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A Gap in the Mass Distribution for Warm Neptune and Terrestrial Planets

  • Authors: David J. Armstrong, Farzana Meru, Daniel Bayliss, Grant M. Kennedy, and Dimitri Veras

2019 The Astrophysical Journal Letters 880 L1.

  • Provider: AAS Journals

Caption: Figure 1.

Left: planets with measured Mp or ﹩{M}_{{\rm{p}}}\sin (i)﹩, using ﹩\sin (i)=\pi /4﹩. Planets with measured inclination (P1 sample) are colored according to discovery method: purple—Kepler, red—K2, green—TESS, black—radial velocity surveys, cyan—mostly ground-based photometric surveys. Circular points denote radial velocity derived masses, triangular points masses from transit timing variations. Points without measured inclination (P2 sample) are gray. The gap is shown by a dashed line. Right: histogram for our P2 (green) and P1 (purple) samples taken on the gradient of the dashed line, limited to planets within 20M. Bins are 3M wide. Data points are shown with a random vertical distribution within the histogram bars.

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