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129 results on '"Troitskaya, Yu. V."'

1. Multi-wavelength picture of the misaligned BL Lac object 3C 371

Author: Otero-Santos, J., Raiteri, C. M., Tramacere, A., Pedrosa, J. Escudero, Acosta-Pulido, J. A., Carnerero, M. I., Villata, M., Agudo, I., Rahimov, I. A., Andreeva, T. S., Ivanov, D. V., Marchili, N., Righini, S., Giroletti, M., Gurwell, M. A., Savchenko, S. S., Carosati, D., Chen, W. P., Kurtanidze, S. O., Joner, M. D., Semkov, E., Pursimo, T., Benítez, E., Damljanovic, G., Andreuzzi, G., Apolonio, G., Borman, G. A., Bozhilov, V., Galindo-Guil, F. J., Grishina, T. S., Hagen-Thorn, V. A., Hiriart, D., Hsiao, H. Y., Ibryamov, S., Ivanidze, R. Z., Kimeridze, G. N., Kopatskaya, E. N., Kurtanidze, O. M., Larionov, V. M., Larionova, E. G., Larionova, L. V., Minev, M., Morozova, D. A., Nikolashvili, M. G., Ovcharov, E., Sigua, L. A., Stojanovic, M., Troitskiy, I. S., Troitskaya, Yu. V., Tsai, A., Valcheva, A., Vasilyev, A. A., Vince, O., Zaharieva, E., and Zhovtan, A. V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: The BL Lac object 3C 371 is one of the targets that are regularly monitored by the Whole Earth Blazar Telescope (WEBT) Collaboration to study blazar variability on both short and long timescales. We aim to evaluate the long-term multiwavelength (MWL) behaviour of 3C 371, comparing it with the results derived for its optical emission in our previous study. For this, we make use of the multi-band campaigns organized by the WEBT Collaboration in optical and radio between January 2018 and December 2020, and of public data from Swift and Fermi satellites and the MOJAVE Very Large Interferometry programme. We evaluate the variability shown by the source in each band with the amplitude variability quantification, as well as possible interband correlation using the z-Discrete Correlation Function. We also present a deep analysis of the optical-UV, X-ray and $\gamma$-ray spectral variability. With the MOJAVE data we perform a kinematics analysis, looking for components propagating along the jet, calculating its kinematics parameters. This set of parameters is later used for the interpretation of the source MWL behaviour, modelling the broadband spectral energy distribution (SED) of the source with theoretical blazar emission scenarios., Comment: Accepted in A&A, 23 pages, 15 figures
Published: 2024

2. A wiggling filamentary jet at the origin of the blazar multi-wavelength behaviour

Author: Raiteri, C. M., Villata, M., Carnerero, M. I., Kurtanidze, S. O., Mirzaqulov, D. O., Benítez, E., Bonnoli, G., Carosati, D., Acosta-Pulido, J. A., Agudo, I., Andreeva, T. S., Apolonio, G., Bachev, R., Borman, G. A., Bozhilov, V., Brown, L. F., Carbonell, W., Casadio, C., Chen, W. P., Damljanovic, G., Ehgamberdiev, S. A., Elsaesser, D., Escudero, J., Feige, M., Fuentes, A., Gabellini, D., Gazeas, K., Giroletti, M., Grishina, T. S., Gupta, A. C., Gurwell, M. A., Hagen-Thorn, V. A., Hamed, G. M., Hiriart, D., Hodges, M., ivanidze, R. Z., Ivanov, D. V., Joner, M. D., Jorstad, S. G., Jovanovic, M. D., Kiehlmann, S., Kimeridze, G. N., Kopatskaya, E. N., Kovalev, Yu. A., Kovalev, Y. Y., Kurtanidze, O. M., Kurtenkov, A., Larionova, E. G., Lessing, A., Lin, H. C., López, J. M., Lorey, C., Ludwig, J., Marchili, N., Marchini, A., Marscher, A. P., Matsumoto, K., Max-Moerbeck, W., Mihov, B., Minev, M., Mingaliev, M. G., Modaressi, A., Morozova, D. A., Mortari, F., Mufakharov, T. V., Myserlis, I., Nikolashvili, M. G., Pearson, T. J., Popkov, A. V., Rahimov, I. A., Readhead, A. C. S., Reinhart, D., Reeves, R., Righini, S., Romanov, F. D., Savchenko, S. S., Semkov, E., Shishkina, E. V., Sigua, L. A., Slavcheva-Mihova, L., Sotnikova, Yu. V., Steineke, R., Stojanovic, M., Strigachev, A., Takey, A., Traianou, E., Troitskaya, Yu. V., Troitskiy, I. S., Tsai, A. L., Valcheva, A., Vasilyev, A. A., Verna, G., Vince, O., Vrontaki, K., Weaver, Z. R., Webb, J., Yuldoshev, Q. X., Zaharieva, E., and Zhovtan, A. V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Blazars are beamed active galactic nuclei known for their strong multi-wavelength variability on timescales from years down to minutes. We aim to investigate the suitability of the twisting jet model presented in previous works to explain the multi-wavelength behaviour of BL Lacertae, the prototype of one of the blazar classes. According to this model, the jet is inhomogeneous, curved, and twisting, and the long-term variability is due to changes in the Doppler factor due to variations in the orientation of the jet-emitting regions. We analysed optical data of the source obtained during monitoring campaigns organised by the Whole Earth Blazar Telescope (WEBT) in 2019-2022, together with radio data from the WEBT and other teams, and gamma-ray data from the Fermi satellite. In this period, BL Lacertae underwent an extraordinary activity phase, reaching its historical optical and gamma-ray brightness maxima. The application of the twisting jet model to the source light curves allows us to infer the wiggling motion of the optical, radio, and gamma-ray jet-emitting regions. The optical-radio correlation shows that the changes in the radio viewing angle follow those in the optical viewing angle by about 120 days, and it suggests that the jet is composed of plasma filaments, which is in agreement with some radio high-resolution observations of other sources. The gamma-ray emitting region is found to be co-spatial with the optical one, and the analysis of the gamma-optical correlation is consistent with both the geometric interpretation and a synchrotron self-Compton (SSC) origin of the high-energy photons. We propose a geometric scenario where the jet is made up of a pair of emitting plasma filaments in a sort of double-helix curved rotating structure, whose wiggling motion produces changes in the Doppler beaming and can thus explain the observed multi-wavelength long-term variability., Comment: In press for A&A
Published: 2024
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3. The Method of Searching for Rotations of the Polarization Position Angle of Quasars

Author: Savchenko, S. S., Morozova, D. A., Jorstad, S. G., Blinov, D. A., Borman, G. A., Vasilyev, A. A., Grishina, T. S., Zhovtan, A. V., Kopatskaya, E. N., Larionova, E. G., Troitskiy, I. S., Troitskaya, Yu. V., Shishkina, E. V., and Shkodkina, E. A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Observations of quasars show that the polarization position angle of the emission coming from them varies greatly over time, including periods called rotations during which the angle changes in an orderly manner. The study proposes a method for identifying such events and assessing their statistical significance. The operation of the method is demonstrated using the example of long-term polarimetric observations of the blazars CTA 102, 3C 454.3, and OT 081. During the analysis of light curves, 51 rotations of the polarization position angle were found and it was shown that for CTA 102 and 3C 454.3 the rotations are predominantly oriented in one direction., Comment: 21 pages, 12 figures
Published: 2024
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4. Optical variability of the blazar 3C 371: from minute to year timescales

Author: Otero-Santos, J., Raiteri, C. M., Acosta-Pulido, J. A., Carnerero, M. I., Villata, M., Savchenko, S. S., Carosati, D., Chen, W. P., Kurtanidze, S. O., Joner, M. D., Semkov, E., Pursimo, T., Benítez, E., Damljanovic, G., Apolonio, G., Borman, G. A., Bozhilov, V., Galindo-Guil, F. J., Grishina, T. S., Hagen-Thorn, V. A., Hiriart, D., Hsiao, H. Y., Ibryamov, S., Ivanidze, R. Z., Kimeridze, G. N., Kopatskaya, E. N., Kurtanidze, O. M., Larionov, V. M., Larionova, E. G., Larionova, L. V., Minev, M., Morozova, D. A., Nikolashvili, M. G., Ovcharov, E., Sigua, L. A., Stojanovic, M., Troitskiy, I. S., Troitskaya, Yu. V., Tsai, A., Valcheva, A., Vasilyev, A. A., Vince, O., Zaharieva, E., and Zhovtan, A. V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The BL Lac object 3C 371 has been observed by the Transiting Exoplanet Survey Satellite (\textit{TESS}) for approximately a year, between July 2019 and July 2020, with an unmatched 2-minute observing cadence. In parallel, the Whole Earth Blazar Telescope (WEBT) Collaboration organized an extensive observing campaign, providing three years of continuous optical monitoring between 2018 and 2020. These datasets allow for a thorough investigation of the variability of the source. The goal of this study is evaluating the optical variability of 3C 371. Taking advantage of the remarkable cadence of \textit{TESS} data, we aim to characterize the intra-day variability (IDV) displayed by the source and identify its shortest variability timescale. With this estimate, constraints on the size of the emitting region and black hole mass can be calculated. Moreover, WEBT data is used to investigate long-term variability (LTV), including understanding spectral behaviour of the source and the polarization variability. Based on the derived characteristics, information on the origin of the variability on different timescales is extracted. We evaluated the variability applying the variability amplitude tool that quantifies how variable the emission is. Moreover, we employed common tools like ANOVA (ANalysis Of VAariance) tests, wavelet and power spectral density (PSD) analyses to characterize the shortest variability timescales present in the emission and the underlying noise affecting the data. Short- and long-term colour behaviours have been evaluated to understand the spectral behaviour of the source. The polarized emission was analyzed, studying its variability and possible rotation patterns of the electric vector position angle (EVPA). Flux distributions of IDV and LTV were also studied with the aim of linking the flux variations to turbulent and/or accretion disc related processes., Comment: Accepted in A&A, 20 pages, 19 figures
Published: 2024
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5. The variability patterns of the TeV blazar PG 1553+113 from a decade of MAGIC and multi-band observations

Author: MAGIC Collaboration, Abe, H., Abe, S., Abhir, J., Acciari, V. A., Agudo, I., Aniello, T., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Arcaro, C., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., de Almeida, U. Barres, Batković, I., Baxter, J., González, J. Becerra, 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., Mendez, C. Delgado, Depaoli, D., Di Pierro, F., Di Venere, L., Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Emery, G., Escudero, J., Fariña, L., Fattorini, A., Foffano, L., Font, L., Fukami, S., Fukazawa, Y., López, R. J. García, Gasparyan, S., Gaug, M., Paiva, J. G. Giesbrecht, 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., Martínez, I. Jiménez, Jormanainen, J., Kerszberg, D., Kluge, G. W., Kobayashi, Y., Kouch, P. M., Kubo, H., Kushida, J., Lezáun, M. Láinez, Lamastra, A., Leone, F., Lindfors, E., Liodakis, I., Lombardi, S., Longo, F., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Fraga, B. Machado de Oliveira, Majumdar, P., Makariev, M., Maneva, G., Mang, N., Manganaro, M., Mannheim, K., Mariotti, M., Martínez, M., Martínez-Chicharro, M., Mas-Aguilar, A., Mazin, D., Menchiari, S., Mender, S., Miceli, D., Miener, T., Miranda, J. M., Mirzoyan, R., González, M. Molero, 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., Moroni, P. G. Prada, 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., collaborators, MWL, 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., Ramazani, V. Fallah, Giroletti, M., Righini, S., Marchili, N., Patricelli, B., Ghirlanda, G., and Lico, R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: 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., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society. 19 pages, 9 figures. Corresponding authors: Elisa Prandini, Antonio Stamerra, Talvikki Hovatta
Published: 2024
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6. Multi-messenger characterization of Mrk 501 during historically low X-ray and $\gamma$-ray activity

Author: MAGIC collaboration, Abe, H., Abe, S., Acciari, V. A., Agudo, I., Aniello, T., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Arcaro, C., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., de Almeida, U. Barres, Barrio, J. A., Batković, I., Baxter, J., González, J. Becerra, Bednarek, W., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Burelli, I., Busetto, G., Carosi, R., Carretero-Castrillo, M., Castro-Tirado, A. J., Ceribella, G., Chai, Y., Chilingarian, 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., Mendez, C. Delgado, Depaoli, D., Di Pierro, F., Di Venere, L., Espiñeira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Emery, G., Escudero, J., Ramazani, V. Fallah, Fariña, L., Fattorini, A., Foffano, L., Font, L., Fruck, C., Fukami, S., Fukazawa, Y., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Paiva, J. G. Giesbrecht, Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Grau, R., Green, D., Green, J. G., Hadasch, D., Hahn, A., Hassan, T., Heckmann, L., Herrera, J., Hrupec, D., Hütten, M., Imazawa, R., Inada, T., Iotov, R., Ishio, K., Martínez, I. Jiménez, Jormanainen, J., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Linhoff, L., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Lyard, E., Fraga, B. Machado de Oliveira, Majumdar, P., Makariev, M., Maneva, G., Mang, N., Manganaro, M., Mangano, S., Mannheim, K., Mariotti, M., Martínez, M., Mas-Aguilar, A., Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Miranda, J. M., Mirzoyan, R., Molina, E., Mondal, H. A., Moralejo, A., Morcuende, D., Moreno, V., Nakamori, T., Nanci, C., Nava, L., Neustroev, V., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Nishijima, K., Ekoume, T. Njoh, Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Okumura, A., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., Persic, M., Pihet, M., Pirola, G., Podobnik, F., Moroni, P. G. Prada, Prandini, E., Principe, G., Priyadarshi, C., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schleicher, B., Schmidt, K., Schmuckermaier, F., Schubert, J. L., Schweizer, T., Sitarek, J., Sliusar, V., Sobczynska, D., Spolon, A., Stamerra, A., Strišković, J., Strom, D., Strzys, M., Suda, Y., Surić, T., Tajima, H., Takahashi, M., Takeishi, R., Tavecchio, F., Temnikov, P., Terauchi, K., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Acosta, M. Vazquez, Ventura, S., Verguilov, V., Viale, I., Vigorito, C. F., Vitale, V., Vovk, I., Walter, R., Will, M., Wunderlich, C., Yamamoto, T., Zarić, D., groups, Other, collaborations, Cerruti, M., Acosta-Pulido, J. A., Apolonio, G., Bachev, R., Baloković, M., Benítez, E., Björklund, I., Bozhilov, V., Brown, L. F., Bugg, A., Carbonell, W., Carnerero, M. I., Carosati, D., Casadio, C., Chamani, W., Chen, W. P., Chigladze, R. A., Damljanovic, G., Epps, K., Erkenov, A., Feige, M., Finke, J., Fuentes, A., Gazeas, K., Giroletti, M., Grishina, T. S., Gupta, A. C., Gurwell, M. A., Heidemann, E., Hiriart, D., Hou, W. J., Hovatta, T., Ibryamov, S., Joner, M. D., Jorstad, S. G., Kania, J., Kiehlmann, S., Kimeridze, G. N., Kopatskaya, E. N., Kopp, M., Korte, M., Kotas, B., Koyama, S., Kramer, J. A., Kunkel, L., Kurtanidze, S. O., Kurtanidze, O. M., Lähteenmäki, A., López, J. M., Larionov, V. M., Larionova, E. G., Larionova, L. V., Leto, C., Lorey, C., Mújica, R., Madejski, G. M., Marchili, N., Marscher, A. P., Minev, M., Modaressi, A., Morozova, D. A., Mufakharov, T., Myserlis, I., Nikiforova, A. A., Nikolashvili, M. G., Ovcharov, E., Perri, M., Raiteri, C. M., Readhead, A. C. S., Reimer, A., Reinhart, D., Righini, S., Rosenlehner, K., Sadun, A. C., Savchenko, S. S., Scherbantin, A., Schneider, L., Schoch, K., Seifert, D., Semkov, E., Sigua, L. A., Singh, C., Sola, P., Sotnikova, Y., Spencer, M., Steineke, R., Stojanovic, M., Strigachev, A., Tornikoski, M., Traianou, E., Tramacere, A., Troitskaya, Yu. V., Troitskiy, I. S., Trump, J. B., Tsai, A., Valcheva, A., Vasilyev, A. A., Verrecchia, F., Villata, M., Vince, O., Vrontaki, K., Weaver, Z. R., Zaharieva, E., and Zottmann, N.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We study the broadband emission of Mrk 501 using multi-wavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi-LAT, NuSTAR, Swift, GASP-WEBT, and OVRO. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wavebands, with the highest occurring at X-rays and very-high-energy (VHE) $\gamma$-rays. A significant correlation ($>$3$\sigma$) between X-rays and VHE $\gamma$-rays is measured, supporting leptonic scenarios to explain the variable parts of the emission, also during low activity. This is further supported when we extend our data from 2008 to 2020, and identify, for the first time, significant correlations between Swift-XRT and Fermi-LAT. We additionally find correlations between high-energy $\gamma$-rays and radio, with the radio lagging by more than 100 days, placing the $\gamma$-ray emission zone upstream of the radio-bright regions in the jet. Furthermore, Mrk 501 showed a historically low activity in X-rays and VHE $\gamma$-rays from mid-2017 to mid-2019 with a stable VHE flux ($>$0.2 TeV) of 5% the emission of the Crab Nebula. The broadband spectral energy distribution (SED) of this 2-year-long low-state, the potential baseline emission of Mrk 501, can be characterized with one-zone leptonic models, and with (lepto)-hadronic models fulfilling neutrino flux constraints from IceCube. We explore the time evolution of the SED towards the low-state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock., Comment: 55 pages, 30 figures, 14 tables, accepted by APJS. Corresponding authors are L. Heckmann, D. Paneque, S. Gasparyan, M. Cerruti, and N. Sahakyan
Published: 2022
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7. Parameters of the type-IIP supernova SN 2012aw

Author: Nikiforova, A. A., Baklanov, P. V., Blinnikov, S. I., Blinov, D. A., Grishina, T. S., Troitskaya, Yu. V., Morozova, D. A., Kopatskaya, E. N., Larionova, E. G., and Troitsky, I. S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results the photometric observations of the Type IIP supernova SN 2012aw obtained for the time interval from 7 till 371 days after the explosion. Using the previously published values of the photospheric velocities we've computed the hydrodynamic model which simultaneously reproduced the photometry observations and velocity measurements. The model was calculated with the multi-energy group radiation hydrodynamics code STELLA. We found the parameters of the pre-supernova: radius $R = 500 R_\odot$, nickel mass $M(^{56}$Ni$)$ $\sim 0.06 M_\odot$, pre-supernova mass $25 M_\odot$, mass of ejected envelope $23.6 M_\odot$, explosion energy $E \sim 2 \times 10^{51}$ erg. The model progenitor mass $M=25 M_\odot$ significantly exceeds the upper limit mass $M=17 M_\odot$, obtained from analysis the pre-SNe observations. This result confirms once more that the 'Red Supergiant Problem' must be resolved by stellar evolution and supernova explosion theories in interaction with observations., Comment: 7 pages, 8 figures, 3 tables. Accepted for publication in MNRAS
Published: 2021
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8. Short-Timescale Variability of the Blazar Mrk 421 from AstroSat and Simultaneous Multi-Wavelength Observations

Author: Chatterjee, Ritaban, Das, Susmita, Khasnovis, Archishman, Ghosh, Ritesh, Kumari, Neeraj, Naik, Sachindra, Larionov, V. M., Grishina, T. S., Kopatskaya, E. N., Larionova, E. G., Nikiforova, A. A., Morozov, D. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., and Vasilyev, A. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: We study the multi-wavelength variability of the blazar Mrk 421 at minutes to days timescales using simultaneous data at $\gamma$-rays from Fermi, 0.7-20 keV energies from AstroSat, and optical and near-infrared (NIR) wavelengths from ground-based observatories. We compute the shortest variability timescales at all of the above wavebands and find its value to be ~1.1 ks at the hard X-ray energies and increasingly longer at soft X-rays, optical and NIR wavelengths as well as at the GeV energies. We estimate the value of the magnetic field to be 0.5 Gauss and the maximum Lorentz factor of the emitting electrons ~1.6 x $10^5$ assuming that synchrotron radiation cooling drives the shortest variability timescale. Blazars vary at a large range of timescales often from minutes to years. These results, as obtained here from the very short end of the range of variability timescales of blazars, are a confirmation of the leptonic scenario and in particular the synchrotron origin of the X-ray emission from Mrk 421 by relativistic electrons of Lorentz factor as high as $10^5$. This particular mode of confirmation has been possible using minutes to days timescale variability data obtained from AstroSat and simultaneous multi-wavelength observations., Comment: 8 pages, 2 figures, accepted for publication in the Journal of Astrophysics and Astronomy
Published: 2021
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9. VHE gamma-ray detection of FSRQ QSO B1420+326 and modeling of its enhanced broadband state in 2020

Author: Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., 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., Delfino, M., Delgado, J., Mendez, C. Delgado, Depaoli, D., Di Pierro, F., Di Venere, L., Espiñeira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Ferrara, G., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, J. G., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jormanainen, J., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Mender, S., Mićanović, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., Peñil, P., Perennes, C., Persic, M., Moroni, P. G. Prada, Prandini, E., Priyadarshi, C., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tosti, L., Truzzi, S., Tutone, A., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zarić, D., Angioni, R., D'Ammando, F., Ciprini, S., Cheung, C. C., Orienti, M., Pacciani, L., Prajapati, P., Kumar, P., Ganesh, S., Kurtenkov, A., Marchini, A., Carrasco, L., Escobedo, G., Porras, A., Recillas, E., Lähteenmäki, A., Tornikoski, M., Berton, M., Tammi, J., Vera, R. J. C., Jorstad, S. G., Marscher, A. P., Weaver, Z. R., Hart, M., Hallum, M. K., Larionov, V. M., Borman, G. A., Grishina, T. S., Kopatskaya, E. N., Larionova, E. G., Nikiforova, A. A., Morozova, D. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., Hodges, M., Hovatta, T., Kiehlmann, S., Max-Moerbeck, W., Readhead, A. C. S., Reeves, R., and Pearson, T. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Context. QSO B1420+326 is a blazar classified as a Flat Spectrum Radio Quasar (FSRQ). In the beginning of 2020 it underwent an enhanced flux state. An extensive multiwavelength campaign allowed us to trace the evolution of the flare. Aims. We search for 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), ultra-violet, X-ray and gamma-ray bands. We use dedicated optical spectroscopy results to estimate the accretion disk and the dust torus luminosity. We perform 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 drastically increased and the peaks were shifted to higher energies. Follow up observations with the MAGIC telescopes led to the detection of very-high-energy 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., Comment: 20 pages, 15 figures, 7 tables, accepted for publication in A&A
Published: 2020
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10. Two Flares with One Shock: the Interesting Case of 3C 454.3

Author: Liodakis, I., Blinov, D., Jorstad, S. G., Arkharov, A. A., Di Paola, A., Efimova, N. V., Grishina, T. S., Kiehlmann, S., Kopatskaya, E. N., Larionov, V. M., Larionova, L. V., Larionova, E. G., Marscher, A. P., Morozova, D. A., Nikiforova, A. A., Pavlidou, V., Traianou, E., Troitskaya, Yu. V., Troitsky, I. S., Uemura, M., and Weaver, Z. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The quasar 3C 454.3 is a blazar known for its rapid and violent outbursts seen across the electromagnetic spectrum. Using gamma-ray, X-ray, multi-band optical, and very long baseline interferometric data we investigate the nature of two such events that occurred in 2013 and 2014 accompanied by strong variations in optical polarization, including a 230 degree electric vector position angle (EVPA) rotation. Our results suggest that a single disturbance was responsible for both flaring events. We interpret the disturbance as a shock propagating down the jet. Under this interpretation the 2013-flare originated most likely due to changes in the viewing angle caused by perhaps a bent or helical trajectory of the shock upstream of the radio core. The 2014-flare and optical polarization behavior are the result of the shock exiting the 43 GHz radio core, suggesting that shock crossings are one of the possible mechanisms for EVPA rotations., Comment: 14 pages, 10 figures, 2 Tables, accepted for publication in The Astrophysical Journal
Published: 2020
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11. Multi-Wavelength Variability of BL Lacertae Measured with High Time Resolution

Author: Weaver, Zachary R., Williamson, K. E., Jorstad, S. G., Marscher, A. P., Larionov, V. M., Raiteri, C. M., Villata, M., Acosta-Pulido, J. A., Bachev, R., Baida, G. V., Balonek, T. J., Benitez, E., Borman, G. A., Bozhilov, V., Carnerero, M. I., Carosati, D., Chen, W. P., Damljanovic, G., Dhiman, V., Dougherty, D. J., Ehgamberdiev, S. A., Grishina, T. S., Gupta, A. C., Hart, M., Hiriart, D., Hsiao, H. Y., Ibryamov, S., Joner, M., Kimeridze, G. N., Kopatskaya, E. N., Kurtanidze, O. M., Kurtanidze, S. O., Larionova, E. G., Matsumoto, K., Matsumura, R., Minev, M., Mirzaqulov, D. O., Morozova, D. A., Nikiforova, A. A., Nikolashvili, M. G., Ovcharov, E., Rizzi, N., Sadun, A., Savchenko, S. S., Semkov, E., Slater, J. J., Smith, K. L., Stojanovic, M., Strigachev, A., Troitskaya, Yu. V., Troitsky, I. S., Tsai, A. L., Vince, O., Valcheva, A., Vasilyev, A. A., Zaharieva, E., and Zhovtan, A. V.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: In an effort to locate the sites of emission at different frequencies and physical processes causing variability in blazar jets, we have obtained high time-resolution observations of BL Lacertae over a wide wavelength range: with the \emph{Transiting Exoplanet Survey Satellite} (TESS) at 6,000-10,000 \AA\ with 2-minute cadence; with the Neil Gehrels \emph{Swift} satellite at optical, UV, and X-ray bands; with the Nuclear Spectroscopic Telescope Array at hard X-ray bands; with the \emph{Fermi} Large Area Telescope at $\gamma$-ray energies; and with the Whole Earth Blazar Telescope for measurement of the optical flux density and polarization. All light curves are correlated, with similar structure on timescales from hours to days. The shortest timescale of variability at optical frequencies observed with TESS is $\sim 0.5$ hr. The most common timescale is $13\pm1$~hr, comparable with the minimum timescale of X-ray variability, 14.5 hr. The multi-wavelength variability properties cannot be explained by a change solely in the Doppler factor of the emitting plasma. The polarization behavior implies that there are both ordered and turbulent components to the magnetic field in the jet. Correlation analysis indicates that the X-ray variations lag behind the $\gamma$-ray and optical light curves by up to $\sim 0.4$ days. The timescales of variability, cross-frequency lags, and polarization properties can be explained by turbulent plasma that is energized by a shock in the jet and subsequently loses energy to synchrotron and inverse Compton radiation in a magnetic field of strength $\sim3$ G, Comment: 33 pages, 25 figures, 14 tables. Accepted to ApJ
Published: 2020

12. Unravelling the complex behavior of Mrk 421 with simultaneous X-ray and VHE observations during an extreme flaring activity in April 2013

Author: MAGIC collaboration, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babic, A., Banerjee, B., de Almeida, U. Barres, Barrio, J. A., Gonzalez, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bosnjak, Z., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Del Puppo, F., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Espineira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Ferrara, G., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., Lopez, R. J. Garcia, Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinovic, N., Green, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Hutten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kajiwara, Y., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Lopez-Coto, R., Lopez-Oramas, A., Loporchio, S., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Mazin, D., Mender, S., Micanovic, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletic, L., Penil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Snidaric, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Suric, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Tosti, L., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zaric, D., groups, Other, Petropoulou, M., Finke, J., D'Ammando, F., Balokovic, M., Madejski, G., Mori, K., Puccetti, Simonetta, Leto, C., Perri, M., Verrecchia, F., Villata, M., Raiteri, C. M., Agudo, I., Bachev, R., Berdyugin, A., Blinov, D. A., Chanishvili, R., Chen, W. P., Chigladze, R., Damljanovic, G., Eswaraiah, C., Grishina, T. S., Ibryamov, S., Jordan, B., Jorstad, S. G., Joshi, M., Kopatskaya, E. N., Kurtanidze, O. M., Kurtanidze, S. O., Larionova, E. G., Larionova, L. V., Larionov, V. M., Latev, G., Lin, H. C., Marscher, A. P., Mokrushina, A. A., Morozova, D. A., Nikolashvili, M. G., Semkov, E., Smith, P. S., Strigachev, A., Troitskaya, Yu. V., Troitsky, I. S., Vince, O., Barnes, J., Guever, T., Moody, J. W., Sadun, A. C., Hovatta, T., Richards, J. L., Max-Moerbeck, W., Readhead, A. C. R., Lahteenmaki, A., Tornikoski, M., Tammi, J., Ramakrishnan, V., and Reinthal, R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on a multi-band variability and correlation study of the TeV blazar Mrk 421 during an exceptional flaring activity observed from 2013 April 11 to 2013 April 19. The study uses, among others, data from GASP-WEBT, Swift, NuSTAR, Fermi-LAT, VERITAS, and MAGIC. The large blazar activity, and the 43 hours of simultaneous NuSTAR and MAGIC/VERITAS observations, permitted variability studies on 15 minute time bins, and over three X-ray bands (3-7 keV, 7-30 keV and 30-80 keV) and three very-high-energy (>0.1 TeV, hereafter VHE) gamma-ray bands (0.2-0.4 TeV, 0.4-0.8 TeV and >0.8 TeV). We detected substantial flux variations on multi-hour and sub-hour timescales in all the X-ray and VHE gamma-ray bands. The characteristics of the sub-hour flux variations are essentially energy-independent, while the multi-hour flux variations can have a strong dependence on the energy of the X-ray and the VHE gamma rays. The three VHE bands and the three X-ray bands are positively correlated with no time-lag, but the strength and the characteristics of the correlation changes substantially over time and across energy bands. Our findings favour multi-zone scenarios for explaining the achromatic/chromatic variability of the fast/slow components of the light curves, as well as the changes in the flux-flux correlation on day-long timescales. We interpret these results within a magnetic reconnection scenario, where the multi-hour flux variations are dominated by the combined emission from various plasmoids of different sizes and velocities, while the sub-hour flux variations are dominated by the emission from a single small plasmoid moving across the magnetic reconnection layer., Comment: 46 pages, 17 figures, 9 tables, accepted for publication in ApJ Supplements
Published: 2020
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13. Multiwavelength behaviour of the blazar 3C279: decade-long study from $\gamma$-ray to radio

Author: Larionov, V. M., Jorstad, S. G., Marscher, A. P., Villata, M., Raiteri, C. M., Smith, P. S., Agudo, I., Savchenko, S. S., Morozova, D. A., Acosta-Pulido, J. A., Aller, M. F., Aller, H. D., Andreeva, T. S., Arkharov, A. A., Bachev, R., Bonnoli, G., Borman, G. A., Bozhilov, V., Calcidese, P., Carnerero, M. I., Carosati, D., Casadio, C., Chen, W. -P., Damljanovic, G., Dementyev, A. V., Di Paola, A., Frasca, A., Fuentes, A., Gómez, J. L., Gónzalez-Morales, P., Giunta, A., Grishina, T. S., Gurwell, M. A., Hagen-Thorn, V. A., Hovatta, T., Ibryamov, S., Joshi, M., Kiehlmann, S., Kim, J. -Y., Kimeridze, G. N., Kopatskaya, E. N., Kovalev, Yu. A., Kovalev, Y. Y., Kurtanidze, O. M., Kurtanidze, S. O., Lähteenmäki, A., Lázaro, C., Larionova, L. V., Larionova, E. G., Leto, G., Marchini, A., Matsumoto, K., Mihov, B., Minev, M., Mingaliev, M. G., Mirzaqulov, D., Dimitrova, R. V. Muñoz, Myserlis, I., Nikiforova, A. A., Nikolashvili, M. G., Nizhelsky, N. A., Ovcharov, E., Pressburger, L. D., Rakhimov, I. A., Righini, S., Rizzi, N., Sadakane, K., Sadun, A. C., Samal, M. R., Sanchez, R. Z., Semkov, E., Sergeev, S. G., Sigua, L. A., Slavcheva-Mihova, L., Sola, P., Sotnikova, Yu. V., Strigachev, A., Thum, C., Traianou, E., Troitskaya, Yu. V., Troitsky, I. S., Tsybulev, P. G., Vasilyev, A. A., Vince, O., Weaver, Z. R., Williamson, K. E., and Zhekanis, G. V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: We report the results of decade-long (2008-2018) $\gamma$-ray to 1 GHz radio monitoring of the blazar 3C 279, including GASP/WEBT, $\it{Fermi}$ and $\it{Swift}$ data, as well as polarimetric and spectroscopic data. The X-ray and $\gamma$-ray light curves correlate well, with no delay > 3 hours, implying general co-spatiality of the emission regions. The $\gamma$-ray-optical flux-flux relation changes with activity state, ranging from a linear to a more complex dependence. The behaviour of the Stokes parameters at optical and radio wavelengths, including 43 GHz VLBA images, supports either a predominantly helical magnetic field or motion of the radiating plasma along a spiral path. Apparent speeds of emission knots range from 10 to 37c, with the highest values requiring bulk Lorentz factors close to those needed to explain $\gamma$-ray variability on very short time scales. The Mg II emission line flux in the `blue' and `red' wings correlates with the optical synchrotron continuum flux density, possibly providing a variable source of seed photons for inverse Compton scattering. In the radio bands we find progressive delays of the most prominent light curve maxima with decreasing frequency, as expected from the frequency dependence of the $\tau=1$ surface of synchrotron self-absorption. The global maximum in the 86 GHz light curve becomes less prominent at lower frequencies, while a local maximum, appearing in 2014, strengthens toward decreasing frequencies, becoming pronounced at $\sim5$ GHz. These tendencies suggest different Doppler boosting of stratified radio-emitting zones in the jet., Comment: 21 pages, 18 figures, accepted for publication in MNRAS
Published: 2020
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14. Quasi-periodic behaviour in the optical and {\gamma}-ray light curves of blazars 3C 66A and B2 1633+38

Author: Otero-Santos, J., Acosta-Pulido, J. A., González, J. Becerra, Raiteri, C. M., Larionov, V. M., Peñil, P., Smith, P. S., Niebla, C. Ballester, Borman, G. A., Carnerero, M. I., Segura, N. Castro, Grishina, T. S., Kopatskaya, E. N., Larionova, E. G., Morozova, D. A., Nikiforova, A. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., and Villata, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on quasi-periodic variability found in two blazars included in the Steward Observatory Blazar Monitoring data sample: the BL Lac object 3C 66A and the Flat Spectrum Radio Quasar B2 1633+38. We collect optical photometric and polarimetric data in V and R bands of these sources from different observatories: St. Petersburg University, Crimean Astrophysical Observatory, WEBT-GASP, Catalina Real-Time Transient Survey, Steward Observatory, STELLA Robotic Observatory and Katzman Automatic Imaging Telescope. In addition, an analysis of the $\gamma$-ray light curves from $\textit{Fermi}$-LAT is included. Three methods are used to search for any periodic behaviour in the data: the Z-transform Discrete Correlation Function, the Lomb-Scargle periodogram and the Weighted Wavelet Z-transform. We find evidences of possible quasi-periodic variability in the optical photometric data of both sources with periods of $\sim$3 years for 3C 66A and $\sim$1.9 years for B2 1633+38, with significances between 3$\sigma$ and 5$\sigma$. Only B2 1633+38 shows evidence of this behaviour in the optical polarized data set at a confidence level of 2$\sigma$-4$\sigma$. This is the first reported evidence of quasi-periodic behaviour in the optical light curve of B2 1633+38. Also a hint of quasi-periodic behaviour is found in the $\gamma$-ray light curve of B2 1633+38 with a confidence level $\geqslant$2$\sigma$, while no periodicity is observed for 3C 66A in this energy range. We propose different jet emission models that could explain the quasi-periodic variability and the differences found between these two sources., Comment: Accepted for publication in MNRAS
Published: 2020
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15. Investigating the multiwavelength behaviour of the flat spectrum radio quasar CTA 102 during 2013-2017

Author: D'Ammando, F., Raiteri, C. M., Villata, M., Acosta-Pulido, J. A., Agudo, I., Arkharov, A. A., Bachev, R., Baida, G. V., Benitez, E., Borman, G. A., Boschin, W., Bozhilov, V., Butuzova, M. S., Calcidese, P., Carnerero, M. I., Carosati, D., Casadio, C., Castro-Segura, N., Chen, W. -P., Damljanovic, G., Di Paola, A., Echevarria, J., Efimova, N. V., Ehgamberdiev, Sh. A., Espinosa, C., Fuentes, A., Giunta, A., Gomez, J. L., Grishina, T. S., Gurwell, M. A., Hiriart, D., Jermak, H., Jordan, B., Jorstad, S. G., Joshi, M., Kimeridze, G. N., Kopatskaya, E. N., Kuratov, K., Kurtanidze, O. M., Kurtanidze, S. O., Lahteenmaki, A., Larionov, V. M., Larionova, E. G., Larionova, L. V., Lazaro, C., Lin, C. S., Malmrose, M. P., Marscher, A. P., Matsumoto, K., McBreen, B., Michel, R., Mihov, B., Minev, M., Mirzaqulov, D. O., Molina, S. N., Moody, J. W., Morozova, D. A., Nazarov, S. V., Nikiforova, A. A., Nikolashvili, M. G., Ohlert, J. M., Okhmat, N., Ovcharov, E., Pinna, F., Polakis, T. A., Protasio, C., Pursimo, T., Redondo-Lorenzo, F. J., Rizzi, N., Rodriguez-Coira, G., Sadakane, K., Sadun, A. C., Samal, M. R., Savchenko, S. S., Semkov, E., Sigua, L., Skiff, B. A., Slavcheva-Mihova, L., Smith, P. S., Steele, I. A., Strigachev, A., Tammi, J., Thum, C., Tornikoski, M., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., Vince, O., Hovatta, T., Kiehlmann, S., Max-Moerbeck, W., Readhead, A. C. S., Reeves, R., Pearson, T. J., Mufakharov, T., Sotnikova, Yu. V., and Mingaliev, M. G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a multiwavelength study of the flat-spectrum radio quasar CTA 102 during 2013-2017. We use radio-to-optical data obtained by the Whole Earth Blazar Telescope, 15 GHz data from the Owens Valley Radio Observatory, 91 and 103 GHz data from the Atacama Large Millimeter Array, near-infrared data from the Rapid Eye Monitor telescope, as well as data from the Swift (optical-UV and X-rays) and Fermi ($\gamma$ rays) satellites to study flux and spectral variability and the correlation between flux changes at different wavelengths. Unprecedented $\gamma$-ray flaring activity was observed during 2016 November-2017 February, with four major outbursts. A peak flux of (2158 $\pm$ 63)$\times$10$^{-8}$ ph cm$^{-2}$ s$^{-1}$, corresponding to a luminosity of (2.2 $\pm$ 0.1)$\times$10$^{50}$ erg s$^{-1}$, was reached on 2016 December 28. These four $\gamma$-ray outbursts have corresponding events in the near-infrared, optical, and UV bands, with the peaks observed at the same time. A general agreement between X-ray and $\gamma$-ray activity is found. The $\gamma$-ray flux variations show a general, strong correlation with the optical ones with no time lag between the two bands and a comparable variability amplitude. This $\gamma$-ray/optical relationship is in agreement with the geometrical model that has successfully explained the low-energy flux and spectral behaviour, suggesting that the long-term flux variations are mainly due to changes in the Doppler factor produced by variations of the viewing angle of the emitting regions. The difference in behaviour between radio and higher energy emission would be ascribed to different viewing angles of the jet regions producing their emission., Comment: 24 pages, 18 figures, and 4 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society
Published: 2019
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16. AGILE, Fermi, Swift, and GASP-WEBT multi-wavelength observations of the high-redshift blazar 4C $+$71.07 in outburst

Author: Vercellone, S., Romano, P., Piano, G., Vittorini, V., Donnarumma, I., Munar-Adrover, P., Raiteri, C. M., Villata, M., Verrecchia, F., Lucarelli, F., Pittori, C., Bulgarelli, A., Fioretti, V., Tavani, M., Acosta-Pulido, J. A., Agudo, I., Arkharov, A. A., Bach, U., Bachev, R., Borman, G. A., Butuzova, M. S., Carnerero, M. I., Casadio, C., Damljanovic, G., D'Ammando, F., Di Paola, A., Doroshenko, V. T., Efimova, N. V., Ehgamberdiev, Sh. A., Giroletti, M., Gómez, J. L., Grishina, T. S., Järvelä, E., Klimanov, S. A., Kopatskaya, E. N., Kurtanidze, O. M., Lähteenmäki, A., Larionov, V. M., Larionova, L. V., Mihov, B., Mirzaqulov, D. O., Molina, S. N., Morozova, D. A., Nazarov, S. V., Orienti, M., Righini, S., Savchenko, S. S., Semkov, E., Slavcheva-Mihova, L., Strigachev, A., Tornikoski, M., Troitskaya, Yu. V., Vince, O., Cattaneo, P. W., Colafrancesco, S., Longo, F., Morselli, A., Paoletti, F., and Parmiggiani, N.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The flat-spectrum radio quasar 4C $+$71.07 is a high-redshift ($z=2.172$), $\gamma$-loud blazar whose optical emission is dominated by the thermal radiation from accretion disc. 4C $+$71.07 has been detected in outburst twice by the AGILE $\gamma$-ray satellite during the period end of October - mid November 2015, when it reached a $\gamma$-ray flux of the order of $F_{\rm E>100\,MeV} = (1.2 \pm 0.3)\times 10^{-6}$ photons cm$^{-2}$ s$^{-1}$ and $F_{\rm E>100\,MeV} = (3.1 \pm 0.6)\times 10^{-6}$ photons cm$^{-2}$ s$^{-1}$, respectively, allowing us to investigate the properties of the jet and of the emission region. We investigated its spectral energy distribution by means of almost simultaneous observations covering the cm, mm, near-infrared, optical, ultra-violet, X-ray and $\gamma$-ray energy bands obtained by the GASP-WEBT Consortium, the Swift and the AGILE and Fermi satellites. The spectral energy distribution of the second $\gamma$-ray flare (the one whose energy coverage is more dense) can be modelled by means of a one-zone leptonic model, yielding a total jet power of about $4\times10^{47}$ erg s$^{-1}$. During the most prominent $\gamma$-ray flaring period our model is consistent with a dissipation region within the broad-line region. Moreover, this class of high-redshift, large-mass black-hole flat-spectrum radio quasars might be good targets for future $\gamma$-ray satellites such as e-ASTROGAM., Comment: Accepted for publication in A&A. 9 pages, 4 Figures, 3 Tables
Published: 2018
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17. The extreme HBL behaviour of Markarian 501 during 2012

Author: Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, A., Bhattacharyya, W., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Doert, M., Domínguez, A., Prester, D. Dominis, Doro, M., Glawion, D. Eisenacher, Engelkemeier, M., Ramazani, V. Fallah, Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Shore, S. N., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zarić, D., Arbet-Engels, A., Baack, D., Balbo, M., Biland, A., Blank, M., Bretz, T., Bruegge, K., Bulinski, M., Buss, J., Dmytriiev, A., Dorner, D., Einecke, S., Elsaesser, D., Herbst, T., Hildebrand, D., Kortmann, L., Linhoff, L., Mahlke, M., Mannheim, K., Mueller, S. A., Neise, D., Neronov, A., Noethe, M., Oberkirch, J., Paravac, A., Rhode, W., Schleicher, B., Schulz, F., Sedlaczek, K., Shukla, A., Sliusar, V., Walter, R., Archer, A., Benbow, W., Bird, R., Brose, R., Buckley, J. H., Bugaev, V., Christiansen, J. L., Cui, W., Daniel, M. K., Falcone, A., Feng, Q., Finley, J. P., Gillanders, G. H., Gueta, O., Hanna, D., Hervet, O., Holder, J., Hughes, G., Hütten, M., Humensky, T. B., Johnson, C. A., Kaaret, P., Kar, P., Kelley-Hoskins, N., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., Maier, G., McArthur, S., Moriarty, P., Mukherjee, R., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pichel, A., Pohl, M., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Rulten, C., Sadeh, I., Santander, M., Sembroski, G. H., Shahinyan, K., Sushch, I., Tyler, J., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhel, A., Williams, D. A., Williamson, T. J, Zitzer, B., Perri, M., Verrecchia, F., Leto, C., Villata, M., Raiteri, C. M., Jorstad, S. G., Larionov, V. M., Blinov, D. A., Grishina, T. S., Kopatskaya, E. N., Larionova, E. G., Nikiforova, A. A., Morozova, D. A., Troitskaya, Yu. V., Troitsky, I. S., Kurtanidze, O. M., Nikolashvili, M. G., Kurtanidze, S. O., Kimeridze, G. N., Chigladze, R. A., Strigachev, A., Sadun, A. C., Moody, J. W., Chen, W. P., Lin, H. C., Acosta-Pulido, J. A., Arévalo, M. J., Carnerero, M. I., González-Morales, P. A., Manilla-Robles, A., Jermak, H., Steele, I., Mundel, C., Benítez, E., Hiriart, D., Smith, P. S., Max-Moerbeck, W., Readhead, A. C. S., Richards, J. L., Hovatta, T., Lähteenmäki, A., Tornikoski, M., Tammi, J., Georganopoulos, M., and Baring, M. G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: A multiwavelength campaign was organized to take place between March and July of 2012. Excellent temporal coverage was obtained with more than 25 instruments, including the MAGIC, FACT and VERITAS Cherenkov telescopes, the instruments on board the Swift and Fermi spacecraft, and the telescopes operated by the GASP-WEBT collaboration. Mrk 501 showed a very high energy (VHE) gamma-ray flux above 0.2 TeV of $\sim$0.5 times the Crab Nebula flux (CU) for most of the campaign. The highest activity occurred on 2012 June 9, when the VHE flux was $\sim$3 CU, and the peak of the high-energy spectral component was found to be at $\sim$2 TeV. This study reports very hard X-ray spectra, and the hardest VHE spectra measured to date for Mrk 501. The fractional variability was found to increase with energy, with the highest variability occurring at VHE, and a significant correlation between the X-ray and VHE bands. The unprecedentedly hard X-ray and VHE spectra measured imply that their low- and high-energy components peaked above 5 keV and 0.5 TeV, respectively, during a large fraction of the observing campaign, and hence that Mrk 501 behaved like an extreme high-frequency- peaked blazar (EHBL) throughout the 2012 observing season. This suggests that being an EHBL may not be a permanent characteristic of a blazar, but rather a state which may change over time. The one-zone synchrotron self-Compton (SSC) scenario can successfully describe the segments of the SED where most energy is emitted, with a significant correlation between the electron energy density and the VHE gamma-ray activity, suggesting that most of the variability may be explained by the injection of high-energy electrons. The one-zone SSC scenario used reproduces the behaviour seen between the measured X-ray and VHE gamma-ray fluxes, and predicts that the correlation becomes stronger with increasing energy of the X-rays., Comment: 25 pages, 9 figures, accepted for publication in A&A. Corresponding authors: Gareth Hughes (gareth.hughes@cfa.harvard.edu), David Paneque (dpaneque@mppmu.mpg.de), Amit Shukla (amit.shukla@astro.uni-wuerzburg.de)
Published: 2018
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18. Multi-wavelength characterization of the blazar S5~0716+714 during an unprecedented outburst phase

Author: MAGIC Collaboration, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Prester, D. Dominis, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takahashi, M., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zarić, D., Collaboration, Fermi-LAT, Bastieri, D., Gasparrini, D., Lott, B., Rani, B., Thompson, D. J., Collaborators, MWL, Agudo, I., Angelakis, E., Borman, G. A., Casadio, C., Grishina, T. S., Gurwell, M., Hovatta, T., Itoh, R., Järvelä, E., Jermak, H., Jorstad, S., Kopatskaya, E. N., Kraus, A., Krichbaum, T. P., Kuin, N. P. M., Lähteenmäki, A., Larionov, V. M., Larionova, L. V., Lien, A. Y., Madejski, G., Marscher, A., Myserlis, I., Max-Moerbeck, W., Molina, S. N., Morozova, D. A., Nalewajko, K., Pearson, T. J., Ramakrishnan, V., Readhead, A. C. S., Reeves, R. A., Savchenko, S. S., Steele, I. A., Tornikoski, M., Troitskaya, Yu. V., Troitsky, I., Vasilyev, A. A., and Zensus, J. Anton
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The BL Lac object S5~0716+714, a highly variable blazar, underwent an impressive outburst in January 2015 (Phase A), followed by minor activity in February (Phase B). The MAGIC observations were triggered by the optical flux observed in Phase A, corresponding to the brightest ever reported state of the source in the R-band. The comprehensive dataset collected is investigated in order to shed light on the mechanism of the broadband emission. Multi-wavelength light curves have been studied together with the broadband Spectral Energy Distributions (SEDs). The data set collected spans from radio, optical photometry and polarimetry, X-ray, high-energy (HE, 0.1 GeV < E < 100 GeV) with \textit{Fermi}-LAT to the very-high-energy (VHE, E>100 GeV) with MAGIC. The flaring state of Phase A was detected in all the energy bands, providing for the first time a multi-wavelength sample of simultaneous data from the radio band to the VHE. In the constructed SED the \textit{Swift}-XRT+\textit{NuSTAR} data constrain the transition between the synchrotron and inverse Compton components very accurately, while the second peak is constrained from 0.1~GeV to 600~GeV by \textit{Fermi}+MAGIC data. The broadband SED cannot be described with a one-zone synchrotron self-Compton model as it severely underestimates the optical flux in order to reproduce the X-ray to $\gamma$-ray data. Instead we use a two-zone model. The EVPA shows an unprecedented fast rotation. An estimation of the redshift of the source by combined HE and VHE data provides a value of $z = 0.31 \pm 0.02_{stats} \pm 0.05_{sys}$, confirming the literature value. The data show the VHE emission originating in the entrance and exit of a superluminal knot in and out a recollimation shock in the inner jet. A shock-shock interaction in the jet seems responsible for the observed flares and EVPA swing. This scenario is also consistent with the SED modelling.
Published: 2018
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19. Exploring the connection between parsec-scale jet activity and broadband outbursts in 3C 279

Author: Rani, B., Jorstad, S. G., Marscher, A. P., Agudo, I., Sokolovsky, K. V., Larionov, V. M., Smith, P., Mosunova, D. A., Borman, G. A., Grishina, T. S., Kopatskaya, E. N., Mokrushina, A. A., Morozova, D. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., Thum, C., Molina, S. N., and Casadio, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We use a combination of high-resolution very long baseline interferometry (VLBI) radio and multi-wavelength flux density and polarization observations to constrain the physics of the dissipation mechanism powering the broadband flares in 3C 279 during an episode of extreme flaring activity in 2013-2014. Six bright flares superimposed on a long-term outburst are detected at $\gamma$-ray energies. Four of the flares have optical and radio counterparts. The two modes of flaring activity (faster flares sitting on top of a long term outburst) present at radio, optical, $\gamma$-ray frequencies are missing in X-rays. X-ray counterparts are only observed for two flares. The first three flares are accompanied by ejection of a new VLBI component (NC2) suggesting the 43 GHz VLBI core as the site of energy dissipation. Another new component, NC3, is ejected after the last three flares, which suggests that the emission is produced upstream from the core (closer to the black hole). The study therefore indicates multiple sites of energy dissipation in the source. An anti-correlation is detected between the optical percentage polarization (PP) and optical/$\gamma$-ray flux variations, while the PP has a positive correlation with optical/$\gamma$-rays spectral indices. Given that the mean polarization is inversely proportional to the number of cells in the emission region, the PP vs. optical/$\gamma$-ray anti-correlation could be due to more active cells during the outburst than at other times. In addition to the turbulent component, our analysis suggests the presence of a combined turbulent and ordered magnetic field, with the ordered component transverse to the jet axis., Comment: ApJ (in press), 14 pages, 19 figures
Published: 2018
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20. The detection of the blazar S4 0954+65 at very-high-energy with the MAGIC telescopes during an exceptionally high optical state

Author: MAGIC Collaboration, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barres, Barrio, J. A., Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Prester, D. Dominis, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., dić, D. Kuvež, Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takahashi, M., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zarić, D., González, J. Becerra, Tanaka, Y., Ojha, R., Finke, J., Lähteenmäki, A., Järvelä, E., Tornikoski, M., Ramakrishnan, V., Hovatta, T., Jorstad, S. G., Marscher, A. P., Larionov, V. M., Borman, G. A., Grishina, T. S., Kopatskaya, E. N., Larionova, L. V., Morozova, D. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., Agudo, I., Molina, S. N., Casadio, C., Gurwell, M., Carnerero, M. I., Protasio, C., and Pulido, J. A Acosta
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The very-high-energy (VHE, $\gtrsim 100$ GeV) $\gamma$-ray MAGIC observations of the blazar S4 0954+65, were triggered by an exceptionally high flux state of emission in the optical. This blazar has a disputed redshift of z=0.368 or z$\geqslant$0.45 and an uncertain classification among blazar subclasses. The exceptional source state described here makes for an excellent opportunity to understand physical processes in the jet of S4 0954+65 and thus contribute to its classification. We investigate the multiwavelength (MWL) light curve and spectral energy distribution (SED) of the S4 0954+65 blazar during an enhanced state in February 2015 and put it in context with possible emission scenarios. We collect photometric data in radio, optical, X-ray, and $\gamma$ ray. We study both the optical polarization and the inner parsec-scale jet behavior with 43 GHz data. Observations with the MAGIC telescopes led to the first detection of S4 0954+65 at VHE. Simultaneous data with Fermi-LAT at high energy $\gamma$ ray\ (HE, 100 MeV < E < 100 GeV) also show a period of increased activity. Imaging at 43 GHz reveals the emergence of a new feature in the radio jet in coincidence with the VHE flare. Simultaneous monitoring of the optical polarization angle reveals a rotation of approximately 100$^\circ$. (...) The broadband spectrum can be modeled with an emission mechanism commonly invoked for flat spectrum radio quasars, i.e. inverse Compton scattering on an external soft photon field from the dust torus, also known as external Compton. The light curve and SED phenomenology is consistent with an interpretation of a blob propagating through a helical structured magnetic field and eventually crossing a standing shock in the jet, a scenario typically applied to flat spectrum radio quasars (FSRQs) and low-frequency peaked BL Lac objects (LBL)., Comment: 15 pages, 7 figures, submitted to A&A
Published: 2018
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21. The light curves of type II-P SN 2017eaw: first 200 days

Author: Tsvetkov, D. Yu., Shugarov, S. Yu., Volkov, I. M., Pavlyuk, N. N., Vozyakova, O. V., Shatsky, N. I., Nikiforova, A. A., Troitsky, I. S., Troitskaya, Yu. V., and Baklanov, P. V.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present UBVRI photometry of the supernova 2017eaw in NGC 6946, obtained in the period from May 14 until December 7, 2017. We derive dates and magnitudes of maximum light in the UBVRI bands and the parameters of the light curves. We discuss colour evolution, extinction and maximum luminosity of SN 2017eaw. Preliminary modeling is carried out, and the results are in satisfactory agreement with the light curves in the UBVRI bands., Comment: 15 pages, 6 figures, accepted by Astronomy Letters
Published: 2017

22. Multi-wavelength temporal and spectral variability of the blazar OJ 287 during and after the December 2015 flare: a major accretion disc contribution

Author: Kushwaha, P., Gupta, A. C., Wiita, P. J., Gaur, H., Pino, E. M. de Gouveia Dal, Bhagwan, J., Kurtanidze, O. M., Larionov, V. M., Damljanovic, G., Uemura, M., Semkov, E., Strigachev, A., Bachev, R., Vince, O., Gu, Minfeng, Zhang, Z., Abe, T., Agarwal, A., Borman, G. A., Fan, J. H., Grishina, T. S., Hirochi, J., Itoh, R., Kawabata, M., Kopatskaya, E. N., Kurtanidze, S. O., Larionova, E. G., Larionova, L. V., Mishra, A., Morozova, D. A., Nakaoka, T., Nikolashvili, M. G., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., and Vasilyev, A. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: We present a multi-wavelength spectral and temporal analysis of the blazar OJ 287 during its recent activity between December 2015 -- May 2016, showing strong variability in the near-infrared (NIR) to X-ray energies with detection at $\gamma$-ray energies as well. Most of the optical flux variations exhibit strong changes in polarization angle and degree. All the inter-band time lags are consistent with simultaneous emissions. Interestingly, on days with excellent data coverage in the NIR--UV bands, the spectral energy distributions (SEDs) show signatures of bumps in the visible--UV bands, never seen before in this source. The optical bump can be explained as accretion-disk emission associated with the primary black hole of mass $\sim \rm 1.8 \times10^{10} M_{\odot}$ while the little bump feature in the optical-UV appears consistent with line emission. Further, the broadband SEDs extracted during the first flare and during a quiescent period during this span show very different $\gamma$-ray spectra compared to previously observed flare or quiescent spectra. The probable thermal bump in the visible seems to have been clearly present since May 2013, as found by examining all available NIR-optical observations, and favors the binary super-massive black hole model. The simultaneous multi-wavelength variability and relatively weak $\gamma$-ray emission that shows a shift in the SED peak is consistent with $\gamma$-ray emission originating from inverse Compton scattering of photons from the line emission that apparently contributes to the little blue bump., Comment: 24 pages, 6 figures, 2 tables, MNRAS in press
Published: 2017
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23. Exceptional outburst of the blazar CTA 102 in 2012: The GASP-WEBT campaign and its extension

Author: Larionov, V. M., Villata, M., Raiteri, C. M., Jorstad, S. G., Marscher, A. P., Agudo, I., Smith, P. S., Acosta-Pulido, J. A., Arévalo, M. J., Arkharov, A. A., Bachev, R., Blinov, D. A., Borisov, G., Borman, G. A., Bozhilov, V., Bueno, A., Carnerero, M. I., Carosati, D., Casadio, C., Chen, W. P., Clemens, D. P., Di Paola, A., Ehgamberdiev, Sh. A., Gómez, J. L., González-Morales, P. A, Griñón-Marín, A., Grishina, T. S., Hagen-Thorn, V. A., Ibryamov, S., Itoh, R., Kopatskaya, E. N., Koptelova, E., Lázaro, C., Larionova, E. G., Larionova, L. V., Manilla-Robles, A., Metodieva, Y., Milanova, Yu. V., Mirzaqulov, D. O., Molina, S. N., Morozova, D. A., Nazarov, S. V., Ovcharov, E., Peneva, S., Ros, J. A., Sadun, A. C., Savchenko, S. S., Semkov, E., Sergeev, S. G., Strigachev, A., Troitskaya, Yu. V., and Troitsky, I. S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: After several years of quiescence, the blazar CTA 102 underwent an exceptional outburst in 2012 September-October. The flare was tracked from gamma-ray to near-infrared frequencies, including Fermi and Swift data as well as photometric and polarimetric data from several observatories. An intensive GASP-WEBT collaboration campaign in optical and NIR bands, with an addition of previously unpublished archival data and extension through fall 2015, allows comparison of this outburst with the previous activity period of this blazar in 2004-2005. We find remarkable similarity between the optical and gamma-ray behaviour of CTA 102 during the outburst, with a time lag between the two light curves of ~1 hour, indicative of co-spatiality of the optical and gamma-ray emission regions. The relation between the gamma-ray and optical fluxes is consistent with the SSC mechanism, with a quadratic dependence of the SSC gamma-ray flux on the synchrotron optical flux evident in the post-outburst stage. However, the gamma-ray/optical relationship is linear during the outburst; we attribute this to changes in the Doppler factor. A strong harder-when-brighter spectral dependence is seen both the in gamma-ray and optical non-thermal emission. This hardening can be explained by convexity of the UV-NIR spectrum that moves to higher frequencies owing to an increased Doppler shift as the viewing angle decreases during the outburst stage. The overall pattern of Stokes parameter variations agrees with a model of a radiating blob or shock wave that moves along a helical path down the jet., Comment: 11 pages, 14 figures, accepted in MNRAS
Published: 2016
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24. Multiwavelength Study of Quiescent States of Mrk 421 with Unprecedented Hard X-Ray Coverage Provided by NuSTAR in 2013

Author: Baloković, M., Paneque, D., Madejski, G., Furniss, A., Chiang, J., team, the NuSTAR, Ajello, M., Alexander, D. M., Barret, D., Blandford, R., Boggs, S. E., Christensen, F. E., Craig, W. W., Forster, K., Giommi, P., Grefenstette, B. W., Hailey, C. J., Harrison, F. A., Hornstrup, A., Kitaguchi, T., Koglin, J. E., Madsen, K. K., Mao, P. H., Miyasaka, H., Mori, K., Perri, M., Pivovaroff, M. J., Puccetti, S., Rana, V., Stern, D., Tagliaferri, G., Urry, C. M., Westergaard, N. J., Zhang, W. W., Zoglauer, A., collaboration, the VERITAS, Archambault, S., Archer, A. A., Barnacka, A., Benbow, W., Bird, R., Buckley, J., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Connolly, M. P., Cui, W., Dickinson, H. J., Dumm, J., Eisch, J. D., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Fortson, L., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Huetten, M., Haakansson, N., Holder, J., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krause, M., Krennrich, F., Lang, M. J., Maier, G., McArthur, S., Meagher, K., Moriarty, P., Nelson, T., Nieto, D., Ong, R. A., Park, N., Pohl, M., Popkow, A., Pueschel, E., Reynolds, P. T., Richards, G. T., Roache, E., Santander, M., Sembroski, G. H., Shahinyan, K., Smith, A. W., Staszak, D., Telezhinsky, I., Todd, N. W., Tucci, J. V., Tyler, J., Vincent, S., Weinstein, A., Wilhelm, A., Williams, D. A., Zitzer, B., collaboration, the MAGIC, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., de Almeida, U. Barres, Barrio, J., González, J. Becerra, Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., de Angelis, A., De Lotto, B., Wilhelmi, E. D. de Oña, Mendez, C. Delgado, Di Pierro, F., Prester, D. Dominis, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Terrats, D. Garrido, Gaug, M., Giammaria, P., Eisenacher, D., Godinović, N., Muñoz, A. González, Guberman, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Lorenz, E., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas-Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palacio, S., Palatiello, M., Paoletti, R., Paredes, J. M., Paredes-Fortuny, X., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Garcia, J. Rodriguez, Saito, T., Satalecka, K., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L. O., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., collaborators, external, Perkins, J., Verrecchia, F., Leto, C., Böttcher, M., Villata, M., Raiteri, C. M., Acosta-Pulido, J. A., Bachev, R., Berdyugin, A., Blinov, D. A., Carnerero, M. I., Chen, W. P., Chinchilla, P., Damljanovic, G., Eswaraiah, C., Grishina, T. S., Ibryamov, S., Jordan, B., Jorstad, S. G., Joshi, M., Kopatskaya, E. N., Kurtanidze, O. M., Kurtanidze, S. O., Larionova, E. G., Larionova, L. V., Larionov, V. M., Latev, G., Lin, H. C., Marscher, A. P., Mokrushina, A. A., Morozova, D. A., Nikolashvili, M. G., Semkov, E., Strigachev, A., Troitskaya, Yu. V., Troitsky, I. S., Vince, O., Barnes, J., Güver, T., Moody, J. W., Sadun, A. C., Sun, S., Hovatta, T., Richards, J. L., Max-Moerbeck, W., Readhead, A. C., Lähteenmäki, A., Tornikoski, M., Tammi, J., Ramakrishnan, V., Reinthal, R., Angelakis, E., Fuhrmann, L., Myserlis, I., Karamanavis, V., Sievers, A., Ungerechts, H., and Zensus, J. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present coordinated multiwavelength observations of the bright, nearby BL Lac object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very-high-energy (VHE) gamma-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79 keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep power law with a photon index of approximately 3, with no evidence for an exponential cutoff or additional hard components up to about 80 keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure which relates to the two bumps of the broadband SED. In each bump, the variability increases with energy which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi-band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in-situ electron acceleration, and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states., Comment: 32 pages, 14 figures; accepted for publication in ApJ
Published: 2015
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25. Review on the materials of a comprehensive study of pedagogical activity in the context of innovative changes

Author: Agureeva, A. V., primary, Anikeeva, I. G., additional, Aryutkina (Baigusheva), A. N., additional, Bakanova, I. G., additional, Berishvili, O. N., additional, Vandysheva, L. V., additional, Vaseltsova, I. A., additional, Zarubina, O. B., additional, Karnikova, O. P., additional, Kozyreva, M. P., additional, Kurylenko, L. V., additional, Kurina, V. A., additional, Merkulova, L. P., additional, Nikulina, I. V., additional, Ovsyannikova, M. N., additional, Podnebesova, M. I., additional, Podublybina, O. I., additional, Pomelnikova, E. A., additional, Rodina, L. I., additional, Savelyev, A. I., additional, Sanko, A. M., additional, Sokolova, Yu. A., additional, Solovova, N. V., additional, Strekalova, N. B., additional, Troitskaya, Yu. V., additional, Shikhanova, E. G., additional, Yudina, O. V., additional, Povetyeva, L. I., additional, E.Yu. Sysoeva (Motina), E. Yu., additional, and Rudneva, T. I., additional
Published: 2024
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26. Light Curves of the Type II-P Supernova SN 2017eaw: The First 200 Days

Author: Tsvetkov, D. Yu., Shugarov, S. Yu., Volkov, I. M., Pavlyuk, N. N., Vozyakova, O. V., Shatsky, N. I., Nikiforova, A. A., Troitsky, I. S., Troitskaya, Yu. V., and Baklanov, P. V.
Published: 2018
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27. Multimessenger Characterization of Markarian 501 during Historically Low X-Ray and γ-Ray Activity

Author: Abe, H., primary, Abe, S., additional, Acciari, V. A., additional, Agudo, I., additional, Aniello, T., additional, Ansoldi, S., additional, Antonelli, L. A., additional, Arbet-Engels, A., additional, Arcaro, C., additional, Artero, M., additional, Asano, K., additional, Baack, D., additional, Babić, A., additional, Baquero, A., additional, de Almeida, U. Barres, additional, Barrio, J. A., additional, Batković, I., additional, Baxter, J., additional, Becerra González, J., additional, Bednarek, W., additional, Bernardini, E., additional, Bernardos, M., additional, Berti, A., additional, Besenrieder, J., additional, Bhattacharyya, W., additional, Bigongiari, C., additional, Biland, A., additional, Blanch, O., additional, Bonnoli, G., additional, Bošnjak, Ž., additional, Burelli, I., additional, Busetto, G., additional, Carosi, R., additional, Carretero-Castrillo, M., additional, Castro-Tirado, A. J., additional, Ceribella, G., additional, Chai, Y., additional, Chilingarian, A., additional, Cikota, S., additional, Colombo, E., additional, Contreras, J. L., additional, Cortina, J., additional, Covino, S., additional, D’Amico, G., additional, D’Elia, V., additional, Da Vela, P., additional, Dazzi, F., additional, De Angelis, A., additional, De Lotto, B., additional, Del Popolo, A., additional, Delfino, M., additional, Delgado, J., additional, Delgado Mendez, C., additional, Depaoli, D., additional, Di Pierro, F., additional, Di Venere, L., additional, Souto Espiñeira, E. Do, additional, Dominis Prester, D., additional, Donini, A., additional, Dorner, D., additional, Doro, M., additional, Elsaesser, D., additional, Emery, G., additional, Escudero, J., additional, Fallah Ramazani, V., additional, Fariña, L., additional, Fattorini, A., additional, Foffano, L., additional, Font, L., additional, Fruck, C., additional, Fukami, S., additional, Fukazawa, Y., additional, García López, R. J., additional, Garczarczyk, M., additional, Gasparyan, S., additional, Gaug, M., additional, Giesbrecht Paiva, J. G., additional, Giglietto, N., additional, Giordano, F., additional, Gliwny, P., additional, Godinović, N., additional, Grau, R., additional, Green, D., additional, Green, J. G., additional, Hadasch, D., additional, Hahn, A., additional, Hassan, T., additional, Heckmann, L., additional, Herrera, J., additional, Hrupec, D., additional, Hütten, M., additional, Imazawa, R., additional, Inada, T., additional, Iotov, R., additional, Ishio, K., additional, Jiménez Martínez, I., additional, Jormanainen, J., additional, Kerszberg, D., additional, Kobayashi, Y., additional, Kubo, H., additional, Kushida, J., additional, Lamastra, A., additional, Lelas, D., additional, Leone, F., additional, Lindfors, E., additional, Linhoff, L., additional, Lombardi, S., additional, Longo, F., additional, López-Coto, R., additional, López-Moya, M., additional, López-Oramas, A., additional, Loporchio, S., additional, Lorini, A., additional, Lyard, E., additional, Machado de Oliveira Fraga, B., additional, Majumdar, P., additional, Makariev, M., additional, Maneva, G., additional, Mang, N., additional, Manganaro, M., additional, Mangano, S., additional, Mannheim, K., additional, Mariotti, M., additional, Martínez, M., additional, Mas-Aguilar, A., additional, Mazin, D., additional, Menchiari, S., additional, Mender, S., additional, Mićanović, S., additional, Miceli, D., additional, Miener, T., additional, Miranda, J. M., additional, Mirzoyan, R., additional, Molina, E., additional, Mondal, H. A., additional, Moralejo, A., additional, Morcuende, D., additional, Moreno, V., additional, Nakamori, T., additional, Nanci, C., additional, Nava, L., additional, Neustroev, V., additional, Nievas Rosillo, M., additional, Nigro, C., additional, Nilsson, K., additional, Nishijima, K., additional, Njoh Ekoume, T., additional, Noda, K., additional, Nozaki, S., additional, Ohtani, Y., additional, Oka, T., additional, Okumura, A., additional, Otero-Santos, J., additional, Paiano, S., additional, Palatiello, M., additional, Paneque, D., additional, Paoletti, R., additional, Paredes, J. M., additional, Pavletić, L., additional, Persic, M., additional, Pihet, M., additional, Pirola, G., additional, Podobnik, F., additional, Moroni, P. G. Prada, additional, Prandini, E., additional, Principe, G., additional, Priyadarshi, C., additional, Rhode, W., additional, Ribó, M., additional, Rico, J., additional, Righi, C., additional, Rugliancich, A., additional, Sahakyan, N., additional, Saito, T., additional, Sakurai, S., additional, Satalecka, K., additional, Saturni, F. G., additional, Schleicher, B., additional, Schmidt, K., additional, Schmuckermaier, F., additional, Schubert, J. L., additional, Schweizer, T., additional, Sitarek, J., additional, Sliusar, V., additional, Sobczynska, D., additional, Spolon, A., additional, Stamerra, A., additional, Strišković, J., additional, Strom, D., additional, Strzys, M., additional, Suda, Y., additional, Surić, T., additional, Tajima, H., additional, Takahashi, M., additional, Takeishi, R., additional, Tavecchio, F., additional, Temnikov, P., additional, Terauchi, K., additional, Terzić, T., additional, Teshima, M., additional, Tosti, L., additional, Truzzi, S., additional, Tutone, A., additional, Ubach, S., additional, van Scherpenberg, J., additional, Acosta, M. Vazquez, additional, Ventura, S., additional, Verguilov, V., additional, Viale, I., additional, Vigorito, C. F., additional, Vitale, V., additional, Vovk, I., additional, Walter, R., additional, Will, M., additional, Wunderlich, C., additional, Yamamoto, T., additional, Zarić, D., additional, Cerruti, M., additional, Acosta-Pulido, J. A., additional, Apolonio, G., additional, Bachev, R., additional, Baloković, M., additional, Benítez, E., additional, Björklund, I., additional, Bozhilov, V., additional, Brown, L. F., additional, Bugg, A., additional, Carbonell, W., additional, Carnerero, M. I., additional, Carosati, D., additional, Casadio, C., additional, Chamani, W., additional, Chen, W. P., additional, Chigladze, R. A., additional, Damljanovic, G., additional, Epps, K., additional, Erkenov, A., additional, Feige, M., additional, Finke, J., additional, Fuentes, A., additional, Gazeas, K., additional, Giroletti, M., additional, Grishina, T. S., additional, Gupta, A. C., additional, Gurwell,, M. A., additional, Heidemann, E., additional, Hiriart, D., additional, Hou, W. J., additional, Hovatta, T., additional, Ibryamov, S., additional, Joner, M. D., additional, Jorstad, S. G., additional, Kania, J., additional, Kiehlmann, S., additional, Kimeridze, G. N., additional, Kopatskaya, E. N., additional, Kopp, M., additional, Korte, M., additional, Kotas, B., additional, Koyama, S., additional, Kramer, J. A., additional, Kunkel, L., additional, Kurtanidze, S. O., additional, Kurtanidze, O. M., additional, Lähteenmäki, A., additional, López, J. M., additional, Larionov, V. M., additional, Larionova, E. G., additional, Larionova, L. V., additional, Leto, C., additional, Lorey, C., additional, Mújica, R., additional, Madejski, G. M., additional, Marchili, N., additional, Marscher, A. P., additional, Minev, M., additional, Modaressi, A., additional, Morozova, D. A., additional, Mufakharov, T., additional, Myserlis, I., additional, Nikiforova, A. A., additional, Nikolashvili, M. G., additional, Ovcharov, E., additional, Perri, M., additional, Raiteri, C. M., additional, Readhead, A. C. S., additional, Reimer, A., additional, Reinhart, D., additional, Righini, S., additional, Rosenlehner, K., additional, Sadun, A. C., additional, Savchenko, S. S., additional, Scherbantin, A., additional, Schneider, L., additional, Schoch, K., additional, Seifert, D., additional, Semkov, E., additional, Sigua, L. A., additional, Singh, C., additional, Sola, P., additional, Sotnikova, Y., additional, Spencer, M., additional, Steineke, R., additional, Stojanovic, M., additional, Strigachev, A., additional, Tornikoski, M., additional, Traianou, E., additional, Tramacere, A., additional, Troitskaya, Yu. V., additional, Troitskiy, I. S., additional, Trump, J. B., additional, Tsai, A., additional, Valcheva, A., additional, Vasilyev, A. A., additional, Verrecchia, F., additional, Villata, M., additional, Vince, O., additional, Vrontaki, K., additional, Weaver, Z. R., additional, Zaharieva, E., additional, and Zottmann, N., additional
Published: 2023
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28. 3C 66A: Variability in 2007–2015

Author: Hagen-Thorn, V. A., Morozova, D. A., Arkharov, A. A., Hagen-Thorn, E. I., Troitsky, I. S., Troitskaya, Yu. V., Milanova, Yu. V., Volkov, E. V., Takalo, L. O., and Sillanpää, A.
Published: 2017
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29. Blazar spectral variability as explained by a twisted inhomogeneous jet

Author: Raiteri, C. M., Villata, M., Acosta-Pulido, J. A., Agudo, I., Arkharov, A. A., Bachev, R., Baida, G. V., Benítez, E., Borman, G. A., Boschin, W., Bozhilov, V., Butuzova, M. S., Calcidese, P., Carnerero, M. I., Carosati, D., Casadio, C., Castro-Segura, N., Chen, W.-P., Damljanovic, G., DʼAmmando, F., Di Paola, A., Echevarría, J., Efimova, N. V., Ehgamberdiev, Sh. A., Espinosa, C., Fuentes, A., Giunta, A., Gómez, J. L., Grishina, T. S., Gurwell, M. A., Hiriart, D., Jermak, H., Jordan, B., Jorstad, S. G., Joshi, M., Kopatskaya, E. N., Kuratov, K., Kurtanidze, O. M., Kurtanidze, S. O., Lähteenmäki, A., Larionov, V. M., Larionova, E. G., Larionova, L. V., Lázaro, C., Lin, C. S., Malmrose, M. P., Marscher, A. P., Matsumoto, K., McBreen, B., Michel, R., Mihov, B., Minev, M., Mirzaqulov, D. O., Mokrushina, A. A., Molina, S. N., Moody, J. W., Morozova, D. A., Nazarov, S. V., Nikolashvili, M. G., Ohlert, J. M., Okhmat, D. N., Ovcharov, E., Pinna, F., Polakis, T. A., Protasio, C., Pursimo, T., Redondo-Lorenzo, F. J., Rizzi, N., Rodriguez-Coira, G., Sadakane, K., Sadun, A. C., Samal, M. R., Savchenko, S. S., Semkov, E., Skiff, B. A., Slavcheva-Mihova, L., Smith, P. S., Steele, I. A., Strigachev, A., Tammi, J., Thum, C., Tornikoski, M., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., and Vince, O.
Published: 2017
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30. Optical variability of the blazar S4 0954+658 in 2008–2012

Author: Hagen-Thorn, V. A., Larionov, V. M., Arkharov, A. A., Hagen-Thorn, E. I., Blinov, D. A., Morozova, D. A., Troitskaya, Yu. V., Takalo, L. O., and Sillanpyää, A.
Published: 2015
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31. Multiwavelength Observations of the Blazar VER J0521+211 during an Elevated TeV Gamma-Ray State

Author: 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., Barrio, J. A., Batković, I., Baxter, J., Becerra González, J., Bednarek, W., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Burelli, I., Busetto, G., Carosi, R., Carretero-Castrillo, M., Castro-Tirado, A. J., Ceribella, G., Chai, Y., Chilingarian, 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., Do Souto Espiñeira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Emery, G., Escudero, J., Fallah Ramazani, V., Fariña, L., Fattorini, A., Foffano, L., Font, L., Fruck, C., Fukami, S., Fukazawa, Y., García López, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giesbrecht Paiva, J. G., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Grau, R., Green, D., Green, J. G., Hadasch, D., Hahn, A., Hassan, T., Heckmann, L., Herrera, J., Hrupec, D., Hütten, M., Imazawa, R., Inada, T., Iotov, R., Ishio, K., Jiménez Martínez, I., Jormanainen, J., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Linhoff, L., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Lyard, E., Machado de Oliveira Fraga, B., Majumdar, P., Makariev, M., Maneva, G., Mang, N., Manganaro, M., Mangano, S., Mannheim, K., Mariotti, M., Martínez, M., Mas-Aguilar, A., Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Miranda, J. M., Mirzoyan, R., Molina, E., Mondal, H. A., Moralejo, A., Morcuende, D., Moreno, V., Nakamori, T., Nanci, C., Nava, L., Neustroev, V., Nievas Rosillo, M., Nigro, C., Nilsson, K., Nishijima, K., Njoh Ekoume, T., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Okumura, A., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., 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., Rugliancich, A., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schleicher, B., Schmidt, K., Schmuckermaier, F., Schubert, J. L., Schweizer, T., Sitarek, J., Sliusar, V., Sobczynska, D., Spolon, A., Stamerra, A., Strišković, J., Strom, D., Strzys, M., Suda, Y., Surić, T., Tajima, H., Takahashi, M., Takeishi, R., Tavecchio, F., Temnikov, P., Terauchi, K., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Vazquez Acosta, M., Ventura, S., Verguilov, V., Viale, I., Vigorito, C. F., Vitale, V., Vovk, I., Walter, R., Will, M., Wunderlich, C., Yamamoto, T., Zarić, D., Other, Groups, Cerruti, collaborations: M., Acosta-Pulido, J. A., Apolonio, G., Bachev, R., Baloković, M., Benítez, E., Björklund, I., Bozhilov, V., Brown, L. F., Bugg, A., Carbonell, W., Carnerero, M. I., Carosati, D., Casadio, C., Chamani, W., Chen, W. P., Chigladze, R. A., Damljanovic, G., Epps, K., Erkenov, A., Feige, M., Finke, J., Fuentes, A., Gazeas, K., Giroletti, M., Grishina, T. S., Gupta, A. C., Gurwell, M. A., Heidemann, E., Hiriart, D., Hou, W. J., Hovatta, T., Ibryamov, S., Joner, M. D., Jorstad, S. G., Kania, J., Kiehlmann, S., Kimeridze, G. N., Kopatskaya, E. N., Kopp, M., Korte, M., Kotas, B., Koyama, S., Kramer, J. A., Kunkel, L., Kurtanidze, S. O., Kurtanidze, O. M., Lähteenmäki, A., López, J. M., Larionov, V. M., Larionova, E. G., Larionova, L. V., Leto, C., Lorey, C., Mújica, R., Madejski, G. M., Marchili, N., Marscher, A. P., Minev, M., Modaressi, A., Morozova, D. A., Mufakharov, T., Myserlis, I., Nikiforova, A. A., Nikolashvili, M. G., Ovcharov, E., Perri, M., Raiteri, C. M., Readhead, A. C. S., Reimer, A., Reinhart, D., Righini, S., Rosenlehner, K., Sadun, A. C., Savchenko, S. S., Scherbantin, A., Schneider, L., Schoch, K., Seifert, D., Semkov, E., Sigua, L. A., Singh, C., Sola, P., Sotnikova, Y., Spencer, M., Steineke, R., Stojanovic, M., Strigachev, A., Tornikoski, M., Traianou, E., Tramacere, A., Troitskaya, Yu. V., Troitskiy, I. S., Trump, J. B., Tsai, A., Valcheva, A., Vasilyev, A. A., Verrecchia, F., Villata, M., Vince, O., Vrontaki, K., Weaver, Z. R., Zaharieva, E., Zottmann, N., Ministerio de Ciencia e Innovación (España), European Commission, Federal Ministry of Education and Research (Germany), Istituto Nazionale di Fisica Nucleare, Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Department of Atomic Energy (India), Ministry of Education, Culture, Sports, Science and Technology (Japan), Ministry of Education and Science (Bulgaria), and Academy of Finland
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), BL Lacertae objects: individual (VER J0521+211 = RGB J0521.8+2112) – galaxies: active – galaxies: jets – gamma rays: galaxies – radiation mechanisms: non-thermal, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Active galactic nuclei, High energy astrophysics, Blazars, BL Lacertae objects, Relativistic jets, Gamma-rays, Non-thermal radiation sources, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ddc:520, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Full list of authors: Adams, C. B.; Batista, P.; Benbow, W.; Brill, A.; Brose, R.; Buckley, J. H.; Capasso, M.; Christiansen, J. L.; Errando, M.; Feng, Q.; Finley, J. P.; Foote, G. M.; Fortson, L.; Furniss, A.; Gallagher, G.; Gent, A.; Giuri, C.; Hanlon, W. F.; Hanna, D.; Hassan, T.; Hervet, O.; Holder, J.; Hona, B.; Hughes, G.; Humensky, T. B.; Jin, W.; Kaaret, P.; Kertzman, M.; Kieda, D.; Kleiner, T. K.; Krennrich, F.; Kumar, S.; Lang, M. J.; Lundy, M.; Maier, G.; Millis, J.; Moriarty, P.; Mukherjee, R.; Nievas-Rosillo, M.; Ong, R. A.; Otte, A. N.; Patel, S.; Patel, S. R.; Pfrang, K.; Pohl, M.; Prado, R. R.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Ribeiro, D.; Roache, E.; Ryan, J. L.; Sadeh, I; Santander, M.; Sembroski, G. H.; Shang, R.; Stevenson, B.; Tucci, J., V; Vassiliev, V. V.; Wakely, S. P.; Weinstein, A.; Wells, R. M.; Williams, D. A.; Williamson, T. J.; Acciari, V. A.; Aniello, T.; Ansoldi, S.; Antonelli, L. A.; Engels, A. Arbet; Arcaro, C.; Artero, M.; Asano, K.; Baack, D.; Babic, A.; Baquero, A.; de Almeida, U. Barres; Barrio, J. A.; Batkovic, I; Becerra Gonzalez, J.; Bednarek, W.; Bernardini, E.; Bernardos, M.; Berti, A.; Besenrieder, J.; Bhattacharyya, W.; Bigongiari, C.; Biland, A.; Blanch, O.; Bokenkamp, H.; Bonnoli, G.; Bosnjak, Z.; Burelli, I; Busetto, G.; Carosi, R.; Ceribella, G.; Cerruti, M.; Chai, Y.; Chilingarian, 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.; Do Souto Espineira, E.; Prester, D. Dominis; Donini, A.; Dorner, D.; Doro, M.; Elsaesser, D.; Ramazani, V. Fallah; Farina, L.; Fattorini, A.; Font, L.; Fruck, C.; Fukami, S.; Fukazawa, Y.; Garcia Lopez, R. J.; Garczarczyk, M.; Gasparyan, S.; Gaug, M.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinovic, N.; Green, J. G.; Green, D.; Hadasch, D.; Hahn, A.; Hassan, T.; Heckmann, L.; Herrera, J.; Hrupec, D.; Hutten, M.; Inada, T.; Iotov, R.; Ishio, K.; Iwamura, Y.; Jimenez Martinez, I; Jormanainen, J.; Jouvin, L.; Kerszberg, D.; Kobayashi, Y.; Kubo, H.; Kushida, J.; Lamastra, A.; Lelas, D.; Leone, F.; Lindfors, E.; Linhoff, L.; Lombardi, S.; Longo, F.; Lopez-Coto, R.; Lopez-Moya, M.; Lopez-Oramas, A.; Loporchio, S.; Lorini, A.; de Oliveira Fraga, B. Machado; Maggio, C.; Majumdar, P.; Makariev, M.; Maneva, G.; Manganaro, M.; Mannheim, K.; Mariotti, M.; Martinez, M.; Aguilar, A. Mas; Mazin, D.; Menchiari, S.; Mender, S.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Molina, E.; Mondal, H. A.; Moralejo, A.; Morcuende, D.; Moreno, V; Nakamori, T.; Nanci, C.; Nava, L.; Neustroev, V; Nievas Rosillo, M.; Nigro, C.; Nilsson, K.; Nishijima, K.; Noda, K.; Nozaki, S.; Ohtani, Y.; Oka, T.; Otero-Santos, J.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Pavletic, L.; Penil, P.; Persic, M.; Pihet, M.; Moroni, P. G. Prada; Prandini, E.; Priyadarshi, C.; Puljak, I; Rhode, W.; Ribo, M.; Rico, J.; Righi, C.; Rugliancich, A.; Sahakyan, N.; Saito, T.; Sakurai, S.; Satalecka, K.; Saturni, F. G.; Schleicher, B.; Schmidt, K.; Schmuckermaier, F.; Schubert, J. L.; Schweizer, T.; Sitarek, J.; Snidaric, I; Sobczynska, D.; Spolon, A.; Stamerra, A.; Striskovic, J.; Strom, D.; Strzys, M.; Suda, Y.; Suric, T.; Takahashi, M.; Takeishi, R.; Tavecchio, F.; Temnikov, P.; Terzic, T.; Teshima, M.; Tosti, L.; Truzzi, S.; Tutone, A.; Ubach, S.; van Scherpenberg, J.; Vanzo, G.; Vazquez Acosta, M.; Ventura, S.; Verguilov, V.; Viale, I; Vigorito, C. F.; Vitale, V.; Vovk, I; Will, M.; Wunderlich, C.; Yamamoto, T.; Zaric, D.; VERITAS Collaboration; MAGIC Collaboration.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We report on a long-lasting, elevated gamma-ray flux state from VER J0521+211 observed by VERITAS, MAGIC, and Fermi-LAT in 2013 and 2014. The peak integral flux above 200 GeV measured with the nightly binned light curve is (8.8 ± 0.4) × 10−7 photons m−2 s−1, or ∼37% of the Crab Nebula flux. Multiwavelength observations from X-ray, UV, and optical instruments are also presented. A moderate correlation between the X-ray and TeV gamma-ray fluxes was observed, and the X-ray spectrum appeared harder when the flux was higher. Using the gamma-ray spectrum and four models of the extragalactic background light (EBL), a conservative 95% confidence upper limit on the redshift of the source was found to be z ≤ 0.31. Unlike the gamma-ray and X-ray bands, the optical flux did not increase significantly during the studied period compared to the archival low-state flux. The spectral variability from optical to X-ray bands suggests that the synchrotron peak of the spectral energy distribution (SED) may become broader during flaring states, which can be adequately described with a one-zone synchrotron self-Compton model varying the high-energy end of the underlying particle spectrum. The synchrotron peak frequency of the SED and the radio morphology of the jet from the MOJAVE program are consistent with the source being an intermediate-frequency-peaked BL Lac object. © 2022. The Author(s). Published by the American Astronomical Society., This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution in the U.S.; by NSERC in Canada; and by the Helmholtz Association in Germany. This research used resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy's Office of Science, and resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under contract No. DE-AC02-05CH11231. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The MAGIC Collaboration would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF, MPG, and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish Ministerio de Ciencia e Innovación (MICINN) (PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-104114RB-C33, PID2019-105510GB-C31,PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107847RB-C44, PID2019-107988GB-C22); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-400/18.12.2020; and the Academy of Finland grant No. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" (SEV-2016-0588, SEV-2017-0709, CEX2019-000920-S), the Unidad de Excelencia "María de Maeztu" (CEX2019-000918-M, MDM-2015-0509-18-2), and the CERCA program of the Generalitat de Catalunya; by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project uniri-prirod-18-48; by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3; by the Polish National Research Centre grant UMO-2016/22/M/ST9/00382; and by the Brazilian MCTIC, CNPq, and FAPERJ. Q.F. was supported by NSF grant PHY-1806554 at Barnard College.
Published: 2022
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32. Development of communicative competence through distance learning

Author: Troitskaya, Yu. V., primary
Published: 2021
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33. Short-timescale variability of the blazar Mrk 421 from AstroSat and simultaneous multi-wavelength observations

Author: Chatterjee, Ritaban, primary, Das, Susmita, additional, Khasnovis, Archishman, additional, Ghosh, Ritesh, additional, Kumari, Neeraj, additional, Naik, Sachindra, additional, Larionov, V. M., additional, Grishina, T. S., additional, Kopatskaya, E. N., additional, Larionova, E. G., additional, Nikiforova, A. A., additional, Morozov, D. A., additional, Savchenko, S. S., additional, Troitskaya, Yu. V., additional, Troitsky, I. S., additional, and Vasilyev, A. A., additional
Published: 2021
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34. Parameters of the type-IIP supernova SN 2012aw

Author: Nikiforova, A A, primary, Baklanov, P V, additional, Blinnikov, S I, additional, Blinov, D A, additional, Grishina, T S, additional, Troitskaya, Yu V, additional, Morozova, D A, additional, Kopatskaya, E N, additional, Larionova, E G, additional, and Troitsky, I S, additional
Published: 2021
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35. Two Flares with One Shock: The Interesting Case of 3C 454.3

Author: Liodakis, I., primary, Blinov, D., additional, Jorstad, S. G., additional, Arkharov, A. A., additional, Paola, A. Di, additional, Efimova, N. V., additional, Grishina, T. S., additional, Kiehlmann, S., additional, Kopatskaya, E. N., additional, Larionov, V. M., additional, Larionova, L. V., additional, Larionova, E. G., additional, Marscher, A. P., additional, Morozova, D. A., additional, Nikiforova, A. A., additional, Pavlidou, V., additional, Traianou, E., additional, Troitskaya, Yu. V., additional, Troitsky, I. S., additional, Uemura, M., additional, and Weaver, Z. R., additional
Published: 2020
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36. Multiwavelength Variability of BL Lacertae Measured with High Time Resolution

Author: Weaver, Z. R., primary, Williamson, K. E., additional, Jorstad, S. G., additional, Marscher, A. P., additional, Larionov, V. M., additional, Raiteri, C. M., additional, Villata, M., additional, Acosta-Pulido, J. A., additional, Bachev, R., additional, Baida, G. V, additional, Balonek, T. J., additional, Benítez, E., additional, Borman, G. A., additional, Bozhilov, V., additional, Carnerero, M. I., additional, Carosati, D., additional, Chen, W. P., additional, Damljanovic, G., additional, Dhiman, V., additional, Dougherty, D. J., additional, Ehgamberdiev, S. A., additional, Grishina, T. S., additional, Gupta, A. C., additional, Hart, M., additional, Hiriart, D., additional, Hsiao, H. Y., additional, Ibryamov, S., additional, Joner, M., additional, Kimeridze, G. N., additional, Kopatskaya, E. N., additional, Kurtanidze, O. M., additional, Kurtanidze, S. O., additional, Larionova, E. G., additional, Matsumoto, K., additional, Matsumura, R., additional, Minev, M., additional, Mirzaqulov, D. O., additional, Morozova, D. A., additional, Nikiforova, A. A., additional, Nikolashvili, M. G., additional, Ovcharov, E., additional, Rizzi, N., additional, Sadun, A., additional, Savchenko, S. S., additional, Semkov, E., additional, Slater, J. J., additional, Smith, K. L., additional, Stojanovic, M., additional, Strigachev, A., additional, Troitskaya, Yu. V., additional, Troitsky, I. S., additional, Tsai, A. L., additional, Vince, O., additional, Valcheva, A., additional, Vasilyev, A. A., additional, Zaharieva, E., additional, and Zhovtan, A. V., additional
Published: 2020
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37. Unraveling the Complex Behavior of Mrk 421 with Simultaneous X-Ray and VHE Observations during an Extreme Flaring Activity in 2013 April *

Author: Acciari, V. A., primary, Ansoldi, S., additional, Antonelli, L. A., additional, Engels, A. Arbet, additional, Baack, D., additional, Babić, A., additional, Banerjee, B., additional, de Almeida, U. Barres, additional, Barrio, J. A., additional, González, J. Becerra, additional, Bednarek, W., additional, Bellizzi, L. K., additional, Bernardini, E., additional, Berti, A., additional, Besenrieder, J., additional, Bhattacharyya, W., additional, Bigongiari, C., additional, Biland, A., additional, Blanch, O., additional, Bonnoli, G., additional, Bošnjak, Ž., additional, Busetto, G., additional, Carosi, R., additional, Ceribella, G., additional, Cerruti, M., additional, Chai, Y., additional, Chilingarian, A., additional, Cikota, S., additional, Colak, S. M., additional, Colin, U., additional, Colombo, E., additional, Contreras, J. L., additional, Cortina, J., additional, Covino, S., additional, D’Elia, V., additional, Vela, P. Da, additional, Dazzi, F., additional, Angelis, A. De, additional, Lotto, B. De, additional, Puppo, F. Del, additional, Delfino, M., additional, Delgado, J., additional, Depaoli, D., additional, Pierro, F. Di, additional, Venere, L. Di, additional, Souto Espiñeira, E. Do, additional, Prester, D. Dominis, additional, Donini, A., additional, Dorner, D., additional, Doro, M., additional, Elsaesser, D., additional, Ramazani, V. Fallah, additional, Fattorini, A., additional, Ferrara, G., additional, Foffano, L., additional, Fonseca, M. V., additional, Font, L., additional, Fruck, C., additional, Fukami, S., additional, López, R. J. García, additional, Garczarczyk, M., additional, Gasparyan, S., additional, Gaug, M., additional, Giglietto, N., additional, Giordano, F., additional, Gliwny, P., additional, Godinović, N., additional, Green, D., additional, Hadasch, D., additional, Hahn, A., additional, Hassan, T., additional, Herrera, J., additional, Hoang, J., additional, Hrupec, D., additional, Hütten, M., additional, Inada, T., additional, Inoue, S., additional, Ishio, K., additional, Iwamura, Y., additional, Jouvin, L., additional, Kajiwara, Y., additional, Kerszberg, D., additional, Kobayashi, Y., additional, Kubo, H., additional, Kushida, J., additional, Lamastra, A., additional, Lelas, D., additional, Leone, F., additional, Lindfors, E., additional, Lombardi, S., additional, Longo, F., additional, López, M., additional, López-Coto, R., additional, López-Oramas, A., additional, Loporchio, S., additional, de Oliveira Fraga, B. Machado, additional, Maggio, C., additional, Majumdar, P., additional, Makariev, M., additional, Mallamaci, M., additional, Maneva, G., additional, Manganaro, M., additional, Mannheim, K., additional, Maraschi, L., additional, Mariotti, M., additional, Martínez, M., additional, Mazin, D., additional, Mender, S., additional, Mićanović, S., additional, Miceli, D., additional, Miener, T., additional, Minev, M., additional, Miranda, J. M., additional, Mirzoyan, R., additional, Molina, E., additional, Moralejo, A., additional, Morcuende, D., additional, Moreno, V., additional, Moretti, E., additional, Munar-Adrover, P., additional, Neustroev, V., additional, Nigro, C., additional, Nilsson, K., additional, Ninci, D., additional, Nishijima, K., additional, Noda, K., additional, Nogués, L., additional, Nozaki, S., additional, Ohtani, Y., additional, Oka, T., additional, Otero-Santos, J., additional, Palatiello, M., additional, Paneque, D., additional, Paoletti, R., additional, Paredes, J. M., additional, Pavletić, L., additional, Peñil, P., additional, Peresano, M., additional, Persic, M., additional, Moroni, P. G. Prada, additional, Prandini, E., additional, Puljak, I., additional, Rhode, W., additional, Ribó, M., additional, Rico, J., additional, Righi, C., additional, Rugliancich, A., additional, Saha, L., additional, Sahakyan, N., additional, Saito, T., additional, Sakurai, S., additional, Satalecka, K., additional, Schleicher, B., additional, Schmidt, K., additional, Schweizer, T., additional, Sitarek, J., additional, Šnidarić, I., additional, Sobczynska, D., additional, Spolon, A., additional, Stamerra, A., additional, Strom, D., additional, Strzys, M., additional, Suda, Y., additional, Surić, T., additional, Takahashi, M., additional, Tavecchio, F., additional, Temnikov, P., additional, Terzić, T., additional, Teshima, M., additional, Torres-Albà, N., additional, Tosti, L., additional, Scherpenberg, J. van, additional, Vanzo, G., additional, Acosta, M. Vazquez, additional, Ventura, S., additional, Verguilov, V., additional, Vigorito, C. F., additional, Vitale, V., additional, Vovk, I., additional, Will, M., additional, Zarić, D., additional, Collaboration), (MAGIC, additional, Petropoulou, M., additional, Finke, J., additional, D’Ammando, F., additional, Baloković, M., additional, Madejski, G., additional, Mori, K., additional, Puccetti, Simonetta, additional, Leto, C., additional, Perri, M., additional, Verrecchia, F., additional, Villata, M., additional, Raiteri, C. M., additional, Agudo, I., additional, Bachev, R., additional, Berdyugin, A., additional, Blinov, D. A., additional, Chanishvili, R., additional, Chen, W. P., additional, Chigladze, R., additional, Damljanovic, G., additional, Eswaraiah, C., additional, Grishina, T. S., additional, Ibryamov, S., additional, Jordan, B., additional, Jorstad, S. G., additional, Joshi, M., additional, Kopatskaya, E. N., additional, Kurtanidze, O. M., additional, Kurtanidze, S. O., additional, Larionova, E. G., additional, Larionova, L. V., additional, Larionov, V. M., additional, Latev, G., additional, Lin, H. C., additional, Marscher, A. P., additional, Mokrushina, A. A., additional, Morozova, D. A., additional, Nikolashvili, M. G., additional, Semkov, E., additional, Smith, P. S., additional, Strigachev, A., additional, Troitskaya, Yu. V., additional, Troitsky, I. S., additional, Vince, O., additional, Barnes, J., additional, Güver, T., additional, Moody, J. W., additional, Sadun, A. C., additional, Hovatta, T., additional, Richards, J. L., additional, Max-Moerbeck, W., additional, Readhead, A. C. S., additional, Lähteenmäki, A., additional, Tornikoski, M., additional, Tammi, J., additional, Ramakrishnan, V., additional, and Reinthal, R., additional
Published: 2020
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38. Multi-Wavelength Variability of BL Lacertae Measured with High Time Resolution

Author: Nikiforova, A. A., Vasilyev, A. A., Gupta, A. C., Tsai, A. L., Marscher, A. P., Sadun, A., Strigachev, A., Zhovtan, A. V., Valcheva, A., Raiteri, C. M., Morozova, D. A., Carosati, D., Hiriart, D., Dougherty, D. J., Mirzaqulov, D. O., Benitez, E., Larionova, E. G., Kopatskaya, E. N., Evgeni Ovcharov, Semkov, E., Zaharieva, E., Borman, G. A., Damljanovic, G., Kimeridze, G. N., Baida, G. V., Hsiao, H. Y., Troitsky, I. S., Acosta-Pulido, J. A., Slater, J. J., Williamson, K. E., Smith, K. L., Matsumoto, K., Nikolashvili, M. G., Hart, M., Carnerero, M. I., Joner, M., Minev, M., Stojanovic, M., Villata, M., Rizzi, N., Kurtanidze, O. M., Vince, O., Bachev, R., Matsumura, R., Ehgamberdiev, S. A., Jorstad, S. G., Ibryamov, S., Kurtanidze, S. O., Savchenko, S. S., Balonek, T. J., Grishina, T. S., Bozhilov, V., Dhiman, V., Larionov, V. M., Chen, W. P., Troitskaya, Yu V., and Weaver, Zachary R.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: In an effort to locate the sites of emission at different frequencies and physical processes causing variability in blazar jets, we have obtained high time-resolution observations of BL Lacertae over a wide wavelength range: with the \emph{Transiting Exoplanet Survey Satellite} (TESS) at 6,000-10,000 \AA\ with 2-minute cadence; with the Neil Gehrels \emph{Swift} satellite at optical, UV, and X-ray bands; with the Nuclear Spectroscopic Telescope Array at hard X-ray bands; with the \emph{Fermi} Large Area Telescope at $\gamma$-ray energies; and with the Whole Earth Blazar Telescope for measurement of the optical flux density and polarization. All light curves are correlated, with similar structure on timescales from hours to days. The shortest timescale of variability at optical frequencies observed with TESS is $\sim 0.5$ hr. The most common timescale is $13\pm1$~hr, comparable with the minimum timescale of X-ray variability, 14.5 hr. The multi-wavelength variability properties cannot be explained by a change solely in the Doppler factor of the emitting plasma. The polarization behavior implies that there are both ordered and turbulent components to the magnetic field in the jet. Correlation analysis indicates that the X-ray variations lag behind the $\gamma$-ray and optical light curves by up to $\sim 0.4$ days. The timescales of variability, cross-frequency lags, and polarization properties can be explained by turbulent plasma that is energized by a shock in the jet and subsequently loses energy to synchrotron and inverse Compton radiation in a magnetic field of strength $\sim3$ G, Comment: 33 pages, 25 figures, 14 tables. Accepted to ApJ
Published: 2020
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39. Quasi-periodic behaviour in the optical and ��-ray light curves of blazars 3C 66A and B2 1633+38

Author: Otero-Santos, J., Acosta-Pulido, J. A., Gonz��lez, J. Becerra, Raiteri, C. M., Larionov, V. M., Pe��il, P., Smith, P. S., Niebla, C. Ballester, Borman, G. A., Carnerero, M. I., Segura, N. Castro, Grishina, T. S., Kopatskaya, E. N., Larionova, E. G., Morozova, D. A., Nikiforova, A. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., and Villata, M.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences
Abstract: We report on quasi-periodic variability found in two blazars included in the Steward Observatory Blazar Monitoring data sample: the BL Lac object 3C 66A and the Flat Spectrum Radio Quasar B2 1633+38. We collect optical photometric and polarimetric data in V and R bands of these sources from different observatories: St. Petersburg University, Crimean Astrophysical Observatory, WEBT-GASP, Catalina Real-Time Transient Survey, Steward Observatory, STELLA Robotic Observatory and Katzman Automatic Imaging Telescope. In addition, an analysis of the $��$-ray light curves from $\textit{Fermi}$-LAT is included. Three methods are used to search for any periodic behaviour in the data: the Z-transform Discrete Correlation Function, the Lomb-Scargle periodogram and the Weighted Wavelet Z-transform. We find evidences of possible quasi-periodic variability in the optical photometric data of both sources with periods of $\sim$3 years for 3C 66A and $\sim$1.9 years for B2 1633+38, with significances between 3$��$ and 5$��$. Only B2 1633+38 shows evidence of this behaviour in the optical polarized data set at a confidence level of 2$��$-4$��$. This is the first reported evidence of quasi-periodic behaviour in the optical light curve of B2 1633+38. Also a hint of quasi-periodic behaviour is found in the $��$-ray light curve of B2 1633+38 with a confidence level $\geqslant$2$��$, while no periodicity is observed for 3C 66A in this energy range. We propose different jet emission models that could explain the quasi-periodic variability and the differences found between these two sources., Accepted for publication in MNRAS
Published: 2020
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40. Unraveling the Complex Behavior of Mrk 421 with Simultaneous X-Ray and VHE Observations during an Extreme Flaring Activity in 2013 April

Author: Federal Ministry of Education and Research (Germany), Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Istituto Nazionale di Fisica Nucleare, Ministerio de Economía y Competitividad (España), European Commission, Department of Atomic Energy (India), Ministry of Education, Culture, Sports, Science and Technology (Japan), Japan Society for the Promotion of Science, Ministry of Education, Youth and Science (Bulgaria), Academy of Finland, Croatian Science Foundation, University of Rijeka, German Research Foundation, National Centre for Research and Development (Poland), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, National Aeronautics and Space Administration (US), Department of Energy (US), Centre National de la Recherche Scientifique (France), Russian Science Foundation, Gordon and Betty Moore Foundation, John Templeton Foundation, Shota Rustaveli National Science Foundation, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Acciari, Victor, Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Baack, D., Babić, A., Banerjee, B., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, Wlodek, Palatiello, M., Max-Moerbeck, W., MAGIC Collaboration, Readhead, A. C. S., Lähteenmäki, Anne, Tornikoski, Merja, Tammi, J., Martínez, M., Ramakrishnan, V., Ishio, K., Do Souto Espiñeira, E., Reinthal, R., Cerruti, Matteo, Paneque, D., Chai, Y., Chilingarian, A., Fattorini, A., Cikota, S., Colak, S.M., Colin, U., Colombo, E., Sitarek, J., Peresano, M., Contreras, J.L., Mazin, D., Cortina, J., Paoletti, R., Covino, Stefano, D'Elia, V., Da Vela, Paolo, Ferrara, G., Dazzi, F., Maneva, G., de Angelis, A., Mannheim, K., de Lotto, B., Del Puppo, F., Delfino, M., Delgado, J., Paredes, Josep M., Mender, S., Depaoli, D., Foffano, L., Šnidarić, I., Fonseca, M.V., Font, L., Iwamura, Y., Fruck, Christian, Fukami, S., García López, R. J., Garczarczyk, M., Gasparyan, S., Pavletić, L., Finke, J., Sobczynska, D., Miceli, D., Gaug, Markus, Giglietto, N., Jouvin, L., Giordano, F., Gliwny, P., Godinović, N., Green, D., Hadasch, D., Hahn, A., Spolon, A., Peñil, P., Hassan, T., Baloković, M., Kajiwara, Y., Kerszberg, Daniel, Miener, T., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Stamerra, A., Kurtanidze, S.O., Perri, M., Lelas, D., Leone, F., Lindfors, E., Madejski, G., Lombardi, S., Longo, F., López, M., Minev, M., Bigongiari, C., López-Coto, R., Busetto, G., López-Oramas, A., di Pierro, F., Loporchio, S., Machado de Oliveira Fraga, B., Maggio, C., Majumdar, P., Mori, K., Makariev, M., Strom, D., Mallamaci, M., Miranda, J. M., Larionova, Elena G., Mirzoyan, R., Molina, E., Persic, M., Moralejo, A., Morcuende, D., Moreno, Vicente, Moretti, E., Marscher, Alan P., Munar-Adrover, P., Puccetti, Simonetta, Bernardini, E., Larionova, Liyudmila V., Neustroev, V., Nigro, C., Nilsson, Kari, Moroni, P. G. Prada, Ninci, D., Nishijima, K., D'Ammando, F., Noda, K., Nogués, L., Nozaki, S., Ohtani, Y., Larionov, Valeri M., Leto, C., Oka, T., Besenrieder, J., Prandini, E., Puljak, I., Strzys, M., Rhode, W., Ribó, Marc, Rico, J., Righi, C., Rugliancich, A., Latev, G., di Venere, L., Bonnoli, G., Saha, L., Sahakyan, N., Suda, Y., Saito, T., Bhattacharyya, W., Sakurai, S., Satalecka, K., Schleicher, B., Schmidt, K., Lin, H. C., Schweizer, T., Prester, D. Dominis, Surić, T., Takahashi, M., Verrecchia, F., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Herrera, J., Ramazani, V. Fallah, Torres-Albà, N., Biland, A., Tosti, L., Donini, A., van Scherpenberg, J., Vanzo, G., Vázquez Acosta, M., Villata, M., Ventura, S., Bellizzi, L. K., Verguilov, V., Berti, A., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Dorner, D., Blanch, O., Zarić, D., Raiteri, C.M., Hoang, J., Agudo, Iván, Bachev, R., Mokrushina, A. A., Berdyugin, A., Blinov, D.A., Chanishvili, R., Chen, W. P., Chigladze, R., Doro, M., Manganaro, M., Hrupec, D., Bošnjak, Ž., Damljanovic, G., Eswaraiah, C., Morozova, D.A., Grishina, T.S., Ibryamov, S., Jordan, B., Jorstad, S.G., Joshi, M., Kopatskaya, Evgenia N., Hütten, M., Elsaesser, D., Kurtanidze, O.M., Maraschi, L., Nikolashvili, M.G., Semkov, E., Carosi, R., Smith, P. S., Strigachev, A., Troitskaya, Yu. V., Troitsky, I. S., Inada, T., Otero-Santos, J., Mićanović, S., Vince, O., Barnes, J., Güver, T., Mariotti, M., Moody, J.W., Sadun, A. C., Hovatta, T., Ceribella, G., Inoue, S., Richards, J. L., Federal Ministry of Education and Research (Germany), Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Istituto Nazionale di Fisica Nucleare, Ministerio de Economía y Competitividad (España), European Commission, Department of Atomic Energy (India), Ministry of Education, Culture, Sports, Science and Technology (Japan), Japan Society for the Promotion of Science, Ministry of Education, Youth and Science (Bulgaria), Academy of Finland, Croatian Science Foundation, University of Rijeka, German Research Foundation, National Centre for Research and Development (Poland), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, National Aeronautics and Space Administration (US), Department of Energy (US), Centre National de la Recherche Scientifique (France), Russian Science Foundation, Gordon and Betty Moore Foundation, John Templeton Foundation, Shota Rustaveli National Science Foundation, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Acciari, Victor, Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Baack, D., Babić, A., Banerjee, B., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, Wlodek, Palatiello, M., Max-Moerbeck, W., MAGIC Collaboration, Readhead, A. C. S., Lähteenmäki, Anne, Tornikoski, Merja, Tammi, J., Martínez, M., Ramakrishnan, V., Ishio, K., Do Souto Espiñeira, E., Reinthal, R., Cerruti, Matteo, Paneque, D., Chai, Y., Chilingarian, A., Fattorini, A., Cikota, S., Colak, S.M., Colin, U., Colombo, E., Sitarek, J., Peresano, M., Contreras, J.L., Mazin, D., Cortina, J., Paoletti, R., Covino, Stefano, D'Elia, V., Da Vela, Paolo, Ferrara, G., Dazzi, F., Maneva, G., de Angelis, A., Mannheim, K., de Lotto, B., Del Puppo, F., Delfino, M., Delgado, J., Paredes, Josep M., Mender, S., Depaoli, D., Foffano, L., Šnidarić, I., Fonseca, M.V., Font, L., Iwamura, Y., Fruck, Christian, Fukami, S., García López, R. J., Garczarczyk, M., Gasparyan, S., Pavletić, L., Finke, J., Sobczynska, D., Miceli, D., Gaug, Markus, Giglietto, N., Jouvin, L., Giordano, F., Gliwny, P., Godinović, N., Green, D., Hadasch, D., Hahn, A., Spolon, A., Peñil, P., Hassan, T., Baloković, M., Kajiwara, Y., Kerszberg, Daniel, Miener, T., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Stamerra, A., Kurtanidze, S.O., Perri, M., Lelas, D., Leone, F., Lindfors, E., Madejski, G., Lombardi, S., Longo, F., López, M., Minev, M., Bigongiari, C., López-Coto, R., Busetto, G., López-Oramas, A., di Pierro, F., Loporchio, S., Machado de Oliveira Fraga, B., Maggio, C., Majumdar, P., Mori, K., Makariev, M., Strom, D., Mallamaci, M., Miranda, J. M., Larionova, Elena G., Mirzoyan, R., Molina, E., Persic, M., Moralejo, A., Morcuende, D., Moreno, Vicente, Moretti, E., Marscher, Alan P., Munar-Adrover, P., Puccetti, Simonetta, Bernardini, E., Larionova, Liyudmila V., Neustroev, V., Nigro, C., Nilsson, Kari, Moroni, P. G. Prada, Ninci, D., Nishijima, K., D'Ammando, F., Noda, K., Nogués, L., Nozaki, S., Ohtani, Y., Larionov, Valeri M., Leto, C., Oka, T., Besenrieder, J., Prandini, E., Puljak, I., Strzys, M., Rhode, W., Ribó, Marc, Rico, J., Righi, C., Rugliancich, A., Latev, G., di Venere, L., Bonnoli, G., Saha, L., Sahakyan, N., Suda, Y., Saito, T., Bhattacharyya, W., Sakurai, S., Satalecka, K., Schleicher, B., Schmidt, K., Lin, H. C., Schweizer, T., Prester, D. Dominis, Surić, T., Takahashi, M., Verrecchia, F., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Herrera, J., Ramazani, V. Fallah, Torres-Albà, N., Biland, A., Tosti, L., Donini, A., van Scherpenberg, J., Vanzo, G., Vázquez Acosta, M., Villata, M., Ventura, S., Bellizzi, L. K., Verguilov, V., Berti, A., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Dorner, D., Blanch, O., Zarić, D., Raiteri, C.M., Hoang, J., Agudo, Iván, Bachev, R., Mokrushina, A. A., Berdyugin, A., Blinov, D.A., Chanishvili, R., Chen, W. P., Chigladze, R., Doro, M., Manganaro, M., Hrupec, D., Bošnjak, Ž., Damljanovic, G., Eswaraiah, C., Morozova, D.A., Grishina, T.S., Ibryamov, S., Jordan, B., Jorstad, S.G., Joshi, M., Kopatskaya, Evgenia N., Hütten, M., Elsaesser, D., Kurtanidze, O.M., Maraschi, L., Nikolashvili, M.G., Semkov, E., Carosi, R., Smith, P. S., Strigachev, A., Troitskaya, Yu. V., Troitsky, I. S., Inada, T., Otero-Santos, J., Mićanović, S., Vince, O., Barnes, J., Güver, T., Mariotti, M., Moody, J.W., Sadun, A. C., Hovatta, T., Ceribella, G., Inoue, S., and Richards, J. L.
Abstract: We report on a multiband variability and correlation study of the TeV blazar Mrk 421 during an exceptional flaring activity observed from 2013 April 11 to 19. The study uses, among others, data from GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT), Swift, Nuclear Spectroscopic Telescope Array (NuSTAR), Fermi Large Area Telescope, Very Energetic Radiation Imaging Telescope Array System (VERITAS), and Major Atmospheric Gamma Imaging Cherenkov (MAGIC). The large blazar activity and the 43 hr of simultaneous NuSTAR and MAGIC/VERITAS observations permitted variability studies on 15 minute time bins over three X-ray bands (3-7 keV, 7-30 keV, and 30-80 keV) and three very-high-energy (VHE; >0.1 TeV) gamma-ray bands (0.2-0.4 TeV, 0.4-0.8 TeV, and >0.8 TeV). We detected substantial flux variations on multi-hour and sub-hour timescales in all of the X-ray and VHE gamma-ray bands. The characteristics of the sub-hour flux variations are essentially energy independent, while the multi-hour flux variations can have a strong dependence on the energy of the X-rays and the VHE gamma-rays. The three VHE bands and the three X-ray bands are positively correlated with no time lag, but the strength and characteristics of the correlation change substantially over time and across energy bands. Our findings favor multi-zone scenarios for explaining the achromatic/chromatic variability of the fast/slow components of the light curves, as well as the changes in the flux-flux correlation on day-long timescales. We interpret these results within a magnetic reconnection scenario, where the multi-hour flux variations are dominated by the combined emission from various plasmoids of different sizes and velocities, while the sub-hour flux variations are dominated by the emission from a single small plasmoid moving across the magnetic reconnection layer. © 2020. The American Astronomical Society. All rights reserved.
Published: 2020

41. Quasi-periodic behaviour in the optical and γ-ray light curves of blazars 3C 66A and B2 1633+38

Author: Otero-Santos, J, primary, Acosta-Pulido, J A, additional, Becerra González, J, additional, Raiteri, C M, additional, Larionov, V M, additional, Peñil, P, additional, Smith, P S, additional, Ballester Niebla, C, additional, Borman, G A, additional, Carnerero, M I, additional, Castro Segura, N, additional, Grishina, T S, additional, Kopatskaya, E N, additional, Larionova, E G, additional, Morozova, D A, additional, Nikiforova, A A, additional, Savchenko, S S, additional, Troitskaya, Yu V, additional, Troitsky, I S, additional, Vasilyev, A A, additional, and Villata, M, additional
Published: 2020
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42. Multiwavelength behaviour of the blazar 3C 279: decade-long study from γ-ray to radio

Author: Larionov, V M, primary, Jorstad, S G, additional, Marscher, A P, additional, Villata, M, additional, Raiteri, C M, additional, Smith, P S, additional, Agudo, I, additional, Savchenko, S S, additional, Morozova, D A, additional, Acosta-Pulido, J A, additional, Aller, M F, additional, Aller, H D, additional, Andreeva, T S, additional, Arkharov, A A, additional, Bachev, R, additional, Bonnoli, G, additional, Borman, G A, additional, Bozhilov, V, additional, Calcidese, P, additional, Carnerero, M I, additional, Carosati, D, additional, Casadio, C, additional, Chen, W-P, additional, Damljanovic, G, additional, Dementyev, A V, additional, Di Paola, A, additional, Frasca, A, additional, Fuentes, A, additional, Gómez, J L, additional, Gónzalez-Morales, P, additional, Giunta, A, additional, Grishina, T S, additional, Gurwell, M A, additional, Hagen-Thorn, V A, additional, Hovatta, T, additional, Ibryamov, S, additional, Joshi, M, additional, Kiehlmann, S, additional, Kim, J-Y, additional, Kimeridze, G N, additional, Kopatskaya, E N, additional, Kovalev, Yu A, additional, Kovalev, Y Y, additional, Kurtanidze, O M, additional, Kurtanidze, S O, additional, Lähteenmäki, A, additional, Lázaro, C, additional, Larionova, L V, additional, Larionova, E G, additional, Leto, G, additional, Marchini, A, additional, Matsumoto, K, additional, Mihov, B, additional, Minev, M, additional, Mingaliev, M G, additional, Mirzaqulov, D, additional, Muñoz Dimitrova, R V, additional, Myserlis, I, additional, Nikiforova, A A, additional, Nikolashvili, M G, additional, Nizhelsky, N A, additional, Ovcharov, E, additional, Pressburger, L D, additional, Rakhimov, I A, additional, Righini, S, additional, Rizzi, N, additional, Sadakane, K, additional, Sadun, A C, additional, Samal, M R, additional, Sanchez, R Z, additional, Semkov, E, additional, Sergeev, S G, additional, Sigua, L A, additional, Slavcheva-Mihova, L, additional, Sola, P, additional, Sotnikova, Yu V, additional, Strigachev, A, additional, Thum, C, additional, Traianou, E, additional, Troitskaya, Yu V, additional, Troitsky, I S, additional, Tsybulev, P G, additional, Vasilyev, A A, additional, Vince, O, additional, Weaver, Z R, additional, Williamson, K E, additional, and Zhekanis, G V, additional
Published: 2020
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43. COMMUNICATION MOBILITY WITHIN THE STRUCTURE OF PROFESSIONAL COMPETENCE

Author: Troitskaya, Yu. V., primary
Published: 2019
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44. The beamed jet and quasar core of the distant blazar 4C 71.07

Author: Raiteri, C M, primary, Villata, M, additional, Carnerero, M I, additional, Acosta-Pulido, J A, additional, Mirzaqulov, D O, additional, Larionov, V M, additional, Romano, P, additional, Vercellone, S, additional, Agudo, I, additional, Arkharov, A A, additional, Bach, U, additional, Bachev, R, additional, Baitieri, S, additional, Borman, G A, additional, Boschin, W, additional, Bozhilov, V, additional, Butuzova, M S, additional, Calcidese, P, additional, Carosati, D, additional, Casadio, C, additional, Chen, W-P, additional, Damljanovic, G, additional, Di Paola, A, additional, Doroshenko, V T, additional, Efimova, N V, additional, Ehgamberdiev, Sh A, additional, Giroletti, M, additional, Gómez, J L, additional, Grishina, T S, additional, Ibryamov, S, additional, Jermak, H, additional, Jorstad, S G, additional, Kimeridze, G N, additional, Klimanov, S A, additional, Kopatskaya, E N, additional, Kurtanidze, O M, additional, Kurtanidze, S O, additional, Lähteenmäki, A, additional, Larionova, E G, additional, Marscher, A P, additional, Mihov, B, additional, Minev, M, additional, Molina, S N, additional, Moody, J W, additional, Morozova, D A, additional, Nazarov, S V, additional, Nikiforova, A A, additional, Nikolashvili, M G, additional, Ovcharov, E, additional, Peneva, S, additional, Righini, S, additional, Rizzi, N, additional, Sadun, A C, additional, Samal, M R, additional, Savchenko, S S, additional, Semkov, E, additional, Sigua, L A, additional, Slavcheva-Mihova, L, additional, Steele, I A, additional, Strigachev, A, additional, Tornikoski, M, additional, Troitskaya, Yu V, additional, Troitsky, I S, additional, and Vince, O, additional
Published: 2019
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45. Variability of the Blazar 4C 38.41 in 2006–2017

Author: Hagen-Thorn, V. A., primary, Troitskaya, Yu. V., additional, Hagen-Thorn, E. I., additional, Troitsky, I. S., additional, Savchenko, S. S., additional, Arharov, A. A., additional, Efimova, N. V., additional, Klimanov, S. K., additional, and Volkov, E. V., additional
Published: 2019
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46. Detection of the blazar S4 0954+65 at very-high-energy with the MAGIC telescopes during an exceptionally high optical state

Author: Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, Giovanna, Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takahashi, M., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Becerra Gonzalez, Josefa, Tanaka, Y., Ojha, R., Finke, J., Lähteenmäki, A., Järvelä, E., Tornikoski, M., Ramakrishnan, V., Hovatta, T., Jorstad, S. G., Marscher, A. P., Larionov, V. M., Borman, G. A., Grishina, T. S., Kopatskaya, E. N., Larionova, L. V., Morozova, D. A., Savchenko, S. S., Troitskaya, Yu. V., Troitsky, I. S., Vasilyev, A. A., Agudo, I., Molina, S. N., Casadio, C., Gurwell, M., Carnerero, M. I., Protasio, C., and Acosta Pulido, J. A.
Abstract: Astronomy and astrophysics 617, A30 (2018). doi:10.1051/0004-6361/201832624, ims.The very high energy (VHE&100GeV)γ-ray MAGIC observations of the blazar S4 0954+65, were triggered by anexceptionally high flux state of emission in the optical. This blazar has a disputed redshift ofz= 0.368 orz>0.45 and an uncertainclassification among blazar subclasses. The exceptional source state described here makes for an excellent opportunity to understandphysical processes in the jet of S4 0954+65 and thus contribute to its classification.Methods.We investigated the multiwavelength (MWL) light curve and spectral energy distribution (SED) of the S4 0954+65 blazarduring an enhanced state in February 2015 and have put it in context with possible emission scenarios. We collected photometric datain radio, optical, X-ray, andγ-ray. We studied both the optical polarization and the inner parsec-scale jet behavior with 43 GHz data.Results.Observations with the MAGIC telescopes led to the first detection of S4 0954+65 at VHE. Simultaneous data withFermi-LAT at high energyγ-ray(HE, 100 MeV, Published by EDP Sciences, Les Ulis
Published: 2018
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47. AGILE, Fermi, Swift, and GASP/WEBT multi-wavelength observations of the high-redshift blazar 4C +71.07 in outburst

Author: Vercellone, S., primary, Romano, P., additional, Piano, G., additional, Vittorini, V., additional, Donnarumma, I., additional, Munar-Adrover, P., additional, Raiteri, C. M., additional, Villata, M., additional, Verrecchia, F., additional, Lucarelli, F., additional, Pittori, C., additional, Bulgarelli, A., additional, Fioretti, V., additional, Tavani, M., additional, Acosta-Pulido, J. A., additional, Agudo, I., additional, Arkharov, A. A., additional, Bach, U., additional, Bachev, R., additional, Borman, G. A., additional, Butuzova, M. S., additional, Carnerero, M. I., additional, Casadio, C., additional, Damljanovic, G., additional, D’Ammando, F., additional, Di Paola, A., additional, Doroshenko, V. T., additional, Efimova, N. V., additional, Ehgamberdiev, Sh. A., additional, Giroletti, M., additional, Gómez, J. L., additional, Grishina, T. S., additional, Järvelä, E., additional, Klimanov, S. A., additional, Kopatskaya, E. N., additional, Kurtanidze, O. M., additional, Lähteenmäki, A., additional, Larionov, V. M., additional, Larionova, L. V., additional, Mihov, B., additional, Mirzaqulov, D. O., additional, Molina, S. N., additional, Morozova, D. A., additional, Nazarov, S. V., additional, Orienti, M., additional, Righini, S., additional, Savchenko, S. S., additional, Semkov, E., additional, Slavcheva-Mihova, L., additional, Strigachev, A., additional, Tornikoski, M., additional, Troitskaya, Yu. V., additional, Vince, O., additional, Cattaneo, P. W., additional, Colafrancesco, S., additional, Longo, F., additional, Morselli, A., additional, Paoletti, F., additional, and Parmiggiani, N., additional
Published: 2019
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48. Extreme HBL behavior of Markarian 501 during 2012

Author: Ahnen, M. L., primary, Ansoldi, S., additional, Antonelli, L. A., additional, Arcaro, C., additional, Babić, A., additional, Banerjee, B., additional, Bangale, P., additional, Barresde Almeida, U., additional, Barrio, J. A., additional, BecerraGonzález, J., additional, Bednarek, W., additional, Bernardini, E., additional, Berti, A., additional, Bhattacharyya, W., additional, Blanch, O., additional, Bonnoli, G., additional, Carosi, R., additional, Carosi, A., additional, Chatterjee, A., additional, Colak, S. M., additional, Colin, P., additional, Colombo, E., additional, Contreras, J. L., additional, Cortina, J., additional, Covino, S., additional, Cumani, P., additional, Da Vela, P., additional, Dazzi, F., additional, De Angelis, A., additional, De Lotto, B., additional, Delfino, M., additional, Delgado, J., additional, Di ierro, F., additional, Doert, M., additional, Domínguez, A., additional, Dominis Prester, D., additional, Doro, M., additional, Eisenacher lawion, D., additional, Engelkemeier, M., additional, Fallah Ramazani, V., additional, Fernández-Barral, A., additional, Fidalgo, D., additional, Fonseca, M. V., additional, Font, L., additional, Fruck, C., additional, Galindo, D., additional, García López, R. J., additional, Garczarczyk, M., additional, Gaug, M., additional, Giammaria, P., additional, Godinović, N., additional, Gora, D., additional, Guberman, D., additional, Hadasch, D., additional, Hahn, A., additional, Hassan, T., additional, Hayashida, M., additional, Herrera, J., additional, Hose, J., additional, Hrupec, D., additional, Ishio, K., additional, Konno, Y., additional, Kubo, H., additional, Kushida, J., additional, Kuveždić, D., additional, Lelas, D., additional, Lindfors, E., additional, Lombardi, S., additional, Longo, F., additional, López, M., additional, Maggio, C., additional, Majumdar, P., additional, Makariev, M., additional, Maneva, G., additional, Manganaro, M., additional, Maraschi, L., additional, Mariotti, M., additional, Martínez, M., additional, Mazin, D., additional, Menzel, U., additional, Minev, M., additional, Miranda, J. M., additional, Mirzoyan, R., additional, Moralejo, A., additional, Moreno, V., additional, Moretti, E., additional, Nagayoshi, T., additional, Neustroev, V., additional, Niedzwiecki, A., additional, Nievas Rosillo, M., additional, Nigro, C., additional, Nilsson, K., additional, Ninci, D., additional, Nishijima, K., additional, Noda, K., additional, Nogués, L., additional, Paiano, S., additional, Palacio, J., additional, Paneque, D., additional, Paoletti, R., additional, Paredes, J. M., additional, Pedaletti, G., additional, Peresano, M., additional, Perri, L., additional, Persic, M., additional, Prada Moroni, P. G., additional, Prandini, E., additional, Puljak, I., additional, Garcia, J. R., additional, Reichardt, I., additional, Ribó, M., additional, Rico, J., additional, Righi, C., additional, Rugliancich, A., additional, Saito, T., additional, Satalecka, K., additional, Schroeder, S., additional, Schweizer, T., additional, Shore, S. N., additional, Sitarek, J., additional, Šnidarić, I., additional, Sobczynska, D., additional, Stamerra, A., additional, Strzys, M., additional, Surić, T., additional, Takalo, L., additional, Tavecchio, F., additional, Temnikov, P., additional, Terzić, T., additional, Teshima, M., additional, Torres-Albà, N., additional, Treves, A., additional, Tsujimoto, S., additional, Vanzo, G., additional, Vazquez Acosta, M., additional, Vovk, I., additional, Ward, J. E., additional, Will, M., additional, Zarić, D., additional, Arbet-Engels, A., additional, Baack, D., additional, Balbo, M., additional, Biland, A., additional, Blank, M., additional, Bretz, T., additional, Bruegge, K., additional, Bulinski, M., additional, Buss, J., additional, Dmytriiev, A., additional, Dorner, D., additional, Einecke, S., additional, Elsaesser, D., additional, Herbst, T., additional, Hildebrand, D., additional, Kortmann, L., additional, Linhoff, L., additional, Mahlke, M., additional, Mannheim, K., additional, Mueller, S. A., additional, Neise, D., additional, Neronov, A., additional, Noethe, M., additional, Oberkirch, J., additional, Paravac, A., additional, Rhode, W., additional, Schleicher, B., additional, Schulz, F., additional, Sedlaczek, K., additional, Shukla, A., additional, Sliusar, V., additional, Walter, R., additional, Archer, A., additional, Benbow, W., additional, Bird, R., additional, Brose, R., additional, Buckley, J. H., additional, Bugaev, V., additional, Christiansen, J. L., additional, Cui, W., additional, Daniel, M. K., additional, Falcone, A., additional, Feng, Q., additional, Finley, J. P., additional, Gillanders, G. H., additional, Gueta, O., additional, Hanna, D., additional, Hervet, O., additional, Holder, J., additional, Hughes, G., additional, Hütten, M., additional, Humensky, T. B., additional, Johnson, C. A., additional, Kaaret, P., additional, Kar, P., additional, Kelley-Hoskins, N., additional, Kertzman, M., additional, Kieda, D., additional, Krause, M., additional, Krennrich, F., additional, Kumar, S., additional, Lang, M. J., additional, Lin, T. T. Y., additional, Maier, G., additional, McArthur, S., additional, Moriarty, P., additional, Mukherjee, R., additional, O’Brien, S., additional, Ong, R. A., additional, Otte, A. N., additional, Park, N., additional, Petrashyk, A., additional, Pichel, A., additional, Pohl, M., additional, Quinn, J., additional, Ragan, K., additional, Reynolds, P. T., additional, Richards, G. T., additional, Roache, E., additional, Rovero, A. C., additional, Rulten, C., additional, Sadeh, I., additional, Santander, M., additional, Sembroski, G. H., additional, Shahinyan, K., additional, Sushch, I., additional, Tyler, J., additional, Wakely, S. P., additional, Weinstein, A., additional, Wells, R. M., additional, Wilcox, P., additional, Wilhel, A., additional, Williams, D. A., additional, J Williamson, T., additional, Zitzer, B., additional, Perri, M., additional, Verrecchia, F., additional, Leto, C., additional, Villata, M., additional, Raiteri, C. M., additional, Jorstad, S. G., additional, Larionov, V. M., additional, Blinov, D. A., additional, Grishina, T. S., additional, Kopatskaya, E. N., additional, Larionova, E. G., additional, Nikiforova, A. A., additional, Morozova, D. A., additional, Troitskaya, Yu. V., additional, Troitsky, I. S., additional, Kurtanidze, O. M., additional, Nikolashvili, M. G., additional, Kurtanidze, S. O., additional, Kimeridze, G. N., additional, Chigladze, R. A., additional, Strigachev, A., additional, Sadun, A. C., additional, Moody, J. W., additional, Chen, W. P., additional, Lin, H. C., additional, Acosta-Pulido, J. A., additional, Arévalo, M. J., additional, Carnerero, M. I., additional, González-Morales, P. A., additional, Manilla-Robles, A., additional, Jermak, H., additional, Steele, I., additional, Mundell, C., additional, Benítez, E., additional, Hiriart, D., additional, Smith, P. S., additional, Max-Moerbeck, W., additional, Readhead, A. C. S., additional, Richards, J. L., additional, Hovatta, T., additional, Lähteenmäki, A., additional, Tornikoski, M., additional, Tammi, J., additional, Georganopoulos, M., additional, and Baring, M. G., additional
Published: 2018
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49. Exploring the Connection between Parsec-scale Jet Activity and Broadband Outbursts in 3C 279

Author: Rani, B., primary, Jorstad, S. G., additional, Marscher, A. P., additional, Agudo, I., additional, Sokolovsky, K. V., additional, Larionov, V. M., additional, Smith, P., additional, Mosunova, D. A., additional, Borman, G. A., additional, Grishina, T. S., additional, Kopatskaya, E. N., additional, Mokrushina, A. A., additional, Morozova, D. A., additional, Savchenko, S. S., additional, Troitskaya, Yu. V., additional, Troitsky, I. S., additional, Thum, C., additional, Molina, S. N., additional, and Casadio, C., additional
Published: 2018
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50. Detection of the blazar S4 0954+65 at very-high-energy with the MAGIC telescopes during an exceptionally high optical state

Author: Ministerio de Economía y Competitividad (España), Swiss National Science Foundation, Federal Ministry of Education and Research (Germany), Junta de Andalucía, Max Planck Society, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babi¿, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Bednarek, Wlodek, Larionova, Liyudmila V., García López, R. J., Vasilyev, A. A., Paoletti, R., Agudo, Iván, Dominis Prester, D., Paiano, S., Makariev, M., Molina, Sol, Schweizer, T., Majumdar, P., Casadio, Carolina, Gurwell, M., Carnerero, M. I., Ishio, K., Kuveždi¿, D., Protasio, C., Ceribella, G., Bonnoli, G., Konno, Y., Chatterjee, A., Satalecka, K., Colak, S.M., Godinović, N., Rugliancich, A., Moralejo, A., Colin, P., Tsujimoto, S., Colombo, E., Contreras, J.L., Cortina, J., Manganaro, M., Mariotti, M., Covino, Stefano, Dorner, D., di Pierro, F., Mannheim, K., Nogués, L., Doro, M., Lelas, D., Teshima, M., Noda, K., Einecke, S., Biland, A., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, Asunción, Moreno, Vicente, Fidalgo, Darío, Gora, D., Gaug, Markus, Moretti, E., Righi, C., Guberman, D., Martínez, M., Lähteenmäki, Anne, Rico, J., Hadasch, D., Hahn, A., Hassan, T., Palacio, J., Peresano, M., Hayashida, M., Paneque, D., Kushida, J., Persic, M., Terzi¿, T., Lindfors, E., Blanch, O., Temnikov, P., Lombardi, S., Longo, F., López, M., Saito, T., Šnidari¿, I., Maggio, C., Berse, R. Ch., Maraschi, L., Finke, J., Masuda, S., Delgado, J., Ojha, R., Mazin, D., Mielke, K., Minev, M., Torres-Albà, N., Vázquez Acosta, M., Miranda, J. M., Nagayoshi, T., Mirzoyan, R., Treves, A., Neustroev, V., Delfino, M., Niedzwiecki, A., Sobczynska, D., Dazzi, F., Morozova, D.A., Nievas Rosillo, M., Garczarczyk, M., Nigro, C., Nilsson, Kari, Ninci, D., Järvelä, E., Hovatta, T., Nishijima, K., Prada Moroni, P. G., Pedaletti, G., Tornikoski, Merja, Bernardini, E., Prandini, E., Vovk, I., Fruck, Christian, Acosta-Pulido, J. A., Puljak, I., Kubo, H., García, J. R, Reichardt, I., Rhode, W., Savchenko, S. S., Ribó, Marc, Stamerra, A., Sitarek, J., Troitskaya, Yu. V., Da Vela, Paolo, Strzys, M., Jorstad, S.G., Hrupec, D., Cumani, P., Surić, T., Takahashi, M., Takalo, L., Berti, A., Carosi, R., Tavecchio, F., Bhattacharyya, W., Vanzo, G., Carosi, A., Font, L., Ward, J. E., Maneva, G., Fonseca, M.V., Will, M., Zari¿, D., Becerra González, J., de Angelis, A., Domínguez, A., Tanaka, Y., de Lotto, B., Ramakrishnan, V., Hose, J., Marscher, Alan P., Paredes, Josep M., Herrera, J., Larionov, Valeri M., Borman, G.A., Grishina, T.S., Galindo, D., Giammaria, P., Kopatskaya, Evgenia N., Troitsky, I. S., Ministerio de Economía y Competitividad (España), Swiss National Science Foundation, Federal Ministry of Education and Research (Germany), Junta de Andalucía, Max Planck Society, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babi¿, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Bednarek, Wlodek, Larionova, Liyudmila V., García López, R. J., Vasilyev, A. A., Paoletti, R., Agudo, Iván, Dominis Prester, D., Paiano, S., Makariev, M., Molina, Sol, Schweizer, T., Majumdar, P., Casadio, Carolina, Gurwell, M., Carnerero, M. I., Ishio, K., Kuveždi¿, D., Protasio, C., Ceribella, G., Bonnoli, G., Konno, Y., Chatterjee, A., Satalecka, K., Colak, S.M., Godinović, N., Rugliancich, A., Moralejo, A., Colin, P., Tsujimoto, S., Colombo, E., Contreras, J.L., Cortina, J., Manganaro, M., Mariotti, M., Covino, Stefano, Dorner, D., di Pierro, F., Mannheim, K., Nogués, L., Doro, M., Lelas, D., Teshima, M., Noda, K., Einecke, S., Biland, A., Elsaesser, D., Fallah Ramazani, V., Fernández-Barral, Asunción, Moreno, Vicente, Fidalgo, Darío, Gora, D., Gaug, Markus, Moretti, E., Righi, C., Guberman, D., Martínez, M., Lähteenmäki, Anne, Rico, J., Hadasch, D., Hahn, A., Hassan, T., Palacio, J., Peresano, M., Hayashida, M., Paneque, D., Kushida, J., Persic, M., Terzi¿, T., Lindfors, E., Blanch, O., Temnikov, P., Lombardi, S., Longo, F., López, M., Saito, T., Šnidari¿, I., Maggio, C., Berse, R. Ch., Maraschi, L., Finke, J., Masuda, S., Delgado, J., Ojha, R., Mazin, D., Mielke, K., Minev, M., Torres-Albà, N., Vázquez Acosta, M., Miranda, J. M., Nagayoshi, T., Mirzoyan, R., Treves, A., Neustroev, V., Delfino, M., Niedzwiecki, A., Sobczynska, D., Dazzi, F., Morozova, D.A., Nievas Rosillo, M., Garczarczyk, M., Nigro, C., Nilsson, Kari, Ninci, D., Järvelä, E., Hovatta, T., Nishijima, K., Prada Moroni, P. G., Pedaletti, G., Tornikoski, Merja, Bernardini, E., Prandini, E., Vovk, I., Fruck, Christian, Acosta-Pulido, J. A., Puljak, I., Kubo, H., García, J. R, Reichardt, I., Rhode, W., Savchenko, S. S., Ribó, Marc, Stamerra, A., Sitarek, J., Troitskaya, Yu. V., Da Vela, Paolo, Strzys, M., Jorstad, S.G., Hrupec, D., Cumani, P., Surić, T., Takahashi, M., Takalo, L., Berti, A., Carosi, R., Tavecchio, F., Bhattacharyya, W., Vanzo, G., Carosi, A., Font, L., Ward, J. E., Maneva, G., Fonseca, M.V., Will, M., Zari¿, D., Becerra González, J., de Angelis, A., Domínguez, A., Tanaka, Y., de Lotto, B., Ramakrishnan, V., Hose, J., Marscher, Alan P., Paredes, Josep M., Herrera, J., Larionov, Valeri M., Borman, G.A., Grishina, T.S., Galindo, D., Giammaria, P., Kopatskaya, Evgenia N., and Troitsky, I. S.
Abstract: The very high energy (VHE ¿ 100 GeV) -ray MAGIC observations of the blazar S4 0954+65, were triggered by an exceptionally high flux state of emission in the optical. This blazar has a disputed redshift of z = 0.368 or z ¿ 0.45 and an uncertain classification among blazar subclasses. The exceptional source state described here makes for an excellent opportunity to understand physical processes in the jet of S4 0954+65 and thus contribute to its classification. Methods. We investigated the multiwavelength (MWL) light curve and spectral energy distribution (SED) of the S4 0954+65 blazar during an enhanced state in February 2015 and have put it in context with possible emission scenarios. We collected photometric data in radio, optical, X-ray, and ¿-ray. We studied both the optical polarization and the inner parsec-scale jet behavior with 43 GHz data. Results. Observations with the MAGIC telescopes led to the first detection of S4 0954+65 at VHE. Simultaneous data with Fermi-LAT at high energy ¿-ray(HE, 100 MeV < E < 100 GeV) also show a period of increased activity. Imaging at 43 GHz reveals the emergence of a new feature in the radio jet in coincidence with the VHE flare. Simultaneous monitoring of the optical polarization angle reveals a rotation of approximately 100. Conclusions. The high emission state during the flare allows us to compile the simultaneous broadband SED and to characterize it in the scope of blazar jet emission models. The broadband spectrum can be modeled with an emission mechanism commonly invoked for flat spectrum radio quasars (FSRQs), that is, inverse Compton scattering on an external soft photon field from the dust torus, also known as external Compton. The light curve and SED phenomenology is consistent with an interpretation of a blob propagating through a helical structured magnetic field and eventually crossing a standing shock in the jet, a scenario typically applied to FSRQs and low-frequency peaked BL Lac objects (LBL). © ESO 2018.
Published: 2018

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