1ES 2344+514 Multi-wavelength study Virtual Observatory Resource

Authors

1. MAGIC Collaboration
2. Acciari V.A.
3. Ansoldi S.
4. Antonelli L.A.,Arbet Engels A.
5. Babic A.
6. Banerjee B.
7. Barres de Almeida U.
8. Barrio J.A.,Becerra Gonzalez J.
9. Bednarek W.
10. Bellizzi L.
11. Bernardini E.
12. Berti A.,Besenrieder J.
13. Bhattacharyya W.
14. Bigongiari C.
15. Blanch O.
16. Bonnoli G.,Bosnjak Z.
17. Busetto G.
18. Carosi R.
19. Ceribella G.
20. Cerruti M.
21. Chai Y.,Chilingaryan A.
22. Cikota S.
23. Colak S.M.
24. Colin U.
25. Colombo E.,Contreras J.L.
26. Cortina J.
27. Covino S.
28. D'Elia V.
29. Da Vela P.
30. Dazzi F.,De Angelis A.
31. De Lotto B.
32. Delno M.
33. Delgado J.
34. Depaoli D.
35. Di Pierro F.,Di Venere L.
36. Do Souto Espi~neira E.
37. Dominis Prester D.
38. Donini A.,Doro M.
39. Elsaessery D.
40. Fallah Ramazani V.
41. Fattorini A.
42. Ferrara G.,Foano L.
43. Fonseca M.V.
44. Font L.
45. Fruck C.
46. Fukami S.
47. Garca Lopez R.J.,Garczarczyk M.
48. Gasparyan S.
49. Gaug M.
50. Giglietto N.
51. Giordano F.,Godinovic N.
52. Gliwny P.
53. Green D.
54. Hadasch D.
55. Hahn A.
56. Herrera J.,Hoang J.
57. Hrupec D.
58. Huetten M.
59. Inada T.
60. Inoue S.
61. Ishio K.
62. Iwamura Y.,Jouvin L.
63. Kajiwara Y.
64. Kerszberg D.
65. Kobayashi Y.
66. Kubo H.
67. Kushida J.,Lamastra A.
68. Lelas D.
69. Leone F.
70. Lindfors E.
71. Lombardi S.
72. Longo F.,Lopez M.
73. Lopez-Coto R.
74. Lopez-Oramas A.
75. Loporchio S.,Machado de Oliveira Fraga B.
76. Maggio C.
77. Majumdar P.
78. Makariev M.,Mallamaci M.
79. Maneva G.
80. Manganaro M.
81. Maraschi L.
82. Mariotti M.
83. Martnez M.,Mazin D.
84. Mender S.
85. Micanovic S.
86. Miceli D.
87. Miener T.
88. Minev M.,Miranda J.M.
89. Mirzoyan R.
90. Molina E.
91. Moralejo A.
92. Morcuende D.
93. Moreno V.,Moretti E.
94. Munar-Adrover P.
95. Neustroev V.
96. Nigro C.
97. Nilsson K.
98. Ninci D.,Nishijima K.
99. Noda K.
100. Nogues L.
101. Nozaki S.
102. Ohtani Y.
103. Oka T.,Otero-Santos J.
104. Palatiello M.
105. Paneque D.
106. Paoletti R.
107. Paredes J.M.,Pavletic L.
108. Pe~nil P.
109. Peresano M.
110. Persic M.
111. Prada Moroni P.G.,Prandini E.
112. Puljak I.
113. Ribo M.
114. Rico J.
115. Righi C.
116. Rugliancich A.
117. Saha L.,Sahakyan N.
118. Saito T.
119. Sakurai S.
120. Satalecka K.
121. Schleicher B.
122. Schmidt K.,Schweizer T.
123. Sitarek J.
124. Snidaric I.
125. Sobczynska D.
126. Spolon A.,Stamerra A.
127. Strom D.
128. Strzys M.
129. Suda Y.
130. Suric T.
131. Takahashi M.,Tavecchio F.
132. Temnikov P.
133. Terzic T.
134. Teshima M.
135. Torres-Alba N.
136. Tosti L.,van Scherpenberg J.
137. Vanzo G.
138. Vazquez Acosta M.
139. Ventura S.
140. Verguilov V.,Vigorito C.F.
141. Vitale V.
142. Vovk I.
143. Will M.
144. Zaric D.,FACT Collaboration
145. Baackz D.
146. Balbo M.
147. Beck M.
148. Biederbeck N.
149. Bilandz A.,Blank M.
150. Bretz T.
151. Bruegge K.
152. Bulinski M.
153. Buss J.
154. Doerr M.
155. Dorner D.,Hildebrand D.
156. Iotov R.
157. Klinger M.
158. Mannheimz K.
159. Achim Mueller S.,Neise D.
160. Neronov A.
161. Noethe M.
162. Paravac A.
163. Rhodez W.
164. Schleicher B.,Sedlaczek K.
165. Shukla A.
166. Sliusar V.
167. Tani L.
168. Theissen F.
169. Walter R.,MWL Collaborators: Acosta Pulido J.
170. Filippenko A.V.
171. Hovatta T.,Kiehlmann S.
172. Larionov V.M.
173. Max-Moerbeck W.
174. Raiteri C.M.
175. Readhead A.C.S.,Segon M.
176. Villata M.
177. Zheng W.

Published by

CDS

Abstract

Extreme High-frequency BL Lacs (EHBL) feature their synchrotron peak of the broadband spectral energy distribution (SED) at {nu}_s_>=10^17^Hz. The BL Lac object 1ES 2344+514 was included in the EHBL family because of its impressive shift of the synchrotron peak in 1996. During the following years, the source appeared to be in a low state without showing any extreme behaviours. In August 2016, 1ES 2344+514 was detected with the ground-based {gamma}-ray telescope FACT during a high {gamma}-ray state, triggering multi-wavelength (MWL) observations. We studied the MWL light curves of 1ES 2344+514 during the 2016 flaring state, using data from radio to VHE {gamma} rays taken with OVRO, KAIT, KVA, NOT, some telescopes of the GASP-WEBT collaboration at the Teide, Crimean, and St. Petersburg observatories, Swift-UVOT, Swift-XRT, Fermi-LAT, FACT and MAGIC. With simultaneous observations of the flare, we built the broadband SED and studied it in the framework of a leptonic and an hadronic model. The VHE {gamma}-ray observations show a flux level of 55% of the Crab Nebula flux above 300GeV, similar to the historical maximum of 1995. The combination of MAGIC and Fermi-LAT spectra provides an unprecedented characterization of the inverse-Compton peak for this object during a flaring episode. The {GAMMA} index of the intrinsic spectrum in the VHE {gamma}-ray band is 2.04+/-0.12stat+/-0.15sys. We find the source in an extreme state with a shift of the position of the synchrotron peak to frequencies above or equal to 10^18^Hz

Keywords

1. BL Lacertae objects
2. Spectral energy distribution

Bibliographic source Bibcode

2020MNRAS.496.3912M

See also HTML

https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/496/3912

IVOA Identifier IVOID

ivo://CDS.VizieR/J/MNRAS/496/3912

Document Object Identifer DOI

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http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/496/3912

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