Files in this item
Discovery of a gas giant planet in microlensing event OGLE-2014-BLG-1760
Item metadata
dc.contributor.author | Bhattacharya, A. | |
dc.contributor.author | Bennett, D. P. | |
dc.contributor.author | Bond, I. A. | |
dc.contributor.author | Sumi, T. | |
dc.contributor.author | Udalski, A. | |
dc.contributor.author | Street, R. | |
dc.contributor.author | Tsapras, Y. | |
dc.contributor.author | Abe, F. | |
dc.contributor.author | Freeman, M. | |
dc.contributor.author | Fukui, A. | |
dc.contributor.author | Hirao, Y. | |
dc.contributor.author | Itow, Y. | |
dc.contributor.author | Koshimoto, N. | |
dc.contributor.author | Li, M. C. A. | |
dc.contributor.author | Ling, C. H. | |
dc.contributor.author | Masuda, K. | |
dc.contributor.author | Matsubara, Y. | |
dc.contributor.author | Muraki, Y. | |
dc.contributor.author | Nagakane, M. | |
dc.contributor.author | Ohnishi, K. | |
dc.contributor.author | Rattenbury, N. | |
dc.contributor.author | Saito, T. | |
dc.contributor.author | Sharan, A. | |
dc.contributor.author | Sullivan, D. J. | |
dc.contributor.author | Suzuki, D. | |
dc.contributor.author | Tristram, P. J. | |
dc.contributor.author | Skowron, J. | |
dc.contributor.author | Szymański, M. K. | |
dc.contributor.author | Soszyński, I. | |
dc.contributor.author | Poleski, R. | |
dc.contributor.author | Mróz, P. | |
dc.contributor.author | Kozlowski, S. | |
dc.contributor.author | Pietrukowicz, P. | |
dc.contributor.author | Ulaczyk, K. | |
dc.contributor.author | Wyrzykowski, L. | |
dc.contributor.author | Bachelet, E. | |
dc.contributor.author | Bramich, D. M. | |
dc.contributor.author | D’Ago, G. | |
dc.contributor.author | Dominik, M. | |
dc.contributor.author | Figuera Jaimes, R. | |
dc.contributor.author | Horne, K. | |
dc.contributor.author | Hundertmark, M. | |
dc.contributor.author | Kains, N. | |
dc.contributor.author | Menzies, J. | |
dc.contributor.author | Schmidt, R. | |
dc.contributor.author | Snodgrass, C. | |
dc.contributor.author | Steele, I. A. | |
dc.contributor.author | Wambsganss, J. | |
dc.date.accessioned | 2016-11-15T13:30:17Z | |
dc.date.available | 2016-11-15T13:30:17Z | |
dc.date.issued | 2016-11 | |
dc.identifier.citation | Bhattacharya , A , Bennett , D P , Bond , I A , Sumi , T , Udalski , A , Street , R , Tsapras , Y , Abe , F , Freeman , M , Fukui , A , Hirao , Y , Itow , Y , Koshimoto , N , Li , M C A , Ling , C H , Masuda , K , Matsubara , Y , Muraki , Y , Nagakane , M , Ohnishi , K , Rattenbury , N , Saito , T , Sharan , A , Sullivan , D J , Suzuki , D , Tristram , P J , Skowron , J , Szymański , M K , Soszyński , I , Poleski , R , Mróz , P , Kozlowski , S , Pietrukowicz , P , Ulaczyk , K , Wyrzykowski , L , Bachelet , E , Bramich , D M , D’Ago , G , Dominik , M , Figuera Jaimes , R , Horne , K , Hundertmark , M , Kains , N , Menzies , J , Schmidt , R , Snodgrass , C , Steele , I A & Wambsganss , J 2016 , ' Discovery of a gas giant planet in microlensing event OGLE-2014-BLG-1760 ' , Astronomical Journal , vol. 152 , no. 5 , 140 . https://doi.org/10.3847/0004-6256/152/5/140 | en |
dc.identifier.issn | 0004-6256 | |
dc.identifier.other | PURE: 247650384 | |
dc.identifier.other | PURE UUID: 9b621c9f-1ef8-4483-878f-d89e646d91dc | |
dc.identifier.other | BibCode: 2016AJ....152..140B | |
dc.identifier.other | Scopus: 84994478256 | |
dc.identifier.other | WOS: 000387255000001 | |
dc.identifier.other | ORCID: /0000-0002-3202-0343/work/75996720 | |
dc.identifier.uri | https://hdl.handle.net/10023/9823 | |
dc.description.abstract | We present the analysis of the planetary microlensing event OGLE-2014-BLG-1760, which shows a strong light-curve signal due to the presence of a Jupiter mass ratio planet. One unusual feature of this event is that the source star is quite blue, with V-I=1.48+/- 0.08. This is marginally consistent with a source star in the Galactic bulge, but it could possibly indicate a young source star on the far side of the disk. Assuming a bulge source, we perform a Bayesian analysis assuming a standard Galactic model, and this indicates that the planetary system resides in or near the Galactic bulge at DL=6.9+/- 1.1 kpc. It also indicates a host-star mass of M*=0.51-0.28/+0.44M_sun, a planet mass of mp=0.56-0.26/+0.34MJ, and a projected star–planet separation of a_perp=1.75-0.33/+0.34 au. The lens–source relative proper motion is μrel=6.5+/- 1.1 mas yr‑1. The lens (and stellar host star) is estimated to be very faint compared to the source star, so it is most likely that it can be detected only when the lens and source stars start to separate. Due to the relatively high relative proper motion, the lens and source will be resolved to about ∼46 mas in 6–8 yr after the peak magnification. So, by 2020–2022, we can hope to detect the lens star with deep, high-resolution images. | |
dc.format.extent | 11 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomical Journal | en |
dc.rights | © 2016, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at iopscience.iop.org / http://dx.doi.org/10.3847/0004-6256/152/5/140 | en |
dc.subject | Gravitational lensing: micro | en |
dc.subject | Planetary systems | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | NDAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Discovery of a gas giant planet in microlensing event OGLE-2014-BLG-1760 | en |
dc.type | Journal article | en |
dc.description.version | Publisher PDF | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | https://doi.org/10.3847/0004-6256/152/5/140 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://arxiv.org/abs/1603.05677 | en |
dc.identifier.url | http://adsabs.harvard.edu/abs/2016AJ....152..140B | en |
This item appears in the following Collection(s)
Items in the St Andrews Research Repository are protected by copyright, with all rights reserved, unless otherwise indicated.