The OGLE-III planet detection efficiency from six years of microlensing observations (2003 to 2008)
We use six years (2003 to 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 extra...
Gespeichert in:
| 1. Verfasser: | |
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| Dokumenttyp: | Article (Journal) Kapitel/Artikel |
| Sprache: | Englisch |
| Veröffentlicht: |
Oct 2015
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| In: |
Arxiv
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| Online-Zugang: | Verlag, kostenfrei, Volltext: http://arxiv.org/abs/1602.02519
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| Verfasserangaben: | Y. Tsapras, M. Hundertmark, Ł Wyrzykowski, K. Horne, A. Udalski and C. Snodgrass, R. Street, D.M. Bramich, M. 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 |
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| 245 | 1 | 4 | |a The OGLE-III planet detection efficiency from six years of microlensing observations (2003 to 2008) |c Y. Tsapras, M. Hundertmark, Ł Wyrzykowski, K. Horne, A. Udalski and C. Snodgrass, R. Street, D.M. Bramich, M. 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 |
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| 520 | |a We use six years (2003 to 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, \alpha/au and M_E. The survey sensitivity to small planets is highest in the range 1 to 4 au, shifting to slightly larger separations for more massive ones. | ||
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