MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging

N. Koshimoto; Y. Shvartzvald; D. P. Bennett; M. T. Penny; M. Hundertmark; I. A. Bond; W. C. Zang; C. B. Henderson; D. Suzuki; N. J. Rattenbury; T. Sumi; F. Abe; Y. Asakura; A. Bhattacharya; M. Donachie; P. Evans; A. Fukui; Y. Hirao; Y. Itow; M. C. A. Li; C. H. Ling; K. Masuda; Y. Matsubara; T. Matsuo; Y. Muraki; M. Nagakane; K. Ohnishi; C. Ranc; To. Saito; A. Sharan; H. Shibai; D. J. Sullivan; P. J. Tristram; T. Yamada; T. Yamada; A. Yonehara; C. R. Gelino; C. Beichman; J.-P. Beaulieu; J.-B. Marquette; V. Batista; M. Friedmann; N. Hallakoun; S. Kaspi; D. Maoz; G. Bryden; S. Calchi Novati; S. B. Howell; T. S. Wang; S. Mao; P. Fouqué; H. Korhonen; U. G. Jørgensen; R. Street; Y. Tsapras; M. Dominik; E. Kerins; A. Cassan; C. Snodgrass; E. Bachelet; V. Bozza; D. M. Bramich

doi:10.3847/1538-3881/aa72e0

MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging

N. Koshimoto, Y. Shvartzvald, D. P. Bennett, M. T. Penny, M. Hundertmark, I. A. Bond, W. C. Zang, C. B. Henderson, D. Suzuki, N. J. Rattenbury, T. Sumi, F. Abe, Y. Asakura, A. Bhattacharya, M. Donachie, P. Evans, A. Fukui, Y. Hirao, Y. Itow, M. C. A. LiC. H. Ling, K. Masuda, Y. Matsubara, T. Matsuo, Y. Muraki, M. Nagakane, K. Ohnishi, C. Ranc, To. Saito, A. Sharan, H. Shibai, D. J. Sullivan, P. J. Tristram, T. Yamada, T. Yamada, A. Yonehara, C. R. Gelino, C. Beichman, J.-P. Beaulieu, J.-B. Marquette, V. Batista, M. Friedmann, N. Hallakoun, S. Kaspi, D. Maoz, G. Bryden, S. Calchi Novati, S. B. Howell, T. S. Wang, S. Mao, P. Fouqué, H. Korhonen, U. G. Jørgensen, R. Street, Y. Tsapras, M. Dominik, E. Kerins, A. Cassan, C. Snodgrass, E. Bachelet, V. Bozza, D. M. Bramich

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

32 Citations (Scopus)

1 Downloads (Pure)

Abstract

We report the discovery of a microlensing planet — MOA-2016-BLG-227Lb — with a large planet/host mass ratio of q ≃ 9 × 10‑3. This event was located near the K2 Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light-curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light-curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar-type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens–source relative proper motion.

Original language	English
Article number	3
Number of pages	15
Journal	Astronomical Journal
Volume	154
Issue number	1
Early online date	9 Jun 2017
DOIs	https://doi.org/10.3847/1538-3881/aa72e0
Publication status	Published - Jul 2017

Keywords

Gravitational lensing: micro
Planetary systems

Access to Document

10.3847/1538-3881/aa72e0

Koshimoto_2017_AJ_154_3
© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at iopscience.iop.org / https://doi.org/10.3847/1538-3881/aa72e0
Final published version, 1.54 MB

http://adsabs.harvard.edu/abs/2017AJ....154....3K

Cite this

Koshimoto, N., Shvartzvald, Y., Bennett, D. P., Penny, M. T., Hundertmark, M., Bond, I. A., Zang, W. C., Henderson, C. B., Suzuki, D., Rattenbury, N. J., Sumi, T., Abe, F., Asakura, Y., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., ... Bramich, D. M. (2017). MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging. Astronomical Journal, 154(1), Article 3. https://doi.org/10.3847/1538-3881/aa72e0

@article{07e49c51eb3243088ca18925c33c0f04,

title = "MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging",

abstract = "We report the discovery of a microlensing planet — MOA-2016-BLG-227Lb — with a large planet/host mass ratio of q ≃ 9 × 10‑3. This event was located near the K2 Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light-curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light-curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar-type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens–source relative proper motion.",

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

author = "N. Koshimoto and Y. Shvartzvald and Bennett, {D. P.} and Penny, {M. T.} and M. Hundertmark and Bond, {I. A.} and Zang, {W. C.} and Henderson, {C. B.} and D. Suzuki and Rattenbury, {N. J.} and T. Sumi and F. Abe and Y. Asakura and A. Bhattacharya and M. Donachie and P. Evans and A. Fukui and Y. Hirao and Y. Itow and Li, {M. C. A.} and Ling, {C. H.} and K. Masuda and Y. Matsubara and T. Matsuo and Y. Muraki and M. Nagakane and K. Ohnishi and C. Ranc and To. Saito and A. Sharan and H. Shibai and Sullivan, {D. J.} and Tristram, {P. J.} and T. Yamada and T. Yamada and A. Yonehara and Gelino, {C. R.} and C. Beichman and J.-P. Beaulieu and J.-B. Marquette and V. Batista and M. Friedmann and N. Hallakoun and S. Kaspi and D. Maoz and G. Bryden and {Calchi Novati}, S. and Howell, {S. B.} and Wang, {T. S.} and S. Mao and P. Fouqu{\'e} and H. Korhonen and J{\o}rgensen, {U. G.} and R. Street and Y. Tsapras and M. Dominik and E. Kerins and A. Cassan and C. Snodgrass and E. Bachelet and V. Bozza and Bramich, {D. M.}",

year = "2017",

month = jul,

doi = "10.3847/1538-3881/aa72e0",

language = "English",

volume = "154",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "1",

}

Koshimoto, N, Shvartzvald, Y, Bennett, DP, Penny, MT, Hundertmark, M, Bond, IA, Zang, WC, Henderson, CB, Suzuki, D, Rattenbury, NJ, Sumi, T, Abe, F, Asakura, Y, Bhattacharya, A, Donachie, M, Evans, P, Fukui, A, Hirao, Y, Itow, Y, Li, MCA, Ling, CH, Masuda, K, Matsubara, Y, Matsuo, T, Muraki, Y, Nagakane, M, Ohnishi, K, Ranc, C, Saito, T, Sharan, A, Shibai, H, Sullivan, DJ, Tristram, PJ, Yamada, T, Yamada, T, Yonehara, A, Gelino, CR, Beichman, C, Beaulieu, J-P, Marquette, J-B, Batista, V, Friedmann, M, Hallakoun, N, Kaspi, S, Maoz, D, Bryden, G, Calchi Novati, S, Howell, SB, Wang, TS, Mao, S, Fouqué, P, Korhonen, H, Jørgensen, UG, Street, R, Tsapras, Y, Dominik, M, Kerins, E, Cassan, A, Snodgrass, C, Bachelet, E, Bozza, V & Bramich, DM 2017, 'MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging', Astronomical Journal, vol. 154, no. 1, 3. https://doi.org/10.3847/1538-3881/aa72e0

TY - JOUR

T1 - MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging

AU - Koshimoto, N.

AU - Shvartzvald, Y.

AU - Bennett, D. P.

AU - Penny, M. T.

AU - Hundertmark, M.

AU - Bond, I. A.

AU - Zang, W. C.

AU - Henderson, C. B.

AU - Suzuki, D.

AU - Rattenbury, N. J.

AU - Sumi, T.

AU - Abe, F.

AU - Asakura, Y.

AU - Bhattacharya, A.

AU - Donachie, M.

AU - Evans, P.

AU - Fukui, A.

AU - Hirao, Y.

AU - Itow, Y.

AU - Li, M. C. A.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Matsuo, T.

AU - Muraki, Y.

AU - Nagakane, M.

AU - Ohnishi, K.

AU - Ranc, C.

AU - Saito, To.

AU - Sharan, A.

AU - Shibai, H.

AU - Sullivan, D. J.

AU - Tristram, P. J.

AU - Yamada, T.

AU - Yonehara, A.

AU - Gelino, C. R.

AU - Beichman, C.

AU - Beaulieu, J.-P.

AU - Marquette, J.-B.

AU - Batista, V.

AU - Friedmann, M.

AU - Hallakoun, N.

AU - Kaspi, S.

AU - Maoz, D.

AU - Bryden, G.

AU - Calchi Novati, S.

AU - Howell, S. B.

AU - Wang, T. S.

AU - Mao, S.

AU - Fouqué, P.

AU - Korhonen, H.

AU - Jørgensen, U. G.

AU - Street, R.

AU - Tsapras, Y.

AU - Dominik, M.

AU - Kerins, E.

AU - Cassan, A.

AU - Snodgrass, C.

AU - Bachelet, E.

AU - Bozza, V.

AU - Bramich, D. M.

PY - 2017/7

Y1 - 2017/7

N2 - We report the discovery of a microlensing planet — MOA-2016-BLG-227Lb — with a large planet/host mass ratio of q ≃ 9 × 10‑3. This event was located near the K2 Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light-curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light-curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar-type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens–source relative proper motion.

AB - We report the discovery of a microlensing planet — MOA-2016-BLG-227Lb — with a large planet/host mass ratio of q ≃ 9 × 10‑3. This event was located near the K2 Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light-curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light-curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar-type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens–source relative proper motion.

KW - Gravitational lensing: micro

KW - Planetary systems

U2 - 10.3847/1538-3881/aa72e0

DO - 10.3847/1538-3881/aa72e0

M3 - Article

SN - 0004-6256

VL - 154

JO - Astronomical Journal

JF - Astronomical Journal

IS - 1

M1 - 3

ER -

MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging

Abstract

Keywords

Access to Document

Fingerprint

Cite this