Measurement of Dependence of Microlensing Planet Frequency on The Host Star Mass and Galactocentric Distance by using a Galactic Model
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2024
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| author | Nunota, Kansuke Koshimoto, Naoki Suzuki, Daisuke Sumi, Takahiro Bennett, David P. Bhattacharya, Aparna Hirao, Yuki Terry, Sean K. Vandorou, Aikaterini |
| author_facet | Nunota, Kansuke Koshimoto, Naoki Suzuki, Daisuke Sumi, Takahiro Bennett, David P. Bhattacharya, Aparna Hirao, Yuki Terry, Sean K. Vandorou, Aikaterini |
| contents | We measure the dependence of planet frequency on host star mass, $M_{\rm L}$, and distance from the Galactic center, $R_{\rm L}$, using a sample of planets discovered by gravitational microlensing. We compare the two-dimensional distribution of the lens-source proper motion, $μ_{\rm rel}$, and the Einstein radius crossing time, $t_{\rm E}$, measured for 22 planetary events from Suzuki et al. (2016) with the distribution expected from Galactic model. Assuming that the planet-hosting probability of a star is proportional to $M_{\rm L}^m R_{\rm L}^r$, we calculate the likelihood distribution of $(m,r)$. We estimate that $r = 0.10^{+0.51}_{-0.37}$ and $m = 0.50^{+0.90}_{-0.70}$ 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 $m=-0.08^{+0.95}_{-0.65}$ for $q < 10^{-3}$ and $1.25^{+1.07}_{-1.14}$ 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_01721 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | 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 Earth and Planetary Astrophysics Astrophysics of Galaxies Solar and Stellar Astrophysics We measure the dependence of planet frequency on host star mass, $M_{\rm L}$, and distance from the Galactic center, $R_{\rm L}$, using a sample of planets discovered by gravitational microlensing. We compare the two-dimensional distribution of the lens-source proper motion, $μ_{\rm rel}$, and the Einstein radius crossing time, $t_{\rm E}$, measured for 22 planetary events from Suzuki et al. (2016) with the distribution expected from Galactic model. Assuming that the planet-hosting probability of a star is proportional to $M_{\rm L}^m R_{\rm L}^r$, we calculate the likelihood distribution of $(m,r)$. We estimate that $r = 0.10^{+0.51}_{-0.37}$ and $m = 0.50^{+0.90}_{-0.70}$ 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 $m=-0.08^{+0.95}_{-0.65}$ for $q < 10^{-3}$ and $1.25^{+1.07}_{-1.14}$ 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. |
| title | Measurement of Dependence of Microlensing Planet Frequency on The Host Star Mass and Galactocentric Distance by using a Galactic Model |
| topic | Earth and Planetary Astrophysics Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2403.01721 |