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Particle Transport within the Pulsar Wind Nebula HESS J1825-137

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arxiv 1810.12676 v2 pith:UXGGYHSZ submitted 2018-10-30 astro-ph.HE

Particle Transport within the Pulsar Wind Nebula HESS J1825-137

H.E.S.S. Collaboration , H. Abdalla , F. Aharonian , F. Ait Benkhali , E.O. Ang\"uner , M. Arakawa , C. Arcaro , C. Armand
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M. Arrieta M. Backes M. Barnard Y. Becherini J. Becker Tjus D. Berge K. Bernl\"ohr R. Blackwell M. B\"ottcher C. Boisson J. Bolmont S. Bonnefoy P. Bordas J. Bregeon F. Brun P. Brun M. Bryan M. B\"uchele T. Bulik T. Bylund M. Capasso S. Caroff A. Carosi S. Casanova M. Cerruti N. Chakraborty T. Chand S. Chandra R.C.G. Chaves A. Chen S. Colafrancesco B. Condon I.D. Davids C. Deil J. Devin P. deWilt L. Dirson A. Djannati-Ata\"i A. Dmytriiev A. Donath V. Doroshenko L.O'C. Drury J. Dyks K. Egberts G. Emery J.-P. Ernenwein S. Eschbach S. Fegan A. Fiasson G. Fontaine S. Funk M. F\"u{\ss}ling S. Gabici Y.A. Gallant F. Gat\'e G. Giavitto D. Glawion J.F. Glicenstein D. Gottschall M.-H. Grondin J. Hahn M. Haupt G. Heinzelmann G. Henri G. Hermann J.A. Hinton W. Hofmann C. Hoischen T. L. Holch M. Holler D. Horns D. Huber H. Iwasaki A. Jacholkowska M. Jamrozy D. Jankowsky F. Jankowsky L. Jouvin I. Jung-Richardt M.A. Kastendieck K. Katarzy\'nski M. Katsuragawa U. Katz D. Kerszberg D. Khangulyan B. Kh\'elifi J. King S. Klepser W. Klu\'zniak Nu. Komin K. Kosack M. Kraus G. Lamanna J. Lau J. Lefaucheur A. Lemi\`ere M. Lemoine-Goumard J.-P. Lenain E. Leser T. Lohse R. L\'opez-Coto I. Lypova D. Malyshev V. Marandon A. Marcowith C. Mariaud G. Mart\'i-Devesa R. Marx G. Maurin P.J. Meintjes A.M.W. Mitchell R. Moderski M. Mohamed L. Mohrmann C. Moore E. Moulin T. Murach S. Nakashima M. de Naurois H. Ndiyavala F. Niederwanger J. Niemiec L. Oakes P. O'Brien H. Odaka S. Ohm M. Ostrowski I. Oya M. Panter R.D. Parsons C. Perennes P.-O. Petrucci B. Peyaud Q. Piel S. Pita V. Poireau A. Priyana Noel D.A. Prokhorov H. Prokoph G. P\"uhlhofer M. Punch A. Quirrenbach S. Raab R. Rauth A. Reimer O. Reimer M. Renaud F. Rieger L. Rinchiuso C. Romoli G. Rowell B. Rudak E. Ruiz-Velasco V. Sahakian S. Saito D.A. Sanchez A. Santangelo M. Sasaki R. Schlickeiser F. Sch\"ussler A. Schulz H. Schutte U. Schwanke S. Schwemmer M. Seglar-Arroyo M. Senniappan A.S. Seyffert N. Shafi I. Shilon K. Shiningayamwe R. Simoni A. Sinha H. Sol A. Specovius M. Spir-Jacob \L. Stawarz R. Steenkamp C. Stegmann C. Steppa T. Takahashi J.-P. Tavernet T. Tavernier A.M. Taylor R. Terrier L. Tibaldo D. Tiziani M. Tluczykont C. Trichard M. Tsirou N. Tsuji R. Tuffs Y. Uchiyama D.J. van der Walt C. van Eldik C. van Rensburg B. van Soelen G. Vasileiadis J. Veh C. Venter P. Vincent J. Vink F. Voisin H.J. V\"olk T. Vuillaume Z.Wadiasingh S.J. Wagner R.M. Wagner R. White A. Wierzcholska R. Yang H. Yoneda D. Zaborov M. Zacharias R. Zanin A.A. Zdziarski A. Zech F. Zefi A. Ziegler J. Zorn N. Zywucka
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keywords nebulaparticletransportgamma-rayhessspectralenergyenergy-dependent
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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 $\propto$ 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)) $\times 10^{-11}$ cm$^{-2}$ s$^{-1}$, 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.

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