Copy the page URI to the clipboard
Tsapras, Y.; Choi, J.-Y.; Street, R. A.; Han, C.; Bozza, V.; Gould, A.; Dominik, M.; Beaulieu, J.-P.; Udalski, A.; Jørgensen, U. G.; Sumi, T.; Bramich, D. M.; Browne, P.; Horne, K.; Hundertmark, M.; Ipatov, S.; Kains, N.; Snodgrass, C.; Steele, I. A.; Alsubai, K. A.; Andersen, J. M.; Calchi Novati, S.; Damerdji, Y.; Diehl, C.; Elyiv, A.; Giannini, E.; Hardis, S.; Harpsøe, K.; Hinse, T. C.; Juncher, D.; Kerins, E.; Korhonen, H.; Liebig, C.; Mancini, L.; Mathiasen, M.; Penny, M. T.; Rabus, M.; Rahvar, S.; Scarpetta, G.; Skottfelt, J.; Southworth, J.; Surdej, J.; Tregloan-Reed, J.; Vilela, C.; Wambsganss, J.; Skowron, J.; Poleski, R.; Kozłowski, S.; Wyrzykowski, Ł.; Szymański, M. K.; Kubiak, M.; Pietrukowicz, P.; Pietrzyński, G.; Soszyński, I.; Ulaczyk, K.; Albrow, M. D.; Bachelet, E.; Barry, R.; Batista, V.; Bhattacharya, A.; Brillant, S.; Caldwell, J. A. R.; Cassan, A.; Cole, A.; Corrales, E.; Coutures, Ch.; Dieters, S.; Dominis Prester, D.; Donatowicz, J.; Fouqué, P.; Greenhill, J.; Kane, S. R.; Kubas, D.; Marquette, J.-B.; Menzies, J.; Père, C.; Pollard, K. R.; Zub, M.; Christie, G.; DePoy, D. L.; Dong, S.; Drummond, J.; Gaudi, B. S.; Henderson, C. B.; Hwang, K. H.; Jung, Y. K.; Kavka, A.; Koo, J.-R.; Lee, C.-U.; Maoz, D.; Monard, L. A. G.; Natusch, T.; Ngan, H.; Park, H.; Pogge, R. W.; Porritt, I.; Shin, I.-G.; Shvartzvald, Y.; Tan, T. G.; Yee, J. C.; 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.; Sweatman, W. L.; Suzuki, D.; Tristram, P. J.; Tsurumi, N.; Wada, K.; Yamai, N.; Yock, P. C. M. and Yonehara, A.
(2014).
DOI: https://doi.org/10.1088/0004-637X/782/1/48
Abstract
We present a detailed analysis of survey and follow-up observations of microlensing event OGLE-2012-BLG-0406 based on data obtained from 10 different observatories. Intensive coverage of the light curve, especially the perturbation part, allowed us to accurately measure the parallax effect and lens orbital motion. Combining our measurement of the lens parallax with the angular Einstein radius determined from finite-source effects, we estimate the physical parameters of the lens system. We find that the event was caused by a 2.73 ± 0.43 MJ planet orbiting a 0.44 ± 0.07 M☉ early M-type star. The distance to the lens is 4.97 ± 0.29 kpc and the projected separation between the host star and its planet at the time of the event is 3.45 ± 0.26 AU. We find that the additional coverage provided by follow-up observations, especially during the planetary perturbation, leads to a more accurate determination of the physical parameters of the lens.
Viewing alternatives
Metrics
Public Attention
Altmetrics from AltmetricNumber of Citations
Citations from DimensionsItem Actions
Export
About
- Item ORO ID
- 43030
- Item Type
- Journal Item
- ISSN
- 1538-4357
- Extra Information
- 9 pp.
- Keywords
- binaries; gravitational lensing; planetary systems
- Academic Unit or School
-
Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM) - Research Group
-
Centre for Electronic Imaging (CEI)
?? space ?? - Copyright Holders
- © 2014 The American Astronomical Society
- Depositing User
- Colin Snodgrass