Multi-messenger characterization of Mrk 501 during historically low X-ray and $γ$-ray activity

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; 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.; Zottmann, N.

doi:10.48550/arxiv.2210.02547

Cited by 2 publications

(1 citation statement)

References 68 publications

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“…In this contribution we study the emergence of narrow features in VHE 𝛾-ray blazar spectra produced via the decay of neutral pions (𝜋 0 bumps). We focus on high-synchrotron-peaked (HSP) blazars, like Mrk 501, which are often detected at VHE energies [1,4]. In fact, HSPs are the majority of the ∼ 90 extragalactic sources detected at VHE by imaging atmospheric Cherenkov telescopes (see TeVCat catalog1).…”

Section: Introductionmentioning

confidence: 99%

Neutral pion bumps in TeV spectra of X-ray flaring blazars

Πετροπούλου¹,

Mastichiadis²,

Paneque³

et al. 2023

Proceedings of 7th Heidelberg International Symposium on High-Energy Gamma-Ray Astronomy — PoS(Gamma2022)

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Very high-energy (VHE, 𝐸 > 100 GeV) observations of blazar Mrk 501 with MAGIC in 2014 have revealed an unusual narrow spectral feature at ∼ 3 TeV during an extreme X-ray flare. The one-zone synchrotron-self Compton scenario, widely used in blazar broadband spectral modeling, fails to explain the narrow TeV component. Motivated by this rare observation, we propose an alternative model where narrow features in VHE blazar spectra result from the decay of neutral pions (𝜋 0 bumps). These are in turn produced by interactions of protons with hard X-ray photons (> 50 keV) whose number density can increase during flares. No 𝜋 0 bumps are predicted in X-ray "quiescence", as the proton energy is not high enough to exceed the threshold for pion production. We explore the physical conditions needed for the emergence of narrow 𝜋 0 bumps in blazar VHE spectra and apply our model to the observations of Mrk 501. We show that the VHE spectrum of Mrk 501 can still be explained by the model, if the energetic photons are provided by an external source of radiation and protons are intermittently accelerated to a different region from the one producing the X-ray flare itself. We also compute the accompanying TeV muon neutrino flux, and find that this would be hidden in the atmospheric muon background.

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Section: Introductionmentioning

confidence: 99%

Neutral pion bumps in TeV spectra of X-ray flaring blazars

Πετροπούλου¹,

Mastichiadis²,

Paneque³

et al. 2023

Proceedings of 7th Heidelberg International Symposium on High-Energy Gamma-Ray Astronomy — PoS(Gamma2022)

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Multiwavelength monitoring of the nucleus in PBC J2333.9−2343: the giant radio galaxy with a blazar-like core

Hernández-García

Panessa

Bruni

et al. 2023

Monthly Notices of the Royal Astronomical Society

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PBC J2333.9-2343 is a giant radio galaxy at z = 0.047 with a bright central core associated to a blazar nucleus. If the nuclear blazar jet is a new phase of the jet activity, then the small orientation angle suggest a dramatic change of the jet direction. We present observations obtained between September 2018 and January 2019 (cadence larger than three days) with Effeslberg, SMARTS-1.3m, ZTF, ATLAS, Swift, and Fermi-LAT, and between April-July 2019 (daily cadence) with SMARTS-1.3m and ATLAS. Large (>2 ×) flux increases are observed on timescales shorter than a month, which are interpreted as flaring events. The cross correlation between the SMARTS-1.3m monitoring in the NIR and optical shows that these data do not show significant time lag within the measured errors. A comparison of the optical variability properties between non-blazars and blazars AGN shows that PBC J2333.9-2343 has properties more comparable to the latter. The SED of the nucleus shows two peaks, that were fitted with a one zone leptonic model. Our data and modelling shows that the high energy peak is dominated by External Compton from the dusty torus with mild contribution from Inverse Compton from the jet. The derived jet angle of 3 degrees is also typical of a blazar. Therefore, we confirm the presence of a blazar-like core in the center of this giant radio galaxy, likely a Flat Spectrum Radio Quasar with peculiar properties.

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Multi-messenger characterization of Mrk 501 during historically low X-ray and $γ$-ray activity

Cited by 2 publications

References 68 publications

Neutral pion bumps in TeV spectra of X-ray flaring blazars

Neutral pion bumps in TeV spectra of X-ray flaring blazars

Multiwavelength monitoring of the nucleus in PBC J2333.9−2343: the giant radio galaxy with a blazar-like core

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