S5 0716+714 multi-wavelength curves Virtual Observatory Resource

Authors

1. MAGIC Collaboration
2. Ahnen M.L.
3. Ansoldi S.
4. Antonelli L.A.
5. Arcaro C.,Baack D.
6. Babic A.
7. Banerjee B.
8. Bangale P.
9. Barres de Almeida U.,Barrio J.A.
10. Becerra Gonzalez J.
11. Bednarek W.
12. Bernardini E.
13. Berse R.C.,Berti A.
14. Bhattacharyya W.
15. Biland A.
16. Blanch O.
17. Bonnoli G.
18. Carosi R.,Carosi A.
19. Ceribella G.
20. Chatterjee A.
21. Colak S.M.
22. Colin P.
23. Colombo E.,Contreras J.L.
24. Cortina J.
25. Covino S.
26. Cumani P.
27. Da Vela P.
28. Dazzi F.,De Angelis A.
29. De Lotto B.
30. Delfino M.
31. Delgado J.
32. Di Pierro F.,Dominguez A.
33. Dominis Prester D.
34. Dorner D.
35. Doro M.
36. Einecke S.,Elsaesser D.
37. Fallah Ramazani V.
38. Fernandez-Barral A.
39. Fidalgo D.,Fonseca M.V.
40. Font L.
41. Fruck C.
42. Galindo D.
43. Gallozzi S.,Garcia Lopez R.J.
44. Garczarczyk M.
45. Gaug M.
46. Giammaria P.
47. Godinovic N.,Gora D.
48. Guberman D.
49. Hadasch D.
50. Hahn A.
51. Hassan T.
52. Hayashida M.,Herrera J.
53. Hose J.
54. Hrupec D.
55. Ishio K.
56. Konno Y.
57. Kubo H.
58. Kushida J.,Kuvezdic D.
59. Lelas D.
60. Lindfors E.
61. Lombardi S.
62. Longo F.
63. Lopez M.,Maggio C.
64. Majumdar P.
65. Makariev M.
66. Maneva G.
67. Manganaro M.
68. Mannheim K.,Maraschi L.
69. Mariotti M.
70. Martinez M.
71. Masuda S.
72. Mazin D.
73. Mielke K.,Minev M.
74. Miranda J.M.
75. Mirzoyan R.
76. Moralejo A.
77. Moreno V.
78. Moretti E.,Nagayoshi T.
79. Neustroev V.
80. Niedzwiecki A.
81. Nievas Rosillo M.
82. Nigro C.,Nilsson K.
83. Ninci D.
84. Nishijima K.
85. Noda K.
86. Nogues L.
87. Paiano S.,Palacio J.
88. Paneque D.
89. Paoletti R.
90. Paredes J.M.
91. Pedaletti G.,Peresano M.
92. Persic M.
93. Prada Moroni P.G.
94. Prandini E.
95. Puljak I.,Garcia J.R.
96. Reichardt I.
97. Rhode W.
98. Ribo M.
99. Rico J.
100. Righi C.,Rugliancich A.
101. Saito T.
102. Satalecka K.
103. Schweizer T.
104. Sitarek J.,Snidaric I.
105. Sobczynska D.
106. Stamerra A.
107. Strzys M.
108. Suric T.,Takahashi M.
109. Takalo L.
110. Tavecchio F.
111. Temnikov P.
112. Terzic T.
113. Teshima M.,Torres-Alba N.
114. Treves A.
115. Tsujimoto S.
116. Vanzo G.
117. Vazquez Acosta M.,Vovk I.
118. Ward J.E.
119. Will M.
120. Zaric D.,Fermi-LAT Collaboration
121. Bastieri D.
122. Gasparrini D.
123. Lott B.
124. Rani B.,Thompson D.J.,MWL Collaborators
125. Agudo I.
126. Angelakis E.
127. Borman G.A.
128. Casadio C.,Grishina T.S.
129. Gurwell M.
130. Hovatta T.
131. Itoh R.
132. Jaervelae E.
133. Jermak H.,Jorstad S.
134. Kopatskaya E.N.
135. Kraus A.
136. Krichbaum T.P.
137. Kuin N.P.M.,Laehteenmaeki A.
138. Larionov V.M.
139. Larionova L.V.
140. Lien A.Y.
141. Madejski G.,Marscher A.
142. Myserlis I.
143. Max-Moerbeck W.
144. Molina S.N.
145. Morozova D.A.,Nalewajko K.
146. Pearson T.J.
147. Ramakrishnan V.
148. Readhead A.C.S.
149. Reeves R.A.,Savchenko S.S.
150. Steele I.A.
151. Tornikoski M.
152. Troitskaya Yu.V.
153. Troitsky I.,Vasilyev A.A.
154. Anton Zensus J.

Published by

CDS

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. Methods. Multi-wavelength light curves have been studied together with the broadband spectral energy distributions (SEDs). The sample includes data from Effelsberg, OVRO, Metsahovi, VLBI, CARMA, IRAM, SMA, Swift-UVOT, KVA, Tuorla, Steward, RINGO3, KANATA, AZT-8+ST7, Perkins, LX-200, Swift-XRT, NuSTAR, Fermi-LAT and 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 very-high-energy (VHE, E>100GeV). In the constructed SED, the Swift-XRT+NuSTAR data constrain the transition between the synchrotron and inverse Compton components very accurately, while the second peak is constrained from 0.1GeV to 600GeV by 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 electric vector position angle (EVPA) shows an unprecedented fast rotation. An estimation of the redshift of the source by combined high-energy (HE, 0.1GeV<E<100GeV) and VHE data provides a value of z=0.31+/-0.02stats+/-0.05sys, confirming the literature value. The data show the VHE emission originating in the entrance and exit of a superluminal knot in and out of 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 modeling.

Keywords

1. bl-lacertae-objects
2. spectral-energy-distribution

Bibliographic source Bibcode

2018A&A...619A..45M

See also HTML

https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/619/A45

IVOA Identifier IVOID

ivo://CDS.VizieR/J/A+A/619/A45

Document Object Identifer DOI

doi:10.26093/cds/vizier.36190045

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