Abstract
Abstract We propose a new parameterization of the impact parameter u 0 and impact angle α for microlensing systems composed by an Earth-like exoplanet around a solar-mass star at 1 au. We present the caustic topology of such system, as well as the related light curves generated by using such a new parameterization. Based on the same density of points and accuracy of regular methods, we obtain results five times faster for discovering Earth-like exoplanets. In this big data revolution of photometric astronomy, our method will impact future missions like WFIRST (NASA) and Euclid (ESA) and their data pipelines, providing a rapid and deep detection of exoplanets for this specific class of microlensing event that might otherwise be lost.
Highlights
INTRODUCTIONThe surveys Microlensing Planet Search (MPS) (Rhie 1999) and Microlensing Observations in Astrophysics (MOA) (Rhie et al 2000; Sumi et al 2003) demonstrated for the first time that microlensing technique is sensitive enough to detect earth-mass exoplanets
From the observational side, the surveys Microlensing Planet Search (MPS) (Rhie 1999) and Microlensing Observations in Astrophysics (MOA) (Rhie et al 2000; Sumi et al 2003) demonstrated for the first time that microlensing technique is sensitive enough to detect earth-mass exoplanets.Shvartzvald et al (2017) show the possibility to detect Earth-mass Planet in a 1 AU Orbit around an Ultracool de Almeida and do Nascimento Jr.Dwarf and Yee et al (2009) present an extreme magnification microlensing event and its sensitivity to planets with masses as small as 0.2M⊕ 2MMars with projected separations near the Einstein ring ( 3 AU). Gould et al (2014) even showed the capability of microlensing technique to discover Earth-mass planets around 1 AU in binary systems
As discussed by Albrow et al (2001); Gaudi et al (2002), more than 77% of exoplanetary systems discovered with microlensing techniques shows planets with masses lower than Jupiter mass and with semimajor axis between 1.5 and 4 AU
Summary
The surveys Microlensing Planet Search (MPS) (Rhie 1999) and Microlensing Observations in Astrophysics (MOA) (Rhie et al 2000; Sumi et al 2003) demonstrated for the first time that microlensing technique is sensitive enough to detect earth-mass exoplanets. As discussed by Albrow et al (2001); Gaudi et al (2002), more than 77% of exoplanetary systems discovered with microlensing techniques shows planets with masses lower than Jupiter mass and with semimajor axis between 1.5 and 4 AU These results are consistent with the fact that massive planets far away from their central stars are easier to be detected with microlensing method (Sumi et al 2006; Han 2006). In this study we propose a parametrization of the source’s path to force it to cross the Caustic Region Of INterest (CROIN by Penny 2014) This offers an advantage for detecting Earth-like planets around Solarlike stars during microlensing events.
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