在2017-2019期间，通过尖锐的多波长眼睛调查Blazar TXS 0506+056

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在2017-2019期间，通过尖锐的多波长眼睛调查Blazar TXS 0506+056

Investigating the blazar TXS 0506+056 through sharp multi-wavelength eyes during 2017-2019

论文作者

MAGIC Collaboration, Acciari, V. A., Aniello, T., 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., Batković, I., González, J. Becerra, Bednarek, W., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bökenkamp, H., Bonnoli, G., Bošnjak, Ž., 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., 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, Fariña, L., Fattorini, A., Font, L., Fruck, C., Fukami, S., Fukazawa, Y., 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., Hassan, T., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Iotov, R., Ishio, K., Iwamura, Y., Martínez, I. Jiménez, 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., 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., Mariotti, M., Martínez, M., Aguilar, A. Mas, Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Nakamori, T., Nava, L., Neustroev, V., Rosillo, M. Nievas, 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., Pavletić, L., Peñil, P., Persic, M., Pihet, M., Moroni, P. G. Prada, Prandini, E., Priyadarshi, C., Puljak, I., 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., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strišković, J., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Takeishi, R., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Ventura, S., Verguilov, V., Viale, I., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Wunderlich, C., Yamamoto, T., Zarić, D., Collaboration, OVRO, :, Hodges, M., Hovatta, T., Kiehlmann, S., Liodakis, I., Max-Moerbeck, W., Pearson, T. J., Readhead, A. C. S., Reeves, R. A., Collaboration, Metsähovi, :, Lähteenmaäki, A., Tornikoski, M., Tammi, J., D'Ammando, F., Marchini, A.

论文摘要

Blazar TXS 0506+056于2017年9月成为天体物理社区的焦点，当时IceCube（Icecube-170922a）检测到的高能源中微子在3 $σ$级别与来自该来源的$γ$ -DRARE相关联。如今，这种多通间的光子中性结合仍然是有史以来最重要的。 TXS 0506+056是在ICECUBE-170922A事件之前研究的对象。为了更好地描述其广泛的发射，我们组织了一场持续16个月（2017年11月至2019年2月）的多波长运动，涵盖了无线电频段（Metsähovi，ovro），光学/UV（asas-sn，kva，kva，kva，kva，rem，swift/uvot），x rays（swift/xrt，nustrt，nustar），form use $ nustar和form use $ gath（form form）（forr nustar）（forr use）（form form）（forr use）（form use）（高能（VHE）$γ$射线（魔术）。在$γ$射线中，来源的行为与2017年的行为显着不同：魔术观察显示2018年12月的燃烧活动，而源在其余活动中仅显示了4 $σ$水平的超额（74小时的累积暴露）；费米/LAT观察结果显示出几种短（天至周的时间尺度）的耀斑，与2017年的长期亮度不同。在较低的能量下未检测到明显的耀斑。无线电曲线显示出越来越多的通量趋势，在其他波长中看不到。我们将多波长光谱能量分布建模在液光 - 狂热场景中，其中X光片中的贝特·希特勒和pion-decay级联反应出现，在X射线和X射线中，并且VHE $γ$ rays出现。根据此处介绍的模型，2018年12月$γ$ -Ray耀斑与中微子的发射相关，该中微子发射太短且不够明亮，无法被当前的中微子仪器检测到。

The blazar TXS 0506+056 got into the spotlight of the astrophysical community in September 2017, when a high-energy neutrino detected by IceCube (IceCube-170922A) was associated at the 3 $σ$ level to a $γ$-ray flare from this source. This multi-messenger photon-neutrino association remains, as per today, the most significant one ever observed. TXS 0506+056 was a poorly studied object before the IceCube-170922A event. To better characterize its broad-band emission, we organized a multi-wavelength campaign lasting 16 months (November 2017 to February 2019), covering the radio-band (Metsähovi, OVRO), the optical/UV (ASAS-SN, KVA, REM, Swift/UVOT), the X-rays (Swift/XRT, NuSTAR), the high-energy $γ$ rays (Fermi/LAT) and the very-high-energy (VHE) $γ$ rays (MAGIC). In $γ$ rays, the behaviour of the source was significantly different from the 2017 one: MAGIC observations show the presence of flaring activity during December 2018, while the source only shows an excess at the 4$σ$ level during the rest of the campaign (74 hours of accumulated exposure); Fermi/LAT observations show several short (days-to-week timescale) flares, different from the long-term brightening of 2017. No significant flares are detected at lower energies. The radio light curve shows an increasing flux trend, not seen in other wavelengths. We model the multi-wavelength spectral energy distributions in a lepto-hadronic scenario, in which the hadronic emission emerges as Bethe-Heitler and pion-decay cascade in the X-rays and VHE $γ$ rays. According to the model presented here, the December 2018 $γ$-ray flare was connected to a neutrino emission that was too brief and not bright enough to be detected by current neutrino instruments.

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