Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model

Nunota, Kansuke; Koshimoto, Naoki; Suzuki, Daisuke; Sumi, Takahiro; Bennett, David P.; Bhattacharya, Aparna; Hirao, Yuki; Terry, Sean K.; Vandorou, Aikaterini

doi:https://doi.org/10.3847/1538-4357/ad3cdc

Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model

Nunota, Kansuke; Koshimoto, Naoki; Suzuki, Daisuke et al.

Astrophysical Journal, 2024, 967(2), 77

アクセス数:532件（2025-07-16 09:05 集計）

固定URL: https://hdl.handle.net/11094/97229

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タイトル	Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model
著者	著者名 Nunota, Kansuke
	NRID 1000090829566 1000090829566 researchmap permalink nkoshimoto nkoshimoto 著者名 Koshimoto, Naoki
	NRID 1000060807717 1000060807717 ORCID 0000-0002-5843-9433 0000-0002-5843-9433 researchmap permalink dsuzuki0214 dsuzuki0214 Scopus Author ID 55702463200 55702463200 著者名 Suzuki, Daisuke
	NRID 1000030432214 1000030432214 researchmap permalink read0139558 read0139558 Scopus Author ID 55573890400 55573890400 著者名 Sumi, Takahiro
	著者名 Bennett, David P.
	著者名 Bhattacharya, Aparna
	著者名 Hirao, Yuki
	著者名 Terry, Sean K.
	著者名 Vandorou, Aikaterini
内容	Nunota K., Koshimoto N., Suzuki D., et al. Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model. Astrophysical Journal 967, 77 (2024); https://doi.org/10.3847/1538-4357/ad3cdc.
抄録	We measure the dependence of planet frequency on host star mass, M L, and distance from the Galactic center, R L, using a sample of planets discovered by gravitational microlensing. We compare the two-dimensional distribution of the lens-source proper motion, μ rel, and the Einstein radius crossing time, t E, measured for 22 planetary events from Suzuki et al. with the distribution expected from Galactic model. Assuming that the planet-hosting probability of a star is proportional to M L m R L r , we calculate the likelihood distribution of (m,r). We estimate that r = 0.10 − 0.37 + 0.51 and m = 0.50 − 0.70 + 0.90 under the assumption that the planet-hosting probability is independent of the mass ratio. We also divide the planet sample into subsamples based on their mass ratio, q, and estimate that m = − 0.08 − 0.65 + 0.95 for q < 10−3 and 1.25 − 1.14 + 1.07 for q > 10−3. Although uncertainties are still large, this result implies a possibility that, in orbits beyond the snowline, massive planets are more likely to exist around more massive stars whereas low-mass planets exist regardless of their host star mass.
出版者	Institute of Physics
収録物名	Astrophysical Journal
巻(号)	967(2)
ページ	77
刊行年月	2024-06-01
言語	英語
ハンドルURL	https://hdl.handle.net/11094/97229
PISSN	0004637X
eISSN	15384357
関連情報 (isIdenticalTo)	DOI (出版社版) https://doi.org/10.3847/1538-4357/ad3cdc
アクセス権	open access
権利情報	This article is licensed under a Creative Commons Attribution 4.0 International License.
出版タイプ	Version of Record
カテゴリ	学術雑誌論文 Journal Article

資源タイプ	学術雑誌論文
ローカル資源タイプ	学術雑誌論文
DCTERMS.bibliographicCitation	Astrophysical Journal. 2024, 967(2), p. 77
DC.title	Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model
DC.creator	Nunota, Kansuke
	Koshimoto, Naoki
	Suzuki, Daisuke
	Sumi, Takahiro
	Bennett, David P.
	Bhattacharya, Aparna
	Hirao, Yuki
	Terry, Sean K.
	Vandorou, Aikaterini
DC.publisher	Institute of Physics
DC.language' scheme='DCTERMS.RFC1766	英語
DCTERMS.issued' scheme='DCTERMS.W3CDTF	2024-06-01
DC.identifier	https://doi.org/10.3847/1538-4357/ad3cdc
DC.description	Nunota K., Koshimoto N., Suzuki D., et al. Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model. Astrophysical Journal 967, 77 (2024); https://doi.org/10.3847/1538-4357/ad3cdc.
DCTERMS.abstract	We measure the dependence of planet frequency on host star mass, M L, and distance from the Galactic center, R L, using a sample of planets discovered by gravitational microlensing. We compare the two-dimensional distribution of the lens-source proper motion, μ rel, and the Einstein radius crossing time, t E, measured for 22 planetary events from Suzuki et al. with the distribution expected from Galactic model. Assuming that the planet-hosting probability of a star is proportional to M L m R L r , we calculate the likelihood distribution of (m,r). We estimate that r = 0.10 − 0.37 + 0.51 and m = 0.50 − 0.70 + 0.90 under the assumption that the planet-hosting probability is independent of the mass ratio. We also divide the planet sample into subsamples based on their mass ratio, q, and estimate that m = − 0.08 − 0.65 + 0.95 for q < 10−3 and 1.25 − 1.14 + 1.07 for q > 10−3. Although uncertainties are still large, this result implies a possibility that, in orbits beyond the snowline, massive planets are more likely to exist around more massive stars whereas low-mass planets exist regardless of their host star mass.
DC.rights	This article is licensed under a Creative Commons Attribution 4.0 International License.
DC.format	97229
citation_title	Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model
citation_author	Nunota, Kansuke
	Koshimoto, Naoki
	Suzuki, Daisuke
	Sumi, Takahiro
	Bennett, David P.
	Bhattacharya, Aparna
	Hirao, Yuki
	Terry, Sean K.
	Vandorou, Aikaterini
citation_publisher	Institute of Physics
citation_language	英語
citation_date	2024-06-01
citation_journal_title	Astrophysical Journal
citation_volume	967
citation_issue	2
citation_firstpage	77
citation_doi	https://doi.org/10.3847/1538-4357/ad3cdc
citation_public_url	https://hdl.handle.net/11094/97229

Measurement of Dependence of Microlensing Planet Frequency on the Host Star Mass and Galactocentric Distance by Using a Galactic Model

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