Particle transport within the pulsar wind nebula HESS J1825–137

Particle transport within the pulsar wind nebula HESS J1825–137
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DOI：
10.1051/0004-6361/201834335
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发表时间：
2018-10
期刊：
Astronomy & Astrophysics
影响因子：
6.5
通讯作者：
H. Abdalla;F. Aharonian;F. Benkhali;F. Benkhali;E. Angüner;M. Arakawa;C. Arcaro;C. Armand;M. Arrieta;Michael Backes;M. Barnard;Y. Becherini;J. Tjus;D. Berge;K. Bernloehr;R. Blackwell;M. Böttcher;C. Boisson;J. Bolmont;S. Bonnefoy;P. Bordas;J. Bregeon;F. Brun;P. Brun;M. Bryan;M. Buechele;T. Bulik;T. Bylund;M. Capasso;S. Caroff;A. Carosi;S. Casanova;M. Cerruti;N. Chakraborty;T. Chand;S. Chandra;R. Chaves;A. Chen;S. Colafrancesco;B. Condon;I. Davids;C. Deil;J. Devin;P. deWilt;L. Dirson;A. Djannati-Ataï;A. Dmytriiev;A. Donath;Doroshenko;L. Drury;J. Dyks;K. Egberts;G. Emery;J. Ernenwein;S. Eschbach;S. Fegan;A. Fiasson;G. Fontaine;S. Funk;M. Fuessling;S. Gabici;Y. Gallant;F. Gaté;G. Giavitto;D. Glawion;J. Glicenstein;D. Gottschall;M. Grondin;J. Hahn;M. Haupt;G. Heinzelmann;G. Henri;G. Hermann;J. Hinton;W. Hofmann;C. Hoischen;T. Holch;M. Holler;D. Horns;D. Huber;H. Iwasaki;A. Jacholkowska;M. Jamrozy;D. Jankowsky;F. Jankowsky;L. Jouvin;I. Jung-Richardt;M. Kastendieck;K. Katarzy'nski;M. Katsuragawa;U. Katz;D. Kerszberg;D. Khangulyan;B. Kh'elifi;J. King;S. Klepser;W. Kluźniak;N. Komin;K. Kosack;M. Kraus;G. Lamanna;J. Lau;J. Lefaucheur;A. Lemière;M. Lemoine-Goumard;J. Lenain;E. Leser;T. Lohse;R. L'opez-Coto;I. Lypova;D. Malyshev;Marandon;A. Marcowith;C. Mariaud;G. Martí-Devesa;R. Marx;G. Maurin;P. Meintjes;A. Mitchell;A. Mitchell;R. Moderski;M. Mohamed;L. Mohrmann;C. Moore;E. Moulin;T. Murach;S. Nakashima;M. Naurois;H. Ndiyavala;F. Niederwanger;J. Niemiec;L. Oakes;P. O’Brien;H. Odaka;S. Ohm;M. Ostrowski;I. Oya;M. Panter;R. Parsons;C. Perennes;P. Petrucci;B. Peyaud;Q. Piel;S. Pita;Poireau;A. Noel;D. Prokhorov;H. Prokoph;G. Puehlhofer;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;Sahakian;S. Saito;David Sánchez;A. Santangelo;M. Sasaki;R. Schlickeiser;F. Schüssler;A. Schulz;H. Schutte;U. Schwanke;S. Schwemmer;M. Seglar-Arroyo;M. Senniappan;A. 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. 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. D. Walt-D.;C. Eldik;C. V. Rensburg;B. V. Soelen;G. Vasileiadis;J. Veh;C. Venter;P. Vincent;J. Vink;F. Voisin;H. Voelk;T. Vuillaume;Z. Wadiasingh;S. Wagner;R. Wagner;R. White;A. Wierzcholska;Rui-zhi Yang;H. Yoneda;D. Zaborov;M. Zacharias;R. Zanin;A. Zdziarski;A. Zech;F. Zefi;A. Ziegler;J. Zorn;N. Żywucka
H. Abdalla;F. Aharonian;F. Benkhali;F. Benkhali;E. Angüner;M. Arakawa;C. Arcaro;C. Armand;M. Arrieta;Michael Backes;M. Barnard;Y. Becherini;J. Tjus;D. Berge;K. Bernloehr;R. Blackwell;M. Böttcher;C. Boisson;J. Bolmont;S. Bonnefoy;P. Bordas;J. Bregeon;F. Brun;P. Brun;M. Bryan;M. Buechele;T. Bulik;T. Bylund;M. Capasso;S. Caroff;A. Carosi;S. Casanova;M. Cerruti;N. Chakraborty;T. Chand;S. Chandra;R. Chaves;A. Chen;S. Colafrancesco;B. Condon;I. Davids;C. Deil;J. Devin;P. deWilt;L. Dirson;A. Djannati-Ataï;A. Dmytriiev;A. Donath;Doroshenko;L. Drury;J. Dyks;K. Egberts;G. Emery;J. Ernenwein;S. Eschbach;S. Fegan;A. Fiasson;G. Fontaine;S. Funk;M. Fuessling;S. Gabici;Y. Gallant;F. Gaté;G. Giavitto;D. Glawion;J. Glicenstein;D. Gottschall;M. Grondin;J. Hahn;M. Haupt;G. Heinzelmann;G. Henri;G. Hermann;J. Hinton;W. Hofmann;C. Hoischen;T. Holch;M. Holler;D. Horns;D. Huber;H. Iwasaki;A. Jacholkowska;M. Jamrozy;D. Jankowsky;F. Jankowsky;L. Jouvin;I. Jung-Richardt;M. Kastendieck;K. Katarzy'nski;M. Katsuragawa;U. Katz;D. Kerszberg;D. Khangulyan;B. Kh'elifi;J. King;S. Klepser;W. Kluźniak;N. Komin;K. Kosack;M. Kraus;G. Lamanna;J. Lau;J. Lefaucheur;A. Lemière;M. Lemoine-Goumard;J. Lenain;E. Leser;T. Lohse;R. L'opez-Coto;I. Lypova;D. Malyshev;Marandon;A. Marcowith;C. Mariaud;G. Martí-Devesa;R. Marx;G. Maurin;P. Meintjes;A. Mitchell;A. Mitchell;R. Moderski;M. Mohamed;L. Mohrmann;C. Moore;E. Moulin;T. Murach;S. Nakashima;M. Naurois;H. Ndiyavala;F. Niederwanger;J. Niemiec;L. Oakes;P. O’Brien;H. Odaka;S. Ohm;M. Ostrowski;I. Oya;M. Panter;R. Parsons;C. Perennes;P. Petrucci;B. Peyaud;Q. Piel;S. Pita;Poireau;A. Noel;D. Prokhorov;H. Prokoph;G. Puehlhofer;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;Sahakian;S. Saito;David Sánchez;A. Santangelo;M. Sasaki;R. Schlickeiser;F. Schüssler;A. Schulz;H. Schutte;U. Schwanke;S. Schwemmer;M. Seglar-Arroyo;M. Senniappan;A. 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. 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. D. Walt-D.;C. Eldik;C. V. Rensburg;B. V. Soelen;G. Vasileiadis;J. Veh;C. Venter;P. Vincent;J. Vink;F. Voisin;H. Voelk;T. Vuillaume;Z. Wadiasingh;S. Wagner;R. Wagner;R. White;A. Wierzcholska;Rui-zhi Yang;H. Yoneda;D. Zaborov;M. Zacharias;R. Zanin;A. Zdziarski;A. Zech;F. Zefi;A. Ziegler;J. Zorn;N. Żywucka
中科院分区：
物理与天体物理2区
文献类型：
--
作者：
H. Abdalla;F. Aharonian;F. Benkhali;F. Benkhali;E. Angüner;M. Arakawa;C. Arcaro;C. Armand;M. Arrieta;Michael Backes;M. Barnard;Y. Becherini;J. Tjus;D. Berge;K. Bernloehr;R. Blackwell;M. Böttcher;C. Boisson;J. Bolmont;S. Bonnefoy;P. Bordas;J. Bregeon;F. Brun;P. Brun;M. Bryan;M. Buechele;T. Bulik;T. Bylund;M. Capasso;S. Caroff;A. Carosi;S. Casanova;M. Cerruti;N. Chakraborty;T. Chand;S. Chandra;R. Chaves;A. Chen;S. Colafrancesco;B. Condon;I. Davids;C. Deil;J. Devin;P. deWilt;L. Dirson;A. Djannati-Ataï;A. Dmytriiev;A. Donath;Doroshenko;L. Drury;J. Dyks;K. Egberts;G. Emery;J. Ernenwein;S. Eschbach;S. Fegan;A. Fiasson;G. Fontaine;S. Funk;M. Fuessling;S. Gabici;Y. Gallant;F. Gaté;G. Giavitto;D. Glawion;J. Glicenstein;D. Gottschall;M. Grondin;J. Hahn;M. Haupt;G. Heinzelmann;G. Henri;G. Hermann;J. Hinton;W. Hofmann;C. Hoischen;T. Holch;M. Holler;D. Horns;D. Huber;H. Iwasaki;A. Jacholkowska;M. Jamrozy;D. Jankowsky;F. Jankowsky;L. Jouvin;I. Jung-Richardt;M. Kastendieck;K. Katarzy'nski;M. Katsuragawa;U. Katz;D. Kerszberg;D. Khangulyan;B. Kh'elifi;J. King;S. Klepser;W. Kluźniak;N. Komin;K. Kosack;M. Kraus;G. Lamanna;J. Lau;J. Lefaucheur;A. Lemière;M. Lemoine-Goumard;J. Lenain;E. Leser;T. Lohse;R. L'opez-Coto;I. Lypova;D. Malyshev;Marandon;A. Marcowith;C. Mariaud;G. Martí-Devesa;R. Marx;G. Maurin;P. Meintjes;A. Mitchell;A. Mitchell;R. Moderski;M. Mohamed;L. Mohrmann;C. Moore;E. Moulin;T. Murach;S. Nakashima;M. Naurois;H. Ndiyavala;F. Niederwanger;J. Niemiec;L. Oakes;P. O’Brien;H. Odaka;S. Ohm;M. Ostrowski;I. Oya;M. Panter;R. Parsons;C. Perennes;P. Petrucci;B. Peyaud;Q. Piel;S. Pita;Poireau;A. Noel;D. Prokhorov;H. Prokoph;G. Puehlhofer;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;Sahakian;S. Saito;David Sánchez;A. Santangelo;M. Sasaki;R. Schlickeiser;F. Schüssler;A. Schulz;H. Schutte;U. Schwanke;S. Schwemmer;M. Seglar-Arroyo;M. Senniappan;A. 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. 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. D. Walt-D.;C. Eldik;C. V. Rensburg;B. V. Soelen;G. Vasileiadis;J. Veh;C. Venter;P. Vincent;J. Vink;F. Voisin;H. Voelk;T. Vuillaume;Z. Wadiasingh;S. Wagner;R. Wagner;R. White;A. Wierzcholska;Rui-zhi Yang;H. Yoneda;D. Zaborov;M. Zacharias;R. Zanin;A. Zdziarski;A. Zech;F. Zefi;A. Ziegler;J. Zorn;N. Żywucka

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上下文。我们展示了脉冲星风星云(PWN)Hess J1825-137的详细图像。我们的目标是限制支配星云内粒子运输的机制，解释其异常大的尺寸和光谱特征。目标。对该星云的研究使用了超过12年的H.E.S.I行动的深度曝光，以及来自H.E.S.II的数据，这些数据改善了低能量的敏感性。增强的依赖能量的形态和空间分辨光谱分析探测星云的极高能量(VHe，E&GT；0.1TeV)γ射线特性。方法：研究方法。星云的发射从脉冲星向外延伸到1.5°，比之前看到的距离长约1.5倍，这使得本征直径约100pC的Hess J1825-137有可能成为目前已知的最大的γ射线脉冲星。刻画星云强烈依赖能量的形态使我们能够限制粒子的传输机制。星云范围与能量的R∝Eα和α=−0.29±0.04stat±0.05sys的依赖关系不利于粒子在星云内的纯粹扩散。1TeV以上星云的总γ射线通量为(1.12±0.03stat±0.25sys)×10−11 cm−2 S−1，相当于蟹状星云通量的~%。结果。Hess J1825-137是一种PWN，在γ射线能量下具有明显的能量依赖性。这个源被用作实验室来研究中龄PWNe内的粒子输运。基于对这一高度空间扩展的PWN的深入观察，我们制作了该区域的光谱图，提供了对星云内光谱变化的洞察。
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 R ∝ Eα 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.