52,463 research outputs found
Internet Service Provider Liability for Contributory Trademark Infringement After Gucci
[I]f a manufacturer or distributor intentionally induces another to infringe a trademark, or if it continues to supply its product to one whom it knows or has reason to know is engaging in trademark infringement, the manufacturer or distributor is contributorially responsible for any harm done as a result of the deceit
A Bayesian analysis of extrasolar planet data for HD 208487
Precision radial velocity data for HD 208487 has been re-analyzed using a new
Bayesian multi-planet Kepler periodogram. The periodgram employs a parallel
tempering Markov chain Monte Carlo algorithm with a novel statistical control
system. We confirm the previously reported orbit (Tinney et al. 2005) of 130
days. In addition, we conclude there is strong evidence for a second planet
with a period of 998 -62 +57 days, an eccentricity of 0.19 -0.18 +0.05, and an
M sin i = 0.46 -0.13 +0.05 of Jupiter's mass.Comment: For publication in ``Bayesian Inference and Maximum Entropy
Methods'', San Jose 2005, K. H. Knuth, A. E. Abbas, R. D. Morris, J. P.
Castle (eds.), AIP Conference Proceedin
A Bayesian periodogram finds evidence for three planets in HD 11964
A Bayesian multi-planet Kepler periodogram has been developed for the
analysis of precision radial velocity data (Gregory 2005b and 2007). The
periodogram employs a parallel tempering Markov chain Monte Carlo algorithm.
The HD 11964 data (Butler et al. 2006) has been re-analyzed using 1, 2, 3 and 4
planet models. Assuming that all the models are equally probable a priori, the
three planet model is found to be >= 600 times more probable than the next most
probable model which is a two planet model. The most probable model exhibits
three periods of 38.02+0.06-0.05, 360+-4 and 1924+44-43 d, and eccentricities
of 0.22+0.11-0.22, 0.63+0.34-0.17 and 0.05+0.03-0.05, respectively. Assuming
the three signals (each one consistent with a Keplerian orbit) are caused by
planets, the corresponding limits on planetary mass (M sin i) and semi-major
axis are 0.090+0.15-0.14 M_J, 0.253+-0.009 au, 0.21+0.06-0.07 M_J, 1.13+-0.04
au, 0.77+-0.08 M_J, 3.46+-0.13 au, respectively. The small difference (1.3
sigma) between the 360 day period and one year suggests that it might be worth
investigating the barycentric correction for the HD 11964 data
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