MOA-2011-BLG-028Lb: a Neptune-mass microlensing planet in the Galactic bulge

J. Skowron; A. Udalski; R. Poleski; S. Kozłowski; M. K. Szymański; Ł. Wyrzykowski; K. Ulaczyk; P. Pietrukowicz; G. Pietrzyński; I. Soszyński; F. Abe; D. P. Bennett; A. Bhattacharya; I. A. Bond; M. Freeman; A. Fukui; Y. Hirao; Y. Itow; N. Koshimoto; C. H. Ling; K. Masuda; Y. Matsubara; Y. Muraki; M. Nagakane; K. Ohnishi; N. Rattenbury; To Saito; D. J. Sullivan; T. Sumi; D. Suzuki; P. J. Tristram; A. Yonehara; Martin Dominik; U. G. Jørgensen; V. Bozza; K. Harpsøe; M. Hundertmark; J. Skottfelt

doi:10.3847/0004-637X/820/1/4

MOA-2011-BLG-028Lb: a Neptune-mass microlensing planet in the Galactic bulge

J. Skowron, A. Udalski, R. Poleski, S. Kozłowski, M. K. Szymański, Ł. Wyrzykowski, K. Ulaczyk, P. Pietrukowicz, G. Pietrzyński, I. Soszyński, F. Abe, D. P. Bennett, A. Bhattacharya, I. A. Bond, M. Freeman, A. Fukui, Y. Hirao, Y. Itow, N. Koshimoto, C. H. LingK. Masuda, Y. Matsubara, Y. Muraki, M. Nagakane, K. Ohnishi, N. Rattenbury, To Saito, D. J. Sullivan, T. Sumi, D. Suzuki, P. J. Tristram, A. Yonehara, Martin Dominik, U. G. Jørgensen, V. Bozza, K. Harpsøe, M. Hundertmark, J. Skottfelt

School of Physics and Astronomy

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Abstract

We present the discovery of a Neptune-mass planet orbiting a star 0.8 ± 0.3M in the Galactic bulge. The planet manifested itself during the microlensing event MOA-2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens star. The analysis of the light curve provides the measurement of the mass ratio (1.2 ± 0.2) × 10^-4 , which indicates that the mass of the planet is 12–60 Earth masses. The lensing system is located at 7.3 ± 0.7 kpc away from the Earth near the direction of Baade's Window. The projected separation of the planet at the time of the microlensing event was 3.1–5.2 au. Although the microlens parallax effect is not detected in the light curve of this event, preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.

Original language	English
Article number	4
Number of pages	13
Journal	Astrophysical Journal
Volume	820
Issue number	1
DOIs	https://doi.org/10.3847/0004-637X/820/1/4
Publication status	Published - 10 Mar 2016

Keywords

Gravitational lensing: micro
Planetary systems

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10.3847/0004-637X/820/1/4

Dominik_2016_Neptune-massMicrolensingPlanet_AJ_FinalPubVersion
© 2016. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.3847/0004-637X/820/1/4
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Skowron, J., Udalski, A., Poleski, R., Kozłowski, S., Szymański, M. K., Wyrzykowski, Ł., Ulaczyk, K., Pietrukowicz, P., Pietrzyński, G., Soszyński, I., Abe, F., Bennett, D. P., Bhattacharya, A., Bond, I. A., Freeman, M., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., ... Skottfelt, J. (2016). MOA-2011-BLG-028Lb: a Neptune-mass microlensing planet in the Galactic bulge. Astrophysical Journal, 820(1), Article 4. https://doi.org/10.3847/0004-637X/820/1/4

@article{9b6ba756977046c489824968015e7406,

title = "MOA-2011-BLG-028Lb: a Neptune-mass microlensing planet in the Galactic bulge",

abstract = "We present the discovery of a Neptune-mass planet orbiting a star 0.8 ± 0.3M in the Galactic bulge. The planet manifested itself during the microlensing event MOA-2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens star. The analysis of the light curve provides the measurement of the mass ratio (1.2 ± 0.2) × 10-4 , which indicates that the mass of the planet is 12–60 Earth masses. The lensing system is located at 7.3 ± 0.7 kpc away from the Earth near the direction of Baade's Window. The projected separation of the planet at the time of the microlensing event was 3.1–5.2 au. Although the microlens parallax effect is not detected in the light curve of this event, preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.",

keywords = "Gravitational lensing: micro, Planetary systems",

author = "J. Skowron and A. Udalski and R. Poleski and S. Koz{\l}owski and Szyma{\'n}ski, {M. K.} and {\L}. Wyrzykowski and K. Ulaczyk and P. Pietrukowicz and G. Pietrzy{\'n}ski and I. Soszy{\'n}ski and F. Abe and Bennett, {D. P.} and A. Bhattacharya and Bond, {I. A.} and M. Freeman and A. Fukui and Y. Hirao and Y. Itow and N. Koshimoto and Ling, {C. H.} and K. Masuda and Y. Matsubara and Y. Muraki and M. Nagakane and K. Ohnishi and N. Rattenbury and To Saito and Sullivan, {D. J.} and T. Sumi and D. Suzuki and Tristram, {P. J.} and A. Yonehara and Martin Dominik and J{\o}rgensen, {U. G.} and V. Bozza and K. Harps{\o}e and M. Hundertmark and J. Skottfelt",

note = "The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U.. J.S. was partially supported by the Space Exploration Research Fund of The Ohio State University. This research was partly supported by the Polish Ministry of Science and Higher Education (MNiSW) through the program {"}Iuventus Plus{"} award No. IP2011 026771. We thank Prof. M. Kubiak for contributing observations to this work as the OGLE Project member. T.S. acknowledges the financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by the grants JSPS25103508 and 23340064.",

year = "2016",

month = mar,

day = "10",

doi = "10.3847/0004-637X/820/1/4",

language = "English",

volume = "820",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

}

Skowron, J, Udalski, A, Poleski, R, Kozłowski, S, Szymański, MK, Wyrzykowski, Ł, Ulaczyk, K, Pietrukowicz, P, Pietrzyński, G, Soszyński, I, Abe, F, Bennett, DP, Bhattacharya, A, Bond, IA, Freeman, M, Fukui, A, Hirao, Y, Itow, Y, Koshimoto, N, Ling, CH, Masuda, K, Matsubara, Y, Muraki, Y, Nagakane, M, Ohnishi, K, Rattenbury, N, Saito, T, Sullivan, DJ, Sumi, T, Suzuki, D, Tristram, PJ, Yonehara, A, Dominik, M, Jørgensen, UG, Bozza, V, Harpsøe, K, Hundertmark, M & Skottfelt, J 2016, 'MOA-2011-BLG-028Lb: a Neptune-mass microlensing planet in the Galactic bulge', Astrophysical Journal, vol. 820, no. 1, 4. https://doi.org/10.3847/0004-637X/820/1/4

TY - JOUR

T1 - MOA-2011-BLG-028Lb

T2 - a Neptune-mass microlensing planet in the Galactic bulge

AU - Skowron, J.

AU - Udalski, A.

AU - Poleski, R.

AU - Kozłowski, S.

AU - Szymański, M. K.

AU - Wyrzykowski, Ł.

AU - Ulaczyk, K.

AU - Pietrukowicz, P.

AU - Pietrzyński, G.

AU - Soszyński, I.

AU - Abe, F.

AU - Bennett, D. P.

AU - Bhattacharya, A.

AU - Bond, I. A.

AU - Freeman, M.

AU - Fukui, A.

AU - Hirao, Y.

AU - Itow, Y.

AU - Koshimoto, N.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Muraki, Y.

AU - Nagakane, M.

AU - Ohnishi, K.

AU - Rattenbury, N.

AU - Saito, To

AU - Sullivan, D. J.

AU - Sumi, T.

AU - Suzuki, D.

AU - Tristram, P. J.

AU - Yonehara, A.

AU - Dominik, Martin

AU - Jørgensen, U. G.

AU - Bozza, V.

AU - Harpsøe, K.

AU - Hundertmark, M.

AU - Skottfelt, J.

N1 - The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U.. J.S. was partially supported by the Space Exploration Research Fund of The Ohio State University. This research was partly supported by the Polish Ministry of Science and Higher Education (MNiSW) through the program "Iuventus Plus" award No. IP2011 026771. We thank Prof. M. Kubiak for contributing observations to this work as the OGLE Project member. T.S. acknowledges the financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by the grants JSPS25103508 and 23340064.

PY - 2016/3/10

Y1 - 2016/3/10

N2 - We present the discovery of a Neptune-mass planet orbiting a star 0.8 ± 0.3M in the Galactic bulge. The planet manifested itself during the microlensing event MOA-2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens star. The analysis of the light curve provides the measurement of the mass ratio (1.2 ± 0.2) × 10-4 , which indicates that the mass of the planet is 12–60 Earth masses. The lensing system is located at 7.3 ± 0.7 kpc away from the Earth near the direction of Baade's Window. The projected separation of the planet at the time of the microlensing event was 3.1–5.2 au. Although the microlens parallax effect is not detected in the light curve of this event, preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.

AB - We present the discovery of a Neptune-mass planet orbiting a star 0.8 ± 0.3M in the Galactic bulge. The planet manifested itself during the microlensing event MOA-2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens star. The analysis of the light curve provides the measurement of the mass ratio (1.2 ± 0.2) × 10-4 , which indicates that the mass of the planet is 12–60 Earth masses. The lensing system is located at 7.3 ± 0.7 kpc away from the Earth near the direction of Baade's Window. The projected separation of the planet at the time of the microlensing event was 3.1–5.2 au. Although the microlens parallax effect is not detected in the light curve of this event, preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.

KW - Gravitational lensing: micro

KW - Planetary systems

U2 - 10.3847/0004-637X/820/1/4

DO - 10.3847/0004-637X/820/1/4

M3 - Article

AN - SCOPUS:84962246343

SN - 0004-637X

VL - 820

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 4

ER -

MOA-2011-BLG-028Lb: a Neptune-mass microlensing planet in the Galactic bulge

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