OGLE-2013-BLG-0911Lb: a secondary on the brown-dwarf planet boundary around an M-dwarf

Shota Miyazaki; Takahiro Sumi; David P. Bennett; Andrzej Udalski; Yossi Shvartzvald; Rachel Street; Valerio Bozza; Jennifer C. Yee; Ian A. Bond; Nicholas Rattenbury; Naoki Koshimoto; Daisuke Suzuki; Akihiko Fukui; F. Abe; A. Bhattacharya; R. Barry; M. Donachie; H. Fujii; Y. Hirao; Y. Itow; Y. Kamei; I. Kondo; M.~C.~A. Li; C.~H. Ling; Y. Matsubara; T. Matsuo; Y. Muraki; M. Nagakane; K. Ohnishi; C. Ranc; T. Saito; A. Sharan; H. Shibai; H. Suematsu; D.~J. Sullivan; P.~J. Tristram; T. Yamakawa; A. Yonehara; J. Skowron; R. Poleski; P. Mróz; M.~K. Szymański; I. Soszyński; P. Pietrukowicz; S. KozŁowski; K. Ulaczyk; L. Wyrzykowski; Matan Friedmann; Shai Kaspi; Dan Maoz; M. Albrow; G. Christie; D.~L. DePoy; A. Gal-Yam; A. Gould; C. -U. Lee; I. Manulis; J. McCormick; T. Natusch; H. Ngan; R.~W. Pogge; I. Porritt; Y. Tsapras; E. Bachelet; M.~P.~G. Hundertmark; M. Dominik; D.~M. Bramich; A. Cassan; R. Figuera Jaimes; K. Horne; R. Schmidt; C. Snodgrass; J. Wambsganss; I.~A. Steele; J. Menzies; S. Mao; U.~G. Jørgensen; M.~J. Burgdorf; S. Ciceri; S. Calchi Novati; G. D'Ago; D.~F. Evans; T.~C. Hinse; N. Kains; E. Kerins; H. Korhonen; L. Mancini; A. Popovas; M. Rabus; S. Rahvar; G. Scarpetta; J. Skottfelt; J. Southworth; G. D'Ago; N. Peixinho; P. Verma

doi:10.3847/1538-3881/ab64de

OGLE-2013-BLG-0911Lb: a secondary on the brown-dwarf planet boundary around an M-dwarf

Shota Miyazaki, Takahiro Sumi, David P. Bennett, Andrzej Udalski, Yossi Shvartzvald, Rachel Street, Valerio Bozza, Jennifer C. Yee, Ian A. Bond, Nicholas Rattenbury, Naoki Koshimoto, Daisuke Suzuki, Akihiko Fukui, F. Abe, A. Bhattacharya, R. Barry, M. Donachie, H. Fujii, Y. Hirao, Y. ItowY. Kamei, I. Kondo, M.~C.~A. Li, C.~H. Ling, Y. Matsubara, T. Matsuo, Y. Muraki, M. Nagakane, K. Ohnishi, C. Ranc, T. Saito, A. Sharan, H. Shibai, H. Suematsu, D.~J. Sullivan, P.~J. Tristram, T. Yamakawa, A. Yonehara, J. Skowron, R. Poleski, P. Mróz, M.~K. Szymański, I. Soszyński, P. Pietrukowicz, S. KozŁowski, K. Ulaczyk, L. Wyrzykowski, Matan Friedmann, Shai Kaspi, Dan Maoz, M. Albrow, G. Christie, D.~L. DePoy, A. Gal-Yam, A. Gould, C. -U. Lee, I. Manulis, J. McCormick, T. Natusch, H. Ngan, R.~W. Pogge, I. Porritt, Y. Tsapras, E. Bachelet, M.~P.~G. Hundertmark, M. Dominik, D.~M. Bramich, A. Cassan, R. Figuera Jaimes, K. Horne, R. Schmidt, C. Snodgrass, J. Wambsganss, I.~A. Steele, J. Menzies, S. Mao, U.~G. Jørgensen, M.~J. Burgdorf, S. Ciceri, S. Calchi Novati, G. D'Ago, D.~F. Evans, T.~C. Hinse, N. Kains, E. Kerins, H. Korhonen, L. Mancini, A. Popovas, M. Rabus, S. Rahvar, G. Scarpetta, J. Skottfelt, J. Southworth, G. D'Ago, N. Peixinho, P. Verma

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Abstract

We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q ≅ 0.03 which differs from that reported in Shvartzvald et al. (2016). The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ∼ 0.15 or s ∼ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M-dwarf orbited by a massive Jupiter companion at very close (M_host= 0.30^+0.08_−0.06M⊙, M_comp= 10.1^+2.9_−2.2M_Jup, a_exp= 0.40^+0.05_−0.04au) or wide (M_host = 0.28^+0.10_−0.08M⊙, M_comp = 9.9^+3.8_−3.5M_Jup, a_exp = 18.0^+3.2_−3.2au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q= 0.03 which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M_Jup. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ∼13M_Jup in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M-dwarfs and even BDs which is challenging for other exoplanet detection methods.

Original language	English
Article number	76
Number of pages	15
Journal	Astronomical Journal
Volume	159
Issue number	2
DOIs	https://doi.org/10.3847/1538-3881/ab64de
Publication status	Published - 31 Jan 2020

Keywords

Microlensing
Exoplanets
Brown dwarfs

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10.3847/1538-3881/ab64de

Miyazaki-2020-OGLE-2013-BLG-0911Lb-AJ-AAM
Copyright © 2020 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/ab64de
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http://adsabs.harvard.edu/abs/2019arXiv191209613M

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021
Jardine, M. M. (PI), Bonnell, I. A. (CoI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Dominik, M. (CoI), Helling, C. (CoI), Horne, K. D. (CoI), Scholz, A. (CoI), Tojeiro, R. (CoI), Weijmans, A.-M. (CoI), Wild, V. (CoI), Woitke, P. (CoI), Wood, K. (CoI) & Zhao, H. (CoI)
1/04/18 → 31/03/22
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Miyazaki, S., Sumi, T., Bennett, D. P., Udalski, A., Shvartzvald, Y., Street, R., Bozza, V., Yee, J. C., Bond, I. A., Rattenbury, N., Koshimoto, N., Suzuki, D., Fukui, A., Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., ... Verma, P. (2020). OGLE-2013-BLG-0911Lb: a secondary on the brown-dwarf planet boundary around an M-dwarf. Astronomical Journal, 159(2), Article 76. https://doi.org/10.3847/1538-3881/ab64de

@article{2b849443896b4d32a473fbeab837df55,

title = "OGLE-2013-BLG-0911Lb: a secondary on the brown-dwarf planet boundary around an M-dwarf",

abstract = "We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q ≅ 0.03 which differs from that reported in Shvartzvald et al. (2016). The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ∼ 0.15 or s ∼ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M-dwarf orbited by a massive Jupiter companion at very close (Mhost= 0.30+0.08−0.06M⊙, Mcomp= 10.1+2.9−2.2MJup, aexp= 0.40+0.05−0.04au) or wide (Mhost = 0.28+0.10−0.08M⊙, Mcomp = 9.9+3.8−3.5MJup, aexp = 18.0+3.2−3.2au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q= 0.03 which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13MJup. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ∼13MJup in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M-dwarfs and even BDs which is challenging for other exoplanet detection methods.",

keywords = "Microlensing, Exoplanets, Brown dwarfs",

author = "Shota Miyazaki and Takahiro Sumi and Bennett, {David P.} and Andrzej Udalski and Yossi Shvartzvald and Rachel Street and Valerio Bozza and Yee, {Jennifer C.} and Bond, {Ian A.} and Nicholas Rattenbury and Naoki Koshimoto and Daisuke Suzuki and Akihiko Fukui and F. Abe and A. Bhattacharya and R. Barry and M. Donachie and H. Fujii and Y. Hirao and Y. Itow and Y. Kamei and I. Kondo and M.~C.~A. Li and C.~H. Ling and Y. Matsubara and T. Matsuo and Y. Muraki and M. Nagakane and K. Ohnishi and C. Ranc and T. Saito and A. Sharan and H. Shibai and H. Suematsu and D.~J. Sullivan and P.~J. Tristram and T. Yamakawa and A. Yonehara and J. Skowron and R. Poleski and P. Mr{\'o}z and M.~K. Szyma{\'n}ski and I. Soszy{\'n}ski and P. Pietrukowicz and S. Koz{\L}owski and K. Ulaczyk and L. Wyrzykowski and Matan Friedmann and Shai Kaspi and Dan Maoz and M. Albrow and G. Christie and D.~L. DePoy and A. Gal-Yam and A. Gould and Lee, {C. -U.} and I. Manulis and J. McCormick and T. Natusch and H. Ngan and R.~W. Pogge and I. Porritt and Y. Tsapras and E. Bachelet and M.~P.~G. Hundertmark and M. Dominik and D.~M. Bramich and A. Cassan and Jaimes, {R. Figuera} and K. Horne and R. Schmidt and C. Snodgrass and J. Wambsganss and I.~A. Steele and J. Menzies and S. Mao and U.~G. J{\o}rgensen and M.~J. Burgdorf and S. Ciceri and Novati, {S. Calchi} and G. D'Ago and D.~F. Evans and T.~C. Hinse and N. Kains and E. Kerins and H. Korhonen and L. Mancini and A. Popovas and M. Rabus and S. Rahvar and G. Scarpetta and J. Skottfelt and J. Southworth and G. D'Ago and N. Peixinho and P. Verma",

note = "Funding: UK STFC grant ST/R000824/1 (KH).",

year = "2020",

month = jan,

day = "31",

doi = "10.3847/1538-3881/ab64de",

language = "English",

volume = "159",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "2",

}

Miyazaki, S, Sumi, T, Bennett, DP, Udalski, A, Shvartzvald, Y, Street, R, Bozza, V, Yee, JC, Bond, IA, Rattenbury, N, Koshimoto, N, Suzuki, D, Fukui, A, Abe, F, Bhattacharya, A, Barry, R, Donachie, M, Fujii, H, Hirao, Y, Itow, Y, Kamei, Y, Kondo, I, Li, MCA, Ling, CH, Matsubara, Y, Matsuo, T, Muraki, Y, Nagakane, M, Ohnishi, K, Ranc, C, Saito, T, Sharan, A, Shibai, H, Suematsu, H, Sullivan, DJ, Tristram, PJ, Yamakawa, T, Yonehara, A, Skowron, J, Poleski, R, Mróz, P, Szymański, MK, Soszyński, I, Pietrukowicz, P, KozŁowski, S, Ulaczyk, K, Wyrzykowski, L, Friedmann, M, Kaspi, S, Maoz, D, Albrow, M, Christie, G, DePoy, DL, Gal-Yam, A, Gould, A, Lee, C-U, Manulis, I, McCormick, J, Natusch, T, Ngan, H, Pogge, RW, Porritt, I, Tsapras, Y, Bachelet, E, Hundertmark, MPG, Dominik, M, Bramich, DM, Cassan, A, Jaimes, RF, Horne, K, Schmidt, R, Snodgrass, C, Wambsganss, J, Steele, IA, Menzies, J, Mao, S, Jørgensen, UG, Burgdorf, MJ, Ciceri, S, Novati, SC, D'Ago, G, Evans, DF, Hinse, TC, Kains, N, Kerins, E, Korhonen, H, Mancini, L, Popovas, A, Rabus, M, Rahvar, S, Scarpetta, G, Skottfelt, J, Southworth, J, D'Ago, G, Peixinho, N & Verma, P 2020, 'OGLE-2013-BLG-0911Lb: a secondary on the brown-dwarf planet boundary around an M-dwarf', Astronomical Journal, vol. 159, no. 2, 76. https://doi.org/10.3847/1538-3881/ab64de

TY - JOUR

T1 - OGLE-2013-BLG-0911Lb

T2 - a secondary on the brown-dwarf planet boundary around an M-dwarf

AU - Miyazaki, Shota

AU - Sumi, Takahiro

AU - Bennett, David P.

AU - Udalski, Andrzej

AU - Shvartzvald, Yossi

AU - Street, Rachel

AU - Bozza, Valerio

AU - Yee, Jennifer C.

AU - Bond, Ian A.

AU - Rattenbury, Nicholas

AU - Koshimoto, Naoki

AU - Suzuki, Daisuke

AU - Fukui, Akihiko

AU - Abe, F.

AU - Bhattacharya, A.

AU - Barry, R.

AU - Donachie, M.

AU - Fujii, H.

AU - Hirao, Y.

AU - Itow, Y.

AU - Kamei, Y.

AU - Kondo, I.

AU - Li, M.~C.~A.

AU - Ling, C.~H.

AU - Matsubara, Y.

AU - Matsuo, T.

AU - Muraki, Y.

AU - Nagakane, M.

AU - Ohnishi, K.

AU - Ranc, C.

AU - Saito, T.

AU - Sharan, A.

AU - Shibai, H.

AU - Suematsu, H.

AU - Sullivan, D.~J.

AU - Tristram, P.~J.

AU - Yamakawa, T.

AU - Yonehara, A.

AU - Skowron, J.

AU - Poleski, R.

AU - Mróz, P.

AU - Szymański, M.~K.

AU - Soszyński, I.

AU - Pietrukowicz, P.

AU - KozŁowski, S.

AU - Ulaczyk, K.

AU - Wyrzykowski, L.

AU - Friedmann, Matan

AU - Kaspi, Shai

AU - Maoz, Dan

AU - Albrow, M.

AU - Christie, G.

AU - DePoy, D.~L.

AU - Gal-Yam, A.

AU - Gould, A.

AU - Lee, C. -U.

AU - Manulis, I.

AU - McCormick, J.

AU - Natusch, T.

AU - Ngan, H.

AU - Pogge, R.~W.

AU - Porritt, I.

AU - Tsapras, Y.

AU - Bachelet, E.

AU - Hundertmark, M.~P.~G.

AU - Dominik, M.

AU - Bramich, D.~M.

AU - Cassan, A.

AU - Jaimes, R. Figuera

AU - Horne, K.

AU - Schmidt, R.

AU - Snodgrass, C.

AU - Wambsganss, J.

AU - Steele, I.~A.

AU - Menzies, J.

AU - Mao, S.

AU - Jørgensen, U.~G.

AU - Burgdorf, M.~J.

AU - Ciceri, S.

AU - Novati, S. Calchi

AU - D'Ago, G.

AU - Evans, D.~F.

AU - Hinse, T.~C.

AU - Kains, N.

AU - Kerins, E.

AU - Korhonen, H.

AU - Mancini, L.

AU - Popovas, A.

AU - Rabus, M.

AU - Rahvar, S.

AU - Scarpetta, G.

AU - Skottfelt, J.

AU - Southworth, J.

AU - D'Ago, G.

AU - Peixinho, N.

AU - Verma, P.

N1 - Funding: UK STFC grant ST/R000824/1 (KH).

PY - 2020/1/31

Y1 - 2020/1/31

N2 - We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q ≅ 0.03 which differs from that reported in Shvartzvald et al. (2016). The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ∼ 0.15 or s ∼ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M-dwarf orbited by a massive Jupiter companion at very close (Mhost= 0.30+0.08−0.06M⊙, Mcomp= 10.1+2.9−2.2MJup, aexp= 0.40+0.05−0.04au) or wide (Mhost = 0.28+0.10−0.08M⊙, Mcomp = 9.9+3.8−3.5MJup, aexp = 18.0+3.2−3.2au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q= 0.03 which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13MJup. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ∼13MJup in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M-dwarfs and even BDs which is challenging for other exoplanet detection methods.

AB - We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q ≅ 0.03 which differs from that reported in Shvartzvald et al. (2016). The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ∼ 0.15 or s ∼ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M-dwarf orbited by a massive Jupiter companion at very close (Mhost= 0.30+0.08−0.06M⊙, Mcomp= 10.1+2.9−2.2MJup, aexp= 0.40+0.05−0.04au) or wide (Mhost = 0.28+0.10−0.08M⊙, Mcomp = 9.9+3.8−3.5MJup, aexp = 18.0+3.2−3.2au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q= 0.03 which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13MJup. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ∼13MJup in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M-dwarfs and even BDs which is challenging for other exoplanet detection methods.

KW - Microlensing

KW - Exoplanets

KW - Brown dwarfs

U2 - 10.3847/1538-3881/ab64de

DO - 10.3847/1538-3881/ab64de

M3 - Article

SN - 0004-6256

VL - 159

JO - Astronomical Journal

JF - Astronomical Journal

IS - 2

M1 - 76

ER -

OGLE-2013-BLG-0911Lb: a secondary on the brown-dwarf planet boundary around an M-dwarf

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