Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742688.0, MPI für Astronomie / Publikationen_mpia
OGLE-2016-BLG-0613LABb: A microlensing planet in a binary system
Authors:Han, C.; Udalski, A.; Gould, A.; Lee, C. -. U.; Shvartzvald, Y.; Zang, W. C.; Mao, S.; Kozłowski, S.; Albrow, M. D.; Chung, S. -. J.; Hwang, K. -. H.; Jung, Y. K.; Kim, D.; Kim, H. -. W.; Ryu, Y. -. H.; Shin, I. -. G.; Yee, J. C.; Zhu, W.; Cha, S. -. M.; Kim, S. -. L.; Kim, D. -. J.; Lee, Y.; Park, B. -. G.; Skowron, J.; Mróz, P.; Pietrukowicz, P.; Poleski, R.; Szymański, M. K.; Soszyński, I.; Ulaczyk, K.; Pawlak, M.; Beichman, C.; Bryden, G.; Calchi Novati, S.; Gaudi, B. S.; Henderson, C. B.; Howell, S. B.; Jacklin, S.; Penny, M. T.; Fouqué, P.; Wang, T. S.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:The Astronomical Journal
Volume:154
Start Page:id. 223 (14 pp)
Audience:Not Specified
Abstract / Description:We present the analysis of OGLE-2016-BLG-0613, for which the lensing light curve appears to be that of a typical binary-lens event with two caustic spikes but with a discontinuous feature on the trough between the spikes. We find that the discontinuous feature was produced by a planetary companion to the binary lens. We find four degenerate triple-lens solution classes, each composed of a pair of solutions according to the well-known wide/close planetary degeneracy. One of these solution classes is excluded due to its relatively poor fit. For the remaining three pairs of solutions, the most-likely primary mass is about {M}1∼ 0.7 {M}ȯ , while the planet is a super Jupiter. In all cases, the system lies in the Galactic disk, about halfway toward the Galactic bulge. However, in one of these three solution classes, the secondary of the binary system is a low-mass brown dwarf, with relative mass ratios (1:0.03:0.003), while in the two others the masses of the binary components are comparable. These two possibilities can be distinguished in about 2024 when the measured lens-source relative proper motion will permit separate resolution of the lens and source.
Free Keywords:binaries: general; gravitational lensing: micro; planetary systems
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-6256
URL:http://adsabs.harvard.edu/abs/2017AJ....154..223H
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.