MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Author:
Olmschenk GregORCID, Bennett David P.ORCID, Bond Ian A., Zang WeichengORCID, Jung Youn KilORCID, Yee Jennifer C.ORCID, Bachelet EtienneORCID, Abe Fumio, Barry Richard K.ORCID, Bhattacharya Aparna, Fujii Hirosane, Fukui AkihikoORCID, Hirao YukiORCID, Silva Stela IshitaniORCID, Itow YoshitakaORCID, Kirikawa Rintaro, Kondo IonaORCID, Koshimoto NaokiORCID, Matsubara YutakaORCID, Matsumoto Sho, Miyazaki ShotaORCID, Munford Brandon, Muraki YasushiORCID, Okamura Arisa, Ranc ClémentORCID, Rattenbury Nicholas J.ORCID, Satoh YukiORCID, Sumi TakahiroORCID, Suzuki DaisukeORCID, Toda Taiga, Tristram Paul J., Vandorou AikateriniORCID, Yama Hibiki, Albrow Michael D.ORCID, Cha Sang-Mok, Chung Sun-JuORCID, Gould Andrew, Han CheonghoORCID, Hwang Kyu-HaORCID, Kim Dong-Jin, Kim Hyoun-WooORCID, Kim Seung-LeeORCID, Lee Chung-UkORCID, Lee Dong-Joo, Lee Yongseok, Park Byeong-GonORCID, Pogge Richard W.ORCID, Ryu Yoon-HyunORCID, Shin In-GuORCID, Shvartzvald YossiORCID, Christie Grant, Cooper Tony, Drummond John, Green Jonathan, Hennerley Steve, McCormick Jennie, Monard L. A. G., Natusch Tim, Porritt Ian, Tan Thiam-GuanORCID, Mao ShudeORCID, Maoz DanORCID, Penny Matthew T.ORCID, Zhu WeiORCID, Bozza V.ORCID, Cassan Arnaud, Dominik MartinORCID, Hundertmark Markus, Jaimes R. Figuera, Kruszyńska K., Rybicki K. A., Street R. A.ORCID, Tsapras Y., Wambsganss JoachimORCID, Wyrzykowski Ł., Zieliński P., Rau GioiaORCID, , , , , ,
Abstract
Abstract
We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio
q
=
3.17
−
0.26
+
0.28
×
10
−
4
, the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass
m
planet
=
46
−
24
+
42
M
⊕
and a host star of mass
M
host
=
0.43
−
0.23
+
0.39
M
⊙
, located at a distance
D
L
=
7.49
−
1.13
+
0.99
kpc
. For the second scenario, we estimate
m
planet
=
69
−
34
+
37
M
⊕
,
M
host
=
0.66
−
0.32
+
0.35
M
⊙
, and
D
L
=
7.81
−
0.93
+
0.93
kpc
. The planet has a projected separation as a fraction of the Einstein ring radius
s
=
1.3807
−
0.0018
+
0.0018
. As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models.
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
3 articles.
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