OGLE-2018-BLG-1185b: a low-mass microlensing planet orbiting a low-mass dwarf

Iona Kondo; Jennifer C. Yee; David P. Bennett; Takahiro Sumi; Naoki Koshimoto; Ian A. Bond; Andrew Gould; Andrzej Udalski; Yossi Shvartzvald; Youn Kil Jung; Weicheng Zang; Valerio Bozza; Etienne Bachelet; Markus P. G. Hundertmark; Nicholas J. Rattenbury; F. Abe; R. Barry; A. Bhattacharya; M. Donachie; A. Fukui; H. Fujii; Y. Hirao; S. Ishitani Silva; Y. Itow; R. Kirikawa; M. C. A. Li; Y. Matsubara; S. Miyazaki; Y. Muraki; G. Olmschenk; C. Ranc; Y. Satoh; H. Shoji; D. Suzuki; Y. Tanaka; P. J. Tristram; T. Yamawaki; A. Yonehara; P. Mróz; R. Poleski; J. Skowron; M. K. Szymański; I. Soszyński; S. Kozłowski; P. Pietrukowicz; K. Ulaczyk; K. A. Rybicki; P. Iwanek; M. Wrona; M. D. Albrow; S.-J. Chung; C. Han; K.-H. Hwang; H.-W. Kim; I.-G. Shin; S.-M. Cha; D.-J. Kim; S.-L. Kim; C.-U. Lee; D.-J. Lee; Y. Lee; B.-G. Park; R. W. Pogge; Y.-H. Ryu; C. A. Beichman; G. Bryden; S. Calchi Novati; S. Carey; B. S. Gaudi; C. B. Henderson; W. Zhu; D. Maoz; M. T. Penny; M. Dominik; U. G. Jørgensen; P. Longa-Peña; N. Peixinho; S. Sajadian; J. Skottfelt; C. Snodgrass; J. Tregloan-Reed; M. J. Burgdorf; J. Campbell-White; S. Dib; Y. I. Fujii; T. C. Hinse; E. Khalouei; S. Rahvar; M. Rabus; J. Southworth; Y. Tsapras; R. A. Street; D. M. Bramich; A. Cassan; K. Horne; J. Wambsganss; S. Mao; A. Saha

doi:10.3847/1538-3881/ac00ba

OGLE-2018-BLG-1185b: a low-mass microlensing planet orbiting a low-mass dwarf

Iona Kondo, Jennifer C. Yee, David P. Bennett, Takahiro Sumi, Naoki Koshimoto, Ian A. Bond, Andrew Gould, Andrzej Udalski, Yossi Shvartzvald, Youn Kil Jung, Weicheng Zang, Valerio Bozza, Etienne Bachelet, Markus P. G. Hundertmark, Nicholas J. Rattenbury, F. Abe, R. Barry, A. Bhattacharya, M. Donachie, A. FukuiH. Fujii, Y. Hirao, S. Ishitani Silva, Y. Itow, R. Kirikawa, M. C. A. Li, Y. Matsubara, S. Miyazaki, Y. Muraki, G. Olmschenk, C. Ranc, Y. Satoh, H. Shoji, D. Suzuki, Y. Tanaka, P. J. Tristram, T. Yamawaki, A. Yonehara, P. Mróz, R. Poleski, J. Skowron, M. K. Szymański, I. Soszyński, S. Kozłowski, P. Pietrukowicz, K. Ulaczyk, K. A. Rybicki, P. Iwanek, M. Wrona, M. D. Albrow, S.-J. Chung, C. Han, K.-H. Hwang, H.-W. Kim, I.-G. Shin, S.-M. Cha, D.-J. Kim, S.-L. Kim, C.-U. Lee, D.-J. Lee, Y. Lee, B.-G. Park, R. W. Pogge, Y.-H. Ryu, C. A. Beichman, G. Bryden, S. Calchi Novati, S. Carey, B. S. Gaudi, C. B. Henderson, W. Zhu, D. Maoz, M. T. Penny, M. Dominik, U. G. Jørgensen, P. Longa-Peña, N. Peixinho, S. Sajadian, J. Skottfelt, C. Snodgrass, J. Tregloan-Reed, M. J. Burgdorf, J. Campbell-White, S. Dib, Y. I. Fujii, T. C. Hinse, E. Khalouei, S. Rahvar, M. Rabus, J. Southworth, Y. Tsapras, R. A. Street, D. M. Bramich, A. Cassan, K. Horne, J. Wambsganss, S. Mao, A. Saha

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Abstract

We report the analysis of planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the Spitzer Space Telescope. The ground-based lightcurve indicates a low planet-host star mass ratio of q = (6.9 ± 0.2) x 10^-5, which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability to host this planet. The flux variation observed by Spitzer was marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be Δf_Spz < 4 instrumental flux units indicates a host mass of M_host = 0.37 ^+0.35_-0.21 M⊙ and a planet mass of m_p = 8.4^+7.9_-4.7 M⊕. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of M_host = 0.091^+0.064_-0.018 M⊙ and m_p = 2.1^+1.5_-0.4 M⊕, respectively. Future high-resolution imaging observations with HST or ELTs could distinguish between these two scenarios and help to reveal the planetary system properties in more detail.

Original language	English
Article number	77
Number of pages	18
Journal	Astronomical Journal
Volume	162
Issue number	2
Early online date	29 Jul 2021
DOIs	https://doi.org/10.3847/1538-3881/ac00ba
Publication status	Published - 1 Aug 2021

Keywords

Gravitational microlensing
Gravitational microlensing exoplanet detection
Satellite microlensing parallax

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10.3847/1538-3881/ac00ba

Kondo-2021-OGLE-2018-BLG-1185b-a-low-mass-ApJ-AAM
Copyright © 2021 American Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-3881/ac00ba.
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http://adsabs.harvard.edu/abs/2021arXiv210402157K

H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON
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European Commission
1/06/20 → 31/05/24
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Kondo, I., Yee, J. C., Bennett, D. P., Sumi, T., Koshimoto, N., Bond, I. A., Gould, A., Udalski, A., Shvartzvald, Y., Jung, Y. K., Zang, W., Bozza, V., Bachelet, E., Hundertmark, M. P. G., Rattenbury, N. J., Abe, F., Barry, R., Bhattacharya, A., Donachie, M., ... Saha, A. (2021). OGLE-2018-BLG-1185b: a low-mass microlensing planet orbiting a low-mass dwarf. Astronomical Journal, 162(2), Article 77. https://doi.org/10.3847/1538-3881/ac00ba

@article{ee3a6f094e7840319dd8b0b140780336,

title = "OGLE-2018-BLG-1185b: a low-mass microlensing planet orbiting a low-mass dwarf",

abstract = "We report the analysis of planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the Spitzer Space Telescope. The ground-based lightcurve indicates a low planet-host star mass ratio of q = (6.9 ± 0.2) x 10-5, which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability to host this planet. The flux variation observed by Spitzer was marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be ΔfSpz < 4 instrumental flux units indicates a host mass of Mhost = 0.37 +0.35-0.21 M⊙ and a planet mass of mp = 8.4+7.9-4.7 M⊕. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of Mhost = 0.091+0.064-0.018 M⊙ and mp = 2.1+1.5-0.4 M⊕, respectively. Future high-resolution imaging observations with HST or ELTs could distinguish between these two scenarios and help to reveal the planetary system properties in more detail.",

keywords = "Gravitational microlensing, Gravitational microlensing exoplanet detection, Satellite microlensing parallax",

author = "Iona Kondo and Yee, {Jennifer C.} and Bennett, {David P.} and Takahiro Sumi and Naoki Koshimoto and Bond, {Ian A.} and Andrew Gould and Andrzej Udalski and Yossi Shvartzvald and Jung, {Youn Kil} and Weicheng Zang and Valerio Bozza and Etienne Bachelet and Hundertmark, {Markus P. G.} and Rattenbury, {Nicholas J.} and F. Abe and R. Barry and A. Bhattacharya and M. Donachie and A. Fukui and H. Fujii and Y. Hirao and {Ishitani Silva}, S. and Y. Itow and R. Kirikawa and Li, {M. C. A.} and Y. Matsubara and S. Miyazaki and Y. Muraki and G. Olmschenk and C. Ranc and Y. Satoh and H. Shoji and D. Suzuki and Y. Tanaka and Tristram, {P. J.} and T. Yamawaki and A. Yonehara and P. Mr{\'o}z and R. Poleski and J. Skowron and Szyma{\'n}ski, {M. K.} and I. Soszy{\'n}ski and S. Koz{\l}owski and P. Pietrukowicz and K. Ulaczyk and Rybicki, {K. A.} and P. Iwanek and M. Wrona and Albrow, {M. D.} and S.-J. Chung and C. Han and K.-H. Hwang and H.-W. Kim and I.-G. Shin and S.-M. Cha and D.-J. Kim and S.-L. Kim and C.-U. Lee and D.-J. Lee and Y. Lee and B.-G. Park and Pogge, {R. W.} and Y.-H. Ryu and Beichman, {C. A.} and G. Bryden and {Calchi Novati}, S. and S. Carey and Gaudi, {B. S.} and Henderson, {C. B.} and W. Zhu and D. Maoz and Penny, {M. T.} and M. Dominik and J{\o}rgensen, {U. G.} and P. Longa-Pe{\~n}a and N. Peixinho and S. Sajadian and J. Skottfelt and C. Snodgrass and J. Tregloan-Reed and Burgdorf, {M. J.} and J. Campbell-White and S. Dib and Fujii, {Y. I.} and Hinse, {T. C.} and E. Khalouei and S. Rahvar and M. Rabus and J. Southworth and Y. Tsapras and Street, {R. A.} and Bramich, {D. M.} and A. Cassan and K. Horne and J. Wambsganss and S. Mao and A. Saha",

note = "Funding: Work by I.K. was supported by JSPS KAKENHI grant No.20J20633. Work by J.C.Y. was supported by Jet Propulsion Laboratory grant 1571564. Work by D.P.B., A.B., and C.R. was supported by NASA through grant NASA-80NSSC18K0274. T.S. acknowledges financial support from the JSPS (JSPS23103002, JSPS24253004, and JSPS26247023). Work by N.K. is supported by JSPS KAKENHI grant No. JP18J00897. A.S. is a University of Auckland doctoral scholar. Y.T. acknowledges the support of DFG priority program SPP 1992 Exploring the Diversity of Extrasolar Planets (WA 1047/11-1). T.C.H. acknowledges financial support from the National Research Foundation (No. 2019R1I1A1A01059609). U.G.J. acknowledges support from H2020-MSCA-ITN-2019, grant No. 860470 (CHAMELEON), and the NovoNordisk Foundation grant No. NNF19OC0057374. W.Z. and S.M. acknowledge support by the National Science Foundation of China (grant Nos. 11821303 and 11761131004). Work by C.H. was supported by grants of the National Research Foundation of Korea (2020R1A4A2002885 and 2019R1A2C2085965). Funding for B.S.G. was provided by NASA grant NNG16PJ32C and the Thomas Jefferson Chair for Discovery and Space Exploration. ",

year = "2021",

month = aug,

day = "1",

doi = "10.3847/1538-3881/ac00ba",

language = "English",

volume = "162",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "2",

}

Kondo, I, Yee, JC, Bennett, DP, Sumi, T, Koshimoto, N, Bond, IA, Gould, A, Udalski, A, Shvartzvald, Y, Jung, YK, Zang, W, Bozza, V, Bachelet, E, Hundertmark, MPG, Rattenbury, NJ, Abe, F, Barry, R, Bhattacharya, A, Donachie, M, Fukui, A, Fujii, H, Hirao, Y, Ishitani Silva, S, Itow, Y, Kirikawa, R, Li, MCA, Matsubara, Y, Miyazaki, S, Muraki, Y, Olmschenk, G, Ranc, C, Satoh, Y, Shoji, H, Suzuki, D, Tanaka, Y, Tristram, PJ, Yamawaki, T, Yonehara, A, Mróz, P, Poleski, R, Skowron, J, Szymański, MK, Soszyński, I, Kozłowski, S, Pietrukowicz, P, Ulaczyk, K, Rybicki, KA, Iwanek, P, Wrona, M, Albrow, MD, Chung, S-J, Han, C, Hwang, K-H, Kim, H-W, Shin, I-G, Cha, S-M, Kim, D-J, Kim, S-L, Lee, C-U, Lee, D-J, Lee, Y, Park, B-G, Pogge, RW, Ryu, Y-H, Beichman, CA, Bryden, G, Calchi Novati, S, Carey, S, Gaudi, BS, Henderson, CB, Zhu, W, Maoz, D, Penny, MT, Dominik, M, Jørgensen, UG, Longa-Peña, P, Peixinho, N, Sajadian, S, Skottfelt, J, Snodgrass, C, Tregloan-Reed, J, Burgdorf, MJ, Campbell-White, J, Dib, S, Fujii, YI, Hinse, TC, Khalouei, E, Rahvar, S, Rabus, M, Southworth, J, Tsapras, Y, Street, RA, Bramich, DM, Cassan, A, Horne, K, Wambsganss, J, Mao, S & Saha, A 2021, 'OGLE-2018-BLG-1185b: a low-mass microlensing planet orbiting a low-mass dwarf', Astronomical Journal, vol. 162, no. 2, 77. https://doi.org/10.3847/1538-3881/ac00ba

TY - JOUR

T1 - OGLE-2018-BLG-1185b

T2 - a low-mass microlensing planet orbiting a low-mass dwarf

AU - Kondo, Iona

AU - Yee, Jennifer C.

AU - Bennett, David P.

AU - Sumi, Takahiro

AU - Koshimoto, Naoki

AU - Bond, Ian A.

AU - Gould, Andrew

AU - Udalski, Andrzej

AU - Shvartzvald, Yossi

AU - Jung, Youn Kil

AU - Zang, Weicheng

AU - Bozza, Valerio

AU - Bachelet, Etienne

AU - Hundertmark, Markus P. G.

AU - Rattenbury, Nicholas J.

AU - Abe, F.

AU - Barry, R.

AU - Bhattacharya, A.

AU - Donachie, M.

AU - Fukui, A.

AU - Fujii, H.

AU - Hirao, Y.

AU - Ishitani Silva, S.

AU - Itow, Y.

AU - Kirikawa, R.

AU - Li, M. C. A.

AU - Matsubara, Y.

AU - Miyazaki, S.

AU - Muraki, Y.

AU - Olmschenk, G.

AU - Ranc, C.

AU - Satoh, Y.

AU - Shoji, H.

AU - Suzuki, D.

AU - Tanaka, Y.

AU - Tristram, P. J.

AU - Yamawaki, T.

AU - Yonehara, A.

AU - Mróz, P.

AU - Poleski, R.

AU - Skowron, J.

AU - Szymański, M. K.

AU - Soszyński, I.

AU - Kozłowski, S.

AU - Pietrukowicz, P.

AU - Ulaczyk, K.

AU - Rybicki, K. A.

AU - Iwanek, P.

AU - Wrona, M.

AU - Albrow, M. D.

AU - Chung, S.-J.

AU - Han, C.

AU - Hwang, K.-H.

AU - Kim, H.-W.

AU - Shin, I.-G.

AU - Cha, S.-M.

AU - Kim, D.-J.

AU - Kim, S.-L.

AU - Lee, C.-U.

AU - Lee, D.-J.

AU - Lee, Y.

AU - Park, B.-G.

AU - Pogge, R. W.

AU - Ryu, Y.-H.

AU - Beichman, C. A.

AU - Bryden, G.

AU - Calchi Novati, S.

AU - Carey, S.

AU - Gaudi, B. S.

AU - Henderson, C. B.

AU - Zhu, W.

AU - Maoz, D.

AU - Penny, M. T.

AU - Dominik, M.

AU - Jørgensen, U. G.

AU - Longa-Peña, P.

AU - Peixinho, N.

AU - Sajadian, S.

AU - Skottfelt, J.

AU - Snodgrass, C.

AU - Tregloan-Reed, J.

AU - Burgdorf, M. J.

AU - Campbell-White, J.

AU - Dib, S.

AU - Fujii, Y. I.

AU - Hinse, T. C.

AU - Khalouei, E.

AU - Rahvar, S.

AU - Rabus, M.

AU - Southworth, J.

AU - Tsapras, Y.

AU - Street, R. A.

AU - Bramich, D. M.

AU - Cassan, A.

AU - Horne, K.

AU - Wambsganss, J.

AU - Mao, S.

AU - Saha, A.

N1 - Funding: Work by I.K. was supported by JSPS KAKENHI grant No.20J20633. Work by J.C.Y. was supported by Jet Propulsion Laboratory grant 1571564. Work by D.P.B., A.B., and C.R. was supported by NASA through grant NASA-80NSSC18K0274. T.S. acknowledges financial support from the JSPS (JSPS23103002, JSPS24253004, and JSPS26247023). Work by N.K. is supported by JSPS KAKENHI grant No. JP18J00897. A.S. is a University of Auckland doctoral scholar. Y.T. acknowledges the support of DFG priority program SPP 1992 Exploring the Diversity of Extrasolar Planets (WA 1047/11-1). T.C.H. acknowledges financial support from the National Research Foundation (No. 2019R1I1A1A01059609). U.G.J. acknowledges support from H2020-MSCA-ITN-2019, grant No. 860470 (CHAMELEON), and the NovoNordisk Foundation grant No. NNF19OC0057374. W.Z. and S.M. acknowledge support by the National Science Foundation of China (grant Nos. 11821303 and 11761131004). Work by C.H. was supported by grants of the National Research Foundation of Korea (2020R1A4A2002885 and 2019R1A2C2085965). Funding for B.S.G. was provided by NASA grant NNG16PJ32C and the Thomas Jefferson Chair for Discovery and Space Exploration.

PY - 2021/8/1

Y1 - 2021/8/1

N2 - We report the analysis of planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the Spitzer Space Telescope. The ground-based lightcurve indicates a low planet-host star mass ratio of q = (6.9 ± 0.2) x 10-5, which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability to host this planet. The flux variation observed by Spitzer was marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be ΔfSpz < 4 instrumental flux units indicates a host mass of Mhost = 0.37 +0.35-0.21 M⊙ and a planet mass of mp = 8.4+7.9-4.7 M⊕. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of Mhost = 0.091+0.064-0.018 M⊙ and mp = 2.1+1.5-0.4 M⊕, respectively. Future high-resolution imaging observations with HST or ELTs could distinguish between these two scenarios and help to reveal the planetary system properties in more detail.

AB - We report the analysis of planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the Spitzer Space Telescope. The ground-based lightcurve indicates a low planet-host star mass ratio of q = (6.9 ± 0.2) x 10-5, which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability to host this planet. The flux variation observed by Spitzer was marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be ΔfSpz < 4 instrumental flux units indicates a host mass of Mhost = 0.37 +0.35-0.21 M⊙ and a planet mass of mp = 8.4+7.9-4.7 M⊕. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of Mhost = 0.091+0.064-0.018 M⊙ and mp = 2.1+1.5-0.4 M⊕, respectively. Future high-resolution imaging observations with HST or ELTs could distinguish between these two scenarios and help to reveal the planetary system properties in more detail.

KW - Gravitational microlensing

KW - Gravitational microlensing exoplanet detection

KW - Satellite microlensing parallax

U2 - 10.3847/1538-3881/ac00ba

DO - 10.3847/1538-3881/ac00ba

M3 - Article

SN - 0004-6256

VL - 162

JO - Astronomical Journal

JF - Astronomical Journal

IS - 2

M1 - 77

ER -

OGLE-2018-BLG-1185b: a low-mass microlensing planet orbiting a low-mass dwarf

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