%0 Journal Article
%4 dpi.inpe.br/plutao/2012/11.28.18.48.43
%2 dpi.inpe.br/plutao/2012/11.28.18.48.44
%@doi 10.1088/0004-637X/755/2/91
%@issn 0004-637X
%@issn 1538-4357
%F lattes: 7812463045514059 86 ShinHCUSGBDFHSKSPPUPKSWABBBCFFFIKLMMMMOORSSSSSTTWYBSSSTABBNDDFGGHHHHHJJKKLLLMMPRRSSSSTWWABCDDGHJLMMMNNPPTTYABBBCCCCDPDGKMMSZ:2012:CHLOBI
%T Characterizing low-mass binaries from observation of long-timescale caustic-crossing gravitational microlensing events
%D 2012
%8 Aug.
%A Shin, I. -G.,
%A Han, C.,
%A Choi, J. -Y.,
%A Udalski, A.,
%A Sumi, T.,
%A Gould, A.,
%A Bozza, V.,
%A Dominik, M.,
%A Fouqué, P.,
%A Horne, K.,
%A Szyma ski, M. K.,
%A Kubiak, M.,
%A Soszy ski, I.,
%A Pietrzy ski, G.,
%A Poleski, R.,
%A Ulaczyk, K.,
%A Pietrukowicz, P.,
%A Koz owski, S.,
%A Skowron, J.,
%A Wyrzykowski, .,
%A Abe, F.,
%A Bennett, D. P.,
%A Bond, I. A.,
%A Botzler, C. S.,
%A Chote, P.,
%A Freeman, M.,
%A Fukui, A.,
%A Furusawa, K.,
%A Itow, Y.,
%A Kobara, S.,
%A Ling, C. H.,
%A Masuda, K.,
%A Matsubara, Y.,
%A Miyake, N.,
%A Muraki, Y.,
%A Ohmori, K.,
%A Ohnishi, K.,
%A Rattenbury, N. J.,
%A Saito, To.,
%A Sullivan, D. J.,
%A Suzuki, D.,
%A Suzuki, K.,
%A Sweatman, W. L.,
%A Takino, S.,
%A Tristram, P. J.,
%A Wada, K.,
%A Yock, P. C. M.,
%A Bramich, D. M.,
%A Snodgrass, C.,
%A Steele, I. A.,
%A Street, R. A.,
%A Tsapras, Y.,
%A Alsubai, K. A.,
%A Browne, P.,
%A Burgdorf, M. J.,
%A Novati, S. Calchi,
%A Dodds, P.,
%A Dreizler, S.,
%A Fang, X. -S.,
%A Grundahl, F.,
%A Gu, C. -H.,
%A Hardis, S.,
%A Harps e, K.,
%A Hinse, T. C.,
%A Hornstrup, A.,
%A Hundertmark, M.,
%A Jessen-Hansen, J.,
%A J rgensen, U. G.,
%A Kains, N.,
%A Kerins, E.,
%A Liebig, C.,
%A Lund, M.,
%A Lunkkvist, M.,
%A Mancini, L.,
%A Mathiasen, M.,
%A Penny, M. T.,
%A Rahvar, S.,
%A Ricci, D.,
%A Scarpetta, G.,
%A Skottfelt, J.,
%A Southworth, J.,
%A Surdej, J.,
%A Tregloan-Reed, J.,
%A Wambsganss, J.,
%A Wertz, O.,
%A Almeida, Leonardo Andrade de,
%A Batista, V.,
%A Christie, G.,
%A Depoy, D. L.,
%A Dong, Subo,
%A Gaudi, B. S.,
%A Henderson, C.,
%A Jablonski, Francisco,
%A Lee, C. -U.,
%A McCormick, J.,
%A McGregor, D.,
%A Moorhouse, D.,
%A Natusch, T.,
%A Ngan, H.,
%A Park, S. -Y.,
%A Pogge, R. W.,
%A Tan, T. -G.,
%A Thornley, G.,
%A Yee, J. C.,
%A Albrow, M. D.,
%A Bachelet, E.,
%A Beaulieu, J. -P.,
%A Brillant, S.,
%A Cassan, A.,
%A Cole, A. A.,
%A Corrales, E.,
%A Coutures, C.,
%A Dieters, S.,
%A Prester, D. Dominis,
%A Donatowicz, J.,
%A Greenhill, J.,
%A Kubas, D.,
%A Marquette, J. -B.,
%A Menzies, J. W.,
%A Sahu, K. C.,
%A Zub,
%A ,
%A M.,
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%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
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%@electronicmailaddress leonardo@das.inpe.br
%B Astrophysical Journal
%V 755
%N 2
%P 91 (10pp)
%K gravitational microlensing, binaries.
%X Despite the astrophysical importance of binary star systems, detections are limited to those located in small ranges of separations, distances, and masses and thus it is necessary to use a variety of observational techniques for a complete view of stellar multiplicity across a broad range of physical parameters. In this paper, we report the detections and measurements of two binaries discovered from observations of microlensing events MOA-2011-BLG-090 and OGLE-2011-BLG-0417. Determinations of the binary masses are possible by simultaneously measuring the Einstein radius and the lens parallax. The measured masses of the binary components are 0.43M and 0.39M for MOA-2011-BLG-090 and 0.57M and 0.17M for OGLE-2011-BLG-0417 and thus both lens components of MOA-2011-BLG-090 and one component of OGLE-2011-BLG-0417 are M dwarfs, demonstrating the usefulness of microlensing in detecting binaries composed of low-mass components. From modeling of the light curves considering full Keplerian motion of the lens, we also measure the orbital parameters of the binaries. The blended light of OGLE-2011-BLG-0417 comes very likely from the lens itself, making it possible to check the microlensing orbital solution by follow-up radial-velocity observation. For both events, the caustic-crossing parts of the light curves, which are critical for determining the physical lens parameters, were resolved by high-cadence survey observations and thus it is expected that the number of microlensing binaries with measured physical parameters will increase in the future.
%@language pt
%3 0004-637X_755_2_91.pdf