@Article{YeeSGBUKHGSSABBCFFFIKLMMMMOORSSSSSTTWSKPSPUWPAABBCDDDFGGHHJKMMMMMMMNNOPSTTSCPLK:2012:TePuSu,
               author = "Yee, J. C. and Shvartzvald, Y. and Gal-Yam, A. and Bond, I. A. and 
                         Udalski, A. and Koz owski, S. and Han, C. and Gould, A. and 
                         Skowron, J. and Suzuki, D. and Abe, F. and Bennett, D. P. and 
                         Botzler, C. S. and Chote, P. and Freeman, M. and Fukui, A. and 
                         Furusawa, K. and Itow, Y. and Kobara, S. and Ling, C. H. and 
                         Masuda, K. and Matsubara, Y. and Miyake, N. and Muraki, Y. and 
                         Ohmori, K. and Ohnishi, K. and Rattenbury, N. J. and Saito, To. 
                         and Sullivan, D. J. and Sumi, T. and Suzuki, K. and Sweatman, W. 
                         L. and Takino, S. and Tristram, P. J. and Wada, K. and Szyma ski, 
                         M. K. and Kubiak, M. and Pietrzy ski, G. and Soszy ski, I. and 
                         Poleski, R. and Ulaczyk, K. and Wyrzykowski, . and Pietrukowicz, 
                         P. and Allen, W. and Almeida, Leonardo Andrade de and Batista, V. 
                         and Bos, M. and Christie, G. and Depoy, D. L. and Dong, Subo and 
                         Drummond, J. and Finkelman, I. and Gaudi, B. S. and Gorbikov, E. 
                         and Henderson, C. and Higgins, D. and Jablonski, Francisco and 
                         Kaspi, S. and Manulis, I. and Maoz, D. and McCormick, J. and 
                         McGregor, D. and Monard, L. A. G. and Moorhouse, D. and Muņoz, J. 
                         A. and Natusch, T. and Ngan, H. and Ofek, E. and Pogge, R. W. and 
                         Santallo, R. and Tan, T. -G. and Thornley, G. and Shin, I. -G. and 
                         Choi, J. -Y. and Park, S. -Y. and Lee, C. -U. and Koo, J. -R.",
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                         {} and {} and {} and {} and {} and {} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)} and {} and {} and {} and {} and {} and 
                         {} and {} and {} and {} and {} and {} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)}",
                title = "MOA-2011-BLG-293Lb: A test of pure survey microlensing planet 
                         detections",
              journal = "Astrophysical Journal",
                 year = "2012",
               volume = "755",
               number = "2",
                pages = "102 (14 pp)",
                month = "Aug.",
             keywords = "gravitational microlensing, detection, individual 
                         (MOA-2011-BLG-293Lb) Jovian-Mass planet, galactic bulge, event 
                         MOA-2007-BLG-192, dwarf stars, photometry, systems, lens, 
                         companions, frequency, jupiter.",
             abstract = "Because of the development of large-format, wide-field cameras, 
                         microlensing surveys are now able to monitor millions of stars 
                         with sufficient cadence to detect planets. These new discoveries 
                         will span the full range of significance levels including 
                         planetary signals too small to be distinguished from the noise. At 
                         present, we do not understand where the threshold is for detecting 
                         planets. MOA-2011-BLG-293Lb is the first planet to be published 
                         from the new surveys, and it also has substantial follow-up 
                         observations. This planet is robustly detected in survey+follow-up 
                         data (Delta chi(2) similar to 5400). The planet/host mass ratio is 
                         q = (5.3 similar to 0.2) x 10(-3). The best-fit projected 
                         separation is s = 0.548 +/- 0.005 Einstein radii. However, due to 
                         the s <-> s(-1) degeneracy, projected separations of s-1 are only 
                         marginally disfavored at Delta chi(2) = 3. A Bayesian estimate of 
                         the host mass gives M-L = 0.43(-0.17)(+0.27) M-circle dot, with a 
                         sharp upper limit of M-L < 1.2 M-circle dot from upper limits on 
                         the lens flux. Hence, the planet mass is m(p) = 2.4(-0.9)(+1.5) 
                         M-Jup, and the physical projected separation is either 
                         r(perpendicular to) similar or equal to 1.0 AU or r(perpendicular 
                         to) similar or equal to 3.4 AU. We show that survey data alone 
                         predict this solution and are able to characterize the planet, but 
                         the Delta chi(2) is much smaller (Delta chi(2) similar to 500) 
                         than with the follow-up data. The Delta chi(2) for the survey data 
                         alone is smaller than for any other securely detected planet. This 
                         event suggests a means to probe the detection threshold, by 
                         analyzing a large sample of events like MOA-2011-BLG-293, which 
                         have both follow-up data and high-cadence survey data, to provide 
                         a guide for the interpretation of pure survey microlensing data.",
                  doi = "10.1088/0004-637X/755/2/102",
                  url = "http://dx.doi.org/10.1088/0004-637X/755/2/102",
                 issn = "0004-637X and 1538-4357",
                label = "lattes: 7812463045514059 45 
                         
                         YeeSGBUKHGSSABBCFFFIKLMMMMOORSSSSSTTWSKPSPUWPAABBCDDDFGGHHJKMMMMMMMNNOPSTTSCPLK:2012:TEPUSU",
             language = "en",
           targetfile = "0004-637X_755_2_102.pdf",
        urlaccessdate = "30 abr. 2024"
}