The broad-band properties of the intermediate synchrotron peaked BL Lac   S2 0109+22 from radio to VHE gamma rays

MAGIC Collaboration: S. Ansoldi (1,20); L. A. Antonelli (2); C. Arcaro; (3); D. Baack (4); A. Babi\'c (5); B. Banerjee (6); P. Bangale (7); U. Barres; de Almeida (7,8); J. A. Barrio (9); J. Becerra Gonz\'alez (10); W. Bednarek; (11); E. Bernardini (12,23); R. Ch. Berse (4); A. Berti (1,24); J.; Besenrieder (7); W. Bhattacharyya (12); C. Bigongiari (2); A. Biland (13); O.; Blanch (14); G. Bonnoli (15); R. Carosi (16); G. Ceribella (7); A. Chatterjee; (6); S. M. Colak (14); P. Colin (7); E. Colombo (10); J. L. Contreras (9); J.; Cortina (14); S. Covino (2); P. Cumani (14); V. D'Elia (2); P. Da Vela (15),; F. Dazzi (2); A. De Angelis (3); B. De Lotto (1); M. Delfino (14,25); J.; Delgado (14,25); F. Di Pierro (3); A. Dom\'inguez (9); D. Dominis Prester; (5); D. Dorner (17); M. Doro (3); S. Einecke (4); D. Elsaesser (4); V. Fallah; Ramazani (18); A. Fattorini (4); A. Fern\'andez-Barral (3); G. Ferrara (2),; D. Fidalgo (9); L. Foffano (3); M. V. Fonseca (9); L. Font (19); C. Fruck; (7); S. Gallozzi (2); R. J. Garc\'ia L\'opez (10); M. Garczarczyk (12); M.; Gaug (19); P. Giammaria (2); N. Godinovi\'c (5); D. Guberman (14); D. Hadasch; (20); A. Hahn (7); T. Hassan (14); M. Hayashida (20); J. Herrera (10); J.; Hoang (9); D. Hrupec (5); S. Inoue (20); K. Ishio (7); Y. Iwamura (20); Y.; Konno (20); H. Kubo (20); J. Kushida (20); A. Lamastra (2); D. Lelas (5); F.; Leone (2); E. Lindfors (18); S. Lombardi (2); F. Longo (1,24); M. L\'opez; (9); C. Maggio (19); P. Majumdar (6); M. Makariev (21); G. Maneva (21); M.; Manganaro (10); K. Mannheim (17); L. Maraschi (2); M. Mariotti (3); M.; Mart\'inez (14); S. Masuda (20); D. Mazin (7,20); K. Mielke (4); M. Minev; (21); J. M. Miranda (15); R. Mirzoyan (7); A. Moralejo (14); V. Moreno (19),; E. Moretti (14); V. Neustroev (18); A. Niedzwiecki (11); M. Nievas Rosillo; (9); C. Nigro (12); K. Nilsson (18); D. Ninci (14); K. Nishijima (20); K.; Noda (20); L. Nogu\'es (14); S. Paiano (3); J. Palacio (14); D. Paneque (7),; R. Paoletti (15); J. M. Paredes (22); G. Pedaletti (12); P. Penil (9); M.; Peresano (1); M. Persic (1,26); K. Pfrang (4); P. G. Prada Moroni (16); E.; Prandini (3); I. Puljak (5); J. R. Garcia (7); W. Rhode (4); M. Rib\'o (22),; J. Rico (14); C. Righi (2); A. Rugliancich (15); L. Saha (9); T. Saito (20),; K. Satalecka (12); T. Schweizer (7); J. Sitarek (11); I. \v{S}nidari\'c (5),; D. Sobczynska (11); A. Stamerra (2); M. Strzys (7); T. Suri\'c (5); F.; Tavecchio (2); P. Temnikov (21); T. Terzi\'c (5); M. Teshima (7,20); N.; Torres-Alb\`a (22); S. Tsujimoto (20); G. Vanzo (10); M. Vazquez Acosta (10),; I. Vovk (7); J. E. Ward (14); M. Will (7); D. Zari\'c (5); Fermi-LAT; Collaboration; S. Ciprini (27,28); R. Desiante (1); MWL Collaborators; S.; Barcewicz (30); T. Hovatta (30); J. Jormanainen (30); L. Takalo (30); R.; Reinthal (30); F. Wierda (30); A. L\"ahteenm\"aki (31,32,33); J. Tammi (31),; M. Tornikoski (31); R. J. C. Vera (31,32); S. Kiehlmann (34); W. Max-Moerbeck; (29); A. C. S. Readhead (34) ((1) Universit\`a di Udine; and INFN Trieste,; Italy; (2) National Institute for Astrophysics (INAF); Rome; Italy; (3); Universit\`a di Padova; INFN; Italy; (4) Technische Universit\"at; Dortmund; Germany; (5) Croatian MAGIC Consortium: University of Rijeka,; University of Split - FESB; University of Zagreb - FER; University of Osijek,; and Rudjer Boskovic Institute; Zagreb; Croatia.; (6) Saha Institute of; Nuclear Physics; HBNI; Kolkata; India; (7) Max-Planck-Institut f\"ur Physik,; M\"unchen; Germany; (8) now at Centro Brasileiro de Pesquisas F\'isicas; (CBPF); Rio de Janeiro (RJ); Brasil; (9) Unidad de Part\'iculas y; Cosmolog\'ia (UPARCOS); Universidad Complutense; Madrid; Spain; (10) Inst. de; Astrof\'isica de Canarias; La Laguna; and Universidad de La Laguna; Dpto.; Astrof\'isica; Tenerife; Spain; (11) University of \L\'od\'z; Department of; Astrophysics; \L\'od\'z; Poland; (12) Deutsches Elektronen-Synchrotron; (DESY); Zeuthen; Germany; (13) ETH Zurich; Zurich; Switzerland; (14) Institut; de F\'isica d'Altes Energies (IFAE); The Barcelona Institute of Science and; Technology (BIST); Bellaterra (Barcelona); Spain; (15) Universit\`a di Siena; and INFN Pisa; Siena; Italy; (16) Universit\`a di Pisa; and INFN Pisa; Italy,; (17) Universit\"at W\"urzburg; Germany; (18) Finnish MAGIC Consortium: Tuorla; Observatory; Finnish Centre of Astronomy with ESO (FINCA); University of; Turku; Piikki\"o; Astronomy Division; University of Oulu; Finland; (19); Departament de F\'isica; and CERES-IEEC; Universitat Aut\'onoma de Barcelona,; Bellaterra; Spain; (20) Japanese MAGIC Consortium: ICRR; The University of; Tokyo; Chiba; Japan; Department of Physics; Kyoto University; Japan; Tokai; University; Kanagawa; Japan; RIKEN; Saitama; Japan; (21) Inst. for Nucl.; Research; Nucl. Energy; Bulgarian Academy of Sciences; Sofia; Bulgaria,; (22) Universitat de Barcelona; ICC; Barcelona; Spain; (23) Humboldt; University of Berlin; Institut f\"ur Physik; Berlin Germany; (24) also at; Dipartimento di Fisica; Universit\`a di Trieste; Trieste; Italy; (25) also at; Port d'Informaci\'o Cient\'ifica (PIC) Bellaterra (Barcelona) Spain; (26); also at INAF-Trieste; Dept. of Physics; Astronomy; University of; Bologna; (27) Agenzia Spaziale Italiana (ASI) Space Science Data Center,; Roma; Italy; (28) Istituto Nazionale di Fisica Nucleare (INFN); Sezione di; Perugia; Perugia; Italy; (29) Departamento de Astronom\'ia; Universidad de; Chile; Las Condes; Santiago; Chile; (30) Tuorla Observatory; University of; Turku; Piikki\"o; Finland; (31) Aalto University Mets\"ahovi Radio; Observatory; Kylm\"al\"a; Finland; (32) Aalto University Department of; Electronics; Nanoengineering; Aalto; Finland; (33) Tartu Observatory,; T\~oravere; Estonia; (34) Owens Valley Radio Observatory; California; Institute of Technology; Pasadena; CA)

arXiv:1807.02095·astro-ph.HE·August 14, 2019

The broad-band properties of the intermediate synchrotron peaked BL Lac S2 0109+22 from radio to VHE gamma rays

MAGIC Collaboration: S. Ansoldi (1,20), L. A. Antonelli (2), C. Arcaro, (3), D. Baack (4), A. Babi\'c (5), B. Banerjee (6), P. Bangale (7), U. Barres, de Almeida (7,8), J. A. Barrio (9), J. Becerra Gonz\'alez (10), W. Bednarek, (11), E. Bernardini (12,23), R. Ch. Berse (4)

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TL;DR

This study characterizes the VHE gamma-ray emission of the ISP BL Lac S2 0109+22 during a flare, analyzing multi-frequency data and modeling its SED, revealing its classification and properties compared to other blazars.

Contribution

First detailed VHE gamma-ray analysis of S2 0109+22 during a flare, including multi-frequency SED modeling and source classification as an ISP BL Lac.

Findings

01

Detected VHE gamma-ray emission at 5.3 sigma significance

02

VHE emission is variable on daily timescales

03

Source classified as an ISP BL Lac with estimated redshift z=0.36

Abstract

The MAGIC telescopes observed S2 0109+22 in 2015 July during its flaring activity in high energy gamma rays observed by Fermi-LAT. We analyse the MAGIC data to characterise the very high energy (VHE) gamma-ray emission of S2 0109+22, which belongs to the subclass of intermediate synchrotron peak (ISP) BL Lac objects. We study the multi-frequency emission in order to investigate the source classification. Finally, we compare the source long-term behaviour to other VHE gamma-ray emitting (TeV) blazars. We performed a temporal and spectral analysis of the data centred around the MAGIC interval of observation (MJD 57225-57231). Long-term radio and optical data have also been investigated using the discrete correlation function. The redshift of the source is estimated through optical host-galaxy imaging and also using the amount of VHE gamma-ray absorption. The quasi-simultaneous…

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