First result from the Alpha Magnetic Spectrometer on the International Space Station: precision measurement of the positron fraction in primary cosmic rays of 0.5-350 GeV
A precision measurement by the Alpha Magnetic Spectrometer on the International Space Station of the positron fraction in primary cosmic rays in the energy range from 0.5 to 350 GeV based on 6.8 × 10(6) positron and electron events is presented. The very accurate data show that the positron fraction...
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| Veröffentlicht in: | Physical review letters 2013-04, Vol.110 (14), p.141102-141102, Article 141102 |
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| creator | Aguilar, M Alberti, G Alpat, B Alvino, A Ambrosi, G Andeen, K Anderhub, H Arruda, L Azzarello, P Bachlechner, A Barao, F Baret, B Barrau, A Barrin, L Bartoloni, A Basara, L Basili, A Batalha, L Bates, J Battiston, R Bazo, J Becker, R Becker, U Behlmann, M Beischer, B Berdugo, J Berges, P Bertucci, B Bigongiari, G Biland, A Bindi, V Bizzaglia, S Boella, G de Boer, W Bollweg, K Bolmont, J Borgia, B Borsini, S Boschini, M J Boudoul, G Bourquin, M Brun, P Buénerd, M Burger, J Burger, W Cadoux, F Cai, X D Capell, M Casadei, D Casaus, J Cascioli, V Castellini, G Cernuda, I Cervelli, F Chae, M J Chang, Y H Chen, A I Chen, C R Chen, H Cheng, G M Chen, H S Cheng, L Chernoplyiokov, N Chikanian, A Choumilov, E Choutko, V Chung, C H Clark, C Clavero, R Coignet, G Commichau, V Consolandi, C Contin, A Corti, C Costado Dios, M T Coste, B Crespo, D Cui, Z Dai, M Delgado, C Della Torre, S Demirkoz, B Dennett, P Derome, L Di Falco, S Diao, X H Diago, A Djambazov, L Díaz, C von Doetinchem, P Du, W J Dubois, J M Duperay, R Duranti, M D'Urso, D Egorov, A Eline, A Eppling, F J Eronen, T van Es, J |
| description | A precision measurement by the Alpha Magnetic Spectrometer on the International Space Station of the positron fraction in primary cosmic rays in the energy range from 0.5 to 350 GeV based on 6.8 × 10(6) positron and electron events is presented. The very accurate data show that the positron fraction is steadily increasing from 10 to ∼ 250 GeV, but, from 20 to 250 GeV, the slope decreases by an order of magnitude. The positron fraction spectrum shows no fine structure, and the positron to electron ratio shows no observable anisotropy. Together, these features show the existence of new physical phenomena. |
| doi_str_mv | 10.1103/physrevlett.110.141102 |
| format | Article |
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The very accurate data show that the positron fraction is steadily increasing from 10 to ∼ 250 GeV, but, from 20 to 250 GeV, the slope decreases by an order of magnitude. The positron fraction spectrum shows no fine structure, and the positron to electron ratio shows no observable anisotropy. 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D</creatorcontrib><creatorcontrib>Casaus, J</creatorcontrib><creatorcontrib>Cascioli, V</creatorcontrib><creatorcontrib>Castellini, G</creatorcontrib><creatorcontrib>Cernuda, I</creatorcontrib><creatorcontrib>Cervelli, F</creatorcontrib><creatorcontrib>Chae, M J</creatorcontrib><creatorcontrib>Chang, Y H</creatorcontrib><creatorcontrib>Chen, A I</creatorcontrib><creatorcontrib>Chen, C R</creatorcontrib><creatorcontrib>Chen, H</creatorcontrib><creatorcontrib>Cheng, G M</creatorcontrib><creatorcontrib>Chen, H S</creatorcontrib><creatorcontrib>Cheng, L</creatorcontrib><creatorcontrib>Chernoplyiokov, N</creatorcontrib><creatorcontrib>Chikanian, A</creatorcontrib><creatorcontrib>Choumilov, E</creatorcontrib><creatorcontrib>Choutko, V</creatorcontrib><creatorcontrib>Chung, C H</creatorcontrib><creatorcontrib>Clark, C</creatorcontrib><creatorcontrib>Clavero, R</creatorcontrib><creatorcontrib>Coignet, G</creatorcontrib><creatorcontrib>Commichau, V</creatorcontrib><creatorcontrib>Consolandi, 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D</creatorcontrib><creatorcontrib>Egorov, A</creatorcontrib><creatorcontrib>Eline, A</creatorcontrib><creatorcontrib>Eppling, F J</creatorcontrib><creatorcontrib>Eronen, T</creatorcontrib><creatorcontrib>van Es, J</creatorcontrib><creatorcontrib>AMS Collaboration</creatorcontrib><title>First result from the Alpha Magnetic Spectrometer on the International Space Station: precision measurement of the positron fraction in primary cosmic rays of 0.5-350 GeV</title><title>Physical review letters</title><addtitle>Phys Rev Lett</addtitle><description>A precision measurement by the Alpha Magnetic Spectrometer on the International Space Station of the positron fraction in primary cosmic rays in the energy range from 0.5 to 350 GeV based on 6.8 × 10(6) positron and electron events is presented. The very accurate data show that the positron fraction is steadily increasing from 10 to ∼ 250 GeV, but, from 20 to 250 GeV, the slope decreases by an order of magnitude. The positron fraction spectrum shows no fine structure, and the positron to electron ratio shows no observable anisotropy. Together, these features show the existence of new physical phenomena.</description><subject>Astrophysics</subject><subject>High Energy Astrophysical Phenomena</subject><subject>Physics</subject><subject>Sciences of the 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result from the Alpha Magnetic Spectrometer on the International Space Station: precision measurement of the positron fraction in primary cosmic rays of 0.5-350 GeV</title><author>Aguilar, M ; Alberti, G ; Alpat, B ; Alvino, A ; Ambrosi, G ; Andeen, K ; Anderhub, H ; Arruda, L ; Azzarello, P ; Bachlechner, A ; Barao, F ; Baret, B ; Barrau, A ; Barrin, L ; Bartoloni, A ; Basara, L ; Basili, A ; Batalha, L ; Bates, J ; Battiston, R ; Bazo, J ; Becker, R ; Becker, U ; Behlmann, M ; Beischer, B ; Berdugo, J ; Berges, P ; Bertucci, B ; Bigongiari, G ; Biland, A ; Bindi, V ; Bizzaglia, S ; Boella, G ; de Boer, W ; Bollweg, K ; Bolmont, J ; Borgia, B ; Borsini, S ; Boschini, M J ; Boudoul, G ; Bourquin, M ; Brun, P ; Buénerd, M ; Burger, J ; Burger, W ; Cadoux, F ; Cai, X D ; Capell, M ; Casadei, D ; Casaus, J ; Cascioli, V ; Castellini, G ; Cernuda, I ; Cervelli, F ; Chae, M J ; Chang, Y H ; Chen, A I ; Chen, C R ; Chen, H ; Cheng, G M ; Chen, H S ; Cheng, L ; Chernoplyiokov, N ; Chikanian, A ; Choumilov, E ; Choutko, V ; Chung, C H ; Clark, C ; Clavero, R ; Coignet, G ; Commichau, V ; Consolandi, C ; Contin, A ; Corti, C ; Costado Dios, M T ; Coste, B ; Crespo, D ; Cui, Z ; Dai, M ; Delgado, C ; Della Torre, S ; Demirkoz, B ; Dennett, P ; Derome, L ; Di Falco, S ; Diao, X H ; Diago, A ; Djambazov, L ; Díaz, C ; von Doetinchem, P ; Du, W J ; Dubois, J M ; Duperay, R ; Duranti, M ; D'Urso, D ; Egorov, A ; Eline, A ; Eppling, F J ; Eronen, T ; van Es, J</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c577t-2d97c0544a9efee5340659707c1123d4155020320a179405481a24ea383f85a03</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>Astrophysics</topic><topic>High Energy Astrophysical Phenomena</topic><topic>Physics</topic><topic>Sciences of the Universe</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aguilar, M</creatorcontrib><creatorcontrib>Alberti, G</creatorcontrib><creatorcontrib>Alpat, B</creatorcontrib><creatorcontrib>Alvino, A</creatorcontrib><creatorcontrib>Ambrosi, G</creatorcontrib><creatorcontrib>Andeen, K</creatorcontrib><creatorcontrib>Anderhub, H</creatorcontrib><creatorcontrib>Arruda, L</creatorcontrib><creatorcontrib>Azzarello, P</creatorcontrib><creatorcontrib>Bachlechner, A</creatorcontrib><creatorcontrib>Barao, F</creatorcontrib><creatorcontrib>Baret, B</creatorcontrib><creatorcontrib>Barrau, A</creatorcontrib><creatorcontrib>Barrin, L</creatorcontrib><creatorcontrib>Bartoloni, A</creatorcontrib><creatorcontrib>Basara, L</creatorcontrib><creatorcontrib>Basili, A</creatorcontrib><creatorcontrib>Batalha, L</creatorcontrib><creatorcontrib>Bates, J</creatorcontrib><creatorcontrib>Battiston, R</creatorcontrib><creatorcontrib>Bazo, J</creatorcontrib><creatorcontrib>Becker, R</creatorcontrib><creatorcontrib>Becker, U</creatorcontrib><creatorcontrib>Behlmann, M</creatorcontrib><creatorcontrib>Beischer, B</creatorcontrib><creatorcontrib>Berdugo, J</creatorcontrib><creatorcontrib>Berges, P</creatorcontrib><creatorcontrib>Bertucci, B</creatorcontrib><creatorcontrib>Bigongiari, G</creatorcontrib><creatorcontrib>Biland, A</creatorcontrib><creatorcontrib>Bindi, V</creatorcontrib><creatorcontrib>Bizzaglia, S</creatorcontrib><creatorcontrib>Boella, G</creatorcontrib><creatorcontrib>de Boer, W</creatorcontrib><creatorcontrib>Bollweg, K</creatorcontrib><creatorcontrib>Bolmont, J</creatorcontrib><creatorcontrib>Borgia, B</creatorcontrib><creatorcontrib>Borsini, S</creatorcontrib><creatorcontrib>Boschini, M J</creatorcontrib><creatorcontrib>Boudoul, G</creatorcontrib><creatorcontrib>Bourquin, M</creatorcontrib><creatorcontrib>Brun, P</creatorcontrib><creatorcontrib>Buénerd, M</creatorcontrib><creatorcontrib>Burger, J</creatorcontrib><creatorcontrib>Burger, W</creatorcontrib><creatorcontrib>Cadoux, F</creatorcontrib><creatorcontrib>Cai, X D</creatorcontrib><creatorcontrib>Capell, M</creatorcontrib><creatorcontrib>Casadei, D</creatorcontrib><creatorcontrib>Casaus, J</creatorcontrib><creatorcontrib>Cascioli, V</creatorcontrib><creatorcontrib>Castellini, G</creatorcontrib><creatorcontrib>Cernuda, I</creatorcontrib><creatorcontrib>Cervelli, F</creatorcontrib><creatorcontrib>Chae, M J</creatorcontrib><creatorcontrib>Chang, Y H</creatorcontrib><creatorcontrib>Chen, A I</creatorcontrib><creatorcontrib>Chen, C R</creatorcontrib><creatorcontrib>Chen, H</creatorcontrib><creatorcontrib>Cheng, G M</creatorcontrib><creatorcontrib>Chen, H S</creatorcontrib><creatorcontrib>Cheng, L</creatorcontrib><creatorcontrib>Chernoplyiokov, N</creatorcontrib><creatorcontrib>Chikanian, A</creatorcontrib><creatorcontrib>Choumilov, E</creatorcontrib><creatorcontrib>Choutko, V</creatorcontrib><creatorcontrib>Chung, C H</creatorcontrib><creatorcontrib>Clark, C</creatorcontrib><creatorcontrib>Clavero, R</creatorcontrib><creatorcontrib>Coignet, G</creatorcontrib><creatorcontrib>Commichau, V</creatorcontrib><creatorcontrib>Consolandi, C</creatorcontrib><creatorcontrib>Contin, A</creatorcontrib><creatorcontrib>Corti, C</creatorcontrib><creatorcontrib>Costado Dios, M T</creatorcontrib><creatorcontrib>Coste, B</creatorcontrib><creatorcontrib>Crespo, D</creatorcontrib><creatorcontrib>Cui, Z</creatorcontrib><creatorcontrib>Dai, M</creatorcontrib><creatorcontrib>Delgado, C</creatorcontrib><creatorcontrib>Della Torre, S</creatorcontrib><creatorcontrib>Demirkoz, B</creatorcontrib><creatorcontrib>Dennett, P</creatorcontrib><creatorcontrib>Derome, L</creatorcontrib><creatorcontrib>Di Falco, S</creatorcontrib><creatorcontrib>Diao, X H</creatorcontrib><creatorcontrib>Diago, A</creatorcontrib><creatorcontrib>Djambazov, L</creatorcontrib><creatorcontrib>Díaz, C</creatorcontrib><creatorcontrib>von Doetinchem, P</creatorcontrib><creatorcontrib>Du, W J</creatorcontrib><creatorcontrib>Dubois, J M</creatorcontrib><creatorcontrib>Duperay, R</creatorcontrib><creatorcontrib>Duranti, M</creatorcontrib><creatorcontrib>D'Urso, D</creatorcontrib><creatorcontrib>Egorov, A</creatorcontrib><creatorcontrib>Eline, A</creatorcontrib><creatorcontrib>Eppling, F J</creatorcontrib><creatorcontrib>Eronen, T</creatorcontrib><creatorcontrib>van Es, J</creatorcontrib><creatorcontrib>AMS Collaboration</creatorcontrib><collection>PubMed</collection><collection>CrossRef</collection><collection>MEDLINE - Academic</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><collection>OSTI.GOV</collection><jtitle>Physical review letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Aguilar, M</au><au>Alberti, G</au><au>Alpat, B</au><au>Alvino, A</au><au>Ambrosi, G</au><au>Andeen, K</au><au>Anderhub, H</au><au>Arruda, L</au><au>Azzarello, P</au><au>Bachlechner, A</au><au>Barao, F</au><au>Baret, B</au><au>Barrau, A</au><au>Barrin, L</au><au>Bartoloni, A</au><au>Basara, L</au><au>Basili, A</au><au>Batalha, L</au><au>Bates, J</au><au>Battiston, R</au><au>Bazo, J</au><au>Becker, R</au><au>Becker, U</au><au>Behlmann, M</au><au>Beischer, B</au><au>Berdugo, J</au><au>Berges, P</au><au>Bertucci, B</au><au>Bigongiari, G</au><au>Biland, A</au><au>Bindi, V</au><au>Bizzaglia, S</au><au>Boella, G</au><au>de Boer, W</au><au>Bollweg, K</au><au>Bolmont, J</au><au>Borgia, B</au><au>Borsini, S</au><au>Boschini, M J</au><au>Boudoul, G</au><au>Bourquin, M</au><au>Brun, P</au><au>Buénerd, M</au><au>Burger, J</au><au>Burger, W</au><au>Cadoux, F</au><au>Cai, X D</au><au>Capell, M</au><au>Casadei, D</au><au>Casaus, J</au><au>Cascioli, V</au><au>Castellini, G</au><au>Cernuda, I</au><au>Cervelli, F</au><au>Chae, M J</au><au>Chang, Y H</au><au>Chen, A I</au><au>Chen, C R</au><au>Chen, H</au><au>Cheng, G M</au><au>Chen, H S</au><au>Cheng, L</au><au>Chernoplyiokov, N</au><au>Chikanian, A</au><au>Choumilov, E</au><au>Choutko, V</au><au>Chung, C H</au><au>Clark, C</au><au>Clavero, R</au><au>Coignet, G</au><au>Commichau, V</au><au>Consolandi, C</au><au>Contin, A</au><au>Corti, C</au><au>Costado Dios, M T</au><au>Coste, B</au><au>Crespo, D</au><au>Cui, Z</au><au>Dai, M</au><au>Delgado, C</au><au>Della Torre, S</au><au>Demirkoz, B</au><au>Dennett, P</au><au>Derome, L</au><au>Di Falco, S</au><au>Diao, X H</au><au>Diago, A</au><au>Djambazov, L</au><au>Díaz, C</au><au>von Doetinchem, P</au><au>Du, W J</au><au>Dubois, J M</au><au>Duperay, R</au><au>Duranti, M</au><au>D'Urso, D</au><au>Egorov, A</au><au>Eline, A</au><au>Eppling, F J</au><au>Eronen, T</au><au>van Es, J</au><aucorp>AMS Collaboration</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>First result from the Alpha Magnetic Spectrometer on the International Space Station: precision measurement of the positron fraction in primary cosmic rays of 0.5-350 GeV</atitle><jtitle>Physical review letters</jtitle><addtitle>Phys Rev Lett</addtitle><date>2013-04-03</date><risdate>2013</risdate><volume>110</volume><issue>14</issue><spage>141102</spage><epage>141102</epage><pages>141102-141102</pages><artnum>141102</artnum><issn>0031-9007</issn><eissn>1079-7114</eissn><abstract>A precision measurement by the Alpha Magnetic Spectrometer on the International Space Station of the positron fraction in primary cosmic rays in the energy range from 0.5 to 350 GeV based on 6.8 × 10(6) positron and electron events is presented. The very accurate data show that the positron fraction is steadily increasing from 10 to ∼ 250 GeV, but, from 20 to 250 GeV, the slope decreases by an order of magnitude. The positron fraction spectrum shows no fine structure, and the positron to electron ratio shows no observable anisotropy. Together, these features show the existence of new physical phenomena.</abstract><cop>United States</cop><pub>American Physical Society</pub><pmid>25166975</pmid><doi>10.1103/physrevlett.110.141102</doi><tpages>1</tpages><orcidid>https://orcid.org/0000-0001-6064-3858</orcidid><orcidid>https://orcid.org/0000-0002-8657-6742</orcidid><orcidid>https://orcid.org/0000-0003-3842-8531</orcidid><orcidid>https://orcid.org/0000-0002-0207-958X</orcidid><orcidid>https://orcid.org/0000-0001-5913-0596</orcidid><orcidid>https://orcid.org/0000-0001-6725-5399</orcidid><orcidid>https://orcid.org/0000-0003-3659-3218</orcidid><orcidid>https://orcid.org/0000-0003-1670-2966</orcidid><orcidid>https://orcid.org/0000-0002-9394-2392</orcidid><orcidid>https://orcid.org/0000-0002-5331-0606</orcidid><orcidid>https://orcid.org/0000-0003-4744-9748</orcidid><orcidid>https://orcid.org/0000-0003-1841-9486</orcidid><orcidid>https://orcid.org/0000-0002-1297-8925</orcidid><orcidid>https://orcid.org/0000-0002-9704-6472</orcidid><orcidid>https://orcid.org/0000-0003-4365-3282</orcidid><orcidid>https://orcid.org/0000-0002-1288-833X</orcidid><orcidid>https://orcid.org/0000-0001-5260-658X</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0031-9007 |
| ispartof | Physical review letters, 2013-04, Vol.110 (14), p.141102-141102, Article 141102 |
| issn | 0031-9007 1079-7114 |
| language | eng |
| recordid | cdi_osti_scitechconnect_1104019 |
| source | American Physical Society Journals |
| subjects | Astrophysics High Energy Astrophysical Phenomena Physics Sciences of the Universe |
| title | First result from the Alpha Magnetic Spectrometer on the International Space Station: precision measurement of the positron fraction in primary cosmic rays of 0.5-350 GeV |
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