Data sets

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Some data sets for consideration by the working group:

HD88133.txt (Fischer et al. 2005 ApJ 620: 481-486)

n=17 observations. This star's orbit has an MLE of eccentricity of approximately 0.

HD46375.txt (Marcy, Butler & Vogt 2000 ApJ 536, L43-46)

n=24 observations. This star's orbit has an MLE of eccentricity of approximately 0.04.

HD73526.txt (Tinney et al. 2003, ApJ 587, 423)

n=18 observations. The published period was P=190 days. Gregory proposed that two other periods worth considering were P=128 days and P=376 days. Using a parallel tempering algorithm he estimated the Bayes factors of these three respective periods to be in the ratio 22:60:600.

HD3651.txt (Fischer et al. 2003, ApJ 590:1081-1087)

n=138 observations of this star at two observatories. It has a medium-length period orbit (P=62.23 days) and a high eccentricity (e=0.63).

HD222582.txt (Vogt et al. 2000, ApJ 536:902-914)

n=24 observations. This star has a rather long-period orbit (P=572 days) and a high eccentricity (e=0.76).

HD30177.txt, HD30177_truncated.txt (Tinney et al. 2003, ApJ 587:423-428)

n=15 observations. This star has a long period (P=2820 days=7.7 years) and a modest eccentricity (e=0.3). The truncated data set contains only the first 13 observations and may be useful to the working group for studying long period orbits.

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Multi-planet systems:

HD37124.txt, Vogt et al. 2005, ApJ, 632:638-658

n=52 observations. This is relatively "hard" but still non-interacting three-planet system.

HD217107.txt, Vogt et al. 2005, ApJ, 632:638-658

n=63 observations from three observatories. This is an "easy" two-planet system.

HD190360.txt, Vogt et al. 2005, ApJ, 632:638-658

n=84 observations. This system has a second planet with a relatively small signal-to-noise ratio.

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