Title: HD 132563
Content:  Based upon radial velocity variations of HD 132563B, the presence of an ordinary giant planet has been inferred by S. Desidera et al. (2011). This object is orbiting the star with a period of 1,544 days, at a distance of about 2.6 AU, and with an orbital eccentricity of 0.22.
Title: HD 131664
Content:  of the Sun's luminosity from its photosphere at an effective temperature of 5,901 K. The discovery of a planet in orbit around HD 131664 was announced on October 26, 2008 and designated HD 131664 b. The object was detected from Doppler measurements of the host star between 2004 and 2008. This planet or brown dwarf has mass of at least 18.15 times that of Jupiter and orbits in a long-period, eccentric orbit that completely overlaps the star's habitable zone. This period (1,951 days or 5.34 years) is among the dozen longest exoplanet periods known, as of 2009. Follow-up studies with the Hipparcos satellite further constrained the predicted mass of the companion, providing a best estimate of 23 Jupiter mass.
Title: HD 13931 b
Content:  HD 13931 b (also known as HIP 10626 b) is an extrasolar planet which orbits the G-type star HD 13931, located approximately 155 light years away in the constellation Andromeda. This planet takes 11.55 years to orbit the star at the average distance of 5.15 AU or 770 Gm. The planet's eccentricity (0.02) is about the same as Earth. The orbital distance for this planet ranges from 5.05 to 5.25 AU. This planet was discovered by using radial velocity method from spectrograph taken at Keck Observatory on November 13, 2009.
Title: HD 8535
Content:  In 2009, a gas giant was found in orbit around the star using the radial velocity method. It has an orbital period of 1313 days and has at least 68% of the mass of Jupiter.
Title: Boötes
Content:  planet, HD 132563B b, was discovered in 2011 by the radial velocity method. , it orbits 2.62 AU from its star with a period of 1544 days. Its orbit is somewhat elliptical, with an eccentricity of 0.22. HD 132563B b is one of very few planets found in triple star systems; it orbits the isolated member of the system, which is separated from the other components, a spectroscopic binary, by 400 AU. Also discovered through the radial velocity method, albeit a year earlier, is HD 136418 b, a two-Jupiter-mass planet that orbits the star HD 136418 at a distance of 1.32 AU with a period of 464.3 days. Its host 
Title: HD 13931
Content:  estimated 6.8 billion years old and it is spinning with a rotation period of about 26 days In 2009, a very long-period giant planet, more massive than Jupiter, was found in orbit around the star by measuring changes in the star's radial velocity. This planet takes 4218 days to orbit the star at the typical distance of 5.15 AU. The planet's eccentricity (0.02) is about the same as Earth. According to a 2018 research, HD 13931 is the most promising Solar System analogue known, since it has a star similar to the Sun and a planet with mass and semimajor axis similar to Jupiter. Those characteristics yield a probability almost 75% for the existence of a dynamically stable habitable zone, where an Earth-like planet may exist and sustain life.
Title: HD 120084
Content:  A planet with at least 4.5 times the mass of Jupiter and a highly eccentric orbit (with an eccentricity of 0.66) was discovered by precisely measuring the radial velocity of the star in 2013. With an average distance of 4.5 AU from its star, this planet has one of the most eccentric orbits discovered.
Title: HD 188015
Content:  A stellar common proper motion candidate was announced in 2006 and designated HD 188015 B. It is located at an angular separation of 13 arcsecond along a position angle of 85°. The photometric distance estimate for this object is 46.9 ±, matching the primary within the margin of error. They have a projected separation of 684 AU. A Jovian planetary companion to this star was announced in 2005, based on radial velocity measurements indicating a periodic perturbation. It is orbiting the host star at a distance of 1.2 AU with a period of 461.2 days and an eccentricity (ovalness) of 0.14. The inclination of the orbital plane remains unknown, so only a lower bound on the planet's mass can be determined. It has a minimum mass equal to 1.5 times the mass of Jupiter. The orbital path of this object intersects the habitable zone of the star, which is likely to eject any Earth-like planet from that region.
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 4308
Content:  In 2005, a low-mass planet was found in orbit around this star using the radial velocity method with the HARPS spectrograph. It is following a circular orbit close to its host star with a period of just 15.6 days. Unusual for a star with planets, HD 4308 has a metallicity lower than that of the Sun.

Question: Verify the following claims with "True" or "False": The planets orbital period is 135589000.0 and its epoch date is 2006.12.31.
Answer: True