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MOA-2010-BLG-523: “FAILED PLANET” = RS CVn STAR
Gould, A.,Yee, J. C.,Bond, I. A.,Udalski, A.,Han, C.,Jørgensen, U. G.,Greenhill, J.,Tsapras, Y.,Pinsonneault, M. H.,Bensby, T.,Allen, W.,Almeida, L. A.,Bos, M.,Christie, G. W.,DePoy, D. L.,Dong, Subo IOP Publishing 2013 The Astrophysical journal Vol.763 No.2
<P>The Galactic bulge source MOA-2010-BLG-523S exhibited short-term deviations from a standard microlensing light curve near the peak of an A(max) similar to 265 high-magnification microlensing event. The deviations originally seemed consistent with expectations for a planetary companion to the principal lens. We combine long-term photometric monitoring with a previously published high-resolution spectrum taken near peak to demonstrate that this is an RS CVn variable, so that planetary microlensing is not required to explain the light-curve deviations. This is the first spectroscopically confirmed RS CVn star discovered in the Galactic bulge.</P>
THE FIRST NEPTUNE ANALOG OR SUPER-EARTH WITH A NEPTUNE-LIKE ORBIT: MOA-2013-BLG-605LB
Sumi, T.,Udalski, A.,Bennett, D. P.,Gould, A.,Poleski, R.,Bond, I. A.,Skowron, J.,Rattenbury, N.,Pogge, R. W.,Bensby, T.,Beaulieu, J. P.,Marquette, J. B.,Batista, V.,Brillant, S.,Abe, F.,Asakura, Y.,B American Astronomical Society 2016 The Astrophysical journal Vol.825 No.2
<P>We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA-2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 similar to 14 times the expected position of the snow line, a(snow), which is similar to Neptune's separation of 11 a(snow) from the Sun. The planet/host-star mass ratio is q = (3.6 +/- 0.7) x 10(-4) and the projected separation normalized by the Einstein radius is s = 2.39 +/- 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate 'the wide degeneracy.' The three models have (i) a Neptune-mass planet with a mass of M-p = 21(-7)(+6)M(circle plus) orbiting a low-mass M-dwarf with a mass of M-h = 0.19(-0.06)(+0.05)M(circle dot), (ii) a mini-Neptune with M-p = 7.9(-1.2)(+1.8)M(circle plus) orbiting a brown dwarf host with M-h = 0.068(-0.011)(+0.019)M(circle dot), and (iii) a super-Earth with M-p = 3.2(-0.3)(+0.5)M(circle plus) orbiting a low-mass brown dwarf host with M-h = 0.025(-0.004)(+0.005)M(circle dot), which is slightly favored. The 3D planet-host separations are 4.6(-1.2)(+4.7) au, 2.1(-0.2) (+1.0) au, and 0.94(-0.02)(+0.67) au, which are 8.9(-1.4)(+10.5), 12(-1)(+7), or 14(-1)(+11) times larger than a(snow) for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems.</P>