Microlensing Surveys for Exoplanets

By B. Gaudi. 2012

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The Habitability of Planets Orbiting M-dwarf Stars (2016, methodology): “…(RV) methods, transit detection missions such as NASA’s Kepler mission (Borucki et al., 2006) and the K2 mission—an ecliptic plane survey that re-purposes the Kepler spacecraft following the loss of two of its reaction wheels (Howell et al., 2014)—and gravitational microlensing (Gaudi, 2012).”
Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates (2018, background): “For stars along the line of sight to the Galactic bulge (where the microlensing event rate is highest) the physical Einstein radius is typically 2–3 AU (see, e.g., the review of Gaudi 2012).”
The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths (2012, background): “…factors invoked to form Jupiter (e.g., Lissauer et al. 2009) and Uranus and Neptune (e.g., Goldreich et al. 2004), and for an observational view, see the microlensing surveys which report order-unity occurrence rates for super-Earths and gas giants from 0.5–10 AU (Gaudi 2012, his section 6.2).”
Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report (2015, methodology): “The WFIRST-AFTA Microlensing Survey 2.4.2.5 The microlensing technique for discovering exoplanets, illustrated in Figure 2-28, is well developed and mature (Gaudi 2012).”