Title: 18 Delphini
Content:  On February 19, 2008, an extrasolar planet was found to be orbiting the star with a period of 993.3 days and a mild eccentricity (ovalness) of 0.08. The mass of this exoplanet is greater than 10 times the mass of Jupiter.
Title: HD 59686
Content:  In November 2003, a planet was announced orbiting the giant star. A doppler spectrometer was used to look for effects on the star caused by the gravitational tug of the orbiting planet. Using the amplitude from the radial velocity method, he calculated the planetary mass as 5.25 Jupiter masses and with period 303 days. However that mass is only a minimum because the inclination of the orbit is not known. Using the stellar mass and period, he calculated the semimajor axis as 0.911 astronomical units. He found that the shape of the stellar wobble is circular, implying that the planet has zero eccentricity.
Title: HD 189733 b
Content:  On October 6, 2005, a team of astronomers announced the discovery of transiting planet HD 189733 b. The planet was then detected using Doppler spectroscopy. Real-time radial velocity measurements detected the Rossiter–McLaughlin effect caused by the planet passing in front of its star before photometric measurements confirmed that the planet was transiting. In 2006, a team led by Drake Deming announced detection of strong infrared thermal emission from the transiting exoplanet planet HD 189733 b, by measuring the flux decrement (decrease of total light) during its prominent secondary eclipse (when the planet passes behind the star). The mass of the planet is estimated to be 13% larger than Jupiter's, with the planet completing an orbit around its host star every 2.2 days and an orbital speed of 152.5 km/s.
Title: Omega Serpentis
Content:  Observations made between 2001–2003 by the Okayama Planet Search Program showed that Omega Serpentis is undergoing periodic radial velocity variations with a preliminary period estimate of 312.3 days. Following this announcement in 2005, further observations were performed that were best explained by a planet following a Keplerian orbit, resulting in confirmation of planet existence in 2013. This companion has an estimated orbital period of 277 days, a semimajor axis of 1.1 AU, and an eccentricity of 0.1. Since the inclination of the orbit is unknown, only a lower bound on the mass of the planet can be determined. The object has at least 170% the mass of Jupiter. However, these values for the semimajor axis and planetary mass are based on an adopted stellar mass of 2.17 times the mass of the Sun. More recent results by Jofré et al. (2015) give a lower stellar mass estimate of 1.20 solar masses.
Title: HD 117618
Content:  In 2005, the Anglo-Australian Planet Search program announced the discovery of a low-mass planet in orbit around HD 117618. This object was found through measurements of radial velocity variation, which were larger than those produced by the intrinsic jitter of the host star. The best Keplerian fit to the data gave a periodicity of 25.8 days with an eccentricity of around 0.37 and a semimajor axis of 0.17 AU. The lower bound on the object's mass was estimated to be 0.16 Jupiter mass. These values were subsequently refined, as shown in the table below.
Title: HD 240237
Content:  In 2011, Gettel et al. announced the discovery of a planet orbiting this star. They estimated a mass around 5 times that of Jupiter, with an orbital period of 745.7 days and a moderate eccentricity. Sousa et al. (2015) gave a much lower estimate of 1.53 Jupiter mass. The designation b for this object, derives from the order of discovery. The designation of b is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet. In the case of HD 240237, there was only one planet, so only the letter b is used.
Title: HD 220773
Content:  The star is orbited by an exoplanet discovered in 2012. It is around 1.45 times the mass of Jupiter, orbiting very eccentric orbit with semimajor axis of around 5 AU and taking 10.2 years to complete an orbit. If additional inner terrestrial planets do exist in HD 220773 system, these must have eccentric orbits for planetary system to remain stable.
Title: 47 Ursae Majoris
Content:  near 2,500 days have a high false-alarm probability, and the best fit model gives an orbital period of 7,586 days at a distance of 7.73 AU from the star. Nevertheless, the parameters of the second planet are still highly uncertain. On the other hand, the Catalog of Nearby Exoplanets gives a period of 2,190 days, which would put the planets close to a 2:1 ratio of orbital periods, though the reference for these parameters is uncertain: the original Fischer et al. paper is cited as a reference in spite of the fact that it gives different parameters, though this solution has 
Title: HD 33636
Content:  HD 33636 B was discovered in 2002 by the Keck telescope in Hawaii. It was independently detected at the Haute-Provence Observatory in France. With this method it showed a minimum mass of 10.58 Jupiter masses, and was initially assumed to be a planet and provisionally labelled "HD 33636 b" (lower-case). In 2007, Bean et al. used the Hubble Space Telescope (HST) and he found that this body has an inclination as little as 4.1 ± 0.1°, which yielded the true mass of 142 Jupiter masses. This is too high to be a planet. It is now classified as an M-dwarf star of spectral type M6V, "HD 33636 B" (upper-case). This star takes 2117 days or 5.797 years to orbit at the average distance of 3.27 Astronomical Units (AU).
Title: Alpha Persei
Content:  In 2010 evidence was presented of a planet orbiting Mirfak. Radial velocity data from repeated observations of the star found a periodic variation with an amplitude of 70.8 ± 1.6 m/s. The proposed planet is estimated to have a minimum mass of approximately 6.6 times that of Jupiter and an orbital period of 128 days, but the claimed period may not be stable over 20 years so the exoplanet is considered doubtful. Rotational modulation due to surface activity such as starspots seem a more likely explanation of the radial velocity variations. In previous publications, periodic radial velocity variations of 87.7 or 77.7 days have been reported, but these have not been confirmed.

Question: Verify the following claims with "True" or "False": A planet, has a mass of 5.7 kgs, an orbital period of, 183309000.0, and the epoch date of, 31 December 2006.
Answer: True