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. Jorgensen; 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. Jorgensen, 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

School of Physics and Astronomy

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Abstract

We report an analysis of the 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 light curve indicates a low planet-host star mass ratio of q = (6.9 0.2) 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 of hosting the planet. The flux variation observed by Spitzer is 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 yields a host mass of {M}_{\mathrm{host}}={0.37}_{-0.21}^{+0.35}\ {M}_{\odot } and a planet mass of {m}_{{\rm{p}}}={8.4}_{-4.7} {+7.9}\ {M}_{\oplus }. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of {M}_{\mathrm{host}}={0.091}_{-0.018} {+0.064}\ {M}_{\odot } and {m}_{{\rm{p}}}={2.1}_{-0.4} {+1.5}\ {M}_{\oplus }, respectively. Future high-resolution imaging observations with the Hubble Space Telescope or Extremely Large Telescope could distinguish between these two scenarios and help reveal the planetary system properties in more detail.

Original language	English
Article number	77
Journal	Astronomical Journal
Volume	162
Issue number	2
DOIs	https://doi.org/10.3847/1538-3881/ac00ba
State	Published - Aug 2021

Funding

Funders	Funder number
Japan Society for the Promotion of Science	20J20633
Japan Society for the Promotion of Science
Horizon 2020 Framework Programme	860470
Horizon 2020 Framework Programme

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10.3847/1538-3881/ac00ba

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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{1648e7d960df422483dd5b53c56748f4,

title = "OGLE-2018-BLG-1185b: A Low-mass Microlensing Planet Orbiting a Low-mass Dwarf",

abstract = "We report an analysis of the 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 light curve indicates a low planet-host star mass ratio of q = (6.9 0.2) 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 of hosting the planet. The flux variation observed by Spitzer is 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 yields a host mass of {M}_{\mathrm{host}}={0.37}_{-0.21}^{+0.35}\ {M}_{\odot } and a planet mass of {m}_{{\rm{p}}}={8.4}_{-4.7} {+7.9}\ {M}_{\oplus }. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of {M}_{\mathrm{host}}={0.091}_{-0.018} {+0.064}\ {M}_{\odot } and {m}_{{\rm{p}}}={2.1}_{-0.4} {+1.5}\ {M}_{\oplus }, respectively. Future high-resolution imaging observations with the Hubble Space Telescope or Extremely Large Telescope could distinguish between these two scenarios and help reveal the planetary system properties in more detail.",

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 Silva, {S. Ishitani} 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 Chung, {S. J.} and C. Han and Hwang, {K. H.} and Kim, {H. W.} and Shin, {I. G.} and Cha, {S. M.} and Kim, {D. J.} and Kim, {S. L.} and Lee, {C. U.} and Lee, {D. J.} and Y. Lee and Park, {B. G.} and Pogge, {R. W.} and Ryu, {Y. H.} and Beichman, {C. A.} and G. Bryden and Novati, {S. Calchi} 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 Jorgensen, {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",

year = "2021",

month = aug,

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

language = "אנגלית",

volume = "162",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

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, Silva, SI, 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, SJ, Han, C, Hwang, KH, Kim, HW, Shin, IG, Cha, SM, Kim, DJ, Kim, SL, Lee, CU, Lee, DJ, Lee, Y, Park, BG, Pogge, RW, Ryu, YH, Beichman, CA, Bryden, G, Novati, SC, Carey, S, Gaudi, BS, Henderson, CB, Zhu, W, Maoz, D, Penny, MT, Dominik, M, Jorgensen, 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 - Silva, S. Ishitani

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 - Novati, S. Calchi

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 - Jorgensen, 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.

PY - 2021/8

Y1 - 2021/8

N2 - We report an analysis of the 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 light curve indicates a low planet-host star mass ratio of q = (6.9 0.2) 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 of hosting the planet. The flux variation observed by Spitzer is 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 yields a host mass of {M}_{\mathrm{host}}={0.37}_{-0.21}^{+0.35}\ {M}_{\odot } and a planet mass of {m}_{{\rm{p}}}={8.4}_{-4.7} {+7.9}\ {M}_{\oplus }. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of {M}_{\mathrm{host}}={0.091}_{-0.018} {+0.064}\ {M}_{\odot } and {m}_{{\rm{p}}}={2.1}_{-0.4} {+1.5}\ {M}_{\oplus }, respectively. Future high-resolution imaging observations with the Hubble Space Telescope or Extremely Large Telescope could distinguish between these two scenarios and help reveal the planetary system properties in more detail.

AB - We report an analysis of the 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 light curve indicates a low planet-host star mass ratio of q = (6.9 0.2) 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 of hosting the planet. The flux variation observed by Spitzer is 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 yields a host mass of {M}_{\mathrm{host}}={0.37}_{-0.21}^{+0.35}\ {M}_{\odot } and a planet mass of {m}_{{\rm{p}}}={8.4}_{-4.7} {+7.9}\ {M}_{\oplus }. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of {M}_{\mathrm{host}}={0.091}_{-0.018} {+0.064}\ {M}_{\odot } and {m}_{{\rm{p}}}={2.1}_{-0.4} {+1.5}\ {M}_{\oplus }, respectively. Future high-resolution imaging observations with the Hubble Space Telescope or Extremely Large Telescope could distinguish between these two scenarios and help reveal the planetary system properties in more detail.

UR - http://www.scopus.com/inward/record.url?scp=85113341833&partnerID=8YFLogxK

U2 - 10.3847/1538-3881/ac00ba

DO - 10.3847/1538-3881/ac00ba

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AN - SCOPUS:85113341833

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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