A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291

David P. Bennett; Andrzej Udalski; Ian A. Bond; Daisuke Suzuki; Yoon Hyun Ryu; Fumio Abe; Richard K. Barry; Aparna Bhattacharya; Martin Donachie; Akihiko Fukui; Yuki Hirao; Kohei Kawasaki; Iona Kondo; Naoki Koshimoto; Man Cheung Alex Li; Yutaka Matsubara; Shota Miyazaki; Yasushi Muraki; Masayuki Nagakane; Koji Ohnishi; Clément Ranc; Nicholas J. Rattenbury; Haruno Suematsu; Takahiro Sumi; Paul J. Tristram; Atsunori Yonehara; Michał K. Szymański; Igor Soszyński; Łukasz Wyrzykowski; Krzysztof Ulaczyk; Radek Poleski; Szymon Kozłowski; Paweł Pietrukowicz; Jan Skowron; Yossi Shvartzvald; Dan Maoz; Shai Kaspi; Matan Friedmann; Virginie Batista; Darren Depoy; Subo Dong; B. Scott Gaudi; Andrew Gould; Cheongho Han; Richard W. Pogge; Thiam Guan Tan; Jennifer C. Yee

doi:https://doi.org/10.3847/1538-3881/aad59c

A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291

David P. Bennett, Andrzej Udalski, Ian A. Bond, Daisuke Suzuki, Yoon Hyun Ryu, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Martin Donachie, Akihiko Fukui, Yuki Hirao, Kohei Kawasaki, Iona Kondo, Naoki Koshimoto, Man Cheung Alex Li, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Masayuki Nagakane, Koji OhnishiClément Ranc, Nicholas J. Rattenbury, Haruno Suematsu, Takahiro Sumi, Paul J. Tristram, Atsunori Yonehara, Michał K. Szymański, Igor Soszyński, Łukasz Wyrzykowski, Krzysztof Ulaczyk, Radek Poleski, Szymon Kozłowski, Paweł Pietrukowicz, Jan Skowron, Yossi Shvartzvald, Dan Maoz, Shai Kaspi, Matan Friedmann, Virginie Batista, Darren Depoy, Subo Dong, B. Scott Gaudi, Andrew Gould, Cheongho Han, Richard W. Pogge, Thiam Guan Tan, Jennifer C. Yee

School of Physics and Astronomy

Tel Aviv University

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

Abstract

We present the analysis of the planetary microlensing event MOA-2011-BLG-291, which has a mass ratio of q = (3.8 ± 0.7) × 10^-4 and a source star that is redder (or brighter) than the bulge main sequence. This event is located at a low Galactic latitude in the survey area that is currently planned for NASA's Wide Field Infrared Survey Telescope (WFIRST) exoplanet microlensing survey. This unusual color for a microlensed source star implies that we cannot assume that the source star is in the Galactic bulge. The favored interpretation is that the source star is a lower main-sequence star at a distance of D _S = 4.9 ± 1.3 kpc in the Galactic disk. However, the source could also be a turn-off star on the far side of the bulge or a subgiant in the far side of the Galactic disk if it experiences significantly more reddening than the bulge red clump stars. However, these possibilities have only a small effect on our mass estimates for the host star and planet. We find host star and planet masses of and from a Bayesian analysis with a standard Galactic model, under the assumption that the planet hosting probability does not depend on the host mass or distance. However, if we attempt to measure the host and planet masses with host star brightness measurements from high angular resolution follow-up imaging, the implied masses will be sensitive to the host star distance. The WFIRST exoplanet microlensing survey is expected to use this method to determine the masses for many of the planetary systems that it discovers, so this issue has important design implications for the WFIRST exoplanet microlensing survey.

Original language	English
Article number	113
Journal	Astronomical Journal
Volume	156
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/aad59c
State	Published - Sep 2018

Keywords

gravitational lensing: micro
planetary systems

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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https://doi.org/10.3847/1538-3881/aad59c

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Bennett, D. P., Udalski, A., Bond, I. A., Suzuki, D., Ryu, Y. H., Abe, F., Barry, R. K., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., ... Yee, J. C. (2018). A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291. Astronomical Journal, 156(3), Article 113. https://doi.org/10.3847/1538-3881/aad59c

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title = "A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291",

abstract = "We present the analysis of the planetary microlensing event MOA-2011-BLG-291, which has a mass ratio of q = (3.8 ± 0.7) × 10-4 and a source star that is redder (or brighter) than the bulge main sequence. This event is located at a low Galactic latitude in the survey area that is currently planned for NASA's Wide Field Infrared Survey Telescope (WFIRST) exoplanet microlensing survey. This unusual color for a microlensed source star implies that we cannot assume that the source star is in the Galactic bulge. The favored interpretation is that the source star is a lower main-sequence star at a distance of D S = 4.9 ± 1.3 kpc in the Galactic disk. However, the source could also be a turn-off star on the far side of the bulge or a subgiant in the far side of the Galactic disk if it experiences significantly more reddening than the bulge red clump stars. However, these possibilities have only a small effect on our mass estimates for the host star and planet. We find host star and planet masses of and from a Bayesian analysis with a standard Galactic model, under the assumption that the planet hosting probability does not depend on the host mass or distance. However, if we attempt to measure the host and planet masses with host star brightness measurements from high angular resolution follow-up imaging, the implied masses will be sensitive to the host star distance. The WFIRST exoplanet microlensing survey is expected to use this method to determine the masses for many of the planetary systems that it discovers, so this issue has important design implications for the WFIRST exoplanet microlensing survey.",

keywords = "gravitational lensing: micro, planetary systems",

author = "Bennett, {David P.} and Andrzej Udalski and Bond, {Ian A.} and Daisuke Suzuki and Ryu, {Yoon Hyun} and Fumio Abe and Barry, {Richard K.} and Aparna Bhattacharya and Martin Donachie and Akihiko Fukui and Yuki Hirao and Kohei Kawasaki and Iona Kondo and Naoki Koshimoto and Li, {Man Cheung Alex} and Yutaka Matsubara and Shota Miyazaki and Yasushi Muraki and Masayuki Nagakane and Koji Ohnishi and Cl{\'e}ment Ranc and Rattenbury, {Nicholas J.} and Haruno Suematsu and Takahiro Sumi and Tristram, {Paul J.} and Atsunori Yonehara and Szyma{\'n}ski, {Micha{\l} K.} and Igor Soszy{\'n}ski and {\L}ukasz Wyrzykowski and Krzysztof Ulaczyk and Radek Poleski and Szymon Koz{\l}owski and Pawe{\l} Pietrukowicz and Jan Skowron and Yossi Shvartzvald and Dan Maoz and Shai Kaspi and Matan Friedmann and Virginie Batista and Darren Depoy and Subo Dong and Gaudi, {B. Scott} and Andrew Gould and Cheongho Han and Pogge, {Richard W.} and Tan, {Thiam Guan} and Yee, {Jennifer C.}",

year = "2018",

month = sep,

doi = "https://doi.org/10.3847/1538-3881/aad59c",

language = "الإنجليزيّة",

volume = "156",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "3",

}

Bennett, DP, Udalski, A, Bond, IA, Suzuki, D, Ryu, YH, Abe, F, Barry, RK, Bhattacharya, A, Donachie, M, Fukui, A, Hirao, Y, Kawasaki, K, Kondo, I, Koshimoto, N, Li, MCA, Matsubara, Y, Miyazaki, S, Muraki, Y, Nagakane, M, Ohnishi, K, Ranc, C, Rattenbury, NJ, Suematsu, H, Sumi, T, Tristram, PJ, Yonehara, A, Szymański, MK, Soszyński, I, Wyrzykowski, Ł, Ulaczyk, K, Poleski, R, Kozłowski, S, Pietrukowicz, P, Skowron, J, Shvartzvald, Y, Maoz, D, Kaspi, S, Friedmann, M, Batista, V, Depoy, D, Dong, S, Gaudi, BS, Gould, A, Han, C, Pogge, RW, Tan, TG & Yee, JC 2018, 'A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291', Astronomical Journal, vol. 156, no. 3, 113. https://doi.org/10.3847/1538-3881/aad59c

TY - JOUR

T1 - A Planetary Microlensing Event with an Unusually Red Source Star

T2 - MOA-2011-BLG-291

AU - Bennett, David P.

AU - Udalski, Andrzej

AU - Bond, Ian A.

AU - Suzuki, Daisuke

AU - Ryu, Yoon Hyun

AU - Abe, Fumio

AU - Barry, Richard K.

AU - Bhattacharya, Aparna

AU - Donachie, Martin

AU - Fukui, Akihiko

AU - Hirao, Yuki

AU - Kawasaki, Kohei

AU - Kondo, Iona

AU - Koshimoto, Naoki

AU - Li, Man Cheung Alex

AU - Matsubara, Yutaka

AU - Miyazaki, Shota

AU - Muraki, Yasushi

AU - Nagakane, Masayuki

AU - Ohnishi, Koji

AU - Ranc, Clément

AU - Rattenbury, Nicholas J.

AU - Suematsu, Haruno

AU - Sumi, Takahiro

AU - Tristram, Paul J.

AU - Yonehara, Atsunori

AU - Szymański, Michał K.

AU - Soszyński, Igor

AU - Wyrzykowski, Łukasz

AU - Ulaczyk, Krzysztof

AU - Poleski, Radek

AU - Kozłowski, Szymon

AU - Pietrukowicz, Paweł

AU - Skowron, Jan

AU - Shvartzvald, Yossi

AU - Maoz, Dan

AU - Kaspi, Shai

AU - Friedmann, Matan

AU - Batista, Virginie

AU - Depoy, Darren

AU - Dong, Subo

AU - Gaudi, B. Scott

AU - Gould, Andrew

AU - Han, Cheongho

AU - Pogge, Richard W.

AU - Tan, Thiam Guan

AU - Yee, Jennifer C.

PY - 2018/9

Y1 - 2018/9

N2 - We present the analysis of the planetary microlensing event MOA-2011-BLG-291, which has a mass ratio of q = (3.8 ± 0.7) × 10-4 and a source star that is redder (or brighter) than the bulge main sequence. This event is located at a low Galactic latitude in the survey area that is currently planned for NASA's Wide Field Infrared Survey Telescope (WFIRST) exoplanet microlensing survey. This unusual color for a microlensed source star implies that we cannot assume that the source star is in the Galactic bulge. The favored interpretation is that the source star is a lower main-sequence star at a distance of D S = 4.9 ± 1.3 kpc in the Galactic disk. However, the source could also be a turn-off star on the far side of the bulge or a subgiant in the far side of the Galactic disk if it experiences significantly more reddening than the bulge red clump stars. However, these possibilities have only a small effect on our mass estimates for the host star and planet. We find host star and planet masses of and from a Bayesian analysis with a standard Galactic model, under the assumption that the planet hosting probability does not depend on the host mass or distance. However, if we attempt to measure the host and planet masses with host star brightness measurements from high angular resolution follow-up imaging, the implied masses will be sensitive to the host star distance. The WFIRST exoplanet microlensing survey is expected to use this method to determine the masses for many of the planetary systems that it discovers, so this issue has important design implications for the WFIRST exoplanet microlensing survey.

AB - We present the analysis of the planetary microlensing event MOA-2011-BLG-291, which has a mass ratio of q = (3.8 ± 0.7) × 10-4 and a source star that is redder (or brighter) than the bulge main sequence. This event is located at a low Galactic latitude in the survey area that is currently planned for NASA's Wide Field Infrared Survey Telescope (WFIRST) exoplanet microlensing survey. This unusual color for a microlensed source star implies that we cannot assume that the source star is in the Galactic bulge. The favored interpretation is that the source star is a lower main-sequence star at a distance of D S = 4.9 ± 1.3 kpc in the Galactic disk. However, the source could also be a turn-off star on the far side of the bulge or a subgiant in the far side of the Galactic disk if it experiences significantly more reddening than the bulge red clump stars. However, these possibilities have only a small effect on our mass estimates for the host star and planet. We find host star and planet masses of and from a Bayesian analysis with a standard Galactic model, under the assumption that the planet hosting probability does not depend on the host mass or distance. However, if we attempt to measure the host and planet masses with host star brightness measurements from high angular resolution follow-up imaging, the implied masses will be sensitive to the host star distance. The WFIRST exoplanet microlensing survey is expected to use this method to determine the masses for many of the planetary systems that it discovers, so this issue has important design implications for the WFIRST exoplanet microlensing survey.

KW - gravitational lensing: micro

KW - planetary systems

UR - http://www.scopus.com/inward/record.url?scp=85053104598&partnerID=8YFLogxK

U2 - https://doi.org/10.3847/1538-3881/aad59c

DO - https://doi.org/10.3847/1538-3881/aad59c

M3 - مقالة

SN - 0004-6256

VL - 156

JO - Astronomical Journal

JF - Astronomical Journal

IS - 3

M1 - 113

ER -

A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291

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Keywords

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