The First Planetary Microlensing Event with Two Microlensed Source Stars

© 2018. The American Astronomical Society. All rights reserved. We present the analysis of the microlensing event MOA-2010-BLG-117, and show that the light curve can only be explained by the gravitational lensing of a binary source star system by a star with a Jupiter-mass ratio planet. It was neces...

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Main Authors:	Bennett, D., Udalski, A., Han, C., Bond, I., Beaulieu, J., Skowron, J., Gaudi, B., Koshimoto, N., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M., Ling, C., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N., Rosenthal, M., Saito, T., Sharan, A., Sullivan, D., Sumi, T., Suzuki, D., Tristram, P., Yonehara, A., Szymanski, M., Poleski, R., Soszynski, I., Ulaczyk, K., Wyrzykowski, Depoy, D., Gould, A., Pogge, R., Yee, J., Albrow, M., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J., Cole, A., Coutures, C., Dieters, S., Prester, D., Donatowicz, J., Fouqué, P., Horne, K., Hundertmark, M., Kains, N., Kane, S., Marquette, J., Menzies, J., Pollard, K., Sahu, K., Wambsganss, J., Williams, Andrew, Zub, M.
Format:	Journal Article
Published:	Institute of Physics Publishing 2018
Online Access:	http://hdl.handle.net/20.500.11937/71703

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author	Bennett, D. Udalski, A. Han, C. Bond, I. Beaulieu, J. Skowron, J. Gaudi, B. Koshimoto, N. Abe, F. Asakura, Y. Barry, R. Bhattacharya, A. Donachie, M. Evans, P. Fukui, A. Hirao, Y. Itow, Y. Li, M. Ling, C. Masuda, K. Matsubara, Y. Muraki, Y. Nagakane, M. Ohnishi, K. Oyokawa, H. Ranc, C. Rattenbury, N. Rosenthal, M. Saito, T. Sharan, A. Sullivan, D. Sumi, T. Suzuki, D. Tristram, P. Yonehara, A. Szymanski, M. Poleski, R. Soszynski, I. Ulaczyk, K. Wyrzykowski Depoy, D. Gould, A. Pogge, R. Yee, J. Albrow, M. Bachelet, E. Batista, V. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cole, A. Coutures, C. Dieters, S. Prester, D. Donatowicz, J. Fouqué, P. Horne, K. Hundertmark, M. Kains, N. Kane, S. Marquette, J. Menzies, J. Pollard, K. Ranc, C. Sahu, K. Wambsganss, J. Williams, Andrew Zub, M.
author_facet	Bennett, D. Udalski, A. Han, C. Bond, I. Beaulieu, J. Skowron, J. Gaudi, B. Koshimoto, N. Abe, F. Asakura, Y. Barry, R. Bhattacharya, A. Donachie, M. Evans, P. Fukui, A. Hirao, Y. Itow, Y. Li, M. Ling, C. Masuda, K. Matsubara, Y. Muraki, Y. Nagakane, M. Ohnishi, K. Oyokawa, H. Ranc, C. Rattenbury, N. Rosenthal, M. Saito, T. Sharan, A. Sullivan, D. Sumi, T. Suzuki, D. Tristram, P. Yonehara, A. Szymanski, M. Poleski, R. Soszynski, I. Ulaczyk, K. Wyrzykowski Depoy, D. Gould, A. Pogge, R. Yee, J. Albrow, M. Bachelet, E. Batista, V. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cole, A. Coutures, C. Dieters, S. Prester, D. Donatowicz, J. Fouqué, P. Horne, K. Hundertmark, M. Kains, N. Kane, S. Marquette, J. Menzies, J. Pollard, K. Ranc, C. Sahu, K. Wambsganss, J. Williams, Andrew Zub, M.
author_sort	Bennett, D.
building	Curtin Institutional Repository
collection	Online Access
description	© 2018. The American Astronomical Society. All rights reserved. We present the analysis of the microlensing event MOA-2010-BLG-117, and show that the light curve can only be explained by the gravitational lensing of a binary source star system by a star with a Jupiter-mass ratio planet. It was necessary to modify standard microlensing modeling methods to find the correct light curve solution for this binary source, binary-lens event. We are able to measure a strong microlensing parallax signal, which yields the masses of the host star, M * = 0.58 ±0.11 M o, and planet, m p = 0.54 ±0.10MJup, at a projected star-planet separation of a = 2.42 ±0.26 au, corresponding to a semimajor axis of a = 2.9-0.6+1.6 au. Thus, the system resembles a half-scale model of the Sun-Jupiter system with a half-Jupiter0mass planet orbiting a half-solar-mass star at very roughly half of Jupiter's orbital distance from the Sun. The source stars are slightly evolved, and by requiring them to lie on the same isochrone, we can constrain the source to lie in the near side of the bulge at a distance of DS = 6.9 ±0.7 kpc, which implies a distance to the planetary lens system of D L = 3.5 ±0.4 kpc. The ability to model unusual planetary microlensing events, like this one, will be necessary to extract precise statistical information from the planned large exoplanet microlensing surveys, such as the WFIRST microlensing survey.
first_indexed	2025-11-14T10:49:21Z
format	Journal Article
id	curtin-20.500.11937-71703
institution	Curtin University Malaysia
institution_category	Local University
last_indexed	2025-11-14T10:49:21Z
publishDate	2018
publisher	Institute of Physics Publishing
recordtype	eprints
repository_type	Digital Repository
spelling	curtin-20.500.11937-717032018-12-13T09:31:54Z The First Planetary Microlensing Event with Two Microlensed Source Stars Bennett, D. Udalski, A. Han, C. Bond, I. Beaulieu, J. Skowron, J. Gaudi, B. Koshimoto, N. Abe, F. Asakura, Y. Barry, R. Bhattacharya, A. Donachie, M. Evans, P. Fukui, A. Hirao, Y. Itow, Y. Li, M. Ling, C. Masuda, K. Matsubara, Y. Muraki, Y. Nagakane, M. Ohnishi, K. Oyokawa, H. Ranc, C. Rattenbury, N. Rosenthal, M. Saito, T. Sharan, A. Sullivan, D. Sumi, T. Suzuki, D. Tristram, P. Yonehara, A. Szymanski, M. Poleski, R. Soszynski, I. Ulaczyk, K. Wyrzykowski Depoy, D. Gould, A. Pogge, R. Yee, J. Albrow, M. Bachelet, E. Batista, V. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cole, A. Coutures, C. Dieters, S. Prester, D. Donatowicz, J. Fouqué, P. Horne, K. Hundertmark, M. Kains, N. Kane, S. Marquette, J. Menzies, J. Pollard, K. Ranc, C. Sahu, K. Wambsganss, J. Williams, Andrew Zub, M. © 2018. The American Astronomical Society. All rights reserved. We present the analysis of the microlensing event MOA-2010-BLG-117, and show that the light curve can only be explained by the gravitational lensing of a binary source star system by a star with a Jupiter-mass ratio planet. It was necessary to modify standard microlensing modeling methods to find the correct light curve solution for this binary source, binary-lens event. We are able to measure a strong microlensing parallax signal, which yields the masses of the host star, M * = 0.58 ±0.11 M o, and planet, m p = 0.54 ±0.10MJup, at a projected star-planet separation of a = 2.42 ±0.26 au, corresponding to a semimajor axis of a = 2.9-0.6+1.6 au. Thus, the system resembles a half-scale model of the Sun-Jupiter system with a half-Jupiter0mass planet orbiting a half-solar-mass star at very roughly half of Jupiter's orbital distance from the Sun. The source stars are slightly evolved, and by requiring them to lie on the same isochrone, we can constrain the source to lie in the near side of the bulge at a distance of DS = 6.9 ±0.7 kpc, which implies a distance to the planetary lens system of D L = 3.5 ±0.4 kpc. The ability to model unusual planetary microlensing events, like this one, will be necessary to extract precise statistical information from the planned large exoplanet microlensing surveys, such as the WFIRST microlensing survey. 2018 Journal Article http://hdl.handle.net/20.500.11937/71703 10.3847/1538-3881/aaadfa Institute of Physics Publishing restricted
spellingShingle	Bennett, D. Udalski, A. Han, C. Bond, I. Beaulieu, J. Skowron, J. Gaudi, B. Koshimoto, N. Abe, F. Asakura, Y. Barry, R. Bhattacharya, A. Donachie, M. Evans, P. Fukui, A. Hirao, Y. Itow, Y. Li, M. Ling, C. Masuda, K. Matsubara, Y. Muraki, Y. Nagakane, M. Ohnishi, K. Oyokawa, H. Ranc, C. Rattenbury, N. Rosenthal, M. Saito, T. Sharan, A. Sullivan, D. Sumi, T. Suzuki, D. Tristram, P. Yonehara, A. Szymanski, M. Poleski, R. Soszynski, I. Ulaczyk, K. Wyrzykowski Depoy, D. Gould, A. Pogge, R. Yee, J. Albrow, M. Bachelet, E. Batista, V. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cole, A. Coutures, C. Dieters, S. Prester, D. Donatowicz, J. Fouqué, P. Horne, K. Hundertmark, M. Kains, N. Kane, S. Marquette, J. Menzies, J. Pollard, K. Ranc, C. Sahu, K. Wambsganss, J. Williams, Andrew Zub, M. The First Planetary Microlensing Event with Two Microlensed Source Stars
title	The First Planetary Microlensing Event with Two Microlensed Source Stars
title_full	The First Planetary Microlensing Event with Two Microlensed Source Stars
title_fullStr	The First Planetary Microlensing Event with Two Microlensed Source Stars
title_full_unstemmed	The First Planetary Microlensing Event with Two Microlensed Source Stars
title_short	The First Planetary Microlensing Event with Two Microlensed Source Stars
title_sort	first planetary microlensing event with two microlensed source stars
url	http://hdl.handle.net/20.500.11937/71703

The First Planetary Microlensing Event with Two Microlensed Source Stars

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