An Indication of Anisotropy in Arrival Directions of Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern of Extragalactic Gamma-Ray Sources
An Indication of Anisotropy in Arrival Directions of Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern of Extragalactic Gamma-Ray Sources
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DOI：
10.3847/2041-8213/aaa66d
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发表时间：
2018-01
期刊：
影响因子：
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通讯作者：
T. P. A. C. A. Aab-T.-P.-A.-C.-A.-Aab-103010298;P. Abreu;M. Aglietta;I. Albuquerque;I. Allekotte;A. Almela;J. A. Castillo;J. Alvarez-Muñiz;G. A. Anastasi;L. Anchordoqui;B. Andrada;S. Andringa;C. Aramo;N. Arsene;Hernán Asorey;P. Assis;G. Avila;A. Badescu;A. Bălăceanu;F. Barbato;R. Luz;J. Beatty;K. Becker;J. Bellido;C. Bérat;M. Bertaina;X. Bertou;P. Biermann;J. Biteau;S. Blaess;A. Blanco;J. Blazek;C. Bleve;M. Boh'avcov'a;C. Bonifazi;N. Borodai;A. Botti;J. Brack;I. Brancus;T. Bretz;A. Bridgeman;F. Briechle;P. Buchholz;A. Bueno;S. Buitink;M. Buscemi;K. Caballero-Mora;L. Caccianiga;A. Cancio;F. Canfora;R. Caruso;A. Castellina;F. Catalani;G. Cataldi;L. Cazon;A. Chavez;J. Chinellato;J. Chudoba;R. Clay;A. Cerutti;R. Colalillo;A. Coleman;L. Collica;M. Coluccia;R. Conceiccao;G. Consolati;F. Contreras;M. Cooper;S. Coutu;C. Covault;J. Cronin;S. D'Amico;B. Daniel;S. Dasso;K. Daumiller;B. Dawson;R. M. Almeida;S. Jong;G. D. Mauro;J. D. M. Neto;I. Mitri;J. D. Oliveira;V. Souza;J. Debatin;O. Deligny;M. L. D. Castro;F. Diogo;C. Dobrigkeit;J. D'Olivo;Q. Dorosti;R. C. Anjos;M. Dova;A. Dundović;J. Ebr;R. Engel;M. Erdmann;M. Erfani;C. Escobar;J. Espadanal;A. Etchegoyen;H. Falcke;J. Farmer;G. Farrar;A. Fauth;N. Fazzini;F. Fenu;B. Fick;J. M. Figueira;A. Filipvcivc;M. Freire;T. Fujii;A. Fuster;R. Gaior;B. Garc'ia;F. Gat'e;H. Gemmeke;A. Gherghel-Lascu;P. Ghia;U. Giaccari;M. Giammarchi;M. Giller;D. Glas;C. Glaser;G. Golup;M. G. Berisso;P. Vitale;N. Gonz'alez;A. Gorgi;A. Grillo;T. D. Grubb;F. Guarino;G. Guedes;R. Halliday;M. Hampel;P. Hansen;D. Harari;T. Harrison;A. Haungs;T. Hebbeker;D. Heck;P. Heimann;A. Hervé;G. Hill;C. Hojvat;E. Holt;P. Homola;J. Horandel;P. Horváth;M. Hrabovsk'y;T. Huege;J. Hulsman;A. Insolia;P. G. Isar;I. Jandt;J. Johnsen;M. Josebachuili;J. Juryšek;A. Kaapa;O. Kambeitz;K. Kampert;B. Keilhauer;N. Kemmerich;E. Kemp;J. Kemp;R. Kieckhafer;H. Klages;M. Kleifges;J. Kleinfeller;R. Krause;N. Krohm;D. Kuempel;G. K. Mezek;N. Kunka;A. Awad;B. Lago;D. LaHurd;R. Lang;M. Lauscher;R. Legumina;M. Oliveira;A. Letessier-Selvon;I. Lhenry-Yvon;K. Link;D. L. Presti;L. Lopes;R. L'opez;A. L. Casado;R. Lorek;Q. Luce;A. Lucero;M. Malacari;M. Mallamaci;D. Mandát;P. Mantsch;A. Mariazzi;I. Marics;G. Marsella;D. Martello;H. Martinez;O. M. Bravo;J. Meza;H. Mathes;S. Mathys;J. Matthews;G. Matthiae;E. Mayotte;P. Mazur;C. Medina;G. Medina-Tanco;D. Melo;A. Menshikov;K. Merenda;S. Michal;M. Micheletti;L. Middendorf;L. Miramonti;B. Mitrica;D. Mockler;S. Mollerach;F. Montanet;C. Morello;G. Morlino;M. Mostaf'a;A. Muller;G. Muller;M. Muller;S. Muller;R. Mussa;I. Naranjo;L. Nellen;P. Nguyen;M. Niculescu-Oglinzanu;M. Niechciol;L. Niemietz;T. Niggemann;D. Nitz;D. Nosek;V. Novotny;L. Novzka;L. N'unez;F. Oikonomou;A. Olinto;M. Palatka;J. Pallotta;P. Papenbreer;G. Parente;A. Parra;T. Paul;M. Pech;F. Pedreira;J. Pkekala;R. Pelayo;J. Peña-Rodríguez;L. Pereira;M. Perlin;L. Perrone;C. Peters;S. Petrera;J. Phuntsok;T. Pierog;M. Pimenta;V. Pirronello;M. Platino;M. Plum;J. Poh;C. Porowski;R. Prado;P. Privitera;M. Prouza;E. Quel;S. Querchfeld;S. Quinn;R. Ramos-Pollán;J. Rautenberg;D. Ravignani;J. Řídký;F. Riehn;M. Risse;P. Ristori;V. Rizi;W. Carvalho;G. R. Fernandez;J. Rojo;M. Roncoroni;M. Roth;E. Roulet;A. Rovero;P. Ruehl;S. Saffi;A. Săftoiu;F. Salamida;H. Salazar;A. Saleh;G. Salina;F. S'anchez;P. Sanchez-Lucas;E. Santos;E. Santos;F. Sarazin;R. Sarmento;C. Sarmiento-Cano;R. Sato;M. Schauer;V. Scherini;H. Schieler;M. Schimp;D. Schmidt;O. Scholten;P. Schov'anek;F. Schroder;S. Schroder;A. Schulz;J. Schumacher;S. Sciutto;A. Segreto;A. Shadkam;R. Shellard;G. Sigl;G. Silli;R. vSm'ida;G. Snow;P. Sommers;S. Sonntag;J. F. Soriano;R. Squartini;D. Stanca;S. Stanivc;J. Stasielak;P. Stassi;M. Stolpovskiy;F. Strafella;A. Streich;F. Suarez;M. S. Dur'an;T. Sudholz;T. Suomijarvi;A. Supanitsky;J. vSup'ik;J. Swain;Z. Szadkowski;A. Taboada;O. Taborda;V. M. Theodoro;C. Timmermans;C. T. Peixoto;L. Tomankova;B. Tom'e;G. T. Elipe;P. Trávníček;M. Trini;R. Ulrich;M. Unger;M. Urban;J. F. V. Galicia;I. Valiño;L. Valore;G. V. Aar;P. Bodegom;A. M. Berg;A. V. Vliet;E. Varela;B. V. C'ardenas;R. V'azquez;D. Veberivc;C. Ventura;I. D. V. Quispe;V. Verzi;J. Vícha;L. Villaseñor;S. Vorobiov;H. Wahlberg;O. Wainberg;D. Walz;A. Watson;M. Weber;A. Weindl;M. Wiede'nski;L. Wiencke;H. Wilczy'nski;M. Wirtz;D. Wittkowski;B. Wundheiler;L. Yang;A. Yushkov;E. Zas;D. Zavrtanik;M. Zavrtanik;A. Zepeda;B. Zimmermann;M. Ziolkowski;Z. Zong;F. Zuccarello
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文献类型：
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作者：
T. P. A. C. A. Aab-T.-P.-A.-C.-A.-Aab-103010298;P. Abreu;M. Aglietta;I. Albuquerque;I. Allekotte;A. Almela;J. A. Castillo;J. Alvarez-Muñiz;G. A. Anastasi;L. Anchordoqui;B. Andrada;S. Andringa;C. Aramo;N. Arsene;Hernán Asorey;P. Assis;G. Avila;A. Badescu;A. Bălăceanu;F. Barbato;R. Luz;J. Beatty;K. Becker;J. Bellido;C. Bérat;M. Bertaina;X. Bertou;P. Biermann;J. Biteau;S. Blaess;A. Blanco;J. Blazek;C. Bleve;M. Boh'avcov'a;C. Bonifazi;N. Borodai;A. Botti;J. Brack;I. Brancus;T. Bretz;A. Bridgeman;F. Briechle;P. Buchholz;A. Bueno;S. Buitink;M. Buscemi;K. Caballero-Mora;L. Caccianiga;A. Cancio;F. Canfora;R. Caruso;A. Castellina;F. Catalani;G. Cataldi;L. Cazon;A. Chavez;J. Chinellato;J. Chudoba;R. Clay;A. Cerutti;R. Colalillo;A. Coleman;L. Collica;M. Coluccia;R. Conceiccao;G. Consolati;F. Contreras;M. Cooper;S. Coutu;C. Covault;J. Cronin;S. D'Amico;B. Daniel;S. Dasso;K. Daumiller;B. Dawson;R. M. Almeida;S. Jong;G. D. Mauro;J. D. M. Neto;I. Mitri;J. D. Oliveira;V. Souza;J. Debatin;O. Deligny;M. L. D. Castro;F. Diogo;C. Dobrigkeit;J. D'Olivo;Q. Dorosti;R. C. Anjos;M. Dova;A. Dundović;J. Ebr;R. Engel;M. Erdmann;M. Erfani;C. Escobar;J. Espadanal;A. Etchegoyen;H. Falcke;J. Farmer;G. Farrar;A. Fauth;N. Fazzini;F. Fenu;B. Fick;J. M. Figueira;A. Filipvcivc;M. Freire;T. Fujii;A. Fuster;R. Gaior;B. Garc'ia;F. Gat'e;H. Gemmeke;A. Gherghel-Lascu;P. Ghia;U. Giaccari;M. Giammarchi;M. Giller;D. Glas;C. Glaser;G. Golup;M. G. Berisso;P. Vitale;N. Gonz'alez;A. Gorgi;A. Grillo;T. D. Grubb;F. Guarino;G. Guedes;R. Halliday;M. Hampel;P. Hansen;D. Harari;T. Harrison;A. Haungs;T. Hebbeker;D. Heck;P. Heimann;A. Hervé;G. Hill;C. Hojvat;E. Holt;P. Homola;J. Horandel;P. Horváth;M. Hrabovsk'y;T. Huege;J. Hulsman;A. Insolia;P. G. Isar;I. Jandt;J. Johnsen;M. Josebachuili;J. Juryšek;A. Kaapa;O. Kambeitz;K. Kampert;B. Keilhauer;N. Kemmerich;E. Kemp;J. Kemp;R. Kieckhafer;H. Klages;M. Kleifges;J. Kleinfeller;R. Krause;N. Krohm;D. Kuempel;G. K. Mezek;N. Kunka;A. Awad;B. Lago;D. LaHurd;R. Lang;M. Lauscher;R. Legumina;M. Oliveira;A. Letessier-Selvon;I. Lhenry-Yvon;K. Link;D. L. Presti;L. Lopes;R. L'opez;A. L. Casado;R. Lorek;Q. Luce;A. Lucero;M. Malacari;M. Mallamaci;D. Mandát;P. Mantsch;A. Mariazzi;I. Marics;G. Marsella;D. Martello;H. Martinez;O. M. Bravo;J. Meza;H. Mathes;S. Mathys;J. Matthews;G. Matthiae;E. Mayotte;P. Mazur;C. Medina;G. Medina-Tanco;D. Melo;A. Menshikov;K. Merenda;S. Michal;M. Micheletti;L. Middendorf;L. Miramonti;B. Mitrica;D. Mockler;S. Mollerach;F. Montanet;C. Morello;G. Morlino;M. Mostaf'a;A. Muller;G. Muller;M. Muller;S. Muller;R. Mussa;I. Naranjo;L. Nellen;P. Nguyen;M. Niculescu-Oglinzanu;M. Niechciol;L. Niemietz;T. Niggemann;D. Nitz;D. Nosek;V. Novotny;L. Novzka;L. N'unez;F. Oikonomou;A. Olinto;M. Palatka;J. Pallotta;P. Papenbreer;G. Parente;A. Parra;T. Paul;M. Pech;F. Pedreira;J. Pkekala;R. Pelayo;J. Peña-Rodríguez;L. Pereira;M. Perlin;L. Perrone;C. Peters;S. Petrera;J. Phuntsok;T. Pierog;M. Pimenta;V. Pirronello;M. Platino;M. Plum;J. Poh;C. Porowski;R. Prado;P. Privitera;M. Prouza;E. Quel;S. Querchfeld;S. Quinn;R. Ramos-Pollán;J. Rautenberg;D. Ravignani;J. Řídký;F. Riehn;M. Risse;P. Ristori;V. Rizi;W. Carvalho;G. R. Fernandez;J. Rojo;M. Roncoroni;M. Roth;E. Roulet;A. Rovero;P. Ruehl;S. Saffi;A. Săftoiu;F. Salamida;H. Salazar;A. Saleh;G. Salina;F. S'anchez;P. Sanchez-Lucas;E. Santos;E. Santos;F. Sarazin;R. Sarmento;C. Sarmiento-Cano;R. Sato;M. Schauer;V. Scherini;H. Schieler;M. Schimp;D. Schmidt;O. Scholten;P. Schov'anek;F. Schroder;S. Schroder;A. Schulz;J. Schumacher;S. Sciutto;A. Segreto;A. Shadkam;R. Shellard;G. Sigl;G. Silli;R. vSm'ida;G. Snow;P. Sommers;S. Sonntag;J. F. Soriano;R. Squartini;D. Stanca;S. Stanivc;J. Stasielak;P. Stassi;M. Stolpovskiy;F. Strafella;A. Streich;F. Suarez;M. S. Dur'an;T. Sudholz;T. Suomijarvi;A. Supanitsky;J. vSup'ik;J. Swain;Z. Szadkowski;A. Taboada;O. Taborda;V. M. Theodoro;C. Timmermans;C. T. Peixoto;L. Tomankova;B. Tom'e;G. T. Elipe;P. Trávníček;M. Trini;R. Ulrich;M. Unger;M. Urban;J. F. V. Galicia;I. Valiño;L. Valore;G. V. Aar;P. Bodegom;A. M. Berg;A. V. Vliet;E. Varela;B. V. C'ardenas;R. V'azquez;D. Veberivc;C. Ventura;I. D. V. Quispe;V. Verzi;J. Vícha;L. Villaseñor;S. Vorobiov;H. Wahlberg;O. Wainberg;D. Walz;A. Watson;M. Weber;A. Weindl;M. Wiede'nski;L. Wiencke;H. Wilczy'nski;M. Wirtz;D. Wittkowski;B. Wundheiler;L. Yang;A. Yushkov;E. Zas;D. Zavrtanik;M. Zavrtanik;A. Zepeda;B. Zimmermann;M. Ziolkowski;Z. Zong;F. Zuccarello
对Pierre Auger天文台数据集的新分析提供了超高能宇宙射线到达方向在中间角尺度上各向异性的证据，这表明来自附近强源的过量到达。这些数据包括2017年4月30日之前记录的天顶角高达80°的5514个事件。天空模型已经创建了两个不同的人口河外伽玛射线发射：活动星系核从第二目录的硬费米-LAT源（2FHL）和星暴星系从一个样本，用费米-LAT检查。通量有限的样本，其中包括所有类型的星系从雨燕BAT和2 MASS调查，进行了比较研究。使用每个目录构建的宇宙射线密度的天空模型有两个自由参数，与天体相关的事件的分数，和一个角标度表征星系外源周围宇宙射线的聚集。最大似然比检验用于评估这些参数的最佳值，并通过与各向同性的对比来量化每个模型的强度。结果表明，星爆模型比各向同性假设更能拟合数据，其统计显著性为4.0σ，最高检验统计量出现在能量大于10000的情况下。三种替代模型均优于各向同性模型，显著性为2.7σ-3.2σ。从各向同性的指示偏差的起源进行了检查和更敏感的未来研究的前景进行了讨论。
A new analysis of the data set from the Pierre Auger Observatory provides evidence for anisotropy in the arrival directions of ultra-high-energy cosmic rays on an intermediate angular scale, which is indicative of excess arrivals from strong, nearby sources. The data consist of 5514 events above with zenith angles up to 80° recorded before 2017 April 30. Sky models have been created for two distinct populations of extragalactic gamma-ray emitters: active galactic nuclei from the second catalog of hard Fermi-LAT sources (2FHL) and starburst galaxies from a sample that was examined with Fermi-LAT. Flux-limited samples, which include all types of galaxies from the Swift-BAT and 2MASS surveys, have been investigated for comparison. The sky model of cosmic-ray density constructed using each catalog has two free parameters, the fraction of events correlating with astrophysical objects, and an angular scale characterizing the clustering of cosmic rays around extragalactic sources. A maximum-likelihood ratio test is used to evaluate the best values of these parameters and to quantify the strength of each model by contrast with isotropy. It is found that the starburst model fits the data better than the hypothesis of isotropy with a statistical significance of 4.0σ, the highest value of the test statistic being for energies above . The three alternative models are favored against isotropy with 2.7σ–3.2σ significance. The origin of the indicated deviation from isotropy is examined and prospects for more sensitive future studies are discussed.