OGLE-2017-BLG-1186: First application of asteroseismology and Gaussian processes to microlensing

S. S. Li; W. Zang; A. Udalski; Y. Shvartzvald; D. Huber; C. U. Lee; T. Sumi; A. Gould; S. Mao; P. Fouqué; T. Wang; S. Dong; U. G. Jørgensen; A. Cole; P. Mróz; M. K. Szymanski; J. Skowron; R. Poleski; I. Soszynski; P. Pietrukowicz; S. Kozłowski; K. Ulaczyk; K. A. Rybicki; P. Iwanek; J. C. Yee; S. Calchi Novati; C. A. Beichman; G. Bryden; S. Carey; B. S. Gaudi; C. B. Henderson; W. Zhu; M. D. Albrow; S. J. Chung; C. Han; K. H. Hwang; Y. K. Jung; Y. H. Ryu; I. G. Shin; S. M. Cha; D. J. Kim; H. W. Kim; S. L. Kim; D. J. Lee; Y. Lee; B. G. Park; R. W. Pogge; I. A. Bond; F. Abe; R. Barry; D. P. Bennett; A. Bhattacharya; M. Donachie; A. Fukui; Y. Hirao; Y. Itow; I. Kondo; N. Koshimoto; M. C.A. Li; Y. Matsubara; Y. Muraki; S. Miyazaki; M. Nagakane; C. Ranc; N. J. Rattenbury; H. Suematsu; D. J. Sullivan; D. Suzuki; P. J. Tristram; A. Yonehara; G. Christie; J. Drummond; J. Green; S. Hennerley; T. Natusch; I. Porritt; E. Bachelet; D. Maoz; R. A. Street; Y. Tsapras; V. Bozza; M. Dominik; M. Hundertmark; N. Peixinho; S. Sajadian; M. J. Burgdorf; D. F. Evans; R. Figuera Jaimes; Y. I. Fujii; L. K. Haikala; C. Helling; T. Henning; T. C. Hinse; L. Mancini; P. Longa-Peña; S. Rahvar; M. Rabus; J. Skottfelt; C. Snodgrass; J. Southworth; E. Unda-Sanzana; C. von Essen; J. P. Beaulieu; J. Blackman; K. Hill

doi:10.1093/mnras/stz1873

OGLE-2017-BLG-1186: First application of asteroseismology and Gaussian processes to microlensing

S. S. Li^*, W. Zang, A. Udalski, Y. Shvartzvald, D. Huber, C. U. Lee, T. Sumi, A. Gould, S. Mao, P. Fouqué, T. Wang, S. Dong, U. G. Jørgensen, A. Cole, P. Mróz, M. K. Szymanski, J. Skowron, R. Poleski, I. Soszynski, P. PietrukowiczS. Kozłowski, K. Ulaczyk, K. A. Rybicki, P. Iwanek, J. C. Yee, S. Calchi Novati, C. A. Beichman, G. Bryden, S. Carey, B. S. Gaudi, C. B. Henderson, W. Zhu, M. D. Albrow, S. J. Chung, C. Han, K. H. Hwang, Y. K. Jung, Y. H. Ryu, I. G. Shin, S. M. Cha, D. J. Kim, H. W. Kim, S. L. Kim, D. J. Lee, Y. Lee, B. G. Park, R. W. Pogge, I. A. Bond, F. Abe, R. Barry, D. P. Bennett, A. Bhattacharya, M. Donachie, A. Fukui, Y. Hirao, Y. Itow, I. Kondo, N. Koshimoto, M. C.A. Li, Y. Matsubara, Y. Muraki, S. Miyazaki, M. Nagakane, C. Ranc, N. J. Rattenbury, H. Suematsu, D. J. Sullivan, D. Suzuki, P. J. Tristram, A. Yonehara, G. Christie, J. Drummond, J. Green, S. Hennerley, T. Natusch, I. Porritt, E. Bachelet, D. Maoz, R. A. Street, Y. Tsapras, V. Bozza, M. Dominik, M. Hundertmark, N. Peixinho, S. Sajadian, M. J. Burgdorf, D. F. Evans, R. Figuera Jaimes, Y. I. Fujii, L. K. Haikala, C. Helling, T. Henning, T. C. Hinse, L. Mancini, P. Longa-Peña, S. Rahvar, M. Rabus, J. Skottfelt, C. Snodgrass, J. Southworth, E. Unda-Sanzana, C. von Essen, J. P. Beaulieu, J. Blackman, K. Hill

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

12 Scopus citations

Abstract

We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average timescale of ∼9 d. The asteroseismic analysis also provides us source properties including the source angular size (∼27 μas) and distance (∼11.5 kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional χ² minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a ∼0.045 M brown dwarf at distance ∼9.0 kpc, or a ∼0.073 M ultracool dwarf at distance ∼9.8 kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a ∼ 35 per cent probability for the lens to be a bulge object and ∼ 65 per cent to be a background disc object.

Original language	English
Pages (from-to)	3308-3323
Number of pages	16
Journal	Monthly Notices of the Royal Astronomical Society
Volume	488
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stz1873
State	Published - 21 Sep 2019

Funding

Funders	Funder number
ANR-18-CE31-0002
Italian Minister of Instruction, University and Research
Universities Space Research Association
National Science Foundation	JP17H02871, JSPS24253004, JSPS15H00781, AST-1516842, JSPS23340064, AST-1717000, JSPS26247023, JP16H06287
National Science Foundation
National Aeronautics and Space Administration
Jet Propulsion Laboratory	2017R1A4A1015178, 11573003, 1500811
Jet Propulsion Laboratory
Australian Research Council	LE110100055
Australian Research Council
University of Tasmania
Deutsche Forschungsgemeinschaft	WA 1047/11-1
Deutsche Forschungsgemeinschaft
Agence Nationale de la Recherche
National Natural Science Foundation of China	11761131004, 11821303
National Natural Science Foundation of China
Fundação para a Ciência e a Tecnologia	UID/Multi/00611/2013
Fundação para a Ciência e a Tecnologia
Centre National d’Etudes Spatiales
Ministero dell’Istruzione, dell’Università e della Ricerca
National Research Foundation of Korea
Narodowe Centrum Nauki	MAESTRO 2014/14/A/ST9/00121
Narodowe Centrum Nauki
European Regional Development Fund	POCI-01-0145-FEDER-006922
European Regional Development Fund

Keywords

Asteroseismology
Gravitational lensing: micro
Stars: fundamental parameters
Stars: oscillations

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10.1093/mnras/stz1873

Cite this

Li, S. S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. U., Sumi, T., Gould, A., Mao, S., Fouqué, P., Wang, T., Dong, S., Jørgensen, U. G., Cole, A., Mróz, P., Szymanski, M. K., Skowron, J., Poleski, R., Soszynski, I., ... Hill, K. (2019). OGLE-2017-BLG-1186: First application of asteroseismology and Gaussian processes to microlensing. Monthly Notices of the Royal Astronomical Society, 488(3), 3308-3323. https://doi.org/10.1093/mnras/stz1873

@article{f63d486bd0164acea0f038d7149b3af3,

title = "OGLE-2017-BLG-1186: First application of asteroseismology and Gaussian processes to microlensing",

abstract = "We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average timescale of ∼9 d. The asteroseismic analysis also provides us source properties including the source angular size (∼27 μas) and distance (∼11.5 kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional χ2 minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a ∼0.045 M brown dwarf at distance ∼9.0 kpc, or a ∼0.073 M ultracool dwarf at distance ∼9.8 kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a ∼ 35 per cent probability for the lens to be a bulge object and ∼ 65 per cent to be a background disc object.",

keywords = "Asteroseismology, Gravitational lensing: micro, Stars: fundamental parameters, Stars: oscillations",

author = "Li, {S. S.} and W. Zang and A. Udalski and Y. Shvartzvald and D. Huber and Lee, {C. U.} and T. Sumi and A. Gould and S. Mao and P. Fouqu{\'e} and T. Wang and S. Dong and J{\o}rgensen, {U. G.} and A. Cole and P. Mr{\'o}z and Szymanski, {M. K.} and J. Skowron and R. Poleski and I. Soszynski and P. Pietrukowicz and S. Koz{\l}owski and K. Ulaczyk and Rybicki, {K. A.} and P. Iwanek and Yee, {J. C.} and Novati, {S. Calchi} and Beichman, {C. A.} and G. Bryden and S. Carey and Gaudi, {B. S.} and Henderson, {C. B.} and W. Zhu and Albrow, {M. D.} and Chung, {S. J.} and C. Han and Hwang, {K. H.} and Jung, {Y. K.} and Ryu, {Y. H.} and Shin, {I. G.} and Cha, {S. M.} and Kim, {D. J.} and Kim, {H. W.} and Kim, {S. L.} and Lee, {D. J.} and Y. Lee and Park, {B. G.} and Pogge, {R. W.} and Bond, {I. A.} and F. Abe and R. Barry and Bennett, {D. P.} and A. Bhattacharya and M. Donachie and A. Fukui and Y. Hirao and Y. Itow and I. Kondo and N. Koshimoto and Li, {M. C.A.} and Y. Matsubara and Y. Muraki and S. Miyazaki and M. Nagakane and C. Ranc and Rattenbury, {N. J.} and H. Suematsu and Sullivan, {D. J.} and D. Suzuki and Tristram, {P. J.} and A. Yonehara and G. Christie and J. Drummond and J. Green and S. Hennerley and T. Natusch and I. Porritt and E. Bachelet and D. Maoz and Street, {R. A.} and Y. Tsapras and V. Bozza and M. Dominik and M. Hundertmark and N. Peixinho and S. Sajadian and Burgdorf, {M. J.} and Evans, {D. F.} and Jaimes, {R. Figuera} and Fujii, {Y. I.} and Haikala, {L. K.} and C. Helling and T. Henning and Hinse, {T. C.} and L. Mancini and P. Longa-Pe{\~n}a and S. Rahvar and M. Rabus and J. Skottfelt and C. Snodgrass and J. Southworth and E. Unda-Sanzana and {von Essen}, C. and Beaulieu, {J. P.} and J. Blackman and K. Hill",

note = "Publisher Copyright: {\textcopyright} 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society",

year = "2019",

month = sep,

day = "21",

doi = "10.1093/mnras/stz1873",

language = "אנגלית",

volume = "488",

pages = "3308--3323",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Li, SS, Zang, W, Udalski, A, Shvartzvald, Y, Huber, D, Lee, CU, Sumi, T, Gould, A, Mao, S, Fouqué, P, Wang, T, Dong, S, Jørgensen, UG, Cole, A, Mróz, P, Szymanski, MK, Skowron, J, Poleski, R, Soszynski, I, Pietrukowicz, P, Kozłowski, S, Ulaczyk, K, Rybicki, KA, Iwanek, P, Yee, JC, Novati, SC, Beichman, CA, Bryden, G, Carey, S, Gaudi, BS, Henderson, CB, Zhu, W, Albrow, MD, Chung, SJ, Han, C, Hwang, KH, Jung, YK, Ryu, YH, Shin, IG, Cha, SM, Kim, DJ, Kim, HW, Kim, SL, Lee, DJ, Lee, Y, Park, BG, Pogge, RW, Bond, IA, Abe, F, Barry, R, Bennett, DP, Bhattacharya, A, Donachie, M, Fukui, A, Hirao, Y, Itow, Y, Kondo, I, Koshimoto, N, Li, MCA, Matsubara, Y, Muraki, Y, Miyazaki, S, Nagakane, M, Ranc, C, Rattenbury, NJ, Suematsu, H, Sullivan, DJ, Suzuki, D, Tristram, PJ, Yonehara, A, Christie, G, Drummond, J, Green, J, Hennerley, S, Natusch, T, Porritt, I, Bachelet, E, Maoz, D, Street, RA, Tsapras, Y, Bozza, V, Dominik, M, Hundertmark, M, Peixinho, N, Sajadian, S, Burgdorf, MJ, Evans, DF, Jaimes, RF, Fujii, YI, Haikala, LK, Helling, C, Henning, T, Hinse, TC, Mancini, L, Longa-Peña, P, Rahvar, S, Rabus, M, Skottfelt, J, Snodgrass, C, Southworth, J, Unda-Sanzana, E, von Essen, C, Beaulieu, JP, Blackman, J & Hill, K 2019, 'OGLE-2017-BLG-1186: First application of asteroseismology and Gaussian processes to microlensing', Monthly Notices of the Royal Astronomical Society, vol. 488, no. 3, pp. 3308-3323. https://doi.org/10.1093/mnras/stz1873

TY - JOUR

T1 - OGLE-2017-BLG-1186

T2 - First application of asteroseismology and Gaussian processes to microlensing

AU - Li, S. S.

AU - Zang, W.

AU - Udalski, A.

AU - Shvartzvald, Y.

AU - Huber, D.

AU - Lee, C. U.

AU - Sumi, T.

AU - Gould, A.

AU - Mao, S.

AU - Fouqué, P.

AU - Wang, T.

AU - Dong, S.

AU - Jørgensen, U. G.

AU - Cole, A.

AU - Mróz, P.

AU - Szymanski, M. K.

AU - Skowron, J.

AU - Poleski, R.

AU - Soszynski, I.

AU - Pietrukowicz, P.

AU - Kozłowski, S.

AU - Ulaczyk, K.

AU - Rybicki, K. A.

AU - Iwanek, P.

AU - Yee, J. C.

AU - Novati, S. Calchi

AU - Beichman, C. A.

AU - Bryden, G.

AU - Carey, S.

AU - Gaudi, B. S.

AU - Henderson, C. B.

AU - Zhu, W.

AU - Albrow, M. D.

AU - Chung, S. J.

AU - Han, C.

AU - Hwang, K. H.

AU - Jung, Y. K.

AU - Ryu, Y. H.

AU - Shin, I. G.

AU - Cha, S. M.

AU - Kim, D. J.

AU - Kim, H. W.

AU - Kim, S. L.

AU - Lee, D. J.

AU - Lee, Y.

AU - Park, B. G.

AU - Pogge, R. W.

AU - Bond, I. A.

AU - Abe, F.

AU - Barry, R.

AU - Bennett, D. P.

AU - Bhattacharya, A.

AU - Donachie, M.

AU - Fukui, A.

AU - Hirao, Y.

AU - Itow, Y.

AU - Kondo, I.

AU - Koshimoto, N.

AU - Li, M. C.A.

AU - Matsubara, Y.

AU - Muraki, Y.

AU - Miyazaki, S.

AU - Nagakane, M.

AU - Ranc, C.

AU - Rattenbury, N. J.

AU - Suematsu, H.

AU - Sullivan, D. J.

AU - Suzuki, D.

AU - Tristram, P. J.

AU - Yonehara, A.

AU - Christie, G.

AU - Drummond, J.

AU - Green, J.

AU - Hennerley, S.

AU - Natusch, T.

AU - Porritt, I.

AU - Bachelet, E.

AU - Maoz, D.

AU - Street, R. A.

AU - Tsapras, Y.

AU - Bozza, V.

AU - Dominik, M.

AU - Hundertmark, M.

AU - Peixinho, N.

AU - Sajadian, S.

AU - Burgdorf, M. J.

AU - Evans, D. F.

AU - Jaimes, R. Figuera

AU - Fujii, Y. I.

AU - Haikala, L. K.

AU - Helling, C.

AU - Henning, T.

AU - Hinse, T. C.

AU - Mancini, L.

AU - Longa-Peña, P.

AU - Rahvar, S.

AU - Rabus, M.

AU - Skottfelt, J.

AU - Snodgrass, C.

AU - Southworth, J.

AU - Unda-Sanzana, E.

AU - von Essen, C.

AU - Beaulieu, J. P.

AU - Blackman, J.

AU - Hill, K.

PY - 2019/9/21

Y1 - 2019/9/21

N2 - We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average timescale of ∼9 d. The asteroseismic analysis also provides us source properties including the source angular size (∼27 μas) and distance (∼11.5 kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional χ2 minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a ∼0.045 M brown dwarf at distance ∼9.0 kpc, or a ∼0.073 M ultracool dwarf at distance ∼9.8 kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a ∼ 35 per cent probability for the lens to be a bulge object and ∼ 65 per cent to be a background disc object.

AB - We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average timescale of ∼9 d. The asteroseismic analysis also provides us source properties including the source angular size (∼27 μas) and distance (∼11.5 kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional χ2 minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a ∼0.045 M brown dwarf at distance ∼9.0 kpc, or a ∼0.073 M ultracool dwarf at distance ∼9.8 kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a ∼ 35 per cent probability for the lens to be a bulge object and ∼ 65 per cent to be a background disc object.

KW - Asteroseismology

KW - Gravitational lensing: micro

KW - Stars: fundamental parameters

KW - Stars: oscillations

UR - http://www.scopus.com/inward/record.url?scp=85082603093&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz1873

DO - 10.1093/mnras/stz1873

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AN - SCOPUS:85082603093

SN - 0035-8711

VL - 488

SP - 3308

EP - 3323

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

OGLE-2017-BLG-1186: First application of asteroseismology and Gaussian processes to microlensing

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