HESS J1825-137 particle transport Virtual Observatory Resource

Authors

1. H.E.S.S. Collaboration
2. Abdalla H.
3. Aharonian F.
4. Ait Benkhali F.,Anguener E.O.
5. Arakawa M.
6. Arcaro C.
7. Armand C.
8. Arrieta M.
9. Backes M.,Barnard M.
10. Becherini Y.
11. Becker Tjus J.
12. Berge D.
13. Bernloehr K.,Blackwell R.
14. Boettcher M.
15. Boisson C.
16. Bolmont J.
17. Bonnefoy S.,Bordas P.
18. Bregeon J.
19. Brun F.
20. Brun P.
21. Bryan M.
22. Buechele M.
23. Bulik T.,Bylund T.
24. Capasso M.
25. Caroff S.
26. Carosi A.
27. Casanova S.
28. Cerruti M.,Chakraborty N.
29. Chand T.
30. Chandra S.
31. Chaves R.C.G.
32. Chen A.,Colafrancesco S.
33. Condon B.
34. Davids I.D.
35. Deil C.
36. Devin J.
37. deWilt P.,Dirson L.
38. Djannati-Atai A.
39. Dmytriiev A.
40. Donath A.
41. Doroshenko V.,Drury L.O'C.
42. Dyks J.
43. Egberts K.
44. Emery G.
45. Ernenwein J.-P.
46. Eschbach S.,Fegan S.
47. Fiasson A.
48. Fontaine G.
49. Funk S.
50. Fuessling M.
51. Gabici S.,Gallant Y.A.
52. Gate F.
53. Giavitto G.
54. Glawion D.
55. Glicenstein J.F.,Gottschall D.
56. Grondin M.-H.
57. Hahn J.
58. Haupt M.
59. Heinzelmann G.
60. Henri G.,Hermann G.
61. Hinton J.A.
62. Hofmann W.
63. Hoischen C.
64. Holch T.L.
65. Holler M.,Horns D.
66. Huber D.
67. Iwasaki H.
68. Jacholkowska A.
69. Jamrozy M.
70. Jankowsky D.,Jankowsky F.
71. Jouvin L.
72. Jung-Richardt I.
73. Kastendieck M.A.,Katarzynski K.
74. Katsuragawa M.
75. Katz U.
76. Kerszberg D.
77. Khangulyan D.,Khelifi B.
78. King J.
79. Klepser S.
80. Kluzniak W.
81. Komin Nu.
82. Kosack K.,Kraus M.
83. Lamanna G.
84. Lau J.
85. Lefaucheur J.
86. Lemiere A.,Lemoine-Goumard M.
87. Lenain J.-P.
88. Leser E.
89. Lohse T.
90. Lopez-Coto R.,Lypova I.
91. Malyshev D.
92. Marandon V.
93. Marcowith A.
94. Mariaud C.,Marti-Devesa G.
95. Marx R.
96. Maurin G.
97. Meintjes P.J.
98. Mitchell A.M.W.,Moderski R.
99. Mohamed M.
100. Mohrmann L.
101. Moore C.
102. Moulin E.
103. Murach T.,Nakashima S.
104. de Naurois M.
105. Ndiyavala H.
106. Niederwanger F.
107. Niemiec J.,Oakes L.
108. O'Brien P.
109. Odaka H.
110. Ohm S.
111. Ostrowski M.
112. Oya I.
113. Panter M.,Parsons R.D.
114. Perennes C.
115. Petrucci P.-O.
116. Peyaud B.
117. Piel Q.
118. Pita S.,Poireau V.
119. Priyana Noel A.
120. Prokhorov D.A.
121. Prokoph H.
122. Puehlhofer G.,Punch M.
123. Quirrenbach A.
124. Raab S.
125. Rauth R.
126. Reimer A.
127. Reimer O.,Renaud M.
128. Rieger F.
129. Rinchiuso L.
130. Romoli C.
131. Rowell G.
132. Rudak B.,Ruiz-Velasco E.
133. Sahakian V.
134. Saito S.
135. Sanchez D.A.
136. Santangelo A.,Sasaki M.
137. Schlickeiser R.
138. Schuessler F.
139. Schulz A.
140. Schutte H.,Schwanke U.
141. Schwemmer S.
142. Seglar-Arroyo M.
143. Senniappan M.,Seyffert A.S.
144. Shafi N.
145. Shilon I.
146. Shiningayamwe K.
147. Simoni R.
148. Sinha A.,Sol H.
149. Specovius A.
150. Spir-Jacob M.
151. Stawarz L.
152. Steenkamp R.
153. Stegmann C.,Steppa C.
154. Takahashi T.
155. Tavernet J.-P.
156. Tavernier T.
157. Taylor A.M.,Terrier R.
158. Tibaldo L.
159. Tiziani D.
160. Tluczykont M.
161. Trichard C.
162. Tsirou M.,Tsuji N.
163. Tuffs R.
164. Uchiyama Y.
165. van der Walt D.J.
166. van Eldik C.,van Rensburg C.
167. van Soelen B.
168. Vasileiadis G.
169. Veh J.
170. Venter C.,Vincent P.
171. Vink J.
172. Voisin F.
173. Voelk H.J.
174. Vuillaume T.
175. Wadiasingh Z.,Wagner S.J.
176. Wagner R.M.
177. White R.
178. Wierzcholska A.
179. Yang R.
180. Yoneda H.,Zaborov D.
181. Zacharias M.
182. Zanin R.
183. Zdziarski A.A.
184. Zech A.
185. Zefi F.,Ziegler A.
186. Zorn J.
187. Zywucka N.

Published by

CDS

Abstract

We present a detailed view of the pulsar wind nebula (PWN) HESS J1825--137. We aim to constrain the mechanisms dominating the particle transport within the nebula, accounting for its anomalously large size and spectral characteristics. The nebula is studied using a deep exposure from over 12 years of H.E.S.S. I operation, together with data from H.E.S.S. II improving the low energy sensitivity. Enhanced energy- dependent morphological and spatially-resolved spectral analyses probe the Very High Energy (VHE, E>0.1TeV) gamma-ray properties of the nebula. The nebula emission is revealed to extend out to 1.5 degrees from the pulsar, ~1.5 times further than previously seen, making HESS J1825-137, with an intrinsic diameter of ~100pc, potentially the largest gamma-ray PWN currently known. Characterisation of the nebula's strongly energy-dependent morphology enables the particle transport mechanisms to be constrained. A dependence of the nebula extent with energy of R{prop.to} E^alpha^ with alpha=-0.29+/-0.04(stat)+/-0.05(sys) disfavours a pure diffusion scenario for particle transport within the nebula. The total gamma-ray flux of the nebula above 1~TeV is found to be (1.12+/-0.03(stat)+/-0.25(sys))x10^-11^cm^-2^s^-1^, corresponding to ~64% of the flux of the Crab Nebula. HESS J1825-137 is a PWN with clear energy-dependent morphology at VHE gamma-ray energies. This source is used as a laboratory to investigate particle transport within middle-aged PWNe. Deep observations of this highly spatially-extended PWN enable a spectral map of the region to be produced, providing insights into the spectral variation within the nebula.

Keywords

1. pulsars
2. gamma-ray-astronomy

Bibliographic source Bibcode

2019A&A...621A.116H

See also HTML

https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/621/A116

IVOA Identifier IVOID

ivo://CDS.VizieR/J/A+A/621/A116

Document Object Identifer DOI

doi:10.26093/cds/vizier.36210116

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