Three microlensing planets with no caustic-crossing features

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dc.contributor.authorHan C
dc.contributor.authorUdalski A
dc.contributor.authorKim D
dc.contributor.authorLee C-U
dc.contributor.authorChung S-J
dc.contributor.authorGould A
dc.contributor.authorHwang K-H
dc.contributor.authorJung YK
dc.contributor.authorRyu Y-H
dc.contributor.authorShin I-G
dc.contributor.authorShvartzvald Y
dc.contributor.authorYee JC
dc.contributor.authorZang W
dc.contributor.authorCha S-M
dc.contributor.authorKim D-J
dc.contributor.authorKim H-W
dc.contributor.authorKim S-L
dc.contributor.authorLee D-J
dc.contributor.authorLee Y
dc.contributor.authorPark B-G
dc.contributor.authorPogge RW
dc.contributor.authorMróz P
dc.contributor.authorSzymański MK
dc.contributor.authorSkowron J
dc.contributor.authorPoleski R
dc.contributor.authorSoszyński I
dc.contributor.authorPietrukowicz P
dc.contributor.authorKozłowski S
dc.contributor.authorUlaczyk K
dc.contributor.authorRybicki KA
dc.contributor.authorIwanek P
dc.contributor.authorWrona M
dc.contributor.authorGromadzki M
dc.contributor.authorAlbrow, Michael
dc.date.accessioned2021-11-02T04:41:32Z
dc.date.available2021-11-02T04:41:32Z
dc.date.issued2021en
dc.date.updated2021-06-17T03:01:42Z
dc.description.abstractWe search for microlensing planets with signals exhibiting no caustic-crossing features, considering the possibility that such signals may be missed due to their weak and featureless nature. For this purpose, we reexamine the lensing events found by the KMTNet survey before the 2019 season. From this investigation, we find two new planetary lensing events, KMT-2018-BLG-1976 and KMT-2018-BLG-1996. We also present the analysis of the planetary event OGLE-2019-BLG-0954, for which the planetary signal was known, but no detailed analysis has been presented before. We identify the genuineness of the planetary signals by checking various interpretations that can generate short-term anomalies in lensing light curves. From Bayesian analyses conducted with the constraint from available observables, we find that the host and planet masses are $(M_1, M_2)\sim (0.65~M_\odot, 2~M_{\rm J})$ for KMT-2018-BLG-1976L, $\sim (0.69~M_\odot, 1~M_{\rm J})$ for KMT-2018-BLG-1996L, and $\sim (0.80~M_\odot, 14~M_{\rm J})$ for OGLE-2019-BLG-0954L. The estimated distance to OGLE-2019-BLG-0954L, $3.63^{+1.22}_{-1.64}$~kpc, indicates that it is located in the disk, and the brightness expected from the mass and distance matches well the brightness of the blend, indicating that the lens accounts for most of the blended flux. The lens of OGLE-2019-BLG-0954 could be resolved from the source by conducting high-resolution follow-up observations in and after 2024.en
dc.identifier.citationHan C, Udalski A, Kim D, Lee C-U, Albrow MD, Chung S-J, Gould A, Hwang K-H, Jung YK, Ryu Y-H, Shin I-G, Shvartzvald Y, Yee JC, Zang W, Cha S-M, Kim D-J, Kim H-W, Kim S-L, Lee D-J, Lee Y, Park B-G, Pogge RW, Mróz P, Szymański MK, Skowron J, Poleski R, Soszyński I, Pietrukowicz P, Kozłowski S, Ulaczyk K, Rybicki KA, Iwanek P, Wrona M, Gromadzki M. Three microlensing planets with no caustic-crossing features. (April 15, 2021) Astronomy & Astrophysics.en
dc.identifier.urihttps://hdl.handle.net/10092/102826
dc.language.isoen
dc.rightsAll rights reserved unless otherwise stateden
dc.rights.urihttp://hdl.handle.net/10092/17651en
dc.subjectastro-ph.EPen
dc.subjectastro-ph.GAen
dc.subjectgravitational microlensing – planets and satellites: detectionen
dc.subject.anzsrcFields of Research::51 - Physical sciences::5101 - Astronomical sciences::510109 - Stellar astronomy and planetary systemsen
dc.subject.anzsrcFields of Research::51 - Physical sciences::5101 - Astronomical sciences::510107 - Planetary science (excl. solar system and planetary geology)en
dc.titleThree microlensing planets with no caustic-crossing featuresen
dc.typeJournal Articleen
uc.collegeFaculty of Science
uc.departmentSchool of Physical & Chemical Sciences
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