OGLE-2018-BLG-1428Lb: a Jupiter-mass planet beyond the snow line of a dwarf star

ABSTRACT We present the analysis of the microlensing event OGLE-2018-BLG-1428, which has a short-duration (∼1 d) caustic-crossing anomaly. The event was caused by a planetary lens system with planet/host mass ratio q = 1.7 × 10−3. Because of the detection of the caustic-crossing anomaly, the finite...

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Veröffentlicht in:Monthly notices of the Royal Astronomical Society 2021-05, Vol.503 (2), p.2706-2712
Hauptverfasser: Kim, Yun Hak, Chung, Sun-Ju, Udalski, Andrej, Gould, Andrew, Albrow, Michael D, Jung, Youn Kil, Hwang, Kyu-Ha, Han, Cheongho, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C, Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W, Mróz, Przemek, Poleski, Radek, Wrona, Marcin, Iwanek, Patryk, Szymański, Michał K, Skowron, Jan, Soszyński, Igor, Kozłowski, Szymon, Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Rybicki, Krzysztof
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Sprache:eng
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Zusammenfassung:ABSTRACT We present the analysis of the microlensing event OGLE-2018-BLG-1428, which has a short-duration (∼1 d) caustic-crossing anomaly. The event was caused by a planetary lens system with planet/host mass ratio q = 1.7 × 10−3. Because of the detection of the caustic-crossing anomaly, the finite source effect was well measured, but the microlens parallax was not constrained due to the relatively short time-scale (tE = 24 d). From a Bayesian analysis, we find that the host star is a dwarf star $M_{\rm host}=0.43^{+0.33}_{-0.22} \ \mathrm{M}_{\odot }$ at a distance $D_{\rm L}=6.22^{+1.03}_{-1.51}\ {\rm kpc}$ and the planet is a Jovian-mass planet $M_{\rm p}=0.77^{+0.77}_{-0.53} \ M_{\rm J}$ with a projected separation $a_{\perp }=3.30^{+0.59}_{-0.83}\ {\rm au}$. The planet orbits beyond the snow line of the host star. Considering the relative lens-source proper motion of $\mu _{\rm rel} = 5.58 \pm 0.38\ \rm mas\ yr^{-1}$, the lens can be resolved by adaptive optics with a 30 m telescope in the future.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stab534