Contamination of stellar-kinematic samples and uncertainty about dark matter annihilation profiles in ultrafaint dwarf galaxies: the example of Segue I
Contamination of stellar-kinematic samples and uncertainty about dark matter annihilation profiles in ultrafaint dwarf galaxies: the example of Segue I
复制标题
恒星运动样本的污染和超微弱矮星系中暗物质湮没剖面的不确定性：Segue I 的例子
DOI：
--
复制
发表时间：
2015
期刊：
影响因子：
--
通讯作者：
M. Walker
中科院分区：
文献类型：
--
作者：
V. Bonnivard;D. Maurin;M. Walker
矮球状星系 (dSph) 中暗物质湮灭产生的预期伽马射线通量取决于所谓的“J 因子”，即暗物质密度平方沿视线的积分。我们研究了 J 估计值对恒星运动学样本污染（前景银河系恒星和恒星流）的敏感程度，这些样本用于推断“超微弱”dSphs 中的暗物质密度。将标准运动学分析应用于数百个包含不同污染程度的模拟数据集，我们发现错误分类的污染物可能会导致 J 因子被高估几个数量级。我们获得这种有偏差估计的恒星运动学数据集往往1）包含相对较大比例的具有不明确成员身份的恒星，2）给出对J的估计，该估计对如何加权和/或排除具有不明确状态的恒星的特定选择敏感。比较附近 dSphs Reticulum II 和 Segue I 的公开恒星运动学样本，我们发现只有后者表现出这两种特征。因此，在规划和解释伽马射线观测时，应更加谨慎地对待 Segue I 的 J 因子的估计。
The expected gamma-ray flux coming from dark matter annihilation in dwarf spheroidal (dSph) galaxies depends on the so-called 'J-factor', the integral of the squared dark matter density along the line-of-sight. We examine the degree to which estimates of J are sensitive to contamination (by foreground Milky Way stars and stellar streams) of the stellar-kinematic samples that are used to infer dark matter densities in 'ultrafaint' dSphs. Applying standard kinematic analyses to hundreds of mock data sets that include varying levels of contamination, we find that mis-classified contaminants can cause J-factors to be overestimated by orders of magnitude. Stellar-kinematic data sets for which we obtain such biased estimates tend 1) to include relatively large fractions of stars with ambiguous membership status, and 2) to give estimates for J that are sensitive to specific choices about how to weight and/or to exclude stars with ambiguous status. Comparing publicly-available stellar-kinematic samples for the nearby dSphs Reticulum II and Segue I, we find that only the latter displays both of these characteristics. Estimates of Segue I's J-factor should therefore be regarded with a larger degree of caution when planning and interpreting gamma-ray observations.
影响因子：
6.4
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
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
DOI：
10.1016/j.cpc.2015.11.012
发表时间：
2015-06
期刊：
Comput. Phys. Commun.
影响因子：
--
作者：
V. Bonnivard;M. Hütten;E. Nezri;A. Charbonnier;C. Combet;D. Maurin
通讯作者：
V. Bonnivard;M. Hütten;E. Nezri;A. Charbonnier;C. Combet;D. Maurin