An Indication of Anisotropy in Arrival Directions of Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern of Extragalactic Gamma-Ray Sources
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 wit...
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| Veröffentlicht in: | Astrophys.J.Lett 2018-02, Vol.853 (2), p.L29 |
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| creator | Aab, A. Abreu, P. Aglietta, M. Albuquerque, I. F. M. Allekotte, I. Almela, A. Castillo, J. Alvarez Alvarez-Muñiz, J. Anastasi, G. A. Anchordoqui, L. Andrada, B. Andringa, S. Aramo, C. Arsene, N. Asorey, H. Assis, P. Avila, G. Badescu, A. M. Balaceanu, A. Barbato, F. Luz, R. J. Barreira Beatty, J. J. Becker, K. H. Bellido, J. A. Berat, C. Bertaina, M. E. Bertou, X. Biermann, P. L. Biteau, J. Blaess, S. G. Blanco, A. Blazek, J. Bleve, C. Boháčová, M. Bonifazi, C. Borodai, N. Botti, A. M. Brack, J. Brancus, I. Bretz, T. Bridgeman, A. Briechle, F. L. Buchholz, P. Bueno, A. Buitink, S. Buscemi, M. Caballero-Mora, K. S. Caccianiga, L. Cancio, A. Canfora, F. Caruso, R. Castellina, A. Catalani, F. Cataldi, G. Cazon, L. Chavez, A. G. Chinellato, J. A. Chudoba, J. Clay, R. W. Cerutti, A. C. Cobos Colalillo, R. Coleman, A. Collica, L. Coluccia, M. R. Conceição, R. Consolati, G. Contreras, F. Cooper, M. J. Coutu, S. Covault, C. E. Cronin, J. D’Amico, S. Daniel, B. Dasso, S. Daumiller, K. Dawson, B. R. Almeida, R. M. de Jong, S. J. de Mauro, G. De de Mello Neto, J. R. T. Mitri, I. De Oliveira, J. de Souza, V. de Debatin, J. Deligny, O. Castro, M. L. Díaz Diogo, F. Dobrigkeit, C. D’Olivo, J. C. Dorosti, Q. Anjos, R. C. dos Dova, M. T. Dundovic, A. Ebr, J. Engel, R. Erdmann, M. Erfani, M. Escobar, C. O. Espadanal, J. Etchegoyen, A. |
| description | 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 4.0
σ
, the highest value of the test statistic being for energies above
. The three alternative models are favored against isotropy with 2.7
σ
–3.2
σ
significance. The origin of the indicated deviation from isotropy is examined and prospects for more sensitive future studies are discussed. |
| doi_str_mv | 10.3847/2041-8213/aaa66d |
| format | Article |
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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 4.0
σ
, the highest value of the test statistic being for energies above
. The three alternative models are favored against isotropy with 2.7
σ
–3.2
σ
significance. The origin of the indicated deviation from isotropy is examined and prospects for more sensitive future studies are discussed.</description><identifier>ISSN: 2041-8205</identifier><identifier>ISSN: 2041-8213</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/aaa66d</identifier><language>eng</language><publisher>Austin: IOP Publishing</publisher><subject>Active galactic nuclei ; Anisotropy ; ASTRONOMY AND ASTROPHYSICS ; Astrophysics ; Augers ; Clustering ; Cosmic ray models ; Cosmic rays ; Emitters ; Galaxies ; Gamma ray sources ; Gamma rays ; High energy astronomy ; Isotropy ; Likelihood ratio ; Mathematical models ; Parameters ; Physics ; Sky models ; Sky surveys (astronomy) ; Starburst galaxies ; Statistical analysis ; Statistical methods</subject><ispartof>Astrophys.J.Lett, 2018-02, Vol.853 (2), p.L29</ispartof><rights>Copyright IOP Publishing Feb 01, 2018</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c440t-b8109d0e6b2106dd88531c3027ec68a73a348467a4b394ebfc47561707ed93a73</citedby><cites>FETCH-LOGICAL-c440t-b8109d0e6b2106dd88531c3027ec68a73a348467a4b394ebfc47561707ed93a73</cites><orcidid>0000-0001-8294-6294 ; 0000-0003-2466-9086</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,27903,27904</link.rule.ids><backlink>$$Uhttps://hal.science/hal-01703798$$DView record in HAL$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/servlets/purl/1418449$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Aab, A.</creatorcontrib><creatorcontrib>Abreu, P.</creatorcontrib><creatorcontrib>Aglietta, M.</creatorcontrib><creatorcontrib>Albuquerque, I. F. M.</creatorcontrib><creatorcontrib>Allekotte, I.</creatorcontrib><creatorcontrib>Almela, A.</creatorcontrib><creatorcontrib>Castillo, J. Alvarez</creatorcontrib><creatorcontrib>Alvarez-Muñiz, J.</creatorcontrib><creatorcontrib>Anastasi, G. A.</creatorcontrib><creatorcontrib>Anchordoqui, L.</creatorcontrib><creatorcontrib>Andrada, B.</creatorcontrib><creatorcontrib>Andringa, S.</creatorcontrib><creatorcontrib>Aramo, C.</creatorcontrib><creatorcontrib>Arsene, N.</creatorcontrib><creatorcontrib>Asorey, H.</creatorcontrib><creatorcontrib>Assis, P.</creatorcontrib><creatorcontrib>Avila, G.</creatorcontrib><creatorcontrib>Badescu, A. M.</creatorcontrib><creatorcontrib>Balaceanu, A.</creatorcontrib><creatorcontrib>Barbato, F.</creatorcontrib><creatorcontrib>Luz, R. J. Barreira</creatorcontrib><creatorcontrib>Beatty, J. J.</creatorcontrib><creatorcontrib>Becker, K. H.</creatorcontrib><creatorcontrib>Bellido, J. 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L.</creatorcontrib><creatorcontrib>Buchholz, P.</creatorcontrib><creatorcontrib>Bueno, A.</creatorcontrib><creatorcontrib>Buitink, S.</creatorcontrib><creatorcontrib>Buscemi, M.</creatorcontrib><creatorcontrib>Caballero-Mora, K. S.</creatorcontrib><creatorcontrib>Caccianiga, L.</creatorcontrib><creatorcontrib>Cancio, A.</creatorcontrib><creatorcontrib>Canfora, F.</creatorcontrib><creatorcontrib>Caruso, R.</creatorcontrib><creatorcontrib>Castellina, A.</creatorcontrib><creatorcontrib>Catalani, F.</creatorcontrib><creatorcontrib>Cataldi, G.</creatorcontrib><creatorcontrib>Cazon, L.</creatorcontrib><creatorcontrib>Chavez, A. G.</creatorcontrib><creatorcontrib>Chinellato, J. A.</creatorcontrib><creatorcontrib>Chudoba, J.</creatorcontrib><creatorcontrib>Clay, R. W.</creatorcontrib><creatorcontrib>Cerutti, A. C. Cobos</creatorcontrib><creatorcontrib>Colalillo, R.</creatorcontrib><creatorcontrib>Coleman, A.</creatorcontrib><creatorcontrib>Collica, L.</creatorcontrib><creatorcontrib>Coluccia, M. R.</creatorcontrib><creatorcontrib>Conceição, R.</creatorcontrib><creatorcontrib>Consolati, G.</creatorcontrib><creatorcontrib>Contreras, F.</creatorcontrib><creatorcontrib>Cooper, M. J.</creatorcontrib><creatorcontrib>Coutu, S.</creatorcontrib><creatorcontrib>Covault, C. E.</creatorcontrib><creatorcontrib>Cronin, J.</creatorcontrib><creatorcontrib>D’Amico, S.</creatorcontrib><creatorcontrib>Daniel, B.</creatorcontrib><creatorcontrib>Dasso, S.</creatorcontrib><creatorcontrib>Daumiller, K.</creatorcontrib><creatorcontrib>Dawson, B. R.</creatorcontrib><creatorcontrib>Almeida, R. M. de</creatorcontrib><creatorcontrib>Jong, S. J. de</creatorcontrib><creatorcontrib>Mauro, G. De</creatorcontrib><creatorcontrib>de Mello Neto, J. R. T.</creatorcontrib><creatorcontrib>Mitri, I. De</creatorcontrib><creatorcontrib>Oliveira, J. de</creatorcontrib><creatorcontrib>Souza, V. de</creatorcontrib><creatorcontrib>Debatin, J.</creatorcontrib><creatorcontrib>Deligny, O.</creatorcontrib><creatorcontrib>Castro, M. L. Díaz</creatorcontrib><creatorcontrib>Diogo, F.</creatorcontrib><creatorcontrib>Dobrigkeit, C.</creatorcontrib><creatorcontrib>D’Olivo, J. C.</creatorcontrib><creatorcontrib>Dorosti, Q.</creatorcontrib><creatorcontrib>Anjos, R. C. dos</creatorcontrib><creatorcontrib>Dova, M. T.</creatorcontrib><creatorcontrib>Dundovic, A.</creatorcontrib><creatorcontrib>Ebr, J.</creatorcontrib><creatorcontrib>Engel, R.</creatorcontrib><creatorcontrib>Erdmann, M.</creatorcontrib><creatorcontrib>Erfani, M.</creatorcontrib><creatorcontrib>Escobar, C. O.</creatorcontrib><creatorcontrib>Espadanal, J.</creatorcontrib><creatorcontrib>Etchegoyen, A.</creatorcontrib><creatorcontrib>The Pierre Auger Collaboration</creatorcontrib><creatorcontrib>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</creatorcontrib><title>An Indication of Anisotropy in Arrival Directions of Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern of Extragalactic Gamma-Ray Sources</title><title>Astrophys.J.Lett</title><description>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 4.0
σ
, the highest value of the test statistic being for energies above
. The three alternative models are favored against isotropy with 2.7
σ
–3.2
σ
significance. The origin of the indicated deviation from isotropy is examined and prospects for more sensitive future studies are discussed.</description><subject>Active galactic nuclei</subject><subject>Anisotropy</subject><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Astrophysics</subject><subject>Augers</subject><subject>Clustering</subject><subject>Cosmic ray models</subject><subject>Cosmic rays</subject><subject>Emitters</subject><subject>Galaxies</subject><subject>Gamma ray sources</subject><subject>Gamma rays</subject><subject>High energy astronomy</subject><subject>Isotropy</subject><subject>Likelihood ratio</subject><subject>Mathematical models</subject><subject>Parameters</subject><subject>Physics</subject><subject>Sky models</subject><subject>Sky surveys (astronomy)</subject><subject>Starburst galaxies</subject><subject>Statistical analysis</subject><subject>Statistical methods</subject><issn>2041-8205</issn><issn>2041-8213</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNo9kUFv2yAYhq1qldq1u_eIutMOXsEQwEcra9pKkTa16xl9wSSmsiEDUsX_pT92eJ5yAr08etCrtyhuCP5OJRN3FWaklBWhdwDAeXtWXJ6iT6c7XlwUn2N8w7jCnMjL4qNx6Mm1VkOy3iG_RY2z0afg9yOyDjUh2Hfo0Q8bjJ6QODGvfQpQdnbXlcaZsBvR0sfBavQMY0SpC_6w63I27CFkm0PJ59SgVX84ol-Qkgn__ro_Zs8OeshqjR5gGKDMCvTiD0GbeF2cb6GP5sv_86p4Xd3_Xj6W658PT8tmXWrGcCo3kuC6xYZvKoJ520q5oERTXAmjuQRBgTLJuAC2oTUzm61mYsGJwMK0Nc3vV8Xt7PUxWRW1TUZ32juXKyvCiGSsztC3GeqgV_tgBwij8mDVY7NWU4azkYpavpPMfp3ZffB_DiYm9ZYbudxBVZQvOK9FJTOFZ0oHH2Mw25OWYDWNqqbV1LSgmkelfwGlbpVB</recordid><startdate>20180201</startdate><enddate>20180201</enddate><creator>Aab, A.</creator><creator>Abreu, P.</creator><creator>Aglietta, M.</creator><creator>Albuquerque, I. 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C. dos</creator><creator>Dova, M. T.</creator><creator>Dundovic, A.</creator><creator>Ebr, J.</creator><creator>Engel, R.</creator><creator>Erdmann, M.</creator><creator>Erfani, M.</creator><creator>Escobar, C. O.</creator><creator>Espadanal, J.</creator><creator>Etchegoyen, A.</creator><general>IOP Publishing</general><general>Institute of Physics (IOP)</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><scope>OIOZB</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0001-8294-6294</orcidid><orcidid>https://orcid.org/0000-0003-2466-9086</orcidid></search><sort><creationdate>20180201</creationdate><title>An Indication of Anisotropy in Arrival Directions of Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern of Extragalactic Gamma-Ray Sources</title><author>Aab, A. ; Abreu, P. ; Aglietta, M. ; Albuquerque, I. F. M. ; Allekotte, I. ; Almela, A. ; Castillo, J. Alvarez ; Alvarez-Muñiz, J. ; Anastasi, G. A. ; Anchordoqui, L. ; Andrada, B. ; Andringa, S. ; Aramo, C. ; Arsene, N. ; Asorey, H. ; Assis, P. ; Avila, G. ; Badescu, A. M. ; Balaceanu, A. ; Barbato, F. ; Luz, R. J. Barreira ; Beatty, J. J. ; Becker, K. H. ; Bellido, J. A. ; Berat, C. ; Bertaina, M. E. ; Bertou, X. ; Biermann, P. L. ; Biteau, J. ; Blaess, S. G. ; Blanco, A. ; Blazek, J. ; Bleve, C. ; Boháčová, M. ; Bonifazi, C. ; Borodai, N. ; Botti, A. M. ; Brack, J. ; Brancus, I. ; Bretz, T. ; Bridgeman, A. ; Briechle, F. L. ; Buchholz, P. ; Bueno, A. ; Buitink, S. ; Buscemi, M. ; Caballero-Mora, K. S. ; Caccianiga, L. ; Cancio, A. ; Canfora, F. ; Caruso, R. ; Castellina, A. ; Catalani, F. ; Cataldi, G. ; Cazon, L. ; Chavez, A. G. ; Chinellato, J. A. ; Chudoba, J. ; Clay, R. W. ; Cerutti, A. C. Cobos ; Colalillo, R. ; Coleman, A. ; Collica, L. ; Coluccia, M. R. ; Conceição, R. ; Consolati, G. ; Contreras, F. ; Cooper, M. J. ; Coutu, S. ; Covault, C. E. ; Cronin, J. ; D’Amico, S. ; Daniel, B. ; Dasso, S. ; Daumiller, K. ; Dawson, B. R. ; Almeida, R. M. de ; Jong, S. J. de ; Mauro, G. De ; de Mello Neto, J. R. T. ; Mitri, I. De ; Oliveira, J. de ; Souza, V. de ; Debatin, J. ; Deligny, O. ; Castro, M. L. Díaz ; Diogo, F. ; Dobrigkeit, C. ; D’Olivo, J. C. ; Dorosti, Q. ; Anjos, R. C. dos ; Dova, M. T. ; Dundovic, A. ; Ebr, J. ; Engel, R. ; Erdmann, M. ; Erfani, M. ; Escobar, C. O. ; Espadanal, J. ; Etchegoyen, A.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c440t-b8109d0e6b2106dd88531c3027ec68a73a348467a4b394ebfc47561707ed93a73</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Active galactic nuclei</topic><topic>Anisotropy</topic><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Astrophysics</topic><topic>Augers</topic><topic>Clustering</topic><topic>Cosmic ray models</topic><topic>Cosmic rays</topic><topic>Emitters</topic><topic>Galaxies</topic><topic>Gamma ray sources</topic><topic>Gamma rays</topic><topic>High energy astronomy</topic><topic>Isotropy</topic><topic>Likelihood ratio</topic><topic>Mathematical models</topic><topic>Parameters</topic><topic>Physics</topic><topic>Sky models</topic><topic>Sky surveys (astronomy)</topic><topic>Starburst galaxies</topic><topic>Statistical analysis</topic><topic>Statistical methods</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aab, A.</creatorcontrib><creatorcontrib>Abreu, P.</creatorcontrib><creatorcontrib>Aglietta, M.</creatorcontrib><creatorcontrib>Albuquerque, I. 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Cobos</creatorcontrib><creatorcontrib>Colalillo, R.</creatorcontrib><creatorcontrib>Coleman, A.</creatorcontrib><creatorcontrib>Collica, L.</creatorcontrib><creatorcontrib>Coluccia, M. R.</creatorcontrib><creatorcontrib>Conceição, R.</creatorcontrib><creatorcontrib>Consolati, G.</creatorcontrib><creatorcontrib>Contreras, F.</creatorcontrib><creatorcontrib>Cooper, M. J.</creatorcontrib><creatorcontrib>Coutu, S.</creatorcontrib><creatorcontrib>Covault, C. E.</creatorcontrib><creatorcontrib>Cronin, J.</creatorcontrib><creatorcontrib>D’Amico, S.</creatorcontrib><creatorcontrib>Daniel, B.</creatorcontrib><creatorcontrib>Dasso, S.</creatorcontrib><creatorcontrib>Daumiller, K.</creatorcontrib><creatorcontrib>Dawson, B. R.</creatorcontrib><creatorcontrib>Almeida, R. M. de</creatorcontrib><creatorcontrib>Jong, S. J. de</creatorcontrib><creatorcontrib>Mauro, G. De</creatorcontrib><creatorcontrib>de Mello Neto, J. R. T.</creatorcontrib><creatorcontrib>Mitri, I. De</creatorcontrib><creatorcontrib>Oliveira, J. de</creatorcontrib><creatorcontrib>Souza, V. de</creatorcontrib><creatorcontrib>Debatin, J.</creatorcontrib><creatorcontrib>Deligny, O.</creatorcontrib><creatorcontrib>Castro, M. L. Díaz</creatorcontrib><creatorcontrib>Diogo, F.</creatorcontrib><creatorcontrib>Dobrigkeit, C.</creatorcontrib><creatorcontrib>D’Olivo, J. C.</creatorcontrib><creatorcontrib>Dorosti, Q.</creatorcontrib><creatorcontrib>Anjos, R. C. dos</creatorcontrib><creatorcontrib>Dova, M. T.</creatorcontrib><creatorcontrib>Dundovic, A.</creatorcontrib><creatorcontrib>Ebr, J.</creatorcontrib><creatorcontrib>Engel, R.</creatorcontrib><creatorcontrib>Erdmann, M.</creatorcontrib><creatorcontrib>Erfani, M.</creatorcontrib><creatorcontrib>Escobar, C. O.</creatorcontrib><creatorcontrib>Espadanal, J.</creatorcontrib><creatorcontrib>Etchegoyen, A.</creatorcontrib><creatorcontrib>The Pierre Auger Collaboration</creatorcontrib><creatorcontrib>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><jtitle>Astrophys.J.Lett</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Aab, A.</au><au>Abreu, P.</au><au>Aglietta, M.</au><au>Albuquerque, I. F. M.</au><au>Allekotte, I.</au><au>Almela, A.</au><au>Castillo, J. Alvarez</au><au>Alvarez-Muñiz, J.</au><au>Anastasi, G. A.</au><au>Anchordoqui, L.</au><au>Andrada, B.</au><au>Andringa, S.</au><au>Aramo, C.</au><au>Arsene, N.</au><au>Asorey, H.</au><au>Assis, P.</au><au>Avila, G.</au><au>Badescu, A. M.</au><au>Balaceanu, A.</au><au>Barbato, F.</au><au>Luz, R. J. Barreira</au><au>Beatty, J. J.</au><au>Becker, K. H.</au><au>Bellido, J. A.</au><au>Berat, C.</au><au>Bertaina, M. E.</au><au>Bertou, X.</au><au>Biermann, P. L.</au><au>Biteau, J.</au><au>Blaess, S. G.</au><au>Blanco, A.</au><au>Blazek, J.</au><au>Bleve, C.</au><au>Boháčová, M.</au><au>Bonifazi, C.</au><au>Borodai, N.</au><au>Botti, A. M.</au><au>Brack, J.</au><au>Brancus, I.</au><au>Bretz, T.</au><au>Bridgeman, A.</au><au>Briechle, F. L.</au><au>Buchholz, P.</au><au>Bueno, A.</au><au>Buitink, S.</au><au>Buscemi, M.</au><au>Caballero-Mora, K. S.</au><au>Caccianiga, L.</au><au>Cancio, A.</au><au>Canfora, F.</au><au>Caruso, R.</au><au>Castellina, A.</au><au>Catalani, F.</au><au>Cataldi, G.</au><au>Cazon, L.</au><au>Chavez, A. G.</au><au>Chinellato, J. A.</au><au>Chudoba, J.</au><au>Clay, R. W.</au><au>Cerutti, A. C. Cobos</au><au>Colalillo, R.</au><au>Coleman, A.</au><au>Collica, L.</au><au>Coluccia, M. R.</au><au>Conceição, R.</au><au>Consolati, G.</au><au>Contreras, F.</au><au>Cooper, M. J.</au><au>Coutu, S.</au><au>Covault, C. E.</au><au>Cronin, J.</au><au>D’Amico, S.</au><au>Daniel, B.</au><au>Dasso, S.</au><au>Daumiller, K.</au><au>Dawson, B. R.</au><au>Almeida, R. M. de</au><au>Jong, S. J. de</au><au>Mauro, G. De</au><au>de Mello Neto, J. R. T.</au><au>Mitri, I. De</au><au>Oliveira, J. de</au><au>Souza, V. de</au><au>Debatin, J.</au><au>Deligny, O.</au><au>Castro, M. L. Díaz</au><au>Diogo, F.</au><au>Dobrigkeit, C.</au><au>D’Olivo, J. C.</au><au>Dorosti, Q.</au><au>Anjos, R. C. dos</au><au>Dova, M. T.</au><au>Dundovic, A.</au><au>Ebr, J.</au><au>Engel, R.</au><au>Erdmann, M.</au><au>Erfani, M.</au><au>Escobar, C. O.</au><au>Espadanal, J.</au><au>Etchegoyen, A.</au><aucorp>The Pierre Auger Collaboration</aucorp><aucorp>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>An Indication of Anisotropy in Arrival Directions of Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern of Extragalactic Gamma-Ray Sources</atitle><jtitle>Astrophys.J.Lett</jtitle><date>2018-02-01</date><risdate>2018</risdate><volume>853</volume><issue>2</issue><spage>L29</spage><pages>L29-</pages><issn>2041-8205</issn><issn>2041-8213</issn><eissn>2041-8213</eissn><abstract>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 4.0
σ
, the highest value of the test statistic being for energies above
. The three alternative models are favored against isotropy with 2.7
σ
–3.2
σ
significance. The origin of the indicated deviation from isotropy is examined and prospects for more sensitive future studies are discussed.</abstract><cop>Austin</cop><pub>IOP Publishing</pub><doi>10.3847/2041-8213/aaa66d</doi><orcidid>https://orcid.org/0000-0001-8294-6294</orcidid><orcidid>https://orcid.org/0000-0003-2466-9086</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 2041-8205 |
| ispartof | Astrophys.J.Lett, 2018-02, Vol.853 (2), p.L29 |
| issn | 2041-8205 2041-8213 2041-8213 |
| language | eng |
| recordid | cdi_osti_scitechconnect_1418449 |
| source | IOP Publishing Free Content; EZB-FREE-00999 freely available EZB journals; IOPscience extra; Alma/SFX Local Collection |
| subjects | Active galactic nuclei Anisotropy ASTRONOMY AND ASTROPHYSICS Astrophysics Augers Clustering Cosmic ray models Cosmic rays Emitters Galaxies Gamma ray sources Gamma rays High energy astronomy Isotropy Likelihood ratio Mathematical models Parameters Physics Sky models Sky surveys (astronomy) Starburst galaxies Statistical analysis Statistical methods |
| title | 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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