000064319 001__ 64319 000064319 005__ 20190709135621.0 000064319 0247_ $$2doi$$a10.3847/2041-8213/aa978b 000064319 0248_ $$2sideral$$a103560 000064319 037__ $$aART-2017-103560 000064319 041__ $$aeng 000064319 100__ $$aAnglada, G. 000064319 245__ $$aALMA Discovery of Dust Belts around Proxima Centauri 000064319 260__ $$c2017 000064319 5060_ $$aAccess copy available to the general public$$fUnrestricted 000064319 5203_ $$aProxima Centauri, the star closest to our Sun, is known to host at least one terrestrial planet candidate in a temperate orbit. Here we report the Atacama Large Millimeter/submillimeter Array (ALMA) detection of the star at 1.3 mm wavelength and the discovery of a belt of dust orbiting around it at distances ranging between 1 and 4 au, approximately. Given the low luminosity of the Proxima Centauri star, we estimate a characteristic temperature of about 40 K for this dust, which might constitute the dust component of a small-scale analog to our solar system''s Kuiper Belt. The estimated total mass, including dust and bodies up to 50 km in size, is of the order of 0.01 Earth masses, which is similar to that of the solar Kuiper Belt. Our data also show a hint of warmer dust closer to the star. We also find signs of two additional features that might be associated with the Proxima Centauri system that still require further observations to be confirmed: an outer extremely cold (about 10 K) belt around the star at about 30 au, with an orbital plane that is tilted about 45° with respect to the plane of the sky; additionally, we marginally detect a compact 1.3 mm emission source at a projected distance of about 1.2 arcsec from the star, the nature of which is still unknown. 000064319 536__ $$9info:eu-repo/grantAgreement/ES/MINECO/ESP2016-76076-R$$9info:eu-repo/grantAgreement/ES/MINECO/ESP2014-54362-P$$9info:eu-repo/grantAgreement/ES/MINECO/ESP2014-54032-R$$9info:eu-repo/grantAgreement/ES/MINECO/AYA2016-79425-C3-3-P$$9info:eu-repo/grantAgreement/ES/MINECO/AYA2015-63939-C2-1-P$$9info:eu-repo/grantAgreement/ES/MINECO/AYA2014-57369-C3-3-P$$9info:eu-repo/grantAgreement/ES/MINECO/AYA2014-56637-C2-1-P 000064319 540__ $$9info:eu-repo/semantics/openAccess$$aby-nc-nd$$uhttp://creativecommons.org/licenses/by-nc-nd/3.0/es/ 000064319 590__ $$a6.634$$b2017 000064319 591__ $$aASTRONOMY & ASTROPHYSICS$$b8 / 66 = 0.121$$c2017$$dQ1$$eT1 000064319 592__ $$a3.186$$b2017 000064319 593__ $$aSpace and Planetary Science$$c2017$$dQ1 000064319 593__ $$aAstronomy and Astrophysics$$c2017$$dQ1 000064319 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion 000064319 700__ $$aAmado, P.J. 000064319 700__ $$aOrtiz, J.L. 000064319 700__ $$aGómez, J.F. 000064319 700__ $$aMacIas, E. 000064319 700__ $$aAlberdi, A. 000064319 700__ $$aOsorio, M. 000064319 700__ $$aGómez, J.L. 000064319 700__ $$aGregorio-Monsalvo, I.D. 000064319 700__ $$0(orcid)0000-0001-5654-0266$$aPérez-Torres, M.A.$$uUniversidad de Zaragoza 000064319 700__ $$aAnglada-Escudé, G. 000064319 700__ $$aBerdinas, Z.M. 000064319 700__ $$aJenkins, J.S. 000064319 700__ $$aJimenez-Serra, I. 000064319 700__ $$aLara, L.M. 000064319 700__ $$aLópez-González, M.J. 000064319 700__ $$aLópez-Puertas, M. 000064319 700__ $$aMorales, N. 000064319 700__ $$aRibas, I. 000064319 700__ $$aRichards, A.M.S. 000064319 700__ $$aRodriguez-López, C. 000064319 700__ $$aRodriguez, E. 000064319 7102_ $$12004$$2405$$aUniversidad de Zaragoza$$bDpto. Física Teórica$$cÁrea Física Teórica 000064319 773__ $$g850, 1 (2017), L6 [5 pp]$$pASTROPHYSICAL JOURNAL LETTERS$$tASTROPHYSICAL JOURNAL LETTERS$$x2041-8205 000064319 8564_ $$s986340$$uhttps://zaguan.unizar.es/record/64319/files/texto_completo.pdf$$yVersión publicada 000064319 8564_ $$s133141$$uhttps://zaguan.unizar.es/record/64319/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada 000064319 909CO $$ooai:zaguan.unizar.es:64319$$particulos$$pdriver 000064319 951__ $$a2019-07-09-12:27:47 000064319 980__ $$aARTICLE