The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008)

Y. Tsapras; M. Hundertmark; Ł. Wyrzykowski; Keith Douglas Horne; A. Udalski; C. Snodgrass; R. Street; D. M. Bramich; Martin Dominik; V. Bozza; R. Figuera Jaimes; N. Kains; J. Skowron; M. K. Szymański; G. Pietrzyński; I. Soszyński; K. Ulaczyk; S. Kozłowski; P. Pietrukowicz; R. Poleski

doi:10.1093/mnras/stw023

The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008)

Y. Tsapras, M. Hundertmark, Ł. Wyrzykowski, Keith Douglas Horne, A. Udalski, C. Snodgrass, R. Street, D. M. Bramich, Martin Dominik, V. Bozza, R. Figuera Jaimes, N. Kains, J. Skowron, M. K. Szymański, G. Pietrzyński, I. Soszyński, K. Ulaczyk, S. Kozłowski, P. Pietrukowicz, R. Poleski

School of Physics and Astronomy

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

Abstract

We use six years (2003–2008) of Optical Gravitational Lensing Experiment-III microlensing observations to derive the survey detection efficiency for a range of planetary masses and projected distances from the host star. We perform an independent analysis of the microlensing light curves to extract the event parameters and compute the planet detection probability given the data. 2433 light curves satisfy our quality selection criteria and are retained for further processing. The aggregate of the detection probabilities over the range explored yields the expected number of microlensing planet detections. We employ a Galactic model to convert this distribution from dimensionless to physical units, α/au and M_⊕. The survey sensitivity to small planets is highest in the range 1–4 au, shifting to slightly larger separations for more massive ones.

Original language	English
Pages (from-to)	1320-1331
Number of pages	12
Journal	Monthly Notices of the Royal Astronomical Society
Volume	457
Issue number	2
Early online date	1 Feb 2016
DOIs	https://doi.org/10.1093/mnras/stw023
Publication status	Published - 1 Apr 2016

Keywords

Gravitational lensing: micro
Planetary systems

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10.1093/mnras/stw023

Horne_2016_OGLE-III_MNRAS_FinalPubVersion
© 2016 The Authors. 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/10.1093/mnras/stw023
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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018
Jardine, M. M. (PI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Horne, K. D. (CoI) & Wood, K. (CoI)
Science & Technology Facilities Council
1/04/15 → 31/03/18
Project: Standard

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Tsapras, Y., Hundertmark, M., Wyrzykowski, Ł., Horne, K. D., Udalski, A., Snodgrass, C., Street, R., Bramich, D. M., Dominik, M., Bozza, V., Figuera Jaimes, R., Kains, N., Skowron, J., Szymański, M. K., Pietrzyński, G., Soszyński, I., Ulaczyk, K., Kozłowski, S., Pietrukowicz, P., & Poleski, R. (2016). The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008). Monthly Notices of the Royal Astronomical Society, 457(2), 1320-1331. https://doi.org/10.1093/mnras/stw023

@article{a046962a6b5e4655a48eae817e920304,

title = "The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008)",

abstract = "We use six years (2003–2008) of Optical Gravitational Lensing Experiment-III microlensing observations to derive the survey detection efficiency for a range of planetary masses and projected distances from the host star. We perform an independent analysis of the microlensing light curves to extract the event parameters and compute the planet detection probability given the data. 2433 light curves satisfy our quality selection criteria and are retained for further processing. The aggregate of the detection probabilities over the range explored yields the expected number of microlensing planet detections. We employ a Galactic model to convert this distribution from dimensionless to physical units, α/au and M⊕. The survey sensitivity to small planets is highest in the range 1–4 au, shifting to slightly larger separations for more massive ones.",

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

author = "Y. Tsapras and M. Hundertmark and {\L}. Wyrzykowski and Horne, {Keith Douglas} and A. Udalski and C. Snodgrass and R. Street and Bramich, {D. M.} and Martin Dominik and V. Bozza and {Figuera Jaimes}, R. and N. Kains and J. Skowron and Szyma{\'n}ski, {M. K.} and G. Pietrzy{\'n}ski and I. Soszy{\'n}ski and K. Ulaczyk and S. Koz{\l}owski and P. Pietrukowicz and R. Poleski",

note = "KH, DB, MD and MH are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of Qatar Foundation). KH acknowledges support from STFC grant ST/M001296/1. NK acknowledges an ESO Fellowship. The research leading to these results has received funding from the European Community{\textquoteright}s Seventh Framework Programme (/FP7/2007-2013/) under grant agreement no. 229517. This publication was made possible by NPRP grant no. X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). CS received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 268421.",

year = "2016",

month = apr,

day = "1",

doi = "10.1093/mnras/stw023",

language = "English",

volume = "457",

pages = "1320--1331",

journal = "Monthly Notices of the Royal Astronomical Society",

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Tsapras, Y, Hundertmark, M, Wyrzykowski, Ł, Horne, KD, Udalski, A, Snodgrass, C, Street, R, Bramich, DM, Dominik, M, Bozza, V, Figuera Jaimes, R, Kains, N, Skowron, J, Szymański, MK, Pietrzyński, G, Soszyński, I, Ulaczyk, K, Kozłowski, S, Pietrukowicz, P & Poleski, R 2016, 'The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008)', Monthly Notices of the Royal Astronomical Society, vol. 457, no. 2, pp. 1320-1331. https://doi.org/10.1093/mnras/stw023

TY - JOUR

T1 - The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008)

AU - Tsapras, Y.

AU - Hundertmark, M.

AU - Wyrzykowski, Ł.

AU - Horne, Keith Douglas

AU - Udalski, A.

AU - Snodgrass, C.

AU - Street, R.

AU - Bramich, D. M.

AU - Dominik, Martin

AU - Bozza, V.

AU - Figuera Jaimes, R.

AU - Kains, N.

AU - Skowron, J.

AU - Szymański, M. K.

AU - Pietrzyński, G.

AU - Soszyński, I.

AU - Ulaczyk, K.

AU - Kozłowski, S.

AU - Pietrukowicz, P.

AU - Poleski, R.

N1 - KH, DB, MD and MH are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of Qatar Foundation). KH acknowledges support from STFC grant ST/M001296/1. NK acknowledges an ESO Fellowship. The research leading to these results has received funding from the European Community’s Seventh Framework Programme (/FP7/2007-2013/) under grant agreement no. 229517. This publication was made possible by NPRP grant no. X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). CS received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 268421.

PY - 2016/4/1

Y1 - 2016/4/1

N2 - We use six years (2003–2008) of Optical Gravitational Lensing Experiment-III microlensing observations to derive the survey detection efficiency for a range of planetary masses and projected distances from the host star. We perform an independent analysis of the microlensing light curves to extract the event parameters and compute the planet detection probability given the data. 2433 light curves satisfy our quality selection criteria and are retained for further processing. The aggregate of the detection probabilities over the range explored yields the expected number of microlensing planet detections. We employ a Galactic model to convert this distribution from dimensionless to physical units, α/au and M⊕. The survey sensitivity to small planets is highest in the range 1–4 au, shifting to slightly larger separations for more massive ones.

AB - We use six years (2003–2008) of Optical Gravitational Lensing Experiment-III microlensing observations to derive the survey detection efficiency for a range of planetary masses and projected distances from the host star. We perform an independent analysis of the microlensing light curves to extract the event parameters and compute the planet detection probability given the data. 2433 light curves satisfy our quality selection criteria and are retained for further processing. The aggregate of the detection probabilities over the range explored yields the expected number of microlensing planet detections. We employ a Galactic model to convert this distribution from dimensionless to physical units, α/au and M⊕. The survey sensitivity to small planets is highest in the range 1–4 au, shifting to slightly larger separations for more massive ones.

KW - Gravitational lensing: micro

KW - Planetary systems

U2 - 10.1093/mnras/stw023

DO - 10.1093/mnras/stw023

M3 - Article

SN - 0035-8711

VL - 457

SP - 1320

EP - 1331

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008)

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Keywords

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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018

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