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dc.contributor.authorShvartzvald, Y.
dc.contributor.authorUdalski, A.
dc.contributor.authorGould, A.
dc.contributor.authorHan, C.
dc.contributor.authorBozza, V.
dc.contributor.authorFriedmann, M.
dc.contributor.authorHundertmark, Markus Peter Gerhard
dc.contributor.authorBeichman, C.
dc.contributor.authorBryden, G.
dc.contributor.authorNovati, S. Calchi
dc.contributor.authorCarey, S.
dc.contributor.authorFausnaugh, M.
dc.contributor.authorGaudi, B. S.
dc.contributor.authorHenderson, C. B.
dc.contributor.authorKerr, T.
dc.contributor.authorPogge, R. W.
dc.contributor.authorVarricatt, W.
dc.contributor.authorWibking, B.
dc.contributor.authorYee, J. C.
dc.contributor.authorZhu, W.
dc.contributor.authorPoleski, R.
dc.contributor.authorPawlak, M.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorSkowron, J.
dc.contributor.authorMróz, P.
dc.contributor.authorKozłowski, S.
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorPietrzyński, G.
dc.contributor.authorSoszyński, I.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorChoi, J.-Y.
dc.contributor.authorPark, H.
dc.contributor.authorJung, Y. K.
dc.contributor.authorShin, I.-G.
dc.contributor.authorAlbrow, M. D.
dc.contributor.authorPark, B.-G.
dc.contributor.authorKim, S.-L.
dc.contributor.authorLee, C.-U.
dc.contributor.authorCha, S.-M.
dc.contributor.authorKim, D.-J.
dc.contributor.authorLee, Y.
dc.contributor.authorMaoz, D.
dc.contributor.authorKaspi, S.
dc.contributor.authorStreet, R. A.
dc.contributor.authorTsapras, Y.
dc.contributor.authorBachelet, E.
dc.contributor.authorDominik, Martin
dc.contributor.authorBramich, D. M.
dc.contributor.authorHorne, Keith Douglas
dc.contributor.authorSnodgrass, C.
dc.contributor.authorSteele, I. A.
dc.contributor.authorMenzies, J.
dc.contributor.authorFiguera Jaimes, Roberto Jose
dc.contributor.authorWambsganss, J.
dc.contributor.authorSchmidt, R.
dc.contributor.authorCassan, A.
dc.contributor.authorRanc, C.
dc.contributor.authorMao, S.
dc.contributor.authorDong, Subo
dc.contributor.authorD’Ago, G.
dc.contributor.authorScarpetta, G.
dc.contributor.authorVerma, P.
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorKerins, E.
dc.contributor.authorSkottfelt, J.
dc.date.accessioned2016-01-05T10:40:08Z
dc.date.available2016-01-05T10:40:08Z
dc.date.issued2015-12-01
dc.identifier240080399
dc.identifier49bc8ce1-a0a4-4deb-b416-cadebe38ae0b
dc.identifier84948784130
dc.identifier000365317300029
dc.identifier.citationShvartzvald , Y , Udalski , A , Gould , A , Han , C , Bozza , V , Friedmann , M , Hundertmark , M P G , Beichman , C , Bryden , G , Novati , S C , Carey , S , Fausnaugh , M , Gaudi , B S , Henderson , C B , Kerr , T , Pogge , R W , Varricatt , W , Wibking , B , Yee , J C , Zhu , W , Poleski , R , Pawlak , M , Szymański , M K , Skowron , J , Mróz , P , Kozłowski , S , Wyrzykowski , Ł , Pietrukowicz , P , Pietrzyński , G , Soszyński , I , Ulaczyk , K , Choi , J-Y , Park , H , Jung , Y K , Shin , I-G , Albrow , M D , Park , B-G , Kim , S-L , Lee , C-U , Cha , S-M , Kim , D-J , Lee , Y , Maoz , D , Kaspi , S , Street , R A , Tsapras , Y , Bachelet , E , Dominik , M , Bramich , D M , Horne , K D , Snodgrass , C , Steele , I A , Menzies , J , Figuera Jaimes , R J , Wambsganss , J , Schmidt , R , Cassan , A , Ranc , C , Mao , S , Dong , S , D’Ago , G , Scarpetta , G , Verma , P , Jørgensen , U G , Kerins , E & Skottfelt , J 2015 , ' Spitzer microlens measurement of a massive remnant in a well-separated binary ' , Astrophysical Journal , vol. 814 , no. 2 , pp. 111 . https://doi.org/10.1088/0004-637X/814/2/111en
dc.identifier.issn0004-637X
dc.identifier.otherBibCode: 2015ApJ...814..111S
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996675
dc.identifier.urihttps://hdl.handle.net/10023/7968
dc.descriptionWork by Y.S. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. L.W. acknowledges support from the Polish NCN Harmonia grant No. 2012/06/M/ST9/00172. D.M. and A.G. acknowledge support by a grant from the US Israel Binational Science Foundation. Work by D.M. is supported by the I-CORE program of the Israel Science Foundation and the Planning and Budgeting Committee. This publication was made possible by NPRP grant # X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). S.D. is supported by "the Strategic Priority Research Program—The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (grant No. XDB09000000). Work by S.M. has been supported by the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences Grant No. XDB09000000, and by the National Natural Science Foundation of China (NSFC) under grant numbers 11333003 and 11390372. M.P.G.H. acknowledges support from the Villum Foundation.en
dc.description.abstractWe report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La,b, with the more massive component having M1 > 1.35 M⊙ (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r⊥ = 6.1 ± 0.4 AU and lies in the Galactic bulge. These measurements are based on the “microlens parallax” effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.
dc.format.extent801403
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.subjectBinaries: generalen
dc.subjectBlack hole physicsen
dc.subjectGalaxy: bulgeen
dc.subjectGravitational lensing: microen
dc.subjectStars: neutronen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSpitzer microlens measurement of a massive remnant in a well-separated binaryen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doi10.1088/0004-637X/814/2/111
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2015ApJ...814..111Sen
dc.identifier.grantnumberST/M001296/1en
dc.identifier.grantnumberST/J001651/1en


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