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2010MNRAS.403..731G - Mon. Not. R. Astron. Soc., 403, 731-747 (2010/April-1)
A bayesian periodogram finds evidence for three planets in 47UrsaeMajoris.
GREGORY P.C. and FISCHER D.A.
Abstract (from CDS):
The measured periods are 1078±2d, 2391+100–87d and 14002+4018–5095d, and the corresponding eccentricities are 0.032 ±0.014,0.098+.047–.096 and 0.16+.09–.16. The results favour low-eccentricity orbits for all three. Assuming the three signals (each one consistent with a Keplerian orbit) are caused by planets, the corresponding limits on planetary mass (M sini) and semimajor axis are (2.53+.07–.06MJ,2.10 ±0.02au), (0.54±0.07 MJ,3.6±0.1au) and (1.6+0.3–0.5MJ,11.6+2.1–2.9au), respectively. Based on a three-planet model, the remaining unaccounted for noise (stellar jitter) is 5.7 m/s.
The velocities of model fit residuals were randomized in multiple trials and processed using a one-planet version of the HMCMC Kepler periodogram. In this situation, periodogram peaks are purely the result of the effective noise. The orbits corresponding to these noise-induced periodogram peaks exhibit a well-defined strong statistical bias towards high eccentricity. We have characterized this eccentricity bias and designed a correction filter that can be used as an alternate prior for eccentricity to enhance the detection of planetary orbits of low or moderate eccentricity.
Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS
Journal keyword(s): methods: numerical - methods: statistical - techniques: radial velocities - stars: individual: 47 Ursae Majoris - planetary systems
Simbad objects: 7
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