M. Bos
Texas A&M University
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Publication
Featured researches published by M. Bos.
The Astrophysical Journal | 2012
J. C. Yee; Y. Shvartzvald; Avishay Gal-Yam; I. A. Bond; A. Udalski; S. Kozłowski; C. Han; A. Gould; J. Skowron; D. Suzuki; F. Abe; D. P. Bennett; C. S. Botzler; P. Chote; M. Freeman; A. Fukui; K. Furusawa; Y. Itow; S. Kobara; C. H. Ling; K. Masuda; Y. Matsubara; N. Miyake; Y. Muraki; K. Ohmori; K. Ohnishi; N. J. Rattenbury; To. Saito; D. J. Sullivan; T. Sumi
Mathematical and Physical Sciences: 1st Place (The Ohio State University Edward F. Hayes Graduate Research Forum)
The Astrophysical Journal | 2009
J. C. Yee; A. Udalski; T. Sumi; Subo Dong; S. Kozłowski; Jonathan C. Bird; Andrew A. Cole; D. Higgins; J. McCormick; L. A. G. Monard; David Polishook; Avi Shporer; Oded Spector; M. K. Szymański; M. Kubiak; G. Pietrzyński; I. Soszyński; O. Szewczyk; K. Ulaczyk; Ł. Wyrzykowski; R. Poleski; W. Allen; M. Bos; G. W. Christie; D. L. DePoy; Jason D. Eastman; B. S. Gaudi; A. Gould; Cheongho Han; Shai Kaspi
We analyze the extreme high-magnification microlensing event OGLE-2008-BLG-279, which peaked at a maximum magnification of A ~ 1600 on 2008 May 30. The peak of this event exhibits both finite-source effects and terrestrial parallax, from which we determine the mass of the lens, Ml = 0.64 ? 0.10 M ?, and its distance, Dl = 4.0 ? 0.6 kpc. We rule out Jupiter-mass planetary companions to the lens star for projected separations in the range 0.5-20 AU. More generally, we find that this event was sensitive to planets with masses as small as with projected separations near the Einstein ring (~3 AU).
The Astrophysical Journal | 2014
C. B. Henderson; H. Park; T. Sumi; A. Udalski; Andrew Gould; Y. Tsapras; C. Han; B. S. Gaudi; V. Bozza; F. Abe; D. P. Bennett; I. A. Bond; C. S. Botzler; M. Freeman; A. Fukui; D. Fukunaga; Y. Itow; N. Koshimoto; C. H. Ling; K. Masuda; Y. Matsubara; Y. Muraki; S. Namba; K. Ohnishi; N. J. Rattenbury; To. Saito; D. J. Sullivan; D. Suzuki; W. L. Sweatman; P. J. Tristram
The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lenssource proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved.
