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  2. 野田 浩司

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

 1

受賞

 1

論文

 153
  • 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.
  • 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.
  • 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
  • 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.
  • 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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 97
  • 溝手雅也, 山本常夏, 奥村曉, 田島宏康, 高橋光成, 齋藤隆之, 猪目祐介, 大岡秀行, 櫻井駿介, 手嶋政廣, 野田浩司, 橋山和明, 窪秀利, 岡知彦, 野崎誠也, HADASCH Daniela, MAZIN Daniel, 片桐秀明, 吉田龍生, 寺内健太, 折戸玲子, 櫛田淳子, 西嶋恭司, 郡司修一, 門叶冬樹, 中森健之, 砂田裕志, 立石大, 寺田幸功, 田中真伸
    日本天文学会年会講演予稿集 2023 2023年  
  • 溝手雅也, 山本常夏, 奥村曉, 奥村曉, 齋藤隆之, 吉田龍生, 猪目祐介, 大岡秀行, 岡知彦, 折戸玲子, 片桐秀明, 櫛田淳子, 窪秀利, 郡司修一, 櫻井駿介, 砂田裕志, 高橋光成, 田島宏康, 立石大, 田中真伸, HADASCH Daniela, MAZIN Daniel, MAZIN Daniel, 手嶋政廣, 手嶋政廣, 寺内健太, 寺田幸功, 門叶冬樹, 中森健之, 西嶋恭司, 野崎誠也, 野田浩司, 橋山和明
    日本物理学会講演概要集(CD-ROM) 78(2) 2023年  
  • A. Berti, Z. Bosnjak, S. Covino, S. Fukami, S. Inoue, F. Longo, D. Miceli, R. Mirzoyan, E. Moretti, L. Nava, K. Noda, A. Stamerra, D. Paneque, Y. Suda, I. Vovk
    Proceedings of Science 395 787 2022年3月  査読有り
  • K. Noda, L. Nava, S. Inoue, S. Fukami, M. Palatiello, A. Berti, F. Longo
    Proceedings of Science 395 776 2022年3月  査読有り
  • 高橋 光成, 猪目 祐介, 今川 要, 岩村 由樹, 大岡 秀行, 岡知 彦, 岡崎 奈緒, 奥村 曉, 折戸 玲子, 梶原 侑貴, 片桐 秀明, 川島 翔太郎, 川村 孔明, 櫛田 淳子, 窪秀 利, 郡司 修一, 小林 志鳳, 齋藤 隆之, 櫻井 駿介, 鈴木 萌, 砂田 裕志, 田中 真伸, 田村 謙治, 町支 勇貴, 塚本 友祐, 手嶋 政廣, 寺田 幸功, 門叶 冬樹, 中森 健之, 永吉 勤, 生天目 康之, 西嶋 恭司, 野上 優人, 野崎 誠也, 野田 浩司, 古田 智也, 増田 周, 山本 常夏, 吉田 龍生, 他 CTA-Japan Consortium, 池野 正弘, 木 寅旭
    日本物理学会講演概要集 75.1 472-472 2020年  
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講演・口頭発表等

 60

共同研究・競争的資金等の研究課題

 4
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