We report the results of the statistical analysis of planetary signals discovered in MOA-II microlensing survey alert system events from 2007 to 2012.Recent studies (Clanton & Gaudi 2014a,b;Montet et al. 2014) have compared the exoplanet distribution found by microlensing with the results of RV observations of M-dwarfs and found that the results from both methods are consistent, although the radial velocity is only sensitive to planets of Jupiter-mass or greater beyond the snow line.1 They used 13 high magnification events from 4-years of observations. 2 They used 199 events from 6-years of observations.

As part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project, we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotating early-type galaxy NGC4697. This estimate is based on Atacama Large Millimeter/submillimeter Array (ALMA) cycle-3 observations of the 12 CO(2-1) emission line with a linear resolution of 29 pc (0. 53). We find that NGC4697 hosts a small relaxed central molecular gas disc with a mass of 1.6×10 7 M , co-spatial with the obscuring dust disc visible in optical Hubble Space Telescope (HST) imaging. We also resolve thermal 1 mm continuum emission from the dust in this disc. NGC4697 is found to have a very low molecular gas velocity dispersion, σ gas =1.65 +0.68 −0.65 km s −1 . This seems to be partially because the giant molecular cloud mass function is not fully sampled, but other mechanisms such as chemical differentiation in a hard radiation field or morphological quenching also seem to be required. We detect a Keplerian increase of the rotation of the molecular gas in the very centre of NGC4697, and use forward modelling of the ALMA data cube in a Bayesian framework with the KIN-EMATIC MOLECULAR SIMULATION (KINMS) code to estimate a SMBH mass of (1.3 +0.18 −0.17 ) ×10 8 M and an i-band mass-to-light ratio of 2.14 +0.04 −0.05 M /L (at the 99% confidence level). Our estimate of the SMBH mass is entirely consistent with previous measurements from stellar kinematics. This increases confidence in the growing number of SMBH mass estimates being obtained in the ALMA era.

As part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotating early-type galaxy NGC4429, that is barred and has a boxy/peanut-shaped bulge. This estimate is based on Atacama Large Millimeter/submillimeter Array (ALMA) cycle-2 observations of the 12 CO(3-2) emission line with a linear resolution of ≈13 pc (0. 18 × 0. 14). NGC4429 has a relaxed, flocculent nuclear disc of molecular gas that is truncated at small radii, likely due to the combined effects of gas stability and tidal shear. The warm/dense 12 CO(3-2) emitting gas is confined to the inner parts of this disc, likely again because the gas becomes more stable at larger radii, preventing star formation. The gas disc has a low velocity dispersion of 2.2 +0.68 −0.65 km s −1 . Despite the inner truncation of the gas disc, we are able to model the kinematics of the gas and estimate a mass of (1.5±0.1 +0.15 −0.35 ) ×10 8 M for the SMBH in NGC4429 (where the quoted uncertainties reflect the random and systematic uncertainties, respectively), consistent with a previous upper limit set using ionised gas kinematics. We confirm that the V-band mass-to-light ratio changes by ≈30% within the inner 400 pc of NGC4429, as suggested by other authors. This SMBH mass measurement based on molecular gas kinematics, the sixth presented in the literature, once again demonstrates the power of ALMA to constrain SMBH masses.