Search for dark matter annihilation in the Wolf-Lundmark-Melotte dwarf irregular galaxy with H.E.S.S.
Search for dark matter annihilation in the Wolf-Lundmark-Melotte dwarf irregular galaxy with H.E.S.S.
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DOI：
10.1103/physrevd.103.102002
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发表时间：
2021-05
影响因子：
5
通讯作者：
H. Collaboration;H. Abdallah;R. Adam;F. Aharonian;F. Benkhali;E. Anguner;C. Arcaro;C. Armand;T. Armstrong;H. Ashkar;Michael Backes;V. Baghmanyan;V. B. Martins;A. Barnacka;M. Barnard;Y. Becherini;D. Berge;K. Bernlohr;B. Bi;M. Bottcher;C. Boisson;J. Bolmont;M. Lavergne;M. Breuhaus;F. Brun;P. Brun;M. Bryan;M. Buchele;T. Bulik;T. Bylund;S. Caroff;A. Carosi;S. Casanova;T. Chand;S. Chandra;A. Chen;G. Cotter;M. Curyło;J. D. Mbarubucyeye;I. Davids;J. Davies;C. Deil;J. Devin;P. deWilt;L. Dirson;A. Djannati-Atai;A. Dmytriiev;A. Donath;V. Doroshenko;C. Duffy;J. Dyks;K. Egberts;F. Eichhorn;S. Einecke;G. Emery;J. Ernenwein;K. Feijen;S. Fegan;A. Fiasson;G. F. D. Clairfontaine;G. Fontaine;S. Funk;M. Fussling;S. Gabici;Y. Gallant;G. Giavitto;L. Giunti;D. Glawion;J. Glicenstein;D. Gottschall;M. Grondin;J. Hahn;M. Haupt;G. Hermann;J. Hinton;W. Hofmann;C. Hoischen;T. Holch;M. Holler;M. Horbe;D. Horns;D. Huber;M. Jamrozy;D. Jankowsky;F. Jankowsky;A. Jardin-Blicq;V. Joshi;I. Jung-Richardt;E. Kasai;M. Kastendieck;K. Katarzy'nski;U. Katz;D. Khangulyan;B. Khélifi;S. Klepser;W. Kluźniak;N. Komin;R. Konno;K. Kosack;D. Kostunin;M. Kreter;G. Lamanna;A. Lemière;M. Lemoine-Goumard;J. Lenain;C. Levy;T. Lohse;I. Lypova;J. Mackey;J. Majumdar;D. Malyshev;V. Marandon;P. Marchegiani;A. Marcowith;A. Mares;G. Martí-Devesa;R. Marx;G. Maurin;P. Meintjes;M. Meyer;R. Moderski;M. Mohamed;L. Mohrmann;A. Montanari;C. Moore;P. Morris;E. Moulin;J. Muller;T. Murach;K. Nakashima;A. Nayerhoda;M. Naurois;H. Ndiyavala;F. Niederwanger;J. Niemiec;L. Oakes;P. O’Brien;H. Odaka;S. Ohm;L. Olivera-Nieto;E. Wilhelmi;M. Ostrowski;M. Panter;S. Panny;R. Parsons;G. Peron;B. Peyaud;Q. Piel;S. Pita;V. Poireau;A. Noel;D. Prokhorov;H. Prokoph;G. Puhlhofer;M. Punch;A. Quirrenbach;S. Raab;R. Rauth;P. Reichherzer;A. Reimer;O. Reimer;Q. Remy;M. Renaud;F. Rieger;L. Rinchiuso;C. Romoli;G. Rowell;B. Rudak;E. Ruiz-Velasco;V. Sahakian;S. Sailer;D. Sanchez;A. Santangelo;M. Sasaki;M. Scalici;F. Schussler;H. Schutte;U. Schwanke;S. Schwemmer;M. Seglar-Arroyo;M. Senniappan;A. Seyffert;N. Shafi;K. Shiningayamwe;R.Simoni;A.Sinha;H. Sol;A. Specovius;S. Spencer;M. Spir-Jacob;L. Stawarz;L. Sun;R. Steenkamp;C. Stegmann;S. Steinmassl;C. Steppa;T. Takahashi;T. Tavernier;A. Taylor;R. Terrier;D. Tiziani;M. Tluczykont;L. Tomankova;C. Trichard;M. Tsirou;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;H. Volk;T. Vuillaume;Z. Wadiasingh;S. Wagner;J. Watson;F. Werner;R. White;A. Wierzcholska;Y. Wong;A. Yusafzai;M. Zacharias;R. Zanin;D. Zargaryan;A. Zdziarski;A. Zech;S. Zhu;J. Zorn;S. Zouari;N. Żywucka
中科院分区：
文献类型：
--
作者：
H. Collaboration;H. Abdallah;R. Adam;F. Aharonian;F. Benkhali;E. Anguner;C. Arcaro;C. Armand;T. Armstrong;H. Ashkar;Michael Backes;V. Baghmanyan;V. B. Martins;A. Barnacka;M. Barnard;Y. Becherini;D. Berge;K. Bernlohr;B. Bi;M. Bottcher;C. Boisson;J. Bolmont;M. Lavergne;M. Breuhaus;F. Brun;P. Brun;M. Bryan;M. Buchele;T. Bulik;T. Bylund;S. Caroff;A. Carosi;S. Casanova;T. Chand;S. Chandra;A. Chen;G. Cotter;M. Curyło;J. D. Mbarubucyeye;I. Davids;J. Davies;C. Deil;J. Devin;P. deWilt;L. Dirson;A. Djannati-Atai;A. Dmytriiev;A. Donath;V. Doroshenko;C. Duffy;J. Dyks;K. Egberts;F. Eichhorn;S. Einecke;G. Emery;J. Ernenwein;K. Feijen;S. Fegan;A. Fiasson;G. F. D. Clairfontaine;G. Fontaine;S. Funk;M. Fussling;S. Gabici;Y. Gallant;G. Giavitto;L. Giunti;D. Glawion;J. Glicenstein;D. Gottschall;M. Grondin;J. Hahn;M. Haupt;G. Hermann;J. Hinton;W. Hofmann;C. Hoischen;T. Holch;M. Holler;M. Horbe;D. Horns;D. Huber;M. Jamrozy;D. Jankowsky;F. Jankowsky;A. Jardin-Blicq;V. Joshi;I. Jung-Richardt;E. Kasai;M. Kastendieck;K. Katarzy'nski;U. Katz;D. Khangulyan;B. Khélifi;S. Klepser;W. Kluźniak;N. Komin;R. Konno;K. Kosack;D. Kostunin;M. Kreter;G. Lamanna;A. Lemière;M. Lemoine-Goumard;J. Lenain;C. Levy;T. Lohse;I. Lypova;J. Mackey;J. Majumdar;D. Malyshev;V. Marandon;P. Marchegiani;A. Marcowith;A. Mares;G. Martí-Devesa;R. Marx;G. Maurin;P. Meintjes;M. Meyer;R. Moderski;M. Mohamed;L. Mohrmann;A. Montanari;C. Moore;P. Morris;E. Moulin;J. Muller;T. Murach;K. Nakashima;A. Nayerhoda;M. Naurois;H. Ndiyavala;F. Niederwanger;J. Niemiec;L. Oakes;P. O’Brien;H. Odaka;S. Ohm;L. Olivera-Nieto;E. Wilhelmi;M. Ostrowski;M. Panter;S. Panny;R. Parsons;G. Peron;B. Peyaud;Q. Piel;S. Pita;V. Poireau;A. Noel;D. Prokhorov;H. Prokoph;G. Puhlhofer;M. Punch;A. Quirrenbach;S. Raab;R. Rauth;P. Reichherzer;A. Reimer;O. Reimer;Q. Remy;M. Renaud;F. Rieger;L. Rinchiuso;C. Romoli;G. Rowell;B. Rudak;E. Ruiz-Velasco;V. Sahakian;S. Sailer;D. Sanchez;A. Santangelo;M. Sasaki;M. Scalici;F. Schussler;H. Schutte;U. Schwanke;S. Schwemmer;M. Seglar-Arroyo;M. Senniappan;A. Seyffert;N. Shafi;K. Shiningayamwe;R.Simoni;A.Sinha;H. Sol;A. Specovius;S. Spencer;M. Spir-Jacob;L. Stawarz;L. Sun;R. Steenkamp;C. Stegmann;S. Steinmassl;C. Steppa;T. Takahashi;T. Tavernier;A. Taylor;R. Terrier;D. Tiziani;M. Tluczykont;L. Tomankova;C. Trichard;M. Tsirou;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;H. Volk;T. Vuillaume;Z. Wadiasingh;S. Wagner;J. Watson;F. Werner;R. White;A. Wierzcholska;Y. Wong;A. Yusafzai;M. Zacharias;R. Zanin;D. Zargaryan;A. Zdziarski;A. Zech;S. Zhu;J. Zorn;S. Zouari;N. Żywucka
我们通过来自Wolf-Lundmark-Melotte（WLM）矮不规则星系的非常高能量的伽马射线来寻找暗物质的间接信号。暗物质粒子的对湮灭将产生最终状态的标准模型粒子，如伽马射线，这可能被地面切伦科夫望远镜探测到。矮不规则星系是有希望的目标，因为它们是暗物质占主导地位的对象，具有良好的测量运动学和小的不确定性，其暗物质分布轮廓。2018年，H.E.S.S.五个望远镜阵列对矮不规则星系WLM进行了18小时的观测。我们提出的第一个分析的基础上获得的数据从成像大气切伦科夫望远镜的矮星系的这个子类。由于我们没有观察到任何显着的过剩的方向WLM，我们解释的结果在速度加权横截面的约束暗物质对湮灭作为一个函数的暗物质粒子质量的各种连续通道，以及提示伽马-伽马发射。对于$\tau^+\tau^-$通道，对于1 TeV的暗物质粒子质量，极限达到约4\times 10^{-22}$cm 3s-1的$\langle \sigma v \rangle$值。对于瞬发伽马-伽马通道，对于370 GeV的质量，上限达到$\langle \sigma v \rangle$值约为$5\times 10 ^{-24}$cm 3 s-1。这些限制代表了一个改进的因素200相对于以前的结果为矮不规则星系TeV的暗物质搜索。
We search for an indirect signal of dark matter through very high-energy gamma rays from the Wolf-Lundmark-Melotte (WLM) dwarf irregular galaxy. The pair annihilation of dark matter particles would produce Standard Model particles in the final state such as gamma rays, which might be detected by ground-based Cherenkov telescopes. Dwarf irregular galaxies represent promising targets as they are dark matter dominated objects with well measured kinematics and small uncertainties on their dark matter distribution profiles. In 2018, the H.E.S.S. five-telescope array observed the dwarf irregular galaxy WLM for 18 hours. We present the first analysis based on data obtained from an imaging atmospheric Cherenkov telescope for this subclass of dwarf galaxy. As we do not observe any significant excess in the direction of WLM, we interpret the result in terms of constraints on the velocity-weighted cross section for dark matter pair annihilation as a function of the dark matter particle mass for various continuum channels as well as the prompt gamma-gamma emission. For the $\tau^+\tau^-$ channel the limits reach a $\langle \sigma v \rangle$ value of about $4\times 10^{-22}$ cm3s-1 for a dark matter particle mass of 1 TeV. For the prompt gamma-gamma channel, the upper limit reaches a $\langle \sigma v \rangle$ value of about $5 \times10^{-24}$ cm3s-1 for a mass of 370 GeV. These limits represent an improvement of up to a factor 200 with respect to previous results for the dwarf irregular galaxies for TeV dark matter search.