properties characterised by a shift of the synchrotron spectral energy distribution (SED) peak energy νsynch;p above 1 keV. While those extreme states have only been observed during high flux levels thus far, additional multi-year observing campaigns are required to achieve a coherent picture. Here, we report the longest investigation of the source from radio to very high energy (VHE) performed so far, focussing on a systematic characterisation of the intermittent extreme states. Methods.We organised a monitoring campaign covering a 3-year period from 2019 to 2021.Morethan ten instruments participated in the observations in order to cover the emission from radio to VHE. In particular, sensitive X-ray measurements by XMM-Newton, NuSTAR, and AstroSat took place simultaneously with multi-hour MAGIC observations, providing an unprecedented constraint of the two SED components for this blazar. Results. While our results confirm that 1ES 2344+514 typically exhibits νsynch;p > 1 keV during elevated flux periods, we also find periods where the extreme state coincides with low flux activity. A strong spectral variability thus happens in the quiescent state, and is likely caused by an increase in the electron acceleration efficiency without a change in the electron injection luminosity. On the other hand, we also report a strong X-ray flare (among the brightest for 1ES 2344+514) without a significant shift of νsynch;p. During this particular flare, the X-ray spectrum is among the softest of the campaign. It unveils complexity in the spectral evolution, where the common harder-when-brighter trend observed in BL Lacs is violated. By combining Swift-XRT and Swift-UVOT measurements during a low and hard X-ray state, we find an excess of the UV flux with respect to an extrapolation of the X-ray spectrum to lower energies. This UV excess implies that at least two regions significantly contribute to the infrared/optical/ultraviolet/X-ray emission. Using the simultaneous MAGIC, XMM-Newton, NuSTAR, and AstroSat observations, we argue that a region possibly associated with the 10 GHz radio core may explain such an excess. Finally, we investigate a VHE flare, showing an absence of simultaneous variability in the 0.3-2 keV band. Using time-dependent leptonic modelling, we show that this behaviour, in contradiction to single-zone scenarios, can instead be explained by a two-component model.
Combined searches for dark matter in dwarf spheroidal galaxies observed with the MAGIC telescopes, including new data from Coma Berenices and Draco

V.A. Acciari, S. Ansoldi, L.A. Antonelli, A. Arbet Engels, M. Artero, K. Asano, D. Baack, A. Babić, A. Baquero, U. Barres de Almeida, J.A. Barrio, I. Batković, J. Becerra González, W. Bednarek, L. Bellizzi, E. Bernardini, M. Bernardos, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, H. Bökenkamp, G. Bonnoli, Ž. Bošnjak, G. Busetto, R. Carosi, G. Ceribella, M. Cerruti, Y. Chai, A. Chilingarian, S. Cikota, S.M. Colak, E. Colombo, J.L. Contreras, J. Cortina, S. Covino, G. D’Amico, V. D’Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, C. Delgado Mendez, D. Depaoli, F. Di Pierro, L. Di Venere, E. Do Souto Espiñeira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, M.V. Fonseca, L. Font, C. Fruck, S. Fukami, R.J. García López, M. Garczarczyk, S. Gasparyan, M. Gaug, N. Giglietto, F. Giordano, P. Gliwny, N. Godinović, J.G. Green, D. Green, D. Hadasch, A. Hahn, L. Heckmann, J. Herrera, J. Hoang, D. Hrupec, M. Hütten, T. Inada, K. Ishio, Y. Iwamura, I. Jiménez, J. Jormanainen, L. Jouvin, M. Karjalainen, D. Kerszberg, Y. Kobayashi, H. Kubo, J. Kushida, A. Lamastra, D. Lelas, F. Leone, E. Lindfors, L. Linhoff, S. Lombardi, F. Longo, R. López-Coto, M. López-Moya, A. López-Oramas, S. Loporchio, B. Machado de Oliveira Fraga, C. Maggio, P. Majumdar, M. Makariev, M. Mallamaci, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, S. Menchiari, S. Mender, S. Mićanović, D. Miceli, T. Miener, J.M. Miranda, R. Mirzoyan, E. Molina, A. Moralejo, D. Morcuende, V. Moreno, E. Moretti, V. Neustroev, C. Nigro, K. Nilsson, D. Ninci, K. Nishijima, K. Noda, S. Nozaki, Y. Ohtani, T. Oka, J. Otero-Santos, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J.M. Paredes, L. Pavletić, P. Peñil, M. Persic, M. Pihet, P.G. Prada Moroni, E. Prandini, C. Priyadarshi, I. Puljak, W. Rhode, M. Ribó, J. Rico, C. Righi, A. Rugliancich, L. Saha, N. Sahakyan, T. Saito, S. Sakurai, K. Satalecka, F.G. Saturni, B. Schleicher, K. Schmidt, T. Schweizer, J. Sitarek, I. Šnidarić, D. Sobczynska, A. Spolon, A. Stamerra, J. Strišković, D. Strom, M. Strzys, Y. Suda, T. Surić, M. Takahashi, R. Takeishi, F. Tavecchio, P. Temnikov, T. Terzić, M. Teshima, L. Tosti, S. Truzzi, A. Tutone, S. Ubach, J. van Scherpenberg, G. Vanzo, M. Vazquez Acosta, S. Ventura, V. Verguilov, C.F. Vigorito, V. Vitale, I. Vovk, M. Will, C. Wunderlich, D. Zarić

Physics of the Dark Universe 35 100912-100912 2022年3月査読有り
First detection of VHE gamma-ray emission from TXS 1515-273, study of its X-ray variability and spectral energy distribution

V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, M. Artero, K. Asano, D. Baack, A. Babić, A. Baquero, U. Barres De Almeida, J. A. Barrio, I. Batković, J. Becerra González, W. Bednarek, L. Bellizzi, E. Bernardini, M. Bernardos, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, Bošnjak, G. Busetto, R. Carosi, G. Ceribella, M. Cerruti, Y. Chai, A. Chilingarian, S. Cikota, S. M. Colak, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, G. D'Amico, V. D'Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, C. Delgado Mendez, D. Depaoli, F. Di Pierro, L. Di Venere, E. Do Souto Espiñeira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, G. Ferrara, M. V. Fonseca, L. Font, C. Fruck, S. Fukami, R. J. García López, M. Garczarczyk, S. Gasparyan, M. Gaug, N. Giglietto, F. Giordano, P. Gliwny, N. Godinović, J. G. Green, D. Green, D. Hadasch, A. Hahn, L. Heckmann, J. Herrera, J. Hoang, D. Hrupec, M. Hütten, T. Inada, S. Inoue, K. Ishio, Y. Iwamura, I. Jiménez, J. Jormanainen, L. Jouvin, Y. Kajiwara, M. Karjalainen, D. Kerszberg, Y. Kobayashi, H. Kubo, J. Kushida, A. Lamastra, D. Lelas, F. Leone, E. Lindfors, S. Lombardi, F. Longo, R. López-Coto, M. López-Moya, A. López-Oramas, S. Loporchio, B. Machado De Oliveira Fraga, C. Maggio, P. Majumdar, M. Makariev, M. Mallamaci, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, S. Menchiari, S. Mender, S. Micánović, D. Miceli, T. Miener, M. Minev, J. M. Miranda, R. Mirzoyan, E. Molina, A. Moralejo, D. Morcuende, V. Moreno, E. Moretti, V. Neustroev, C. Nigro, K. Nilsson, K. Nishijima, K. Noda, S. Nozaki, Y. Ohtani, T. Oka, J. Otero-Santos, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, L. Pavletić, P. Peñil, C. Perennes, M. Persic, P. G. Prada Moroni, E. Prandini, C. Priyadarshi, I. Puljak, W. Rhode, M. Ribó, J. Rico, C. Righi, A. Rugliancich, L. Saha, N. Sahakyan, T. Saito, S. Sakurai, K. Satalecka, F. G. Saturni, B. Schleicher, K. Schmidt, T. Schweizer, J. Sitarek, I. Šnidarić, D. Sobczynska, A. Spolon, A. Stamerra, D. Strom, M. Strzys, Y. Suda, T. Surić, M. Takahashi, F. Tavecchio, P. Temnikov, T. Terzić, M. Teshima, L. Tosti, S. Truzzi, A. Tutone, S. Ubach, J. Van Scherpenberg, G. Vanzo, M. Vazquez Acosta, S. Ventura, V. Verguilov, C. F. Vigorito, V. Vitale, I. Vovk, M. Will, C. Wunderlich, D. Zarić, E. Bissaldi, G. Bonnoli, S. Cutini, F. D'Ammando, A. Nabizadeh, A. Marchini, M. Orienti, MAGIC Collaboration

Monthly Notices of the Royal Astronomical Society 507(1) 1528-1545 2021年10月1日

We report here on the first multiwavelength (MWL) campaign on the blazar TXS 1515-273, undertaken in 2019 and extending from radio to very-high-energy gamma-rays (VHE). Up until now, this blazar had not been the subject of any detailed MWL observations. It has a rather hard photon index at GeV energies and was considered a candidate extreme high-synchrotron-peaked source. MAGIC observations resulted in the first-time detection of the source in VHE with a statistical significance of 7.6σ. The average integral VHE flux of the source is 6 ± 1 per cent of the Crab nebula flux above 400 GeV. X-ray coverage was provided by Swift-XRT, XMM-Newton, and NuSTAR. The long continuous X-ray observations were separated by ∼9 h, both showing clear hour scale flares. In the XMM-Newton data, both the rise and decay time-scales are longer in the soft X-ray than in the hard X-ray band, indicating the presence of a particle cooling regime. The X-ray variability time-scales were used to constrain the size of the emission region and the strength of the magnetic field. The data allowed us to determine the synchrotron peak frequency and classify the source as a flaring high, but not extreme synchrotron-peaked object. Considering the constraints and variability patterns from the X-ray data, we model the broad-band spectral energy distribution. We applied a simple one-zone model, which could not reproduce the radio emission and the shape of the optical emission, and a two-component leptonic model with two interacting components, enabling us to reproduce the emission from radio to VHE band.
VHE gamma-ray detection of FSRQ QSO B1420+326 and modeling of its enhanced broadband state in 2020

V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, M. Artero, K. Asano, D. Baack, A. Babic, A. Baquero, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, L. Bellizzi, E. Bernardini, M. Bernardos, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, Z. Bosnjak, G. Busetto, R. Carosi, G. Ceribella, M. Cerruti, Y. Chai, A. Chilingarian, S. Cikota, S. M. Colak, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, G. D'Amico, V. D'Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, C. Delgado Mendez, D. Depaoli, F. Di Pierro, L. Di Venere, E. Do Souto Espineira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, G. Ferrara, L. Foffano, M. V. Fonseca, L. Font, C. Fruck, S. Fukami, R. J. Garcia Lopez, M. Garczarczyk, S. Gasparyan, M. Gaug, N. Giglietto, F. Giordano, P. Gliwny, N. Godinovic, J. G. Green, D. Green, D. Hadasch, A. Hahn, L. Heckmann, J. Herrera, J. Hoang, D. Hrupec, M. Hutten, T. Inada, S. Inoue, K. Ishio, Y. Iwamura, J. Jormanainen, L. Jouvin, Y. Kajiwara, M. Karjalainen, D. Kerszberg, Y. Kobayashi, H. Kubo, J. Kushida, A. Lamastra, D. Lelas, F. Leone, E. Lindfors, S. Lombardi, F. Longo, R. Lopez-Coto, M. Lopez-Moya, A. Lopez-Oramas, S. Loporchio, B. Machado de Oliveira Fraga, C. Maggio, P. Majumdar, M. Makariev, M. Mallamaci, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martinez, D. Mazin, S. Mender, S. Micanovic, D. Miceli, T. Miener, M. Minev, J. M. Miranda, R. Mirzoyan, E. Molina, A. Moralejo, D. Morcuende, V. Moreno, E. Moretti, V. Neustroev, C. Nigro, K. Nilsson, D. Ninci, K. Nishijima, K. Noda, S. Nozaki, Y. Ohtani, T. Oka, J. Otero-Santos, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, L. Pavletic, P. Penil, C. Perennes, M. Persic, P. G. Prada Moroni, E. Prandini, C. Priyadarshi, I. Puljak, W. Rhode, M. Ribo, J. Rico, C. Righi, A. Rugliancich, L. Saha, N. Sahakyan, T. Saito, S. Sakurai, K. Satalecka, F. G. Saturni, B. Schleicher, K. Schmidt, T. Schweizer, J. Sitarek, I. Snidaric, D. Sobczynska, A. Spolon, A. Stamerra, D. Strom, M. Strzys, Y. Suda, T. Suric, M. Takahashi, F. Tavecchio, P. Temnikov, T. Terzic, M. Teshima, N. Torres-Alba, L. Tosti, S. Truzzi, A. Tutone, J. van Scherpenberg, G. Vanzo, M. Vazquez Acosta, S. Ventura, V. Verguilov, C. F. Vigorito, V. Vitale, I. Vovk, M. Will, D. Zaric, R. Angioni, F. D'Ammando, S. Ciprini, C. C. Cheung, M. Orienti, L. Pacciani, P. Prajapati, P. Kumar, S. Ganesh, M. Minev, A. Kurtenkov, A. Marchini, L. Carrasco, G. Escobedo, A. Porras, E. Recillas, A. Lahteenmaki, M. Tornikoski, M. Berton, J. Tammi, R. J. C. Vera, S. G. Jorstad, A. P. Marscher, Z. R. Weaver, M. Hart, M. K. Hallum, V. M. Larionov, G. A. Borman, T. S. Grishina, E. N. Kopatskaya, E. G. Larionova, A. A. Nikiforova, D. A. Morozova, S. S. Savchenko, Yu. V. Troitskaya, I. S. Troitsky, A. A. Vasilyev, M. Hodges, T. Hovatta, S. Kiehlmann, W. Max-Moerbeck, A. C. S. Readhead, R. Reeves, T. J. Pearson

ASTRONOMY & ASTROPHYSICS 647 2021年3月査読有り

Context. QSO B1420+326 is a blazar classified as a flat-spectrum radio quasar (FSRQ). At the beginning of the year 2020, it was found to be in an enhanced flux state and an extensive multiwavelength campaign allowed us to trace the evolution of the flare.Aims. We search for very high-energy (VHE) gamma-ray emission from QSO B1420+326 during this flaring state. We aim to characterize and model the broadband emission of the source over different phases of the flare.Methods. The source was observed with a number of instruments in radio, near-infrared, optical (including polarimetry and spectroscopy), ultraviolet, X-ray, and gamma-ray bands. We use dedicated optical spectroscopy results to estimate the accretion disk and the dust torus luminosity. We performed spectral energy distribution modeling in the framework of combined synchrotron-self-Compton and external Compton scenario in which the electron energy distribution is partially determined from acceleration and cooling processes.Results. During the enhanced state, the flux of both SED components of QSO B1420+326 drastically increased and the peaks were shifted to higher energies. Follow-up observations with the MAGIC telescopes led to the detection of VHE gamma-ray emission from this source, making it one of only a handful of FSRQs known in this energy range. Modeling allows us to constrain the evolution of the magnetic field and electron energy distribution in the emission region. The gamma-ray flare was accompanied by a rotation of the optical polarization vector during a low -polarization state. Also, a new superluminal radio knot contemporaneously appeared in the radio image of the jet. The optical spectroscopy shows a prominent FeII bump with flux evolving together with the continuum emission and a MgII line with varying equivalent width.

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MAGIC detection of short-term variability of the high-peaked BL Lac object lES 0806+524

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, E. de Ona Wilhelmi, C. Delgado Mendez, F. Di Pierro, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, A. Fernandez-Barral, D. Fidalgo, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, Y. Hanabata, M. Hayashida, J. Herrera, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, M. L. Knoetig, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, F. Longo, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, V. Neustroev, A. Niedzwiecki, M. Nievas Rosillo, K. Nilsson, K. Nishijima, K. Noda, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, M. Persic, J. Poutanen, P. G. Prada Moroni, E. Prandini, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, A. Stamerra, T. Steinbring, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, D. F. Torres, T. Toyama, A. Treves, P. Vogler, M. Will, R. Zanin, K. Berger, S. Buson, F. D'Ammando, D. Gasparrini, T. Hovatta, W. Max-Moerbeck, A. Readhead, J. Richards

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 451(1) 739-750 2015年7月

The high-frequency-peaked BL Lac (HBL) 1ES 0806+524 (z = 0.138) was discovered in very high energy (VHE) gamma-rays in 2008. Until now, the broad-band spectrum of lES 0806+524 has been only poorly characterized, in particular at high energies. We analysed multiwave-length observations from gamma-rays to radio performed from 2011 January to March, which were triggered by the high activity detected at optical frequencies. These observations constitute the most precise determination of the broad-band emission of ES 0806+524 to date. The stereoscopic Major Atmospheric Gamma-Ray Imaging Cherenkov (MAGIC) observations yielded a gamma-ray signal above 250 GeV of (3.7 +/- 0.7) per cent of the Crab Nebula flux with a statistical significance of 9.9a. The multiwavelength observations showed significant variability in essentially all energy bands, including a VHE gamma-ray flare that lasted less than one night, which provided unprecedented evidence for short-term variability in lES 0806+524. The spectrum of this flare is well described by a power law with a photon index of 2.97 +/- 0.29 between similar to 150 GeV and 1 TeV and an integral flux of (9.3 +/- 1.9) per cent of the Crab nebula flux above 250 GeV. The spectrum during the non-flaring VHE activity is compatible with the only available VHE observation performed in 2008 with VERITAS when the source was in a low optical state. The broad-band spectral energy distribution can be described with a one-zone synchrotron self-Compton model with parameters typical for HBLs, indicating that lES 0806+524 is not substantially different from the HBLs previously detected.
Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010

J. Aleksi, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, A. Boller, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, E. de Ona Wilhelmi, C. Delgado Mendez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, Y. Hanabata, M. Hayashida, J. Herrera, D. Hildebrand, J. Hose, D. Hrupec, G. Hughes, W. Idec, V. Kadenius, H. Kellermann, M. L. Knoetig, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, M. Persic, P. G. Prada Moroni, E. Prandini, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Rugamer, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. Sun, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, B. Steinke, J. Storz, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. Zanin, S. Archambault, A. Archer, M. Beilicke, W. Benbow, K. Berger, R. Bird, J. Biteau, J. H. Buckley, V. Bugaev, M. Cerruti, X. Chen, L. Ciupik, E. Collins-Hughes, W. Cui, J. D. Eisch, A. Falcone, Q. Feng, J. P. Finley, P. Fortin, L. Fortson, A. Furniss, N. Galante, G. H. Gillanders, S. Griffin, G. Gyuk, N. Hakansson, J. Holder, C. A. Johnson, P. Kaaret, P. Kar, M. Kertzman, D. Kieda, M. J. Lang, S. McArthur, A. McCann, K. Meagher, J. Millis, P. Moriarty, R. A. Ong, A. N. Otte, J. S. Perkins, A. Pichel, M. Pohl, A. Popkow, H. Prokoph, E. Pueschel, K. Ragan, L. C. Reyes, P. T. Reynolds, G. T. Richards, E. Roache, A. C. Rovero, G. H. Sembroski, K. Shahinyan, D. Staszak, I. Telezhinsky, J. V. Tucci, J. Tyler, A. Varlotta, S. P. Wakely, R. Welsing, A. Wilhelm, D. A. Williams, S. Buson, J. Finke, M. Villata, C. Raiteri, H. D. Aller, M. F. Aller, A. Cesarini, W. P. Chen, M. A. Gurwell, S. G. Jorstad, G. N. Kimeridze, E. Koptelova, O. M. Kurtanidze, S. O. Kurtanidze, A. Lahteenmaki, V. M. Larionov, E. G. Larionova, H. C. Lin, B. McBreen, J. W. Moody, D. A. Morozova, A. P. Marscher, W. Max-Moerbeck, M. G. Nikolashvili, M. Perri, A. C. S. Readhead, J. L. Richards, J. A. Ros, A. C. Sadun, T. Sakamoto, L. A. Sigua, P. S. Smith, M. Tornikoski, I. S. Troitsky, A. E. Wehrle, B. Jordan

ASTRONOMY & ASTROPHYSICS 578 2015年6月

Context. Because of its proximity, Mrk 421 is one of the best sources on which to study the nature of BL Lac objects. Its proximity allows us to characterize its broadband spectral energy distribution (SED). Aims. The goal is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk 421. These mechanisms may also apply to more distant blazars that cannot be studied with the same level of detail. Methods. A flare occurring in March 2010 was observed for 13 consecutive days (from MJD 55 265 to MJD 55 277) with unprecedented wavelength coverage from radio to very high energy (VHE; E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, Fermi-LAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We modeled the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigated the physical parameters, and evaluated whether the observed broadband SED variability can be associated with variations in the relativistic particle population. Results. The activity of Mrk 421 initially was high and then slowly decreased during the 13-day period. The flux variability was remarkable at the X-ray and VHE bands, but it was minor or not significant at the other bands. The variability in optical polarization was also minor. These observations revealed an almost linear correlation between the X-ray flux at the 2-10 keV band and the VHE gamma-ray flux above 200 GeV, consistent with the gamma-rays being produced by inverse-Compton scattering in the Klein-Nishina regime in the framework of SSC models. The one-zone SSC model can describe the SED of each day for the 13 consecutive days reasonably well, which once more shows the success of this standard theoretical scenario to describe the SEDs of VHE BL Lacs such as Mrk 421. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission, while the other smaller zone, which is spatially separated from the first, contributes to the daily variable emission occurring at X-rays and VHE gamma-rays. The second blob is assumed to have a smaller volume and a narrow electron energy distribution with 3 x 10(4) < gamma < 6 x 10(5), where. is the Lorentz factor of the electrons. Such a two-zone scenario would naturally lead to the correlated variability at the X-ray and VHE bands without variability at the optical/UV band, as well as to shorter timescales for the variability at the X-ray and VHE bands with respect to the variability at the other bands. Conclusions. Both the one-zone and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly with the underlying particle population. This shows that the particle acceleration and cooling mechanism that produces the radiating particles might be the main mechanism responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement with the observed SED at the narrow peaks of the low-and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by varying the parameters related to the emitting region itself (delta, B and R), in addition to the parameters related to the particle population.
MAGIC observations of MWC 656, the only known Be/BH system

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, E. de Ona Wilhelmi, C. Delgado Mendez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, D. Fidalgo, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, Y. Hanabata, M. Hayashida, J. Herrera, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, M. L. Knoetig, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, F. Longo, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, V. Neustroev, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, M. Persic, J. Poutanen, P. G. Prada Moroni, E. Prandini, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, P. Vogler, M. Will, R. Zanin, J. Casares, J. Moldon

ASTRONOMY & ASTROPHYSICS 576 2015年4月

Context. MWC 656 has recently been established as the first observationally detected high-mass X-ray binary system containing a Be star and a black hole (BH). The system has been associated with a gamma-ray flaring event detected by the AGILE satellite in July 2010. Aims. Our aim is to evaluate whether the MWC 656 gamma-ray emission extends to very high energy (VHE > 100 GeV) gamma rays. Methods. We observed MWC 656 with the MAGIC telescopes for similar to 23 h during two observation periods: between May and June 2012, and in June 2013. During the last period, observations were performed contemporaneously with X-ray (XMM-Newton) and optical (STELLA) instruments. Results. We did not detect the MWC 656 binary system at TeV energies with the MAGIC telescopes in either of the two campaigns. Upper limits (ULs) to the integral flux above 300 GeV have been set, as well as differential ULs at a level of similar to 5% of the Crab nebula flux. The results obtained from the MAGIC observations do not support persistent emission of VHE gamma rays from this system at a level of 2.4% the Crab flux.
Measurement of the Crab Nebula spectrum over three decades in energy with the MAGIC telescopes

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, E. de Ona Wilhelmi, C. Delgado Mendez, M. Doert, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, Y. Hanabata, M. Hayashida, J. Herrera, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, M. Persic, P. G. Prada Moroni, E. Prandini, S. Preziuso, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Rugamer, A. Saggion, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpuaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. M. Wagner, R. Zanin, D. Horns, J. Martin, M. Meyer

JOURNAL OF HIGH ENERGY ASTROPHYSICS 5-6 30-38 2015年3月

The MAGIC stereoscopic system collected 69 hours of Crab Nebula data between October 2009 and April 2011. Analysis of this data sample using the latest improvements in the MAGIC stereoscopic software provided an unprecedented precision of spectral and night-by-night light curve determination at gamma rays. We derived a differential spectrum with a single instrument from 50 GeV up to almost 30 TeV with 5 bins per energy decade. At low energies, MAGIC results, combined with Fermi-LAT data, show a flat and broad Inverse Compton peak. The overall fit to the data between 1 GeV and 30 TeV is not well described by a log-parabola function. We find that a modified log-parabola function with an exponent of 2.5 instead of 2 provides a good description of the data (chi(2)(red) = 35/26). Using systematic uncertainties of the MAGIC and Fermi-LAT measurements we determine the position of the Inverse Compton peak to be at (53 +/- 3(stat)+ 31(syst)-13(syst)) GeV, which is the most precise estimation up to date and is dominated by the systematic effects. There is no hint of the integral flux variability on daily scales at energies above 300 GeV when systematic uncertainties are included in the flux measurement. We consider three state-of-the-art theoretical models to describe the overall spectral energy distribution of the Crab Nebula. The constant B-field model cannot satisfactorily reproduce the VHE spectral measurements presented in this work, having particular difficulty reproducing the broadness of the observed IC peak. Most probably this implies that the assumption of the homogeneity of the magnetic field inside the nebula is incorrect. On the other hand, the time-dependent 1D spectral model provides a good fit of the new VHE results when considering a 80 mu G magnetic field. However, it fails to match the data when including the morphology of the nebula at lower wavelengths. (C) 2015 Elsevier B.V. All rights reserved.
MAGIC報告52:Mrk501多波長観測(2011年他)

野田浩司, 池野祐平, 石尾一馬, 井上進, 岩村由樹, 折戸玲子, 加藤翔, 櫛田淳子, 窪秀利, 今野裕介, 齋藤隆之, 齋藤隆之, 高橋光成, 谷川俊介, 辻本晋平, 手嶋政廣, 手嶋政廣, 遠山健, 中嶋大輔, 永吉勤, 西嶋恭司, HADASCH Daniela, 林田将明, 平井亘, 深見哲志, 増田周, MAZIN Daniel, MAZIN Daniel, 吉田麻佑, BIASUZZI Barbara, BIASUZZI Barbara, PANEQUE David

日本物理学会講演概要集(CD-ROM) 70(2) 2015年
First broadband characterization and redshift determination of the VHE blazar MAGIC J2001+439

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, D. Carreto Fidalgo, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, C. Delgado Mendez, M. Doert, A. Dominguez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, E. Farina, D. Ferenc, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, M. Hayashida, J. Herrera, A. Herrero, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, M. Meucci, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, S. Partini, M. Persic, F. Prada, P. G. Prada Moroni, E. Prandini, S. Preziuso, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, A. Saggion, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, S. Sun, T. Suric, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. M. Wagner, F. Zandanel, R. Zanin, F. D'Ammando, T. Hovatta, V. M. Larionov, W. Max-Moerbeck, M. Perri, A. C. S. Readhead, J. L. Richards, T. Sakamoto, R. D. Schwartz, F. Verrecchia, L. C. Reyes

ASTRONOMY & ASTROPHYSICS 572 2014年12月

Aims. We aim to characterize the broadband emission from 2FGL J2001.1+4352, which has been associated with the unknown-redshift blazar MG4 J200112+4352. Based on its gamma-ray spectral properties, it was identified as a potential very high energy (VHE; E > 100 GeV) gamma-ray emitter. We investigate whether this object is a VHE emitter, characterize its gamma-ray spectrum, and study the broadband emission within the one-zone synchrotron self-Compton (SSC) scenario, which is commonly used to describe the emission in blazars. Moreover, we also intend to determine the redshift of this object, which is a crucial parameter for its scientific interpretation. Methods. The source was observed with MAGIC first in 2009 and later in 2010 within a multi-instrument observation campaign. The MAGIC observations yielded 14.8 h of good quality stereoscopic data. Besides MAGIC, the campaign involved, observations with Fermi-LAT, Swift-XRT/UVOT, the optical telescopes KVA, Goddard Robotic Telescope, Galaxy View observatory, Crimean Astrophysical observatory, St. Petersburg observatory, and the Owens Valley Radio Observatory. The object was monitored at radio, optical and gamma-ray energies during the years 2010 and 2011. We characterize the radio to VHE spectral energy distribution and quantify the multiband variability and correlations over short (few days) and long (many months) timescales. We also organized deep imaging optical observations with the Nordic Optical Telescope in 2013 to determine the source redshift. Results. The source, named MAGIC J2001+ 439, is detected for the first time at VHE with MAGIC at a statistical significance of 6.3s (E > 70 GeV) during a 1.3 h long observation on 2010 July 16. The multi-instrument observations show variability in all energy bands with the highest amplitude of variability in the X-ray and VHE bands. Besides the variability on few-day timescales, the long-term monitoring of MAGIC J2001+ 439 shows that, the gamma-ray, optical, and radio emissions gradually decreased on few-month timescales from 2010 through 2011, indicating that at least some of the radio, optical and gamma-ray emission is produced in a single region by the same population of particles. We also determine for the first time the redshift of this BL Lac object through the measurement of its host galaxy during low blazar activity. Using the observational evidence that the luminosities of BL Lac host galaxies are confined to a relatively narrow range, we obtain z = 0.18 +/- 0.04. Additionally, we use the Fermi-LAT and MAGIC gamma-ray spectra to provide an independent redshift estimation, z = 0.17 +/- 0.10. Using the former (more accurate) redshift value, we adequately describe the broadband emission with a one-zone SSC model for different activity states and interpret the few-day timescale variability as produced by changes in the high-energy component of the electron energy distribution.
MAGIC reveals a complex morphology within the unidentified gamma-ray source HESS J1857+026

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, D. Carreto Fidalgo, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, C. Delgado Mendez, M. Doert, A. Dominguez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, E. Farina, D. Ferenc, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, M. Hayashida, J. Herrera, A. Herrero, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, S. Klepser, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, M. Meucci, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, E. de Ona Wilhelmi, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, S. Partini, M. Persic, F. Prada, P. G. Prada Moroni, E. Prandini, S. Preziuso, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, A. Saggion, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, S. Sun, T. Suric, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. M. Wagner, F. Zandanel, R. Zanin

ASTRONOMY & ASTROPHYSICS 571 2014年11月

Aims. HESS J1857+026 is an extended TeV gamma-ray source that was discovered by H. E. S. S. as part of its Galactic plane survey. Given its broadband spectral energy distribution and its spatial coincidence with the young energetic pulsar PSR J1856+0245, the source has been put forward as a pulsar wind nebula (PWN) candidate. MAGIC has performed follow-up observations aimed at mapping the source down to energies approaching 100 GeV in order to better understand its complex morphology. Methods. HESS J1857+026 was observed by MAGIC in 2010, yielding 29 h of good quality stereoscopic data that allowed us to map the source region in two separate ranges of energy. Results. We detected very-high-energy gamma-ray emission from HESS J1857+026 with a significance of 12 sigma above 150 GeV. The differential energy spectrum between 100 GeV and 13 TeV is described well by a power law function dN/dE = N-0(E/1TeV)(-Gamma) with N-0 = (5.37 +/- 0.44(stat) +/- 1.5(sys)) X 10(-12) (TeV-1 cm(-2) s(-1)) and Gamma = 2.16 +/- 0.07(stat) +/- 0.15(sys), which bridges the gap between the GeV emission measured by Fermi-LAT and the multi-TeV emission measured by H.E.S.S.. In addition, we present a detailed analysis of the energy-dependent morphology of this region. We couple these results with archival multiwavelength data and outline evidence in favor of a two-source scenario, whereby one source is associated with a PWN, while the other could be linked with a molecular cloud complex containing an HII region and a possible gas cavity.
Black hole lightning due to particle acceleration at subhorizon scales

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, E. de Ona Wilhelmi, C. Delgado Mendez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, Y. Hanabata, M. Hayashida, J. Herrera, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, F. Longo, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, M. Persic, J. Poutanen, P. G. Prada Moroni, E. Prandini, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. Zanin, M. Kadler, R. Schulz, E. Ros, U. Bach, F. Krauss, J. Wilms

SCIENCE 346(6213) 1080-1084 2014年11月

Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet.
Discovery of very high energy gamma-ray emission from the blazar 1ES 0033+595 by the MAGIC telescopes

J. Aleksić, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres, de Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, K. Berger, E. Bernardini, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, D. Carreto Fidalgo, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, C. Delgado Mendez, M. Doert, A. Domínguez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, E. Farina, D. Ferenc, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, R. J, García López, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinović, A. González Muñoz, S. R. Gozzini, D. Hadasch, M. Hayashida, J. Herrera, A. Herrero, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. López, R. López-Coto, A. López-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martínez, D. Mazin, U. Menzel, M. Meucci, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, S. Partini, M. Persic, F. Prada, P. G, Prada Moroni, E. Prandini, S. Preziuso, I. Puljak, R. Reinthal, W. Rhode, M. Ribó, J. Rico, J. Rodriguez Garcia, S. Rügamer, A. Saggion, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpää, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, S. Sun, T. Surić, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzić, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. M. Wagner, F. Zandanel, R. Zanin, V. Tronconi, S. Buson

2014年10月27日

The number of known very high energy (VHE) blazars is $\sim\,50$, which is very small in comparison to the number of blazars detected in other frequencies. This situation is a handicap for population studies of blazars, which emit about half of their luminosity in the $\gamma$-ray domain. Moreover, VHE blazars, if distant, allow for the study of the environment that the high-energy $\gamma$-rays traverse in their path towards the Earth, like the extragalactic background light (EBL) and the intergalactic magnetic field (IGMF), and hence they have a special interest for the astrophysics community. We present the first VHE detection of 1ES\,0033+595 with a statistical significance of 5.5\,$\sigma$. The VHE emission of this object is constant throughout the MAGIC observations (2009 August and October), and can be parameterized with a power law with an integral flux above 150 GeV of $(7.1\pm1.3)\times 10^{-12} {\mathrm{ph\,cm^{-2}\,s^{-1 } }}$ and a photon index of ($3.8\pm0.7$). We model its spectral energy distribution (SED) as the result of inverse Compton scattering of synchrotron photons. For the study of the SED we used simultaneous optical R-band data from the KVA telescope, archival X-ray data by \textit{Swift} as well as \textit{INTEGRAL}, and simultaneous high energy (HE, $300$\,MeV~--~$10$\,GeV) $\gamma$-ray data from the \textit{Fermi} LAT observatory. Using the empirical approach of Prandini et al. (2010) and the \textit{Fermi}-LAT and MAGIC spectra for this object, we estimate the redshift of this source to be $0.34\pm0.08\pm0.05$. This is a relevant result because this source is possibly one of the ten most distant VHE blazars known to date, and with further (simultaneous) observations could play an important role in blazar population studies, as well as future constraints on the EBL and IGMF.
MAGIC gamma-ray and multi-frequency observations of flat spectrum radio quasar PKS 1510-089 in early 2012

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bratz, E. Carmona, A. Carosi, D. Carreto Fidalgo, P. Colin, E. Colombo, J. L. Contreras, I. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, C. Delgado Mendez, M. Doert, A. Dominguez, D. Dominis Presters, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, E. Farina, D. Ferenc, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, M. Hayashida, J. Herrera, A. Herrero, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallotw, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, M. Meucci, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, S. Partini, M. Persic, F. Prada, P. G. Prada Moroni, E. Prandini, S. Preziuso, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, A. Saggion, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, S. Sun, T. Suric, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. M. Wagner, F. Zandanel, R. Zanin, F. Lucarelli, C. Pittori, S. Vercellone, F. Verrecchia, S. Buson, F. D'Ammando, L. Stawarz, M. Giroletti, M. Orienti, C. Mundell, I. Steele, B. Zarpudin, C. M. Raiteri, M. Villata, A. Sandrinelli, A. Lahteenmaki, J. Tammi, M. Tornikoski, T. Hovatta, A. C. S. Readhead, W. Max-Moerbeck, J. L. Richards, S. Jorstad, A. Marscher, M. A. Gurwell, V. M. Larionov, D. A. Blinov, T. S. Konstantinova, E. N. Kopatskaya, L. V. Larionova, E. G. Earionova, D. A. Morozova, I. S. Troitky, A. A. Mokrushina, Yu. V. Pavlova, W. P. Chen, H. C. Lin, N. Panwar, I. Agudo, C. Casadio, J. L. Gomez, S. N. Molina, O. M. Kurtanidze, M. G. Nikolashvili, S. O. Kurtanidze, R. A. Chigladze, J. A. Acosta-Pulido, M. I. Carnerero, A. Manilla-Robles, E. Ovcharov, V. Bozhilov, I. Metodieva, M. F. Aller, H. D. Aller, L. Fuhrman, E. Angelakis, I. Nestoras, T. P. Krichbaue, J. A. Zensue, H. Ungerechts, A. Sievers

ASTRONOMY & ASTROPHYSICS 569 2014年9月

Aims. Amongst more than fifty blazars detected in very high energy (VHE, E > 100 GeV) gamma rays, only three belong to the subclass of flat spectrum radio quasars (FSRQs). The detection of FSRQs in the VHE range is challenging, mainly because of their soft spectra in the GeV-TeV regime. MAGIC observed PKS 1510-089 (z = 0.36) starting 2012 February 3 until April 3 during a high activity state in the high energy (HE, E > 100 MeV) gamma-ray band observed by AGILE and Fermi. MAGIC observations result in the detection of a source with significance of 6.0 standard deviations (sigma). We study the multi-frequency behaviour of the source at the epoch of MAGIC observation, collecting quasi-simultaneous data at radio and optical (GASP-WEBT and F-Gamma collaborations, REM, Steward, Perkins, Liverpool, OVRO, and VLBA telescopes), X-ray (Swift satellite), and HE gamma-ray frequencies. Methods. We study the VHE gamma-ray emission, together with the multi-frequency light curves, 43 GHz radio maps, and spectral energy distribution (SED) of the source. The quasi-simultaneous multi-frequency SED from the millimetre radio band to VHE gamma rays is modelled with a one-zone inverse Compton model. We study two different origins of the seed photons for the inverse Compton scattering, namely the infrared torus and a slow sheath surrounding the jet around the Very Long Baseline Array (VLBA) core. Results. We find that the VHE gamma-ray emission detected from PKS 1510-089 in 2012 February-April agrees with the previous VHE observations of the source from 2009 March-April. We find no statistically significant variability during the MAGIC observations on daily, weekly, or monthly time scales, while the other two known VHE FSRQs (3C 279 and PKS 1222+216) have shown daily scale to sub-hour variability. The gamma-ray SED combining AGILE, Fermi and MAGIC data joins smoothly and shows no hint of a break. The multi-frequency light curves suggest a common origin for the millimetre radio and HE gamma-ray emission, and the HE gamma-ray flaring starts when the new component is ejected from the 43GHz VLBA core and the studied SED models fit the data well. However, the fast HE gamma-ray variability requires that within the modelled large emitting region, more compact regions must exist. We suggest that these observed signatures would be most naturally explained by a turbulent plasma flowing at a relativistic speed down the jet and crossing a standing conical shock.
18pSB-1 MAGIC報告49 : 超新星残骸W44の超高エネルギーガンマ線観測(18pSB 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

花畑義隆, 齋藤浩二, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野祐介, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 野田浩司, 林田将明, MAGIC Collaboration

日本物理学会講演概要集 69(2) 32-32 2014年8月22日
18pSB-11 CTA報告83 : CTA大口径望遠鏡分割鏡の性能評価とシミュレーションによる光学系パラメータの考察(18pSB 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

荻野桃子, 林田将明, 野田浩司, 奥村曉, 小野祥弥, 加賀谷美佳, 片桐秀明, 小島拓実, 斎藤浩二, 齋藤隆之, 千川道幸, 長紀仁, 手嶋政廣, 中嶋大輔, 花畑義隆, 深見哲志, 柳田昭平, 山本常夏, 吉田龍生, CTA-Japan Consortium

日本物理学会講演概要集 69(2) 34-34 2014年8月22日
18pSB-12 CTA報告84 : CTA大口径望遠鏡用試験構造体を用いた光学系組立試験(18pSB 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

深見哲志, 荻野桃子, 奥村曉, 小野祥弥, 加賀谷美佳, 片桐秀明, 小島拓実, 斎藤浩二, 齋藤隆之, 千川道幸, 長紀仁, 手嶋政廣, 中嶋大輔, 野田浩司, 花畑義隆, 林田将明, 柳田昭平, 山本常夏, 吉田龍生

日本物理学会講演概要集 69(2) 34-34 2014年8月22日
MAGIC search for VHE $γ$-ray emission from AE Aquarii in a multiwavelength context

J. Aleksić, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, J. A. Barrio, J. Becerra González, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, E. de, Oña Wilhelmi, C. Delgado Mendez, M. Doert, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J, García López, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinović, A. González Muñoz, S. R. Gozzini, D. Hadasch, Y. Hanabata, M. Hayashida, J. Herrera, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. López, R. López-Coto, A. López-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martínez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, M. Persic, P. G, Prada Moroni, E. Prandini, S. Preziuso, I. Puljak, R. Reinthal, W. Rhode, M. Ribó, J. Rico, J. Rodriguez Garcia, S. Rügamer, A. Saggion, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, A. Sillanpää, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzić, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. M. Wagner, R. Zanin, M. Bogosavljevic, Z. Ioannou, C. W. Mauche, E. V. Palaiologou, M. A. Pérez-Torres, T. Tuominen

A&A 568, A109 (2014) 568 2014年8月

It has been claimed that the nova-like cataclysmic variable (CV) AE Aquarii (AE Aqr) is a very-high-energy (VHE, $E>$100 GeV) source both on observational and theoretical grounds. We aim to search for VHE gamma-ray emission from AE Aqr during different states of the source at several wavelengths to confirm or rule out previous claims of detection of gamma-ray emission from this object. We report on observations of AE Aqr performed by MAGIC. The source was observed during 12 hours as part of a multiwavelength campaign carried out between May and June 2012 covering the optical, X-ray, and gamma-ray ranges. Besides MAGIC, the other facilities involved were the KVA, Skinakas, and Vidojevica telescopes in the optical and Swift in X-rays. We calculated integral upper limits coincident with different states of the source in the optical. We computed upper limits to the pulsed emission limiting the signal region to 30% of the phaseogram and we also searched for pulsed emission at different frequencies applying the Rayleigh test. AE Aqr was not detected at VHE energies during the multiwavelength campaign. We establish integral upper limits at the 95\% confidence level for the steady emission assuming the differential flux proportional to a power-law function d\phi/dE \propto E^{-Gamma}, with a Crab-like photon spectral index of Gamma=2.6. The upper limit above 200 GeV is 6.4\times10^{-12} cm^{-2}s^{-1} and above 1 TeV is 7.4\times10^{-13} cm^{-2}s^{-1}. We obtained an upper limit for the pulsed emission of 2.6\times10^{-12} cm^{-2}s^{-1} for energies above 200 GeV. Applying the Rayleigh test for pulsed emission at different frequencies we did not find any significant signal. Our results indicate that AE Aqr is not a VHE gamma-ray emitter at the level of emission previously claimed. We have established the most constraining upper limits for the VHE gamma-ray emission of AE Aqr.
Discovery of TeV gamma-ray emission from the pulsar wind nebula 3C 58 by MAGIC

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, E. de Ona Wilhelmi, C. Delgado Mendez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, D. Galindo, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, Y. Hanabata, M. Hayashida, J. Herrera, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, M. Persie, P. G. Prada Moroni, E. Prandini, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, T. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, M. Strzys, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. Zanin, J. Martin, M. A. Perez-Torres

ASTRONOMY & ASTROPHYSICS 567 2014年7月

Context. The pulsar wind nebula (PWN) 3C 58 is one of the historical very high-energy (VHE; E > 100 GeV) gamma-ray source candidates. It is energized by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared with the Crab nebula because of their morphological similarities. This object was previously observed by imaging atmospheric Cherenkov telescopes (Whipple, VERITAS and MAGIC), although it was not detected, with an upper limit of 2.3% Crab unit (C. U.) at VHE. It was detected by the Fermi Large Area Telescope (LAT) with a spectrum extending beyond 100 GeV. Aims. We aim to extend the spectrum of 3C 58 beyond the energies reported by the Fermi Collaboration and probe acceleration of particles in the PWN up to energies of a few tens of TeV. Methods. We analyzed 81 h of 3C 58 data taken in the period between August 2013 and January 2014 with the MAGIC telescopes. Results. We detected VHE gamma-ray emission from 3C 58 with a significance of 5.7 sigma and an integral flux of 0.65% C. U. above 1 TeV. According to our results, 3C 58 is the least luminous VHE gamma-ray PWN ever detected at VHE and has the lowest flux at VHE to date. The differential energy spectrum between 400 GeV and 10 TeV is well described by a power-law function d phi/dE = f(0)(E/1 TeV)(-r) with f(0) = (2.0 + 0.4(stat) + 0.6(sys)) X 10(-13) cm(-2) S-1 TeV-1 and F = 2.4 +/- 0.2(stat) +/- 0.2(sys). The skymap is compatible with an unresolved source. Conclusions. We report the first significant detection of PWN 3C 58 at TeV energies. We compare our results with the expectations of time-dependent models in which electrons upscatter photon fields. The best representation favors a distance to the PWN of 2 kpc and far-infrared (FIR) values similar to cosmic microwave background photon fields. If we consider an unexpectedly high FIR density, the data can also be reproduced by models assuming a 3.2 kpc distance. A low magnetic field, far from equipartition, is required to explain the VHE data. Hadronic contribution from the hosting supernova remnant (SNR) requires an unrealistic energy budget given the density of the medium, disfavoring cosmic-ray acceleration in the SNR as origin of the VHE gamma-ray emission.
MAGIC long-term study of the distant TeV blazar PKS 1424+240 in a multiwavelength context

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, K. Berger, E. Bernardini, A. Biland, O. Blanch, R. K. Bock, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carrnona, A. Carosi, D. Carreto Fidalgo, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, C. Delgado Mendez, M. Doert, A. Dominguez, D. Dorninis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, E. Farina, D. Ferene, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, G. Giavitto, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, M. Hayashida, A. Herrero, D. Hildebrand, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellertnann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, M. Mencei, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, N. Nowak, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, S. Partini, M. Persic, F. Prada, P. G. Prada Moroni, E. Prandini, S. Prezinso, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, A. Saggion, T. Saito, K. Saito, M. Salvati, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Siilanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, F. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, J. Storz, S. Sun, T. Suric, L. Takalo, H. Takarni, F. Taveeehio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. F. Torres, T. Toyama, A. Trevesu, M. Uellenheck, P. Vogler, R. M. Wagner, F. Zandanel, R. Zanin, S. Cutini, D. Gasparrini, A. Furniss, T. Hovatta, T. Kangas, E. Kankare, J. Kotilainen, M. Lister, A. Lahteemaki, W. Max-Moerbeck, V. Pavlidou, A. Readhead, J. Richards

ASTRONOMY & ASTROPHYSICS 567 2014年7月

Aims. We present a study of the very high-energy (VHE; E > 100 GeV) gamma-ray emission of the blazar PKS 1424+240 observed with the MAGIC telescopes. The primary aim of this paper is the multiwavelength spectral characterization and modeling of this blazar, which is made particularly interesting by the recent discovery of a lower limit of its redshift of z greater than or similar to 0.6 and makes it a promising candidate to be the most distant VHE source. Methods. The source has been observed with the MAGIC telescopes in VHE gamma rays for a total observation time of similar to 33.6 h from 2009 to 2011. A detailed analysis of its gamma-ray spectrum and time evolution has been carried out. Moreover, we have collected and analyzed simultaneous and quasi-simultaneous multiwavelength data. Results. The source was marginally detected in VHE gamma rays during 2009 and 2010, and later, the detection was confirmed during an optical outburst in 2011. The combined significance of the stacked sample is similar to 7.2 sigma. The differential spectra measured during the different campaigns can be described by steep power laws with the indices ranging from 3.5 +/- 1.2 to 5.0 +/- 1.7. The MAGIC spectra corrected for the absorption due to the extragalactic background light connect smoothly, within systematic errors, with the mean spectrum in 2009-2011 observed at lower energies by the Fermi-LAT. The absorption-corrected MAGIC spectrum is flat with no apparent turn down up to 400 GeV. The multiwavelength light curve shows increasing flux in radio and optical bands that could point to a common origin from the same region of the jet. The large separation between the two peaks of the constructed non-simultaneous spectral energy distribution also requires an extremely high Doppler factor if an one zone synchrotron self-Compton model is applied. We find that a two-component synchrotron self-Compton model describes the spectral energy distribution of the source well, if the source is located at z similar to 0.6.
Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes

J. Aleksic, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres de Almeida, J. A. Barrio, J. Becerra Gonzalez, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P. Colin, E. Colombos, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, E. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, C. C. Delgado Mendez, M. Doert, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, E. Farina, D. Ferenc, D. Fidalgo, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, R. J. Garcia Lopez, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinovic, A. Gonzalez Munoz, S. R. Gozzini, D. Hadasch, M. Hayashida, J. Herrera, A. Herrero, D. Hildebrand, K. Hirotani, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. Lopez, R. Lopez-Coto, A. Lopez-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martinez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, R. Orito, A. Overkemping, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, X. Paredes-Fortuny, S. Partini, M. Persic, P. G. Prada Moroni, E. Prandini, S. Preziuso, I. Puljak, R. Reinthal, W. Rhode, M. Ribo, J. Rico, J. Rodriguez Garcia, S. Ruegamer, A. Saggion, T. Y. Saito, K. Saito, K. Satalecka, V. Scalzotto, V. Scapin, C. Schultz, T. Schweizer, S. N. Shore, A. Sillanpaa, J. Sitarek, I. Snidaric, D. Sobczynska, E. Spanier, V. Stamatescu, A. Stamerra, T. Steinbring, M. Storz, M. Strzys, S. Sun, T. Suric, L. Takalo, H. Takami, F. Tavecchio, P. Temnikov, T. Terzic, D. Tescaro, M. Teshima, J. Thaele, O. Tibolla, D. E. Forres, T. Toyama, A. Treves, M. Uellenbeck, P. Vogler, R. M. Wagner, R. Zanin

ASTRONOMY & ASTROPHYSICS 565 2014年5月

Context. The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E > 100 GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. Aims. In order to test new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. Methods. We analyzed 135 h of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 5.5 years of Fermi-LAT data were also analyzed. Results. The known two pulses per period were detected with a significance of 8.0 sigma and 12.6 sigma. In addition, significant emission was found between the two pulses with 6.2 sigma. Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models.
27pTS-6 CTA報告72 : CTA大口径望遠鏡の分割鏡の性能評価(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

荻野桃子, 馬場浩則, 林田将明, 奥村曉, 加賀谷美佳, 片桐秀明, 小島拓実, 斎藤浩二, 田中駿也, 千川道幸, 手嶋政廣, 中嶋大輔, 野里明香, 野田浩司, 花畑義隆, 柳田昭平, 山本常夏, 吉田龍生, CTA-Japan Consortium

日本物理学会講演概要集 69(1) 117-117 2014年3月5日
27pTS-8 CTA報告74 : CTA大型望遠鏡における光学系調整のための分割鏡支持構造設計(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

花畑義隆, 野田浩司, 手嶋政廣, 荻野桃子, 奥村曉, 加賀谷美佳, 片桐秀明, 小島拓実, 齋藤浩二, 田中駿也, 千川道幸, 中嶋大輔, 野里明日香, 馬場浩則, 林田将明, 柳田昭平, 山本常夏, 吉田龍生, the CTA-Japan Consortium

日本物理学会講演概要集 69(1) 118-118 2014年3月5日
27pTS-5 CTA報告71 : CTA大口径望遠鏡用ライトガイドの試作機性能評価及び形状最適化に向けた研究(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

田中駿也, 林田将明, 奥村曉, 片桐秀明, 手嶋政廣, 大岡秀行, 荻野桃子, 加賀谷美佳, 小島拓実, 齋藤浩二, 千川道幸, 中嶋大輔, 野里明香, 野田浩司, 花畑義隆, 馬場浩則, 柳田昭平, 山本常夏, 吉田龍生, CTA-Japan consortium

日本物理学会講演概要集 69(1) 117-117 2014年3月5日
27pTS-7 CTA報告73 : CTA大口径望遠鏡に用いる分割鏡制御システムの開発(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

小島拓実, 野里明香, 千川道幸, 林田将明, 荻野桃子, 奥村曉, 加賀谷美佳, 片桐秀明, 斉藤浩二, 田中駿也, 手嶋政廣, 中嶋大輔, 野田浩司, 花畑義隆, 馬場浩則, 柳田昭平, 山本常夏, 吉田龍生, the CTA-Japan consortium

日本物理学会講演概要集 69(1) 117-117 2014年3月5日
27pTS-9 MAGIC報告42 : HBL天体1ES 0229+200の観測と磁場ハローのシミュレーション(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

今野裕介, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 野田浩司, 花畑義隆, 林田将明, the MAGIC Collaboration

日本物理学会講演概要集 69(1) 118-118 2014年3月5日
27pTS-10 MAGIC報告43 : BL Lac型天体MAGIC J2001+435の多波長観測と赤方偏移(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

小谷一仁, 西嶋恭司, 櫛田淳子, 井上進, 折戸玲子, 窪秀利, 今野裕介, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 野田浩司, 花畑義隆, 林田将明, the MAGIC Collaboration

日本物理学会講演概要集 69(1) 118-118 2014年3月5日
27pTS-11 MAGIC報告44 : ブレーザーMrk501の多波長観測2013(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

野田浩司, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 花畑義隆, 林田将明, the MAGIC Collaboration

日本物理学会講演概要集 69(1) 118-118 2014年3月5日
27pTS-12 MAGIC報告45 : 遠方ブレーザーH 1722+119の観測(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

齋藤浩二, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 野田浩司, 花畑義隆, 林田将明, the MAGIC Collaboration

日本物理学会講演概要集 69(1) 119-119 2014年3月5日
27pTS-14 MAGIC報告47 : 新型アナログSum Triggerのインストールおよびコミッショニング(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

中嶋大輔, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 西嶋恭司, 野田浩司, 花畑義隆, 林田将明, the MAGIC Collaboration

日本物理学会講演概要集 69(1) 119-119 2014年3月5日
27pTS-15 MAGIC報告48 : 50GeV以下ガンマ線解析のためのイメージクリーニング法の開発(27pTS 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

齋藤隆之, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤浩二, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 野田浩司, 花畑義隆, 林田将明, the MAGIC Collaboration

日本物理学会講演概要集 69(1) 119-119 2014年3月5日
MAGIC望遠鏡による50-400GeVにおけるCrabパルサーの波形の精密測定

齋藤隆之, 窪秀利, 今野裕介, 井上進, 手嶋政廣, 遠山健, 野田浩司, 折戸玲子, 櫛田淳子, 小谷一仁, 西嶋恭司, 齋藤浩二, 中嶋大輔, 花畑義隆, 林田将明, 高見一

日本天文学会年会講演予稿集 2014 2014年
MAGIC望遠鏡によるBL Lac天体MAGIC J2001+435の観測結果と赤方偏移

小谷一仁, 西嶋恭司, 櫛田淳子, 井上進, 手嶋政廣, 遠山健, 野田浩司, 折戸玲子, 窪秀利, 今野裕介, 齋藤隆之, 齋藤浩二, 中嶋大輔, 花畑義隆, 林田将明, 高見一

日本天文学会年会講演予稿集 2014 2014年
MAGIC望遠鏡による遠方ブレーザーH 1722+119の観測

齋藤浩二, 中嶋大輔, 花畑義隆, 林田将明, 井上進, 手嶋政廣, 折戸玲子, 櫛田淳子, 小谷一仁, 西嶋恭司, 窪秀利, 今野裕介, 齋藤隆之, 高見一, 遠山健, 野田浩司

日本天文学会年会講演予稿集 2014 2014年
MAGIC望遠鏡のためのアナログSumトリガーのインストールおよびコミッショニング

中嶋大輔, 齋藤浩二, 手嶋政廣, 花畑義隆, 林田将明, 井上進, 遠山健, 野田浩司, 折戸玲子, 窪秀利, 今野裕介, 齋藤隆之, 櫛田淳子, 小谷一仁, 西嶋恭司, 高見一

日本天文学会年会講演予稿集 2014 2014年
MAGIC望遠鏡による超新星残骸W44領域の超高エネルギーガンマ線観測

花畑義隆, 井上進, 齋藤浩二, 中嶋大輔, 林田将明, 折戸玲子, 櫛田淳子, 小谷一仁, 西嶋恭司, 窪秀利, 今野祐介, 齋藤隆之, 高見一, 手嶋政廣, 手嶋政廣, 遠山健, 野田浩司

日本天文学会年会講演予稿集 2014 2014年
The Large Size Telescope of the Cherenkov Telescope Array

G. Ambrosi, Y. Awane, H. Baba, A. Bamba, M. Barcelo, U. Barres de Almeida, J. A. Barrio, O. Blanch Bigas, J. Boix, L. Brunetti, E. Carmona, E. Chabanne, M. Chikawa, P. Colin, J. Cortina, J. L. Contreras, F. Dazzi, A. de Angelis, G. Deleglise, C. Delgado, C. Diaz, A. Fiasson, D. Fink, N. Fouque, L. Freixas, C. Fruck, A. Gadola, R. Garcia, D. Gascon, N. Geffroy, N. Giglietto, F. Giordano, F. Granena, S. Gunji, R. Hagiwara, N. Hamer, Y. Hanabata, T. Hassan, K. Hatanaka, T. Haubold, M. Hayashida, R. Hermel, D. Herranz, K. Hirotani, S. Inoue, Y. Inoue, K. Ioka, C. Jablonski, M. Kagaya, H. Katagiri, T. Kishimoto, K. Kodani, K. Kohri, Y. Konno, S. Koyama, H. Kubo, J. Kushida, G. Lamanna, T. Le Flour, E. Lorenz, R. Lopez, M. Lopez-Moya, P. Majumdar, A. Manalaysay, M. Mariotti, G. Martinez, M. Martinez, D. Mazin, J. M. Miranda, R. Mirzoyan, I. Monteiro, A. Moralejo, K. Murase, S. Nagataki, D. Nakajima, T. Nakamori, K. Nishijima, K. Noda, A. Nozato, Y. Ohira, M. Ohishi, H. Ohoka, A. Okumura, R. Orito, J. L. Panazol, D. Paneque, R. Paoletti, J. M. Paredes, G. Pauletta, S. Podkladkin, J. Prast, R. Rando, O. Reimann, M. Ribo, S. Rosier-Lees, K. Saito, T. Saito, Y. Saito, N. Sakaki, R. Sakonaka, A. Sanuy, H. Sasaki, M. Sawada, V. Scalzotto, S. Schultz, T. Schweizer, T. Shibata, S. Shu, J. Sieiro, V. Stamatescu, S. Steiner, U. Straumann, R. Sugawara, H. Tajima, H. Takami, S. Tanaka, M. Tanaka, L. A. Tejedor, Y. Terada, M. Teshima, T. Totani, H. Ueno, K. Umehara, A. Vollhardt, R. Wagner, H. Wetteskind, T. Yamamoto, R. Yamazaki, A. Yoshida, T. Yoshida, T. Yoshikoshi

GROUND-BASED AND AIRBORNE TELESCOPES V 9145 2014年

The Cherenkov Telescope Array (CTA) project aims to implement the world's largest next generation of Very High Energy gamma-ray Imaging Atmospheric Cherenkov Telescopes devoted to the observation from a few tens of GeV to more than 100 TeV. To view the whole sky, two CTA sites are foreseen, one for each hemisphere. The sensitivity at the lowest energy range will be dominated by four Large Size Telescopes, LSTs, located at the center of each array and designed to achieve observations of high red-shift objects with the threshold energy of 20 GeV. The LST is optimized also for transient low energy sources, such as Gamma Ray Bursts (GRB), which require fast repositioning of the telescope. The overall design and the development status of the first LST telescope will be discussed.
20pSR-7 CTA報告62 : CTA大口径望遠鏡用ライトガイドの試作機性能評価及び大量生産に向けた開発(高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

田中駿也, 林田将明, 奥村暁, 手嶋政廣, 大岡秀行, 加賀谷美佳, 片桐秀明, 齋藤浩二, 千川道幸, 中嶋大輔, 野里明香, 野田浩司, 花畑義隆, 馬場浩則, 柳田昭平, 山本常夏, 吉田龍生, CTA-Japan consortium

日本物理学会講演概要集 68(2) 104-104 2013年8月26日
20pSR-9 CTA 報告64 : CTA大口径望遠鏡用AMCのアクチュエータ制御開発(高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

野里明香, 千川道幸, 奥村暁, 加賀谷美佳, 片桐秀明, 齋藤浩二, 田中駿也, 手嶋政廣, 中嶋大輔, 野田浩司, 林田将明, 馬場浩則, 花畑義隆, 柳田昭平, 山本常夏, 吉田龍生, CTA-Japan

日本物理学会講演概要集 68(2) 105-105 2013年8月26日
20pSR-10 CTA 報告65 : CTA大口径望遠鏡の光学系調整と光学性能(高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

野田浩司, 手嶋政廣, 奥村暁, 加賀谷美佳, 片桐秀享, 齋藤浩二, 田中駿也, 千川道幸, 中嶋大輔, 野里明香, 花畑義隆, 馬場浩則, 林田将明, 柳田昭平, 山本常夏, 吉田龍生, CTA-Japan consortium, Schweizer T, Watteskind H

日本物理学会講演概要集 68(2) 105-105 2013年8月26日
20pSR-8 CTA報告63 : CTA大口径望還鏡用分割鏡の形状測定システムであるPhase Measuring Deflectometry法の開発(高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

馬場浩則, 手嶋政廣, 中嶋大輔, 林田将明, 花畑義隆, 吉田龍生, 齋藤浩二, 佐々木浩人, 奥村暁, 加賀谷美佳, 片桐秀明, 田中駿也, 千川道幸, 野里明香, 野田浩司, 柳田昭平, 山本常夏, CTA-Japan consortium, Krobot Roman

日本物理学会講演概要集 68(2) 105-105 2013年8月26日
20pSR-1 MAGIC報告40 : FSRQ天体PKS1510-089の多波長観測(高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

齋藤浩二, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 野田浩司, 林田将明, MAGIC Collaborations

日本物理学会講演概要集 68(2) 103-103 2013年8月26日
The Cherenkov Telescope Array Large Size Telescope

G. Ambrosi, Y. Awane, H. Baba, A. Bamba, M. Barceló, U. Barres, de Almeida, J. A. Barrio, O. Blanch Bigas, J. Boix, L. Brunetti, E. Carmona, E. Chabanne, M. Chikawa, P. Colin, J. L. Conteras, J. Cortina, F. Dazzi, A. Deangelis, G. Deleglise, C. Delgado, C. Díaz, F. Dubois, A. Fiasson, D. Fink, N. Fouque, L. Freixas, C. Fruck, A. Gadola, R. García, D. Gascon, N. Geffroy, N. Giglietto, F. Giordano, F. Grañena, S. Gunji, R. Hagiwara, N. Hamer, Y. Hanabata, T. Hassan, K. Hatanaka, T. Haubold, M. Hayashida, R. Hermel, D. Herranz, K. Hirotani, S. Inoue, Y. Inoue, K. Ioka, C. Jablonski, M. Kagaya, H. Katagiri, T. Kishimoto, K. Kodani, K. Kohri, Y. Konno, S. Koyama, H. Kubo, J. Kushida, G. Lamanna, T. Le Flour, M. López-Moya, R. López, E. Lorenz, P. Majumdar, A. Manalaysay, M. Mariotti, G. Martínez, M. Martínez, D. Mazin, J. M. Miranda, R. Mirzoyan, I. Monteiro, A. Moralejo, K. Murase, S. Nagataki, D. Nakajima, T. Nakamori, K. Nishijima, K. Noda, A. Nozato, Y. Ohira, M. Ohishi, H. Ohoka, A. Okumura, R. Orito, J. L. Panazol, D. Paneque, R. Paoletti, J. M. Paredes, G. Pauletta, S. Podkladkin, J. Prast, R. Rando, O. Reimann, M. Ribó, S. Rosier-Lees, K. Saito, T. Saito, Y. Saito, N. Sakaki, R. Sakonaka, A. Sanuy, H. Sasaki, M. Sawada, V. Scalzotto, S. Schultz, T. Schweizer, T. Shibata, S. Shu, J. Sieiro, V. Stamatescu, S. Steiner, U. Straumann, R. Sugawara, H. Tajima, H. Takami, S. Tanaka, M. Tanaka, L. A. Tejedor, Y. Terada, M. Teshima, T. Totani, H. Ueno, K. Umehara, A. Vollhardt, R. Wagner, H. Wetteskind, T. Yamamoto, R. Yamazaki, A. Yoshida, T. Yoshida, T. Yoshikoshi, for the CTA Consortium

2013年7月17日

The two arrays of the Very High Energy gamma-ray observatory Cherenkov Telescope Array (CTA) will include four Large Size Telescopes (LSTs) each with a 23 m diameter dish and 28 m focal distance. These telescopes will enable CTA to achieve a low-energy threshold of 20 GeV, which is critical for important studies in astrophysics, astroparticle physics and cosmology. This work presents the key specifications and performance of the current LST design in the light of the CTA scientific objectives.
CTA contributions to the 33rd International Cosmic Ray Conference (ICRC2013)

The CTA Consortium, O. Abril, B. S. Acharya, M. Actis, G. Agnetta, J. A. Aguilar, F. Aharonian, M. Ajello, A. Akhperjanian, M. Alcubierre, J. Aleksic, R. Alfaro, E. Aliu, A. J. Allafort, D. Allan, I. Allekotte, R. Aloisio, E. Amato, G. Ambrosi, M. Ambrosio, J. Anderson, E. O. Angüner, L. A. Antonelli, V. Antonuccio, M. Antonucci, P. Antoranz, A. Aravantinos, A. Argan, T. Arlen, C. Aramo, T. Armstrong, H. Arnaldi, L. Arrabito, K. Asano, T. Ashton, H. G. Asorey, T. Aune, Y. Awane, H. Baba, A. Babic, N. Baby, J. Bähr, A. Bais, C. Baixeras, S. Bajtlik, M. Balbo, D. Balis, C. Balkowski, J. Ballet, A. Bamba, R. Bandiera, A. Barber, C. Barbier, M. Barceló, A. Barnacka, J. Barnstedt, U. Barres, de Almeida, J. A. Barrio, A. Basili, S. Basso, D. Bastieri, C. Bauer, A. Baushev, U. Becciani, J. Becerra, J. Becerra, Y. Becherini, K. C. Bechtol, J. Becker Tjus, V. Beckmann, W. Bednarek, B. Behera, M. Belluso, W. Benbow, J. Berdugo, D. Berge, K. Berger, F. Bernard, T. Bernardino, K. Bernlöhr, B. Bertucci, N. Bhat, S. Bhattacharyya, B. Biasuzzi, C. Bigongiari, A. Biland, S. Billotta, T. Bird, E. Birsin, E. Bissaldi, J. Biteau, M. Bitossi, S. Blake, O. Blanch Bigas, P. Blasi, A. Bobkov, V. Boccone, M. Böttcher, L. Bogacz, J. Bogart, M. Bogdan, C. Boisson, J. Boix Gargallo, J. Bolmont, G. Bonanno, A. Bonardi, T. Bonev, P. Bonifacio, G. Bonnoli, P. Bordas, A. Borgland, J. Borkowski, R. Bose, O. Botner, A. Bottani, L. Bouchet, M. Bourgeat, C. Boutonnet, A. Bouvier, S. Brau-Nogué, I. Braun, T. Bretz, M. Briggs, M. Brigida, T. Bringmann, R. Britto, P. Brook, P. Brun, L. Brunetti, P. Bruno, N. Bucciantini, T. Buanes, J. Buckley, R. Bühler, V. Bugaev, A. Bulgarelli, T. Bulik, G. Busetto, S. Buson, K. Byrum, M. Cailles, R. Cameron, J. Camprecios, R. Canestrari, S. Cantu, M. Capalbi, P. Caraveo, E. Carmona, A. Carosi, R. Carosi, J. Carr, J. Carter, P. -H. Carton, R. Caruso, S. Casanova, E. Cascone, M. Casiraghi, A. Castellina, O. Catalano, S. Cavazzani, S. Cazaux, P. Cerchiara, M. Cerruti, E. Chabanne, P. Chadwick, C. Champion, R. Chaves, P. Cheimets, A. Chen, J. Chiang, L. Chiappetti, M. Chikawa, V. R. Chitnis, F. Chollet, A. Christof, J. Chudoba, M. Cieślar, A. Cillis, M. Cilmo, A. Codino, J. Cohen-Tanugi, S. Colafrancesco, P. Colin, J. Colome, S. Colonges, M. Compin, P. Conconi, V. Conforti, V. Connaughton, J. Conrad, J. L. Contreras, P. Coppi, J. Coridian, P. Corona, D. Corti, J. Cortina, L. Cossio, A. Costa, H. Costantini, G. Cotter, B. Courty, S. Couturier, S. Covino, G. Crimi, S. J. Criswell, J. Croston, G. Cusumano, M. Dafonseca, O. Dale, M. Daniel, J. Darling, I. Davids, F. Dazzi, A. de Angelis, V. De Caprio, F. De Frondat, E. M. de, Gouveia, Dal Pino, I. de la Calle, G. A. De La Vega, R. de, los Reyes Lopez, B. de Lotto, A. De Luca, M. de Naurois, Y. de Oliveira, E. de, Oña Wilhelmi, F. de Palma, V. de Souza, G. Decerprit, G. Decock, C. Deil, E. Delagnes, G. Deleglise, C. Delgado, D. della Volpe, P. Demange, G. Depaola, A. Dettlaff, T. Di Girolamo, C. Di Giulio, A. Di Paola, F. Di Pierro, G. di Sciascio, C. Díaz, J. Dick, R. Dickherber, H. Dickinson, V. Diez-Blanco, S. Digel, D. Dimitrov, G. Disset, A. Djannati-Ataï, M. Doert, M. Dohmke, W. Domainko, D. Dominis Prester, A. Donat, D. Dorner, M. Doro, J. -L. Dournaux, G. Drake, D. Dravins, L. Drury, F. Dubois, R. Dubois, G. Dubus, C. Dufour, D. Dumas, J. Dumm, D. Durand, V. Dwarkadas, J. Dyks, M. Dyrda, J. Ebr, E. Edy, K. Egberts, P. Eger, S. Einecke, C. Eleftheriadis, S. Elles, D. Emmanoulopoulos, D. Engelhaupt, R. Enomoto, J. -P. Ernenwein, M. Errando, A. Etchegoyen, P. A. Evans, A. Falcone, A. Faltenbacher, D. Fantinel, K. Farakos, C. Farnier, E. Farrell, G. Fasola, B. W. Favill, E. Fede, S. Federici, S. Fegan, F. Feinstein, D. Ferenc, P. Ferrando, M. Fesquet, P. Fetfatzis, A. Fiasson, E. Fillin-Martino, D. Fink, C. Finley, J. P. Finley, M. Fiorini, R. Firpo Curcoll, E. Flandrini, H. Fleischhack, H. Flores, D. Florin, W. Focke, C. Föhr, E. Fokitis, L. Font, G. Fontaine, M. Fornasa, A. Förster, L. Fortson, N. Fouque, A. Franckowiak, F. J. Franco, A. Frankowski, C. Fransson, G. W. Fraser, R. Frei, L. Fresnillo, C. Fruck, D. Fugazza, Y. Fujita, Y. Fukazawa, Y. Fukui, S. Funk, W. Gäbele, S. Gabici, R. Gabriele, A. Gadola, N. Galante, D. Gall, Y. Gallant, J. Gámez-García, M. Garczarczyk, B. García, R. Garcia López, D. Gardiol, F. Gargano, D. Garrido, L. Garrido, D. Gascon, M. Gaug, J. Gaweda, L. Gebremedhin, N. Geffroy, L. Gerard, A. Ghedina, M. Ghigo, P. Ghislain, E. Giannakaki, F. Gianotti, S. Giarrusso, G. Giavitto, B. Giebels, N. Giglietto, V. Gika, M. Giomi, P. Giommi, F. Giordano, N. Girard, E. Giro, A. Giuliani, T. Glanzman, J. -F. Glicenstein, N. Godinovic, V. Golev, M. Gomez Berisso, J. Gómez-Ortega, M. M. Gonzalez, A. González, F. González, A. González Muñoz, K. S. Gothe, T. Grabarczyk, M. Gougerot, R. Graciani, P. Grandi, F. Grañena, J. Granot, G. Grasseau, R. Gredig, A. Green, T. Greenshaw, T. Grégoire, A. Grillo, O. Grimm, M. -H. Grondin, J. Grube, M. Grudzinska, V. Gruev, S. Grünewald, J. Grygorczuk, V. Guarino, S. Gunji, G. Gyuk, D. Hadasch, A. Hagedorn, R. Hagiwara, J. Hahn, N. Hakansson, A. Hallgren, N. Hamer Heras, S. Hara, M. J. Hardcastle, D. Harezlak, J. Harris, T. Hassan, K. Hatanaka, T. Haubold, A. Haupt, T. Hayakawa, M. Hayashida, R. Heller, F. Henault, G. Henri, G. Hermann, R. Hermel, A. Herrero, O. Hervet, N. Hidaka, J. A. Hinton, K. Hirotani, D. Hoffmann, W. Hofmann, P. Hofverberg, J. Holder, J. R. Hörandel, D. Horns, D. Horville, J. Houles, M. Hrabovsky, D. Hrupec, H. Huan, B. Huber, J. -M. Huet, G. Hughes, T. B. Humensky, J. Huovelin, J. -F. Huppert, A. Ibarra, D. Ikawa, J. M. Illa, D. Impiombato, S. Incorvaia, S. Inoue, Y. Inoue, F. Iocco, K. Ioka, G. L. Israel, C. Jablonski, A. Jacholkowska, J. Jacquemier, M. Jamrozy, M. Janiak, P. Jean, C. Jeanney, J. J. Jimenez, T. Jogler, C. Johnson, T. Johnson, L. Journet, C. Juffroy, I. Jung, P. Kaaret, S. Kabuki, M. Kagaya, J. Kakuwa, C. Kalkuhl, R. Kankanyan, A. Karastergiou, K. Kärcher, M. Karczewski, S. Karkar, J. Kasperek, D. Kastana, H. Katagiri, J. Kataoka, K. Katarzyński, U. Katz, N. Kawanaka, D. Kazanas, N. Kelley-Hoskins, B. Kellner-Leidel, H. Kelly, E. Kendziorra, B. Khélifi, D. B. Kieda, T. Kifune, T. Kihm, T. Kishimoto, K. Kitamoto, W. Kluźniak, C. Knapic, J. Knapp, J. Knödlseder, F. Köck, J. Kocot, K. Kodani, J. -H. Köhne, K. Kohri, K. Kokkotas, D. Kolitzus, N. Komin, I. Kominis, Y. Konno, H. Köppel, P. Korohoda, K. Kosack, G. Koss, R. Kossakowski, R. Koul, G. Kowal, S. Koyama, J. Kozioł, T. Krähenbühl, J. Krause, H. Krawzcynski, F. Krennrich, A. Krepps, A. Kretzschmann, R. Krobot, P. Krueger, H. Kubo, V. A. Kudryavtsev, J. Kushida, A. Kuznetsov, A. La Barbera, N. La Palombara, V. La Parola, G. La Rosa, K. Lacombe, G. Lamanna, J. Lande, D. Languignon, J. S. Lapington, P. Laporte, B. Laurent, C. Lavalley, T. Le Flour, A. Le Padellec, S. -H. Lee, W. H. Lee, J. -P. Lefèvre, H. Leich, M. A. Leigui de Oliveira, D. Lelas, J. -P. Lenain, R. Leoni, D. J. Leopold, T. Lerch, L. Lessio, G. Leto, B. Lieunard, S. Lieunard, R. Lindemann, E. Lindfors, A. Liolios, A. Lipniacka, H. Lockart, T. Lohse, S. Lombardi, F. Longo, A. Lopatin, M. Lopez, R. López-Coto, A. López-Oramas, A. Lorca, E. Lorenz, F. Louis, P. Lubinski, F. Lucarelli, H. Lüdecke, J. Ludwin, P. L. Luque-Escamilla, W. Lustermann, O. Luz, E. Lyard, M. C. Maccarone, T. J. Maccarone, G. M. Madejski, A. Madhavan, M. Mahabir, G. Maier, P. Majumdar, G. Malaguti, G. Malaspina, S. Maltezos, A. Manalaysay, A. Mancilla, D. Mandat, G. Maneva, A. Mangano, P. Manigot, K. Mannheim, I. Manthos, N. Maragos, A. Marcowith, M. Mariotti, M. Marisaldi, S. Markoff, A. Marszałek, C. Martens, J. Martí, J. -M. Martin, P. Martin, G. Martínez, F. Martínez, M. Martínez, F. Massaro, A. Masserot, A. Mastichiadis, A. Mathieu, H. Matsumoto, F. Mattana, S. Mattiazzo, A. Maurer, G. Maurin, S. Maxfield, J. Maya, D. Mazin, L. Mc Comb, A. McCann, N. McCubbin, I. McHardy, R. McKay, K. Meagher, C. Medina, C. Melioli, D. Melkumyan, D. Melo, S. Mereghetti, P. Mertsch, M. Meucci, M. Meyer, J. Michałowski, P. Micolon, A. Mihailidis, T. Mineo, M. Minuti, N. Mirabal, F. Mirabel, J. M. Miranda, R. Mirzoyan, A. Mistò, T. Mizuno, B. Moal, R. Moderski, I. Mognet, E. Molinari, M. Molinaro, T. Montaruli, C. Monte, I. Monteiro, P. Moore, A. Moralejo Olaizola, M. Mordalska, C. Morello, K. Mori, G. Morlino, A. Morselli, F. Mottez, Y. Moudden, E. Moulin, I. Mrusek, R. Mukherjee, P. Munar-Adrover, H. Muraishi, K. Murase, A. StJ. Murphy, S. Nagataki, T. Naito, D. Nakajima, T. Nakamori, K. Nakayama, C. Naumann, D. Naumann, M. Naumann-Godo, P. Nayman, D. Nedbal, D. Neise, L. Nellen, A. Neronov, V. Neustroev, N. Neyroud, L. Nicastro, J. Nicolau-Kukliński, A. Niedźwiecki, J. Niemiec, D. Nieto, A. Nikolaidis, K. Nishijima, K. -I. Nishikawa, K. Noda, S. Nolan, R. Northrop, D. Nosek, N. Nowak, A. Nozato, L. Oakes, P. T. O'Brien, Y. Ohira, M. Ohishi, S. Ohm, H. Ohoka, T. Okuda, A. Okumura, J. -F. Olive, R. A. Ong, R. Orito, M. Orr, J. P. Osborne, M. Ostrowski, L. A. Otero, N. Otte, E. Ovcharov, I. Oya, A. Ozieblo, L. Padilla, I. Pagano, S. Paiano, D. Paillot, A. Paizis, S. Palanque, M. Palatka, J. Pallota, M. Palatiello, K. Panagiotidis, J. -L. Panazol, D. Paneque, M. Panter, M. R. Panzera, R. Paoletti, A. Papayannis, G. Papyan, J. M. Paredes, G. Pareschi, J. -M. Parraud, D. Parsons, G. Pauletta, M. Paz Arribas, M. Pech, G. Pedaletti, V. Pelassa, D. Pelat, M, d. C. Perez, M. Persic, P. -O. Petrucci, B. Peyaud, A. Pichel, D. Pieloth, E. Pierre, S. Pita, G. Pivato, F. Pizzolato, M. Platino, Ł. Platos, R. Platzer, S. Podkladkin, L. Pogosyan, M. Pohl, G. Pojmanski, J. D. Ponz, W. Potter, J. Poutanen, E. Prandini, J. Prast, R. Preece, F. Profeti, H. Prokoph, M. Prouza, M. Proyetti, I. Puerto-Giménez, G. Pühlhofer, I. Puljak, M. Punch, R. Pyzioł, E. J. Quel, J. Quesada, J. Quinn, A. Quirrenbach, E. Racero, S. Rainò, P. J. Rajda, M. Rameez, P. Ramon, R. Rando, R. C. Rannot, M. Rataj, M. Raue, D. Ravignani, P. Reardon, O. Reimann, A. Reimer, O. Reimer, K. Reitberger, M. Renaud, S. Renner, B. Reville, W. Rhode, M. Ribó, M. Ribordy, G. Richards, M. G. Richer, J. Rico, J. Ridky, F. Rieger, P. Ringegni, J. Ripken, P. R. Ristori, A. Rivière, S. Rivoire, L. Rob, G. Rodeghiero, U. Roeser, R. Rohlfs, G. Rojas, P. Romano, W. Romaszkan, G. E. Romero, S. R. Rosen, S. Rosier Lees, D. Ross, G. Rouaix, J. Rousselle, S. Rousselle, A. C. Rovero, F. Roy, S. Royer, B. Rudak, C. Rulten, M. Rupiński, F. Russo, F. Ryde, O. Saavedra, B. Sacco, E. O. Saemann, A. Saggion, V. Sahakian, K. Saito, T. Saito, Y. Saito, N. Sakaki, R. Sakonaka, A. Salini, F. Sanchez, M. Sanchez-Conde, A. Sandoval, H. Sandaker, E. Sant'Ambrogio, A. Santangelo, E. M. Santos, A. Sanuy, L. Sapozhnikov, S. Sarkar, N. Sartore, H. Sasaki, K. Satalecka, M. Sawada, V. Scalzotto, V. Scapin, M. Scarcioffolo, J. Schafer, T. Schanz, S. Schlenstedt, R. Schlickeiser, T. Schmidt, J. Schmoll, P. Schovanek, M. Schroedter, A. Schubert, C. Schultz, J. Schultze, A. Schulz, K. Schure, F. Schussler, T. Schwab, U. Schwanke, J. Schwarz, S. Schwarzburg, T. Schweizer, S. Schwemmer, U. Schwendicke, C. Schwerdt, A. Segreto, J. -H. Seiradakis, G. H. Sembroski, M. Servillat, K. Seweryn, M. Sharma, M. Shayduk, R. C. Shellard, J. Shi, T. Shibata, A. Shibuya, S. Shore, E. Shum, E. Sideras-Haddad, L. Sidoli, M. Sidz, J. Sieiro, M. Sikora, J. Silk, A. Sillanpää, B. B. Singh, G. Sironi, J. Sitarek, C. Skole, R. Smareglia, A. Smith, D. Smith, J. Smith, N. Smith, D. Sobczyńska, H. Sol, G. Sottile, M. Sowiński, F. Spanier, D. Spiga, S. Spyrou, V. Stamatescu, A. Stamerra, R. L. C. Starling, Ł. Stawarz, R. Steenkamp, C. Stegmann, S. Steiner, C. Stella, N. Stergioulas, R. Sternberger, M. Sterzel, F. Stinzing, M. Stodulski, Th. Stolarczyk, U. Straumann, E. Strazzeri, L. Stringhetti, A. Suarez, M. Suchenek, R. Sugawara, K. -H. Sulanke, S. Sun, A. D. Supanitsky, T. Suric, P. Sutcliffe, J. M. Sykes, M. Szanecki, T. Szepieniec, A. Szostek, G. Tagliaferri, H. Tajima, H. Takahashi, K. Takahashi, L. Takalo, H. Takami, G. Talbot, J. Tammi, M. Tanaka, S. Tanaka, J. Tasan, M. Tavani, J. -P. Tavernet, L. A. Tejedor, I. Telezhinsky, P. Temnikov, C. Tenzer, Y. Terada, R. Terrier, M. Teshima, V. Testa, D. Tezier, J. Thayer, D. Thuermann, L. Tibaldo, L. Tibaldo, O. Tibolla, A. Tiengo, M. C. Timpanaro, M. Tluczykont, C. J. Todero Peixoto, F. Tokanai, M. Tokarz, K. Toma, A. Tonachini, K. Torii, M. Tornikoski, D. F. Torres, M. Torres, S. Toscano, G. Toso, G. Tosti, T. Totani, F. Toussenel, G. Tovmassian, P. Travnicek, A. Treves, M. Trifoglio, I. Troyano, K. Tsinganos, H. Ueno, G. Umana, K. Umehara, S. S. Upadhya, T. Usher, M. Uslenghi, F. Vagnetti, J. F. Valdes-Galicia, P. Vallania, G. Vallejo, W. van Driel, C. van Eldik, J. Vandenbrouke, J. Vanderwalt, H. Vankov, G. Vasileiadis, V. Vassiliev, D. Veberic, I. Vegas, S. Vercellone, S. Vergani, V. Verzi, G. P. Vettolani, C. Veyssière, J. P. Vialle, A. Viana, M. Videla, C. Vigorito, P. Vincent, S. Vincent, J. Vink, N. Vlahakis, L. Vlahos, P. Vogler, V. Voisin, A. Vollhardt, H. -P. von Gunten, S. Vorobiov, C. Vuerli, V. Waegebaert, R. Wagner, R. G. Wagner, S. Wagner, S. P. Wakely, R. Walter, T. Walther, K. Warda, R. S. Warwick, P. Wawer, R. Wawrzaszek, N. Webb, P. Wegner, A. Weinstein, Q. Weitzel, R. Welsing, M. Werner, H. Wetteskind, R. J. White, A. Wierzcholska, S. Wiesand, A. Wilhelm, M. I. Wilkinson, D. A. Williams, R. Willingale, M. Winde, K. Winiarski, R. Wischnewski, Ł. Wiśniewski, P. Wojcik, M. Wood, A. Wörnlein, Q. Xiong, K. K. Yadav, H. Yamamoto, T. Yamamoto, R. Yamazaki, S. Yanagita, J. M. Yebras, D. Yelos, A. Yoshida, T. Yoshida, T. Yoshikoshi, P. Yu, V. Zabalza, M. Zacharias, A. Zajczyk, L. Zampieri, R. Zanin, A. Zdziarski, A. Zech, A. Zhao, X. Zhou, K. Zietara, J. Ziolkowski, P. Ziółkowski, V. Zitelli, C. Zurbach, P. Zychowski

2013年7月8日

Compilation of CTA contributions to the proceedings of the 33rd International Cosmic Ray Conference (ICRC2013), which took place in 2-9 July, 2013, in Rio de Janeiro, Brazil
26aBD-1 MAGIC報告36:MAGIC望遠鏡によるBL Lac型天体2FGL J2001.1+4352の観測結果(26aBD 高エネルギーガンマ線,宇宙線・宇宙物理領域)

小谷一仁, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 今野裕介, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 林田将明, MAGIC Collaboration

日本物理学会講演概要集 68(1) 114-114 2013年3月26日
26aBD-2 MAGIC報告37:MAGIC望遠鏡のアップグレードおよび新型アナログSumトリガーの開発(26aBD 高エネルギーガンマ線,宇宙線・宇宙物理領域)

中嶋大輔, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 西嶋恭司, 林田将明, MAGIC Collaboration

日本物理学会講演概要集 68(1) 114-114 2013年3月26日
26aBD-3 MAGIC報告38:MAGIC望遠鏡アップグレード後のGRB観測(26aBD 高エネルギーガンマ線,宇宙線・宇宙物理領域)

遠山健, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 中嶋大輔, 西嶋恭司, 林田将明, MAGIC Collaboration

日本物理学会講演概要集 68(1) 114-114 2013年3月26日
MAGIC報告 40:FSRQ天体PKS 1510-089の多波長観測

齋藤浩二, 井上進, 折戸玲子, 櫛田淳子, 窪秀利, 小谷一仁, 今野裕介, 齋藤隆之, 齋藤隆之, 高見一, 手嶋政廣, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 野田浩司, 林田将明

日本物理学会講演概要集 68(2) 2013年
MAGIC望遠鏡を用いたブレーザーMrk501の高エネルギーガンマ線フレアの多波長観測

野田浩司, 遠山健, 中嶋大輔, 井上進, 齋藤浩二, 手嶋政廣, 林田将明, 折戸玲子, 櫛田淳子, 小谷一仁, 西嶋恭司, 窪秀利, 今野裕介, 齋藤隆之, 高見一

日本天文学会年会講演予稿集 2013 2013年
13aSP-10 MAGIC報告33 : MAGIC望遠鏡によるHBL天体1ES 1727+502の観測結果(13aSP 高・超高エネルギー宇宙線,高エネルギー宇宙線(CALET・MAGIC),宇宙線・宇宙物理領域)

小谷一仁, 井上進, 折戸玲子, 片桐秀明, 櫛田淳子, 窪秀利, 今野裕介, 齋藤浩二, 齋藤隆之, 高見一, 手嶋政廣, 遠山健, 中嶋大輔, 西嶋恭司, 林田将明, 宮本寛子, MAGIC Collaboration

日本物理学会講演概要集 67(2) 111-111 2012年8月24日
広角高精度望遠鏡を利用した大気透過率計測手法の開発(2.1.1.3 第3プロジェクト共同利用研究の内容と成果,2.1.1.共同利用プロジェクト研究の詳細,2.1.共同利用研究概観,[2] 共同利用研究)

佐々木真人, 浅岡陽一, 小川了, 眞子直弘, 上橋雅志, 会田勇一, 奥村暁, 野田浩司, 安田雅弘

千葉大学環境リモートセンシング研究センター年報 11 55-56 2006年6月

講演・口頭発表等

CTA報告130：全体報告

手嶋政廣, 井上剛志, 藤田裕, He Haoning, Majumdar Pratik, Mazin Daniel, 増田周, 松本浩典, 三浦智佳, 水野恒史, 村石浩, 村瀬孔大, 井上芳幸, 森浩二, 柳田昭平, 山崎了, 山本常夏, 山本宏昭, 吉池智史, 吉越貴紀, 吉田篤正, 吉田龍生, 李健, 猪目祐介, 李兆衡, Consortium for, the CTA-Japan, 岩村由樹, Warren Donald, 内山泰伸, 大石理子, 大岡秀行, 大平豊, 岡崎奈緒, 窪秀利, 奥村曉, 折戸玲子, 加賀谷美佳, 格和純, 片岡淳, 片桐秀明, 勝倉大輔, 勝田哲, 加藤翔, 神本匠, 戸谷友則, 川中宣太, 木坂将大, 木村颯一朗, Cui Xiaohong, 櫛田淳子, 久門拓, 黒田隼人, 郡司修一, 郡和範, 小山志勇, 浅野勝晃, Kong Albert K. H, 齋藤隆之, 榊直人, 櫻井駿介, 佐々井義矩, 佐野栄俊, 澤田真理, 柴田徹, Dzhatdoev Timur, 砂田裕志, 朝野彰, 関崎晴仁, 高田順平, 高橋慶太郎, 高橋知也, 高橋弘充, 高橋光成, 高原大, 田島宏康, 立原研悟, 田中周太, 井岡邦仁, 田中孝明, 田中真伸, 田中康之, 種田裕貴, Tam Thomas P. H, Cheng K. S, 千川道幸, 辻本晋平, 鶴剛, Tian Wenwu, 石尾一馬, 寺田幸功, 當真賢二, 門叶冬樹, 内藤統也, 中嶋大輔, 長瀧重博, 中村裕樹, 中森健之, 中山和則, 永吉勤, 稲田知大, 西嶋恭司, 西山楽, 野崎誠也, 野田浩司, Barkov Maxim, Hadasch Daniela, 早川貴敬, 林克洋, 林田将明, 原敏, 井上進, 馬場彩, 日高直哉, 平子丈, 廣島渚, 広谷幸一, Hui David, C. Y, Ferrand Gilles, 深沢泰司, 深見哲志, 福井康雄

日本物理学会講演概要集 2018年
CTA報告139：全体報告

窪秀利, 井上剛志, 深見哲志, 福井康雄, 藤田裕, 藤原千賀己, He Haoning, Majumdar Pratik, Mazin Daniel, 増田周, 松本浩典, 三浦智佳, 井上芳幸, 水野恒史, 村石浩, 村瀬孔大, 森浩二, 柳田昭平, 山崎了, 山本常夏, 山本宏昭, 吉池智史, 吉越貴紀, 猪目祐介, 吉田篤正, 吉田龍生, 李健, 李兆衡, 岩村由樹, Warren Donald, 内山泰伸, 大石理子, 大岡秀行, 大平豊, 岡崎奈緒, 手嶋政廣, 奥村曉, 折戸玲子, 加賀谷美佳, 格和純, 片岡淳, 片桐秀明, 勝倉大輔, 勝田哲, 加藤翔, 神本匠, 戸谷友則, 川中宣太, 木坂将大, 木村颯一朗, Cui Xiaohong, 櫛田淳子, 久門拓, 黒田隼人, 郡司修一, 郡和範, 小山志勇, 朝野彰, Kong Albert K. H, 齋藤隆之, 榊直人, 櫻井駿介, 佐々井義矩, 佐野栄俊, 澤田真理, 柴田徹, Dzhatdoev Timur, 鈴木萌, 浅野勝晃, 砂田裕志, 関崎晴仁, Zenin Anatolii, 高田順平, 高橋慶太郎, 高橋知也, 高橋弘充, 高橋光成, 髙原大, 田島宏康, 井岡邦仁, 立原研悟, 田中周太, 田中孝明, 田中真伸, 田中康之, 種田裕貴, Tam Thomas P. H, Cheng K. S, 千川道幸, 辻本晋平, 石尾一馬, 鶴剛, Tian Wenwu, 寺田幸功, 當真賢二, 門叶冬樹, 内藤統也, 中嶋大輔, 長瀧重博, 中村裕樹, 中森健之, 稲田知大, 中山和則, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 野田浩司, Barkov Maxim, Hadasch Daniela, 早川貴敬, 林克洋, 井上進, 林田将明, 原敏, 馬場彩, 日高直哉, 平子丈, 廣島渚, 広谷幸一, Hui David, C. Y, Ferrand Gilles, 深沢泰司

日本物理学会講演概要集 2018年一般社団法人日本物理学会
Observations of IceCube HESE track directions with the MAGIC telescopes

K. Satalecka, E. Bernardini, D. Gora, K. Noda, G. Pedaletti

HIGH ENERGY GAMMA-RAY ASTRONOMY 2017年 AMER INST PHYSICS

The MAGIC telescopes are strongly involved in several multimessenger programs. One of them are follow-up observations of astrophysical neutrino events, to search for hadronic gamma-ray emission from the neutrino direction and identify potential neutrino sources. In 2013 the IceCube collaboration reported the first detection of astrophysical neutrinos and up to now 55 events, which interact inside the IceCube detector active volume, dubbed High Energy Starting Events (HESE), have been reported. These include 13 track-like events, caused usually by muon neutrino charge current interactions. The track-like events ( as opposed to cascade-like neutral current interactions) are characterised by a very good angular resolution of < 1 deg, which facilitates follow-up observations and potential source identification. The MAGIC telescopes performed follow-up observations of 4 HESE track-like events from the Northern hemisphere: HESE-37, HESE-38, HET (ATel #7856) and the GCN HESE alert from 27/04/2016 (GCN #19363). No signal was detected. Here we present the results of those observations and discuss the implications for the constraints on the density of the astrophysical neutrino sources.
18pSB-12 CTA報告84 : CTA大口径望遠鏡用試験構造体を用いた光学系組立試験(18pSB 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

深見哲志, 荻野桃子, 奥村曉, 小野祥弥, 加賀谷美佳, 片桐秀明, 小島拓実, 斎藤浩二, 齋藤隆之, 千川道幸, 長紀仁, 手嶋政廣, 中嶋大輔, 野田浩司, 花畑義隆, 林田将明, 柳田昭平, 山本常夏, 吉田龍生

日本物理学会講演概要集 2014年8月22日一般社団法人日本物理学会
18pSB-11 CTA報告83 : CTA大口径望遠鏡分割鏡の性能評価とシミュレーションによる光学系パラメータの考察(18pSB 高エネルギーガンマ線(CTA,MAGIC),宇宙線・宇宙物理領域)

荻野桃子, 林田将明, 野田浩司, 奥村曉, 小野祥弥, 加賀谷美佳, 片桐秀明, 小島拓実, 斎藤浩二, 齋藤隆之, 千川道幸, 長紀仁, 手嶋政廣, 中嶋大輔, 花畑義隆, 深見哲志, 柳田昭平, 山本常夏, 吉田龍生, CTA-Japan Consortium

日本物理学会講演概要集 2014年8月22日一般社団法人日本物理学会

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野田浩司, 齋藤隆之, 高橋光成, 中森健之, 稲田知大
チェレンコフ望遠鏡アレイ国際共同実験による突発天体の研究

日本学術振興会科学研究費助成事業研究活動スタート支援 2019年4月 - 2020年3月

野田浩司
広視野・高分解能の宇宙線望遠鏡による高エネルギー天体の観測的研究

日本学術振興会科学研究費助成事業特別研究員奨励費 2006年 - 2008年

野田浩司

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野田 浩司

基本情報

研究分野

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論文

MISC

講演・口頭発表等

共同研究・競争的資金等の研究課題

野田浩司