A stacked analysis of brightest cluster galaxies observed with the Fermi Large Area Telescope
A stacked analysis of brightest cluster galaxies observed with the Fermi Large Area Telescope
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用费米大面积望远镜观测到的最亮星团星系的叠加分析
DOI：
10.1093/mnras/sts477
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发表时间：
2013
影响因子：
4.8
通讯作者：
Dutson K
中科院分区：
文献类型：
--
作者：
Dutson K
我们提出了一个大样本的星系团的高能γ射线发射的搜索结果，共享现有的三个费米大面积望远镜探测（英仙座，室女座和A3392），即一个强大的无线电源在他们最亮的集群星系（BCG）的属性。从863个星系团的父源X射线通量有限样本中，我们选择了114个核心主导的BCG射电通量超过50/75 mJy的系统（分别在国家射电天文台甚大阵列巡天和悉尼大学莫龙洛巡天），将费米任务前45个月的数据在三个能带中叠加，对于大于300 MeV的选择，对于显著性<3σ的样品，整个样品的探测显著性分布与整个对照样品的分布一致，但是具有延伸到更高值的尾部，包括与先前识别的γ射线发射无关的三个>4σ信号。对这些字段中的数据进行建模，结果检测到4个非2FGL费米子，尽管这些似乎都与BCG候选者无关。只有一个足够接近，可以作为可能的对应物（RXC J0132.6 - 0804），其余三个似乎是背景活动星系核。在能量>3 GeV的搜索暗示了A2055中BCG的发射，它拥有一个BL Lac天体。在叠加数据中没有信号的证据，而对于每个波段的平均射电亮BCG的γ射线通量上限的推导比单个天体的计算值至少要严格一个数量级。对于样品中的平均BCG，F1 GeV/F1.4 GHz <15，而英仙座的NGC 1275则为120，这可能表明在高能量下探测到的天体是一个特例。从成员星系发出的点状光束构成了星系团中主要的明亮γ射线源，这一试探性的建议意味着寻找暗物质湮灭或大规模合并激波特征的证据，例如，需要考虑来自每个星系团内部的显著水平的污染，这种污染既具有高度随机性，又随着时间的推移而显著变化。
We present the results of a search for high-energy γ-ray emission from a large sample of galaxy clusters sharing the properties of three existingFermiLarge Area Telescope detections (in Perseus, Virgo and A3392), namely a powerful radio source within their brightest cluster galaxy (BCG). From a parent, X-ray flux-limited sample of 863 clusters, we select 114 systems with a core-dominated BCG radio flux above 50/75 mJy (in the National Radio Astronomy Observatory Very Large Array Sky Survey and the Sydney University Molonglo Sky Survey, respectively), stacking data from the first 45 months of theFermimission in three energy bands, to determine statistical limits on the γ-ray fluxes of the ensemble of candidate sources.For a >300 MeV selection, the distribution of detection significance across the sample is consistent with that across control samples for significances <3σ, but has a tail extending to higher values, including three >4σ signals which are not associated with previously identified γ-ray emission. Modelling of the data in these fields results in the detection of four non-2FGLFermisources, though none of these appear to beunambiguouslyassociated with the BCG candidate. Only one is sufficiently close to be a plausible counterpart (RXC J0132.6−0804) and the remaining three appear to be background active galactic nuclei. A search at energies >3 GeV hints at emission from the BCG in A2055, which hosts a BL Lac object.There is no evidence for a signal in the stacked data, and the upper limit derived on the γ-ray flux of an average radio-bright BCG in each band is at least an order of magnitude more constraining than that calculated for individual objects.F1 GeV/F1.4 GHzfor an average BCG in the sample is <15, compared with ≈120 for NGC 1275 in Perseus, which might indicate a special case for those objects detected at high energies. The tentative suggestion that point-likebeamedemission from member galaxies comprise the dominant bright γ-ray sources in clusters implies searches for evidence of dark matter annihilation or large-scale merger shock signatures, for example, need to account for a significant level of contamination from within each cluster that is both highly stochastic and varies significantly over time.
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影响因子：
5.5
作者：
M. C. J. Aleksi'c;E. Alvarez;L. A. Antonelli;P. Antoranz;M. Asensio;Michael Backes;U. D. Almeida;J. Barrio;D. Bastieri;J. Gonz'alez;W. Bednarek;A. Berdyugin;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;A. Boller;G. Bonnoli;D. Tridon;I. Braun;T. Bretz;A. Cañellas;E. Carmona;A. Carosi;P. Colin;E. Colombo;J. Contreras;J. Cortina;L. Cossio;S. Covino;F. Dazzi;A. Angelis;G. Caneva;E. C. D. Pozo;B. Lotto;C. Mendez;A. Ortega;M. Doert;A. Domínguez;D. D. Prester-D.;D. Dorner;M. Doro;D. Eisenacher;D. Elsaesser;D. Ferenc;M. V. Fonseca;L. Font;C. Fruck;R. L'opez;M. Garczarczyk;D. Garrido;G. Giavitto;N. Godinovi'c;S. Gozzini;D. Hadasch;D. Hafner;A. Herrero;D. Hildebrand;D. Hohne-Monch;J. Hose;D. Hrupec;T. Jogler;H. Kellermann;S. Klepser;T. Krahenbuhl;J. Krause;J. Kushida;A. Barbera;D. Lelas;E. Leonardo;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;M. Makariev;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;A. Niedźwiecki;D. Nieto;K. Nilsson;N. Nowak;R. Orito;S. Paiano;D. Paneque;R. Paoletti;S. Pardo;J. Paredes;S. Partini;M. Pérez-Torres;M. Persic;L. Peruzzo;M. Pilia;J. Pochon;F. Prada;P. Moroni;E. Prandini;I. Gimenez;I. Puljak;I. Reichardt;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;S. Rugamer;A. Saggion;K. Saito;T. Saito;M. Salvati;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;M. Shayduk;S. Shore;A. Sillanpaa;J. Sitarek;I. Šnidarić;D. Sobczynska;F. Spanier;S. Spiro;V. Stamatescu;A. Stamerra;B. Steinke;J. Storz;N. Strah;S. Sun;T. Suri'c;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzi'c;D. Tescaro;M. Teshima;O. Tibolla;D. Torres;A. Treves;M. Uellenbeck;H. Vankov;P. Vogler;R. Wagner;Q. Weitzel;V. Zabalza;F. Zandanel;R. Zanin;C. Pfrommer;A. P. Ifae;Edifici Cn.;Campus Uab;Bellaterra;Spain.;U. Complutense;Madrid;I. I. F. Astrophysics-I.;Romé;Italy.;U. Siena;I. Pisa;Siena;Technische Universitat Dortmund;Dortmund;H Germany;M. F. Physik;Munchen;U. Padova;Infn;Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;La Laguna;Tenerife;D. Astrof'isica;U. L. Laguna;University of L'od'z;Lodz;Poland;T. Observatory;U. Turku;Piikkio;Finland.;D. Elektronen-Synchrotron;Zeuthen;E. Zurich;Zurich;Switzerland.;U. Wurzburg;Wurzburg;U. Barcelona;Barcelona;U. Udine;I. Trieste;Udine;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;Granada;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;Zagreb;Croatia.;U. Barcelona;Inst. for Nucl. Research;Nucl. Energy;Sofía;Bulgaria.;INAF-Osservatorio Astronomico;Trieste;Universita' dell'Insubria;Como;U. Pisa;Pisa;Icrea;N. C. E. P. F. D. Lausanne;Lausanne;supported by Infn Padova;Now at Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;N. Eso;Hits;Heidelberg;U. Barbara;Santa Barbara;Ca;Usa
通讯作者：
M. C. J. Aleksi'c;E. Alvarez;L. A. Antonelli;P. Antoranz;M. Asensio;Michael Backes;U. D. Almeida;J. Barrio;D. Bastieri;J. Gonz'alez;W. Bednarek;A. Berdyugin;K. Berger;E. Bernardini;A. Biland;O. Blanch;R. Bock;A. Boller;G. Bonnoli;D. Tridon;I. Braun;T. Bretz;A. Cañellas;E. Carmona;A. Carosi;P. Colin;E. Colombo;J. Contreras;J. Cortina;L. Cossio;S. Covino;F. Dazzi;A. Angelis;G. Caneva;E. C. D. Pozo;B. Lotto;C. Mendez;A. Ortega;M. Doert;A. Domínguez;D. D. Prester-D.;D. Dorner;M. Doro;D. Eisenacher;D. Elsaesser;D. Ferenc;M. V. Fonseca;L. Font;C. Fruck;R. L'opez;M. Garczarczyk;D. Garrido;G. Giavitto;N. Godinovi'c;S. Gozzini;D. Hadasch;D. Hafner;A. Herrero;D. Hildebrand;D. Hohne-Monch;J. Hose;D. Hrupec;T. Jogler;H. Kellermann;S. Klepser;T. Krahenbuhl;J. Krause;J. Kushida;A. Barbera;D. Lelas;E. Leonardo;N. Lewandowska;E. Lindfors;S. Lombardi;M. L'opez;R. L'opez-Coto;A. L'opez-Oramas;E. Lorenz;M. Makariev;G. Maneva;N. Mankuzhiyil;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart'inez;D. Mazin;M. Meucci;J. Miranda;R. Mirzoyan;J. Mold'on;A. Moralejo;P. Munar-Adrover;A. Niedźwiecki;D. Nieto;K. Nilsson;N. Nowak;R. Orito;S. Paiano;D. Paneque;R. Paoletti;S. Pardo;J. Paredes;S. Partini;M. Pérez-Torres;M. Persic;L. Peruzzo;M. Pilia;J. Pochon;F. Prada;P. Moroni;E. Prandini;I. Gimenez;I. Puljak;I. Reichardt;R. Reinthal;W. Rhode;M. Rib'o;J. Rico;S. Rugamer;A. Saggion;K. Saito;T. Saito;M. Salvati;K. Satalecka;V. Scalzotto;V. Scapin;C. Schultz;T. Schweizer;M. Shayduk;S. Shore;A. Sillanpaa;J. Sitarek;I. Šnidarić;D. Sobczynska;F. Spanier;S. Spiro;V. Stamatescu;A. Stamerra;B. Steinke;J. Storz;N. Strah;S. Sun;T. Suri'c;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzi'c;D. Tescaro;M. Teshima;O. Tibolla;D. Torres;A. Treves;M. Uellenbeck;H. Vankov;P. Vogler;R. Wagner;Q. Weitzel;V. Zabalza;F. Zandanel;R. Zanin;C. Pfrommer;A. P. Ifae;Edifici Cn.;Campus Uab;Bellaterra;Spain.;U. Complutense;Madrid;I. I. F. Astrophysics-I.;Romé;Italy.;U. Siena;I. Pisa;Siena;Technische Universitat Dortmund;Dortmund;H Germany;M. F. Physik;Munchen;U. Padova;Infn;Padova;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-102997450;La Laguna;Tenerife;D. Astrof'isica;U. L. Laguna;University of L'od'z;Lodz;Poland;T. Observatory;U. Turku;Piikkio;Finland.;D. Elektronen-Synchrotron;Zeuthen;E. Zurich;Zurich;Switzerland.;U. Wurzburg;Wurzburg;U. Barcelona;Barcelona;U. Udine;I. Trieste;Udine;Institut de Ci'encies de l'Espai-Institut-de-Ci'encies-de-l'Espai-123080358;Inst. de Astrof'isica de Andaluc'ia-Inst.-de-Astrof'isica-de-Andaluc'ia-102813830;Granada;Croatian Magic Consortium;Rudjer Boskovic Institute;University of Rijeka;University of Split;Zagreb;Croatia.;U. Barcelona;Inst. for Nucl. Research;Nucl. Energy;Sofía;Bulgaria.;INAF-Osservatorio Astronomico;Trieste;Universita' dell'Insubria;Como;U. Pisa;Pisa;Icrea;N. C. E. P. F. D. Lausanne;Lausanne;supported by Infn Padova;Now at Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;N. Eso;Hits;Heidelberg;U. Barbara;Santa Barbara;Ca;Usa
影响因子：
3.5
作者：
H. Völk;A. Atoyan;A. Atoyan
通讯作者：
A. Atoyan
影响因子：
7.9
作者：
Ackermann, M.;Ajello, M.;Ziegler, M.
通讯作者：
Ziegler, M.
影响因子：
4.9
作者：
Atwood, W. B.;Abdo, A. A.;Ziegler, M.
通讯作者：
Ziegler, M.
DOI：
10.1046/j.1365-8711.2003.06605.x
发表时间：
2003-03
影响因子：
4.8
作者：
T. Mauch;T. Murphy;H. Buttery;J. Curran;R. Hunstead;B. Piestrzynski;J. Robertson;E. B. G. U. O. Sydney;U. Cambridge
通讯作者：
T. Mauch;T. Murphy;H. Buttery;J. Curran;R. Hunstead;B. Piestrzynski;J. Robertson;E. B. G. U. O. Sydney;U. Cambridge