Optimized dark matter searches in deep observations of Segue 1 with MAGIC
Optimized dark matter searches in deep observations of Segue 1 with MAGIC
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DOI：
10.1088/1475-7516/2014/02/008
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发表时间：
2013-12
影响因子：
6.4
通讯作者：
J. Aleksi'c;S. Ansoldi;L. A. Antonelli;P. Antoranz;A. Babić;P. Bangale;U. D. Almeida;J. Barrio;J. B. Gonz'alez;W. Bednarek;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;S. Bonnefoy;G. Bonnoli;F. Borracci;T. Bretz;E. Carmona;A. Carosi;D. Fidalgo;P. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;P. D. Vela;F. Dazzi;A. Angelis;G. Caneva;B. Lotto;C. Mendez;M. Doert;A. Dom'inguez;D. D. Prester-D.;D. Dorner;M. Doro;S. Einecke;D. Eisenacher;D. Elsaesser;E. Farina;D. Ferenc;M. Fonseca;L. Font;K. Frantzen;C. Fruck;R. L'opez;M. Garczarczyk;D. G. Terrats;M. Gaug;G. Giavitto;N. Godinovi'c;A. G. Muñoz;S. Gozzini;D. Hadasch;M. Hayashida;A. Herrero;D. Hildebrand;J. Hose;D. Hrupec;W. Idec;V. Kadenius;H. Kellermann;K. Kodani;Y. Konno;J. Krause;H. Kubo;J. Kushida;A. Barbera;D. Lelas;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;I. Lozano;M. Makariev;K. Mallot;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;B. Marcote;M. Mariotti;M. Mart'inez;D. Mazin;U. Menzel;M. Meucci;J. Miranda;R. Mirzoyan;A. Moralejo;P. Munar-Adrover;D. Nakajima;A. Niedźwiecki;K. Nilsson;K. Nishijima;N. Nowak;R. Orito;A. Overkemping;S. Paiano;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;X. Paredes-Fortuny;S. Partini;M. Persic;F. Prada;P. Moroni;E. Prandini;S. Preziuso;I. Puljak;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;J. Garcia;S. Rugamer;A. Saggion;T. Saito;K. Saito;M. Salvati;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;A. Sillanpaa;J. Sitarek;I. Šnidarić;D. Sobczynska;F. Spanier;V. Stamatescu;A. Stamerra;T. Steinbring;J. Storz;S. Sun;T. Suri'c;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzi'c;D. Tescaro;M. Teshima;J. Thaele;O. Tibolla;D. Torres;T. Toyama;A. Treves;M. Uellenbeck;P. Vogler;R. Wagner;F. Zandanel;R. Zanin;A. Ibarra;Ifae;Campus Uab;E-08193 Bellaterra;Spain.;U. Udine;I. Trieste;I. Udine;Italy;I. I. F. Astrophysics-I.;I. Rome;U. Siena;I. Pisa;I. Siena;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;HR-10000 Zagreb;Croatia.;M. F. Physik;D-80805 Munchen;H Germany;U. Complutense;E. Madrid;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;E-38200 La Laguna;Tenerife;University of L'od'z;PL-90236 Lodz;Poland.;D. Elektronen-Synchrotron;D. Zeuthen;E. Zurich;CH-8093 Zurich;Switzerland.;U. Wurzburg;D-97074 Wurzburg;Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;Technische Universitat Dortmund;D. Dortmund;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;E. Granada;U. Padova;Infn;I-35131 Padova;Universita' dell'Insubria;Como;I-22100 Como;Unitat de F'isica de les Radiacions-Unitat-de-F'isica-de-les-Radiacions-1381421020;D. D. F'isica-D.;CERES-IEEC;U. Barcelona;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Japanese Magic Consortium;D. Physics;Astronomy;Kyoto University;Japan.;Finnish Magic Consortium;T. Observatory;U. Turku;D. Physics;U. Oulu;Finland.;Inst. for Nucl. Research;Nucl. Energy;BG-1784 Sofia;Bulgaria.;U. Barcelona;Icc;IEEC-UB;E. Barcelona;U. Pisa;I. Pisa;now at Nasa Goddard Space Flight Center;Greenbelt;MD 20771;Usa;D. O. Astronomy;U. Maryland;College Park;MD 20742;N. C. E. P. F. D. Lausanne;Lausanne;now at Department of PhysicsAstronomy;Uc Riverside;CA 92521;N. Eso;Turku;also at INAF-Trieste;A. M. D. D. F. Teorica-A.-M.-D.-D.-F.-Teorica-1381421114;Uamcsic;E. Madrid;now at Stockholm University;Oskar Klein Centre for Cosmoparticle Physics;S. Stockholm;Sweden.;Now at Grappa Institute;U. Amsterdam;1098XH Amsterdam;Netherlands.;Physik-Department T30d;T. U. Munchen;85748 Garching
中科院分区：
文献类型：
--
作者：
J. Aleksi'c;S. Ansoldi;L. A. Antonelli;P. Antoranz;A. Babić;P. Bangale;U. D. Almeida;J. Barrio;J. B. Gonz'alez;W. Bednarek;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;S. Bonnefoy;G. Bonnoli;F. Borracci;T. Bretz;E. Carmona;A. Carosi;D. Fidalgo;P. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;P. D. Vela;F. Dazzi;A. Angelis;G. Caneva;B. Lotto;C. Mendez;M. Doert;A. Dom'inguez;D. D. Prester-D.;D. Dorner;M. Doro;S. Einecke;D. Eisenacher;D. Elsaesser;E. Farina;D. Ferenc;M. Fonseca;L. Font;K. Frantzen;C. Fruck;R. L'opez;M. Garczarczyk;D. G. Terrats;M. Gaug;G. Giavitto;N. Godinovi'c;A. G. Muñoz;S. Gozzini;D. Hadasch;M. Hayashida;A. Herrero;D. Hildebrand;J. Hose;D. Hrupec;W. Idec;V. Kadenius;H. Kellermann;K. Kodani;Y. Konno;J. Krause;H. Kubo;J. Kushida;A. Barbera;D. Lelas;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;I. Lozano;M. Makariev;K. Mallot;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;B. Marcote;M. Mariotti;M. Mart'inez;D. Mazin;U. Menzel;M. Meucci;J. Miranda;R. Mirzoyan;A. Moralejo;P. Munar-Adrover;D. Nakajima;A. Niedźwiecki;K. Nilsson;K. Nishijima;N. Nowak;R. Orito;A. Overkemping;S. Paiano;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;X. Paredes-Fortuny;S. Partini;M. Persic;F. Prada;P. Moroni;E. Prandini;S. Preziuso;I. Puljak;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;J. Garcia;S. Rugamer;A. Saggion;T. Saito;K. Saito;M. Salvati;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;A. Sillanpaa;J. Sitarek;I. Šnidarić;D. Sobczynska;F. Spanier;V. Stamatescu;A. Stamerra;T. Steinbring;J. Storz;S. Sun;T. Suri'c;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzi'c;D. Tescaro;M. Teshima;J. Thaele;O. Tibolla;D. Torres;T. Toyama;A. Treves;M. Uellenbeck;P. Vogler;R. Wagner;F. Zandanel;R. Zanin;A. Ibarra;Ifae;Campus Uab;E-08193 Bellaterra;Spain.;U. Udine;I. Trieste;I. Udine;Italy;I. I. F. Astrophysics-I.;I. Rome;U. Siena;I. Pisa;I. Siena;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;HR-10000 Zagreb;Croatia.;M. F. Physik;D-80805 Munchen;H Germany;U. Complutense;E. Madrid;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;E-38200 La Laguna;Tenerife;University of L'od'z;PL-90236 Lodz;Poland.;D. Elektronen-Synchrotron;D. Zeuthen;E. Zurich;CH-8093 Zurich;Switzerland.;U. Wurzburg;D-97074 Wurzburg;Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;Technische Universitat Dortmund;D. Dortmund;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;E. Granada;U. Padova;Infn;I-35131 Padova;Universita' dell'Insubria;Como;I-22100 Como;Unitat de F'isica de les Radiacions-Unitat-de-F'isica-de-les-Radiacions-1381421020;D. D. F'isica-D.;CERES-IEEC;U. Barcelona;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Japanese Magic Consortium;D. Physics;Astronomy;Kyoto University;Japan.;Finnish Magic Consortium;T. Observatory;U. Turku;D. Physics;U. Oulu;Finland.;Inst. for Nucl. Research;Nucl. Energy;BG-1784 Sofia;Bulgaria.;U. Barcelona;Icc;IEEC-UB;E. Barcelona;U. Pisa;I. Pisa;now at Nasa Goddard Space Flight Center;Greenbelt;MD 20771;Usa;D. O. Astronomy;U. Maryland;College Park;MD 20742;N. C. E. P. F. D. Lausanne;Lausanne;now at Department of PhysicsAstronomy;Uc Riverside;CA 92521;N. Eso;Turku;also at INAF-Trieste;A. M. D. D. F. Teorica-A.-M.-D.-D.-F.-Teorica-1381421114;Uamcsic;E. Madrid;now at Stockholm University;Oskar Klein Centre for Cosmoparticle Physics;S. Stockholm;Sweden.;Now at Grappa Institute;U. Amsterdam;1098XH Amsterdam;Netherlands.;Physik-Department T30d;T. U. Munchen;85748 Garching
我们展示了 2011 年至 2013 年间使用 MAGIC 望远镜对卫星星系 Segue 1 进行的立体观测结果。凭借近 160 小时的高质量数据，这是迄今为止在电磁频谱极高能量范围内对矮星系进行的最深入的观测活动。我们在这个大数据样本中搜索质量范围在 100 GeV 到 20 TeV 之间的暗物质粒子信号。为此，我们使用完全似然分析方法，该方法为特征伽马射线光谱特征提供最佳灵敏度，例如暗物质湮灭或衰变所预期的特征。特别是，我们将搜索重点放在不同最终状态标准模型粒子产生的伽马射线、内部轫致辐射湮灭、单色线和盒形信号上。我们的结果代表了对卫星星系观测中获得的湮没截面或衰变寿命最严格的限制，质量超过数百吉伏。特别是，我们的最强极限（95% 置信水平）对应于 ∼ 500 GeV 暗物质粒子湮灭成 τ+τ−，其量级为 ⟨σannv⟩ ≃ 1.2 × 10−24 cm3 s−1 — 比 ⟨σannv⟩ ≃ 热值高出 ∼ 40 倍。
We present the results of stereoscopic observations of the satellite galaxy Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours of good-quality data, this is the deepest observational campaign on any dwarf galaxy performed so far in the very high energy range of the electromagnetic spectrum. We search this large data sample for signals of dark matter particles in the mass range between 100 GeV and 20 TeV. For this we use the full likelihood analysis method, which provides optimal sensitivity to characteristic gamma-ray spectral features, like those expected from dark matter annihilation or decay. In particular, we focus our search on gamma-rays produced from different final state Standard Model particles, annihilation with internal bremsstrahlung, monochromatic lines and box-shaped signals. Our results represent the most stringent constraints to the annihilation cross-section or decay lifetime obtained from observations of satellite galaxies, for masses above few hundred GeV. In particular, our strongest limit (95% confidence level) corresponds to a ∼ 500 GeV dark matter particle annihilating into τ+τ−, and is of order ⟨σannv⟩ ≃ 1.2 × 10−24 cm3 s−1 — a factor ∼ 40 above the ⟨σannv⟩ ≃ thermal value.