Constraints on an Annihilation Signal from a Core of Constant Dark Matter Density around the Milky Way Center with H.E.S.S.
Constraints on an Annihilation Signal from a Core of Constant Dark Matter Density around the Milky Way Center with H.E.S.S.
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DOI：
10.1103/physrevlett.114.081301
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发表时间：
2015-02
影响因子：
8.6
通讯作者：
A. Abramowski;F. Aharonian;F. Ait Benkhali;A. Akhperjanian;E. Angüner;M. Backes;S. Balenderan;A. Balzer;A. Barnacka;Y. Becherini;J. Becker Tjus;D. Berge;S. Bernhard;K. Bernlöhr;E. Birsin;J. Biteau;M. Böttcher;C. Boisson;J. Bolmont;P. Bordas;J. Bregeon;F. Brun;P. Brun;M. Bryan;T. Bulik;S. Carrigan;S. Casanova;P. Chadwick;N. Chakraborty;R. Chalme-Calvet;R. Chaves;M. Chretien;S. Colafrancesco;G. Cologna;J. Conrad;Camille Couturier;Y. Cui;I. Davids;B. Degrange;C. Deil;P. deWilt;A. Djannati-Ataï;W. Domainko;A. Donath;L. Drury;G. Dubus;K. Dutson;J. Dyks;M. Dyrda;T. Edwards;K. Egberts;P. Eger;P. Espigat;C. Farnier;S. Fegan;F. Feinstein;M. V. Fernandes;D. Fernandez;A. Fiasson;G. Fontaine;A. Förster;M. Füssling;S. Gabici;M. Gajdus;Y. Gallant;T. Garrigoux;G. Giavitto;B. Giebels;J. Glicenstein;D. Gottschall;M. Grondin;M. Grudzinska;D. Hadasch;S. Häffner;J. Hahn;J. Harris;G. Heinzelmann;G. Henri;G. Hermann;O. Hervet;A. Hillert;J. Hinton;W. Hofmann;P. Hofverberg;M. Holler;D. Horns;A. Ivascenko;A. Jacholkowska;C. Jahn;M. Jamrozy;M. Janiak;F. Jankowsky;I. Jung-Richardt;M. Kastendieck;K. Katarzyński;U. Katz;S. Kaufmann;B. Khélifi;M. Kieffer;S. Klepser;D. Klochkov;W. Kluźniak;D. Kolitzus;N. Komin;K. Kosack;S. Krakau;F. Krayzel;P. Krüger;H. Laffon;G. Lamanna;J. Lefaucheur;V. Lefranc;A. Lemière;M. Lemoine-Goumard;J. Lenain;T. Lohse;A. Lopatin;C.-C. Lu-C.;V. Marandon;A. Marcowith;R. Marx;G. Maurin;N. Maxted;M. Mayer;T. Mccomb;J. Méhault;P. Meintjes;U. Menzler;M. Meyer;A. Mitchell;R. Moderski;M. Mohamed;K. Mora;E. Moulin;T. Murach;M. de Naurois;J. Niemiec;S. Nolan;L. Oakes;H. Odaka;S. Ohm;B. Opitz;M. Ostrowski;I. Oya;M. Panter;R. Parsons;M. Paz Arribas;N. Pekeur;G. Pelletier;P. Petrucci;B. Peyaud;S. Pita;H. Poon;G. Pühlhofer;M. Punch;A. Quirrenbach;S. Raab;I. Reichardt;A. Reimer;O. Reimer;M. Renaud;R. de los Reyes;F. Rieger;C. Romoli;S. Rosier-Lees;G. Rowell;B. Rudak;C. Rulten;V. Sahakian;D. Šálek;D. Sanchez;A. Santangelo;R. Schlickeiser;F. Schüssler;A. Schulz;U. Schwanke;S. Schwarzburg;S. Schwemmer;H. Sol;F. Spanier;G. Spengler;F. Spies;Ł. Stawarz;R. Steenkamp;C. Stegmann;F. Stinzing;K. Stycz;I. Sushch;J. Tavernet;T. Tavernier;A. Taylor;R. Terrier;M. Tluczykont;C. Trichard;K. Valerius;C. van Eldik;B. van Soelen;G. Vasileiadis;J. Veh;C. Venter;A. Viana;P. Vincent;J. Vink;H. Völk;F. Volpe;M. Vorster;T. Vuillaume;S. Wagner;P. Wagner;R. Wagner;M. Ward;M. Weidinger;Q. Weitzel;R. White;A. Wierzcholska;P. Willmann;A. Wörnlein;D. Wouters;R. Yang;V. Zabalza;D. Zaborov;M. Zacharias;A. Zdziarski;A. Zech;H. Zechlin
中科院分区：
文献类型：
--
作者：
A. Abramowski;F. Aharonian;F. Ait Benkhali;A. Akhperjanian;E. Angüner;M. Backes;S. Balenderan;A. Balzer;A. Barnacka;Y. Becherini;J. Becker Tjus;D. Berge;S. Bernhard;K. Bernlöhr;E. Birsin;J. Biteau;M. Böttcher;C. Boisson;J. Bolmont;P. Bordas;J. Bregeon;F. Brun;P. Brun;M. Bryan;T. Bulik;S. Carrigan;S. Casanova;P. Chadwick;N. Chakraborty;R. Chalme-Calvet;R. Chaves;M. Chretien;S. Colafrancesco;G. Cologna;J. Conrad;Camille Couturier;Y. Cui;I. Davids;B. Degrange;C. Deil;P. deWilt;A. Djannati-Ataï;W. Domainko;A. Donath;L. Drury;G. Dubus;K. Dutson;J. Dyks;M. Dyrda;T. Edwards;K. Egberts;P. Eger;P. Espigat;C. Farnier;S. Fegan;F. Feinstein;M. V. Fernandes;D. Fernandez;A. Fiasson;G. Fontaine;A. Förster;M. Füssling;S. Gabici;M. Gajdus;Y. Gallant;T. Garrigoux;G. Giavitto;B. Giebels;J. Glicenstein;D. Gottschall;M. Grondin;M. Grudzinska;D. Hadasch;S. Häffner;J. Hahn;J. Harris;G. Heinzelmann;G. Henri;G. Hermann;O. Hervet;A. Hillert;J. Hinton;W. Hofmann;P. Hofverberg;M. Holler;D. Horns;A. Ivascenko;A. Jacholkowska;C. Jahn;M. Jamrozy;M. Janiak;F. Jankowsky;I. Jung-Richardt;M. Kastendieck;K. Katarzyński;U. Katz;S. Kaufmann;B. Khélifi;M. Kieffer;S. Klepser;D. Klochkov;W. Kluźniak;D. Kolitzus;N. Komin;K. Kosack;S. Krakau;F. Krayzel;P. Krüger;H. Laffon;G. Lamanna;J. Lefaucheur;V. Lefranc;A. Lemière;M. Lemoine-Goumard;J. Lenain;T. Lohse;A. Lopatin;C.-C. Lu-C.;V. Marandon;A. Marcowith;R. Marx;G. Maurin;N. Maxted;M. Mayer;T. Mccomb;J. Méhault;P. Meintjes;U. Menzler;M. Meyer;A. Mitchell;R. Moderski;M. Mohamed;K. Mora;E. Moulin;T. Murach;M. de Naurois;J. Niemiec;S. Nolan;L. Oakes;H. Odaka;S. Ohm;B. Opitz;M. Ostrowski;I. Oya;M. Panter;R. Parsons;M. Paz Arribas;N. Pekeur;G. Pelletier;P. Petrucci;B. Peyaud;S. Pita;H. Poon;G. Pühlhofer;M. Punch;A. Quirrenbach;S. Raab;I. Reichardt;A. Reimer;O. Reimer;M. Renaud;R. de los Reyes;F. Rieger;C. Romoli;S. Rosier-Lees;G. Rowell;B. Rudak;C. Rulten;V. Sahakian;D. Šálek;D. Sanchez;A. Santangelo;R. Schlickeiser;F. Schüssler;A. Schulz;U. Schwanke;S. Schwarzburg;S. Schwemmer;H. Sol;F. Spanier;G. Spengler;F. Spies;Ł. Stawarz;R. Steenkamp;C. Stegmann;F. Stinzing;K. Stycz;I. Sushch;J. Tavernet;T. Tavernier;A. Taylor;R. Terrier;M. Tluczykont;C. Trichard;K. Valerius;C. van Eldik;B. van Soelen;G. Vasileiadis;J. Veh;C. Venter;A. Viana;P. Vincent;J. Vink;H. Völk;F. Volpe;M. Vorster;T. Vuillaume;S. Wagner;P. Wagner;R. Wagner;M. Ward;M. Weidinger;Q. Weitzel;R. White;A. Wierzcholska;P. Willmann;A. Wörnlein;D. Wouters;R. Yang;V. Zabalza;D. Zaborov;M. Zacharias;A. Zdziarski;A. Zech;H. Zechlin
从银河系中心区域寻找暗物质的湮灭信号。用H.E.S.S.对银河系中心区域进行专门的开-关观测所获得的数据。为此目的进行了分析。在总计约9小时的开-关观察中未发现显著信号。的速度平均截面上的上限，为湮灭的暗物质粒子的质量范围内类似于300 GeV类似于10 TeV的推导。与以前从银河系中心区域的观测中得出的约束相反，这里得出的约束也适用于银河系中心周围暗物质密度恒定的中央核心的假设。对于质量在95% C. L时介于1和4 TeV之间的暗物质粒子，不包括大于3 x 10（-24）cm（3）/s的值。如果中心暗物质密度核心的半径不超过500 pc。这是最强的约束，是来自湮灭TeV质量的暗物质，而不假设在搜索区域的中心尖暗物质密度分布。
An annihilation signal of dark matter is searched for from the central region of the Milky Way. Data acquired in dedicated on-off observations of the Galactic center region with H.E.S.S. are analyzed for this purpose. No significant signal is found in a total of similar to 9 h of on-off observations. Upper limits on the velocity averaged cross section, , for the annihilation of dark matter particles with masses in the range of similar to 300 GeV to similar to 10 TeV are derived. In contrast to previous constraints derived from observations of the Galactic center region, the constraints that are derived here apply also under the assumption of a central core of constant dark matter density around the center of the Galaxy. Values of that are larger than 3 x 10(-24) cm(3)/s are excluded for dark matter particles with masses between similar to 1 and similar to 4 TeV at 95% C.L. if the radius of the central dark matter density core does not exceed 500 pc. This is the strongest constraint that is derived on for annihilating TeV mass dark matter without the assumption of a centrally cusped dark matter density distribution in the search region.