Issue |
A&A
Volume 655, November 2021
|
|
---|---|---|
Article Number | A21 | |
Number of page(s) | 10 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/202141517 | |
Published online | 04 November 2021 |
Three faint-source microlensing planets detected via the resonant-caustic channel
1
Department of Physics, Chungbuk National University,
Cheongju
28644,
Republic of Korea
e-mail: cheongho@astroph.chungbuk.ac.kr
2
Astronomical Observatory, University of Warsaw,
Al. Ujazdowskie 4,
00-478
Warszawa,
Poland
3
Korea Astronomy and Space Science Institute,
Daejon
34055,
Republic of Korea
4
Dipartimento di Fisica “E. R. Caianiello”, Università di Salerno,
Via Giovanni Paolo II,
84084
Fisciano (SA),
Italy
5
Istituto Nazionale di Fisica Nucleare, Sezione di Napoli,
Via Cintia,
80126
Napoli,
Italy
6
University of Canterbury, Department of Physics and Astronomy,
Private Bag 4800,
Christchurch
8020,
New Zealand
7
Korea University of Science and Technology,
217 Gajeong-ro,
Yuseong-gu,
Daejeon
34113,
Republic of Korea
8
Max Planck Institute for Astronomy,
Königstuhl 17,
69117
Heidelberg,
Germany
9
Department of Astronomy, The Ohio State University,
140 W. 18th Ave.,
Columbus,
OH
43210,
USA
10
Department of Particle Physics and Astrophysics, Weizmann Institute of Science,
Rehovot
76100,
Israel
11
Center for Astrophysics, Harvard & Smithsonian 60 Garden St.,
Cambridge,
MA
02138,
USA
12
Department of Astronomy, Tsinghua University,
Beijing
100084,
PR China
13
School of Space Research, Kyung Hee University,
Yongin,
Kyeonggi
17104,
Republic of Korea
14
Division of Physics, Mathematics, and Astronomy, California Institute of Technology,
Pasadena,
CA
91125,
USA
15
Department of Physics, University of Warwick,
Gibbet Hill Road,
Coventry,
CV4 7AL,
UK
Received:
11
June
2021
Accepted:
14
September
2021
Aims. We conducted a project of reinvestigating the 2017–2019 microlensing data collected by high-cadence surveys with the aim of finding planets that were missed due to the deviations of planetary signals from the typical form of short-term anomalies.
Methods. The project led us to find three planets, KMT-2017-BLG-2509Lb, OGLE-2017-BLG-1099Lb, and OGLE-2019-BLG-0299Lb. The lensing light curves of the events have a common characteristic: the planetary signals were produced by the crossings of faint source stars over the resonant caustics formed by giant planets located near the Einstein rings of host stars.
Results. For all planetary events, the lensing solutions are uniquely determined without any degeneracy. It is estimated that the host masses are in the range of 0.45 ≲ M∕M⊙≲ 0.59, which corresponds to early M to late K dwarfs, and thus the host stars are less massive than the Sun. On the other hand, the planets, with masses in the range of 2.1 ≲ M∕MJ ≲ 6.2, are heavier than the heaviest planet of the Solar System, that is, Jupiter. The planets in all systems lie beyond the snow lines of the hosts, and thus the discovered planetary systems, together with many other microlensing planetary systems, support the idea that massive gas-giant planets are commonplace around low-mass stars. We discuss the role of late-time high-resolution imaging in clarifying resonant-image lenses with very faint sources.
Key words: gravitational lensing: micro / planets and satellites: detection
© ESO 2021
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