Particle Transport within the Pulsar Wind Nebula HESS J1825-137
Abstract
Aims: 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. Methods: 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 > 0.1 TeV) gamma-ray properties of the nebula. Results: 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 ~100 pc, 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 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)) cm s, corresponding to ~64% of the flux of the Crab Nebula. Conclusions: 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
Cite
@article{arxiv.1810.12676,
title = {Particle Transport within the Pulsar Wind Nebula HESS J1825-137},
author = {H. E. S. S. Collaboration and H. Abdalla and F. Aharonian and F. Ait Benkhali and E. O. Angüner and M. Arakawa and C. Arcaro and C. Armand and M. Arrieta and M. Backes and M. Barnard and Y. Becherini and J. Becker Tjus and D. Berge and K. Bernlöhr and R. Blackwell and M. Böttcher and C. Boisson and J. Bolmont and S. Bonnefoy and P. Bordas and J. Bregeon and F. Brun and P. Brun and M. Bryan and M. Büchele and T. Bulik and T. Bylund and M. Capasso and S. Caroff and A. Carosi and S. Casanova and M. Cerruti and N. Chakraborty and T. Chand and S. Chandra and R. C. G. Chaves and A. Chen and S. Colafrancesco and B. Condon and I. D. Davids and C. Deil and J. Devin and P. deWilt and L. Dirson and A. Djannati-Ataï and A. Dmytriiev and A. Donath and V. Doroshenko and L. O'C. Drury and J. Dyks and K. Egberts and G. Emery and J. -P. Ernenwein and S. Eschbach and S. Fegan and A. Fiasson and G. Fontaine and S. Funk and M. Füßling and S. Gabici and Y. A. Gallant and F. Gaté and G. Giavitto and D. Glawion and J. F. Glicenstein and D. Gottschall and M. -H. Grondin and J. Hahn and M. Haupt and G. Heinzelmann and G. Henri and G. Hermann and J. A. Hinton and W. Hofmann and C. Hoischen and T. L. Holch and M. Holler and D. Horns and D. Huber and H. Iwasaki and A. Jacholkowska and M. Jamrozy and D. Jankowsky and F. Jankowsky and L. Jouvin and I. Jung-Richardt and M. A. Kastendieck and K. Katarzyński and M. Katsuragawa and U. Katz and D. Kerszberg and D. Khangulyan and B. Khélifi and J. King and S. Klepser and W. Kluźniak and Nu. Komin and K. Kosack and M. Kraus and G. Lamanna and J. Lau and J. Lefaucheur and A. Lemière and M. Lemoine-Goumard and J. -P. Lenain and E. Leser and T. Lohse and R. López-Coto and I. Lypova and D. Malyshev and V. Marandon and A. Marcowith and C. Mariaud and G. Martí-Devesa and R. Marx and G. Maurin and P. J. Meintjes and A. M. W. Mitchell and R. Moderski and M. Mohamed and L. Mohrmann and C. Moore and E. Moulin and T. Murach and S. Nakashima and M. de Naurois and H. Ndiyavala and F. Niederwanger and J. Niemiec and L. Oakes and P. O'Brien and H. Odaka and S. Ohm and M. Ostrowski and I. Oya and M. Panter and R. D. Parsons and C. Perennes and P. -O. Petrucci and B. Peyaud and Q. Piel and S. Pita and V. Poireau and A. Priyana Noel and D. A. Prokhorov and H. Prokoph and G. Pühlhofer and M. Punch and A. Quirrenbach and S. Raab and R. Rauth and A. Reimer and O. Reimer and M. Renaud and F. Rieger and L. Rinchiuso and C. Romoli and G. Rowell and B. Rudak and E. Ruiz-Velasco and V. Sahakian and S. Saito and D. A. Sanchez and A. Santangelo and M. Sasaki and R. Schlickeiser and F. Schüssler and A. Schulz and H. Schutte and U. Schwanke and S. Schwemmer and M. Seglar-Arroyo and M. Senniappan and A. S. Seyffert and N. Shafi and I. Shilon and K. Shiningayamwe and R. Simoni and A. Sinha and H. Sol and A. Specovius and M. Spir-Jacob and Ł. Stawarz and R. Steenkamp and C. Stegmann and C. Steppa and T. Takahashi and J. -P. Tavernet and T. Tavernier and A. M. Taylor and R. Terrier and L. Tibaldo and D. Tiziani and M. Tluczykont and C. Trichard and M. Tsirou and N. Tsuji and R. Tuffs and Y. Uchiyama and D. J. van der Walt and C. van Eldik and C. van Rensburg and B. van Soelen and G. Vasileiadis and J. Veh and C. Venter and P. Vincent and J. Vink and F. Voisin and H. J. Völk and T. Vuillaume and Z. Wadiasingh and S. J. Wagner and R. M. Wagner and R. White and A. Wierzcholska and R. Yang and H. Yoneda and D. Zaborov and M. Zacharias and R. Zanin and A. A. Zdziarski and A. Zech and F. Zefi and A. Ziegler and J. Zorn and N. Zywucka},
journal= {arXiv preprint arXiv:1810.12676},
year = {2019}
}
Comments
20 pages, 10 figures, 5 tables, accepted for publication by Astronomy and Astrophysics