| Title | CANDIDAIE GRAVITATIONAL MICROLENSING EVENTS FOR FUTURE DIRECT LENS IMAGING |
| Authors | Henderson, C. B. Park, H. Sumi, T. Udalski, A. Gould, A. Tsapras, Y. Han, C. Gaudi, B. S. Bozza, V. Abe, F. Bennett, D. P. Bond, I. A. Botzler, C. S. Freeman, M. Fukui, A. Fukunaga, D. Itow, Y. Koshimoto, N. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Rattenbury, N. J. Saito, To Sullivan, D. J. Suzuki, D. Sweatman, W. L. Tristram, P. J. Tsurumi, N. Wada, K. Yamai, N. Yock, P. C. M. Yonehara, A. Szymanski, M. K. Kubiak, M. Pietrzynski, G. Soszynski, I. Skowron, J. Kozlowski, S. Pole |
| Affiliation | Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. Univ London, Sch Math Sci, London E1 4NS, England. Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy. Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Auckland 0745, New Zealand. Univ Auckland, Dept Phys, Auckland 1001, New Zealand. Victoria Univ, Sch Chem & Phys Sci, Wellington 6140, New Zealand. Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan. Nagano Natl Coll Technol, Nagano 3818550, Japan. Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. Mt John Univ Observ, Lake Tekapo 8770, New Zealand. Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. Univ Concepcion, Dept Astron, Concepcion, Chile. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Inst Astron Geofis & Ciecias Atmosfer IAG USP, Sao Paulo, Brazil. Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, SP, Brazil. Molehill Astron Observ, North Shore, New Zealand. Auckland Observ, Auckland, New Zealand. Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Obsev Pico dos Dias, Brazopolis, MG, Brazil. Korea Astron & Space Sci Inst, Taejon 305348, South Korea. Farm Cove Observ, Ctr Backyard Astrophys, Auckland, New Zealand. Kumeu Observ, Kumeu, New Zealand. AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand. Perth Exoplanet Survey Telescope, Perth, WA, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. European So Observ, D-85748 Garching, Germany. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Liverpool John Moores Univ, Astrophys Res Inst, Wirral CH41 1LD, Merseyside, England. |
| Keywords | binaries: general gravitational lensing: micro GALACTIC BULGE BINARY-LENS CHEMICAL EVOLUTION PLANETARY COMPANION ORBITAL MOTION OPTICAL DEPTH MASS PLANET BROWN DWARF OGLE-III PARALLAX |
| Issue Date | 2014 |
| Publisher | astrophysical journal |
| Citation | ASTROPHYSICAL JOURNAL.2014,794,(1). |
| Abstract | 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. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. We provide a list of microlensing events toward the Galactic bulge with high relative lens-source proper motion that are therefore good candidates for constraining the lens mass with future high-resolution imaging. We investigate all events from 2004 to 2013 that display detectable finite-source effects, a feature that allows us to measure the proper motion. In total, we present 20 events with mu >= 8 mas yr(-1). Of these, 14 were culled from previous analyses while 6 are new, including OGLE-2004-BLG-368, MOA-2005-BLG-36, OGLE-2012-BLG-0211, OGLE-2012-BLG-0456, MOA-2012-BLG-532, and MOA-2013-BLG-029. In <= 12 yr from the time of each event the lens and source of each event will be sufficiently separated for ground-based telescopes with AO systems or space telescopes to resolve each component and further characterize the lens system. Furthermore, for the most recent events, comparison of the lens flux estimates from images taken immediately to those estimated from images taken when the lens and source are resolved can be used to empirically check the robustness of the single-epoch method currently being used to estimate lens masses for many events. |
| URI | http://hdl.handle.net/20.500.11897/208052 |
| ISSN | 0004-637X |
| DOI | 10.1088/0004-637X/794/1/71 |
| Indexed | SCI(E) |
| Appears in Collections: | 科维理天文与天体物理研究所 |
