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. Fouque; T. Wang; S. Dong; U. G. Jorgensen; A. Cole; P. Mroz; M. K. Szymanski; J. Skowron; R. Poleski; I. Soszynski; P. Pietrukowicz; S. Kozlowski; 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-Pena; 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. Fouque, T. Wang, S. Dong, U. G. Jorgensen, A. Cole, P. Mroz, M. K. Szymanski, J. Skowron, R. Poleski, I. Soszynski, P. PietrukowiczS. Kozlowski, 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-Pena, S. Rahvar, M. Rabus, J. Skottfelt, C. Snodgrass, J. Southworth, E. Unda-Sanzana, C. von Essen, J. -P. Beaulieu, J. Blackman, K. Hill

Astrofysik og Planetforskning

5 Citationer (Scopus)

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.

Originalsprog	Engelsk
Tidsskrift	Monthly Notices of the Royal Astronomical Society
Vol/bind	488
Udgave nummer	3
Sider (fra-til)	3308-3323
ISSN	0035-8711
DOI	https://doi.org/10.1093/mnras/stz1873
Status	Udgivet - 21 sep. 2019

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10.1093/mnras/stz1873

https://academic.oup.com/mnras/article-pdf/488/3/3308/29025849/stz1873.pdf

Citationsformater

Li, S. -S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. -U., Sumi, T., Gould, A., Mao, S., Fouque, P., Wang, T., Dong, S., Jorgensen, U. G., Cole, A., Mroz, 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

Li, S-S, Zang, W, Udalski, A, Shvartzvald, Y, Huber, D, Lee, C-U, Sumi, T, Gould, A, Mao, S, Fouque, P, Wang, T, Dong, S, Jorgensen, UG, Cole, A, Mroz, P, Szymanski, MK, Skowron, J, Poleski, R, Soszynski, I, Pietrukowicz, P, Kozlowski, 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, S-J, Han, C, Hwang, K-H, Jung, YK, Ryu, Y-H, Shin, I-G, Cha, S-M, Kim, D-J, Kim, H-W, Kim, S-L, Lee, D-J, Lee, Y, Park, B-G, 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-Pena, P, Rahvar, S, Rabus, M, Skottfelt, J, Snodgrass, C, Southworth, J, Unda-Sanzana, E, von Essen, C, Beaulieu, J-P, 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, bind 488, nr. 3, s. 3308-3323. https://doi.org/10.1093/mnras/stz1873

@article{0fc477ebfaab4bb186f647f07c7f0955,

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. Fouque and T. Wang and S. Dong and Jorgensen, {U. G.} and A. Cole and P. Mroz and Szymanski, {M. K.} and J. Skowron and R. Poleski and I. Soszynski and P. Pietrukowicz and S. Kozlowski 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-Pena 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",

year = "2019",

month = sep,

day = "21",

doi = "10.1093/mnras/stz1873",

language = "English",

volume = "488",

pages = "3308--3323",

journal = "Royal Astronomical Society. Monthly Notices",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

TY - JOUR

T1 - OGLE-2017-BLG-1186: 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 - Fouque, P.

AU - Wang, T.

AU - Dong, S.

AU - Jorgensen, U. G.

AU - Cole, A.

AU - Mroz, P.

AU - Szymanski, M. K.

AU - Skowron, J.

AU - Poleski, R.

AU - Soszynski, I.

AU - Pietrukowicz, P.

AU - Kozlowski, 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-Pena, 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

U2 - 10.1093/mnras/stz1873

DO - 10.1093/mnras/stz1873

M3 - Journal article

SN - 0035-8711

VL - 488

SP - 3308

EP - 3323

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

IS - 3

ER -

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

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