Particle transport within the pulsar wind nebula HESS J1825-137

H. E.S.S. Collaboration; H. Abdalla; F. Aharonian; F. Ait Benkhali; E. O. Angüner; M. Arakawa; C. Arcaro; C. Armand; M. Arrieta; M. Backes; M. Barnard; Y. Becherini; J. Becker Tjus; D. Berge; K. Bernlöhr; R. Blackwell; M. Böttcher; C. Boisson; J. Bolmont; S. Bonnefoy; P. Bordas; J. Bregeon; F. Brun; P. Brun; M. Bryan; M. Büchele; 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-Ataï; 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. Füßling; S. Gabici; Y. A. Gallant; F. Gaté; 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. Katarzyński; M. Katsuragawa; U. Katz; D. Kerszberg; D. Khangulyan; B. Khélifi; J. King; S. Klepser; W. Kluzniak; Nu Komin; K. Kosack; M. Kraus; G. Lamanna; J. Lau; J. Lefaucheur; A. Lemière; M. Lemoine-Goumard; J. P. Lenain; E. Leser; T. Lohse; R. López-Coto; I. Lypova; D. Malyshev; V. Marandon; A. Marcowith; C. Mariaud; G. Martí-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. Pühlhofer; 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. Schüssler; 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; 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. Völk; 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

doi:10.1051/0004-6361/201834335

Particle transport within the pulsar wind nebula HESS J1825-137

H. E.S.S. Collaboration, H. Abdalla, F. Aharonian, F. Ait Benkhali, E. O. Angüner, M. Arakawa, C. Arcaro, C. Armand, M. Arrieta, M. Backes, M. Barnard, Y. Becherini, J. Becker Tjus, D. Berge, K. Bernlöhr, R. Blackwell, M. Böttcher, C. Boisson, J. Bolmont, S. BonnefoyP. Bordas, J. Bregeon, F. Brun, P. Brun, M. Bryan, M. Büchele, 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-Ataï, 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. Füßling, S. Gabici, Y. A. Gallant, F. Gaté, 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. Katarzyński, M. Katsuragawa, U. Katz, D. Kerszberg, D. Khangulyan, B. Khélifi, J. King, S. Klepser, W. Kluzniak, Nu Komin, K. Kosack, M. Kraus, G. Lamanna, J. Lau, J. Lefaucheur, A. Lemière, M. Lemoine-Goumard, J. P. Lenain, E. Leser, T. Lohse, R. López-Coto, I. Lypova, D. Malyshev, V. Marandon, A. Marcowith, C. Mariaud, G. Martí-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. Pühlhofer, 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. Schüssler, 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, 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. Völk, 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

Research output: Contribution to journal › Article › peer-review

44 Scopus citations

Abstract

Context. 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. Aims. The nebula was 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 that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) γ-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5° from the pulsar, ∼1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of ∼100 pc, potentially the largest γ-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of RE^α with α = -0.29 ± 0.04_stat ± 0.05_sys disfavours a pure diffusion scenario for particle transport within the nebula. The total γ-ray flux of the nebula above 1 TeV is found to be (1.12 ± 0.03_stat ± 0.25_sys) × 10^-11 cm^-2 s^-1, corresponding to ∼64% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE γ-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula.

Original language	English
Article number	A116
Journal	Astronomy and Astrophysics
Volume	621
DOIs	https://doi.org/10.1051/0004-6361/201834335
State	Published - 1 Jan 2019
Externally published	Yes

Keywords

Acceleration of particles
Convection
Diffusion
Gamma rays: General
Pulsars: General

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1051/0004-6361/201834335

Cite this

Collaboration, H. E. S. S., Abdalla, H., Aharonian, F., Ait Benkhali, F., Angüner, E. O., Arakawa, M., Arcaro, C., Armand, C., Arrieta, M., Backes, M., Barnard, M., Becherini, Y., Becker Tjus, J., Berge, D., Bernlöhr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., ... Zywucka, N. (2019). Particle transport within the pulsar wind nebula HESS J1825-137. Astronomy and Astrophysics, 621, Article A116. https://doi.org/10.1051/0004-6361/201834335

@article{6e329631d99d480ab74b6b1fc86a6cb0,

title = "Particle transport within the pulsar wind nebula HESS J1825-137",

abstract = "Context. 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. Aims. The nebula was 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 that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) γ-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5° from the pulsar, ∼1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of ∼100 pc, potentially the largest γ-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of REα with α = -0.29 ± 0.04stat ± 0.05sys disfavours a pure diffusion scenario for particle transport within the nebula. The total γ-ray flux of the nebula above 1 TeV is found to be (1.12 ± 0.03stat ± 0.25sys) × 10-11 cm-2 s-1, corresponding to ∼64% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE γ-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula.",

keywords = "Acceleration of particles, Convection, Diffusion, Gamma rays: General, Pulsars: General",

author = "Collaboration, {H. E.S.S.} and H. Abdalla and F. Aharonian and {Ait Benkhali}, F. and Ang{\"u}ner, {E. O.} and M. Arakawa and C. Arcaro and C. Armand and M. Arrieta and M. Backes and M. Barnard and Y. Becherini and {Becker Tjus}, J. and D. Berge and K. Bernl{\"o}hr and R. Blackwell and M. B{\"o}ttcher 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. B{\"u}chele 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 Chaves, {R. C.G.} and A. Chen and S. Colafrancesco and B. Condon and Davids, {I. D.} and C. Deil and J. Devin and P. Dewilt and L. Dirson and A. Djannati-Ata{\"i} and A. Dmytriiev and A. Donath and V. Doroshenko and Drury, {L. O.C.} and J. Dyks and K. Egberts and G. Emery and Ernenwein, {J. P.} and S. Eschbach and S. Fegan and A. Fiasson and G. Fontaine and S. Funk and M. F{\"u}{\ss}ling and S. Gabici and Gallant, {Y. A.} and F. Gat{\'e} and G. Giavitto and D. Glawion and Glicenstein, {J. F.} and D. Gottschall and Grondin, {M. H.} and J. Hahn and M. Haupt and G. Heinzelmann and G. Henri and G. Hermann and Hinton, {J. A.} and W. Hofmann and C. Hoischen and Holch, {T. L.} 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 Kastendieck, {M. A.} and K. Katarzy{\'n}ski and M. Katsuragawa and U. Katz and D. Kerszberg and D. Khangulyan and B. Kh{\'e}lifi and J. King and S. Klepser and W. Kluzniak and Nu Komin and K. Kosack and M. Kraus and G. Lamanna and J. Lau and J. Lefaucheur and A. Lemi{\`e}re and M. Lemoine-Goumard and Lenain, {J. P.} and E. Leser and T. Lohse and R. L{\'o}pez-Coto and I. Lypova and D. Malyshev and V. Marandon and A. Marcowith and C. Mariaud and G. Mart{\'i}-Devesa and R. Marx and G. Maurin and Meintjes, {P. J.} and Mitchell, {A. M.W.} and R. Moderski and M. Mohamed and L. Mohrmann and C. Moore and E. Moulin and T. Murach and S. Nakashima and {De Naurois}, M. 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 Parsons, {R. D.} and C. Perennes and Petrucci, {P. O.} and B. Peyaud and Q. Piel and S. Pita and V. Poireau and {Priyana Noel}, A. and Prokhorov, {D. A.} and H. Prokoph and G. P{\"u}hlhofer 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 Sanchez, {D. A.} and A. Santangelo and M. Sasaki and R. Schlickeiser and F. Sch{\"u}ssler and A. Schulz and H. Schutte and U. Schwanke and S. Schwemmer and M. Seglar-Arroyo and M. Senniappan and Seyffert, {A. S.} 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 Stawarz and R. Steenkamp and C. Stegmann and C. Steppa and T. Takahashi and Tavernet, {J. P.} and T. Tavernier and Taylor, {A. M.} 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 {Van Der Walt}, {D. J.} and {Van Eldik}, C. and {Van Rensburg}, C. and {Van Soelen}, B. and G. Vasileiadis and J. Veh and C. Venter and P. Vincent and J. Vink and F. Voisin and V{\"o}lk, {H. J.} and T. Vuillaume and Z. Wadiasingh and Wagner, {S. J.} and Wagner, {R. M.} and R. White and A. Wierzcholska and R. Yang and H. Yoneda and D. Zaborov and M. Zacharias and R. Zanin and Zdziarski, {A. A.} and A. Zech and F. Zefi and A. Ziegler and J. Zorn and N. Zywucka",

note = "Publisher Copyright: {\textcopyright} ESO 2019.",

year = "2019",

month = jan,

day = "1",

doi = "10.1051/0004-6361/201834335",

language = "English",

volume = "621",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Collaboration, HESS, Abdalla, H, Aharonian, F, Ait Benkhali, F, Angüner, EO, Arakawa, M, Arcaro, C, Armand, C, Arrieta, M, Backes, M, Barnard, M, Becherini, Y, Becker Tjus, J, Berge, D, Bernlöhr, K, Blackwell, R, Böttcher, M, Boisson, C, Bolmont, J, Bonnefoy, S, Bordas, P, Bregeon, J, Brun, F, Brun, P, Bryan, M, Büchele, M, Bulik, T, Bylund, T, Capasso, M, Caroff, S, Carosi, A, Casanova, S, Cerruti, M, Chakraborty, N, Chand, T, Chandra, S, Chaves, RCG, Chen, A, Colafrancesco, S, Condon, B, Davids, ID, Deil, C, Devin, J, Dewilt, P, Dirson, L, Djannati-Ataï, A, Dmytriiev, A, Donath, A, Doroshenko, V, Drury, LOC, Dyks, J, Egberts, K, Emery, G, Ernenwein, JP, Eschbach, S, Fegan, S, Fiasson, A, Fontaine, G, Funk, S, Füßling, M, Gabici, S, Gallant, YA, Gaté, F, Giavitto, G, Glawion, D, Glicenstein, JF, Gottschall, D, Grondin, MH, Hahn, J, Haupt, M, Heinzelmann, G, Henri, G, Hermann, G, Hinton, JA, Hofmann, W, Hoischen, C, Holch, TL, Holler, M, Horns, D, Huber, D, Iwasaki, H, Jacholkowska, A, Jamrozy, M, Jankowsky, D, Jankowsky, F, Jouvin, L, Jung-Richardt, I, Kastendieck, MA, Katarzyński, K, Katsuragawa, M, Katz, U, Kerszberg, D, Khangulyan, D, Khélifi, B, King, J, Klepser, S, Kluzniak, W, Komin, N, Kosack, K, Kraus, M, Lamanna, G, Lau, J, Lefaucheur, J, Lemière, A, Lemoine-Goumard, M, Lenain, JP, Leser, E, Lohse, T, López-Coto, R, Lypova, I, Malyshev, D, Marandon, V, Marcowith, A, Mariaud, C, Martí-Devesa, G, Marx, R, Maurin, G, Meintjes, PJ, Mitchell, AMW, Moderski, R, Mohamed, M, Mohrmann, L, Moore, C, Moulin, E, Murach, T, Nakashima, S, De Naurois, M, Ndiyavala, H, Niederwanger, F, Niemiec, J, Oakes, L, O'Brien, P, Odaka, H, Ohm, S, Ostrowski, M, Oya, I, Panter, M, Parsons, RD, Perennes, C, Petrucci, PO, Peyaud, B, Piel, Q, Pita, S, Poireau, V, Priyana Noel, A, Prokhorov, DA, Prokoph, H, Pühlhofer, G, Punch, M, Quirrenbach, A, Raab, S, Rauth, R, Reimer, A, Reimer, O, Renaud, M, Rieger, F, Rinchiuso, L, Romoli, C, Rowell, G, Rudak, B, Ruiz-Velasco, E, Sahakian, V, Saito, S, Sanchez, DA, Santangelo, A, Sasaki, M, Schlickeiser, R, Schüssler, F, Schulz, A, Schutte, H, Schwanke, U, Schwemmer, S, Seglar-Arroyo, M, Senniappan, M, Seyffert, AS, Shafi, N, Shilon, I, Shiningayamwe, K, Simoni, R, Sinha, A, Sol, H, Specovius, A, Spir-Jacob, M, Stawarz, Steenkamp, R, Stegmann, C, Steppa, C, Takahashi, T, Tavernet, JP, Tavernier, T, Taylor, AM, Terrier, R, Tibaldo, L, Tiziani, D, Tluczykont, M, Trichard, C, Tsirou, M, Tsuji, N, Tuffs, R, Uchiyama, Y, Van Der Walt, DJ, Van Eldik, C, Van Rensburg, C, Van Soelen, B, Vasileiadis, G, Veh, J, Venter, C, Vincent, P, Vink, J, Voisin, F, Völk, HJ, Vuillaume, T, Wadiasingh, Z, Wagner, SJ, Wagner, RM, White, R, Wierzcholska, A, Yang, R, Yoneda, H, Zaborov, D, Zacharias, M, Zanin, R, Zdziarski, AA, Zech, A, Zefi, F, Ziegler, A, Zorn, J & Zywucka, N 2019, 'Particle transport within the pulsar wind nebula HESS J1825-137', Astronomy and Astrophysics, vol. 621, A116. https://doi.org/10.1051/0004-6361/201834335

TY - JOUR

T1 - Particle transport within the pulsar wind nebula HESS J1825-137

AU - Collaboration, H. E.S.S.

AU - Abdalla, H.

AU - Aharonian, F.

AU - Ait Benkhali, F.

AU - Angüner, E. O.

AU - Arakawa, M.

AU - Arcaro, C.

AU - Armand, C.

AU - Arrieta, M.

AU - Backes, M.

AU - Barnard, M.

AU - Becherini, Y.

AU - Becker Tjus, J.

AU - Berge, D.

AU - Bernlöhr, K.

AU - Blackwell, R.

AU - Böttcher, M.

AU - Boisson, C.

AU - Bolmont, J.

AU - Bonnefoy, S.

AU - Bordas, P.

AU - Bregeon, J.

AU - Brun, F.

AU - Brun, P.

AU - Bryan, M.

AU - Büchele, M.

AU - Bulik, T.

AU - Bylund, T.

AU - Capasso, M.

AU - Caroff, S.

AU - Carosi, A.

AU - Casanova, S.

AU - Cerruti, M.

AU - Chakraborty, N.

AU - Chand, T.

AU - Chandra, S.

AU - Chaves, R. C.G.

AU - Chen, A.

AU - Colafrancesco, S.

AU - Condon, B.

AU - Davids, I. D.

AU - Deil, C.

AU - Devin, J.

AU - Dewilt, P.

AU - Dirson, L.

AU - Djannati-Ataï, A.

AU - Dmytriiev, A.

AU - Donath, A.

AU - Doroshenko, V.

AU - Drury, L. O.C.

AU - Dyks, J.

AU - Egberts, K.

AU - Emery, G.

AU - Ernenwein, J. P.

AU - Eschbach, S.

AU - Fegan, S.

AU - Fiasson, A.

AU - Fontaine, G.

AU - Funk, S.

AU - Füßling, M.

AU - Gabici, S.

AU - Gallant, Y. A.

AU - Gaté, F.

AU - Giavitto, G.

AU - Glawion, D.

AU - Glicenstein, J. F.

AU - Gottschall, D.

AU - Grondin, M. H.

AU - Hahn, J.

AU - Haupt, M.

AU - Heinzelmann, G.

AU - Henri, G.

AU - Hermann, G.

AU - Hinton, J. A.

AU - Hofmann, W.

AU - Hoischen, C.

AU - Holch, T. L.

AU - Holler, M.

AU - Horns, D.

AU - Huber, D.

AU - Iwasaki, H.

AU - Jacholkowska, A.

AU - Jamrozy, M.

AU - Jankowsky, D.

AU - Jankowsky, F.

AU - Jouvin, L.

AU - Jung-Richardt, I.

AU - Kastendieck, M. A.

AU - Katarzyński, K.

AU - Katsuragawa, M.

AU - Katz, U.

AU - Kerszberg, D.

AU - Khangulyan, D.

AU - Khélifi, B.

AU - King, J.

AU - Klepser, S.

AU - Kluzniak, W.

AU - Komin, Nu

AU - Kosack, K.

AU - Kraus, M.

AU - Lamanna, G.

AU - Lau, J.

AU - Lefaucheur, J.

AU - Lemière, A.

AU - Lemoine-Goumard, M.

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PY - 2019/1/1

Y1 - 2019/1/1

N2 - Context. 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. Aims. The nebula was 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 that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) γ-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5° from the pulsar, ∼1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of ∼100 pc, potentially the largest γ-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of REα with α = -0.29 ± 0.04stat ± 0.05sys disfavours a pure diffusion scenario for particle transport within the nebula. The total γ-ray flux of the nebula above 1 TeV is found to be (1.12 ± 0.03stat ± 0.25sys) × 10-11 cm-2 s-1, corresponding to ∼64% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE γ-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula.

AB - Context. 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. Aims. The nebula was 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 that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) γ-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5° from the pulsar, ∼1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of ∼100 pc, potentially the largest γ-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of REα with α = -0.29 ± 0.04stat ± 0.05sys disfavours a pure diffusion scenario for particle transport within the nebula. The total γ-ray flux of the nebula above 1 TeV is found to be (1.12 ± 0.03stat ± 0.25sys) × 10-11 cm-2 s-1, corresponding to ∼64% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE γ-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula.

KW - Acceleration of particles

KW - Convection

KW - Diffusion

KW - Gamma rays: General

KW - Pulsars: General

UR - http://www.scopus.com/inward/record.url?scp=85060367011&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201834335

DO - 10.1051/0004-6361/201834335

M3 - Article

AN - SCOPUS:85060367011

SN - 0004-6361

VL - 621

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A116

ER -

Particle transport within the pulsar wind nebula HESS J1825-137

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