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 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 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 131496
Content:  A planet with a mass roughly 2.2 times that of Jupiter orbiting at a distance of 2.09 astronomical units (AU) once every 883 days was discovered in 2011. HD 131496 and its planet, HD 131496b, were chosen as part of the 2019 NameExoWorlds campaign organised by the International Astronomical Union, which assigned each country a star and planet to be named. HD 131496 was assigned to Andorra. The winning proposal for the name of the star was Arcalís, after a mountain peak in northern Andorra where the Sun shines through a gap twice a year at fixed dates, leading to its use as a primitive Solar calendar. The planet was named Madriu, after a glacial valley and river in southeastern Andorra that forms the major part of the Madriu-Perafita-Claror UNESCO world heritage site.
Title: Lalande 21185
Content:  Data published in 2017 from the HIRES system at the Keck Observatory on Mauna Kea supported the existence of a close-in planet with an orbital period of just 9.8693±0.0016 days, being at least. Further radial velocity research with the SOPHIE échelle spectrograph and review of the original signal found that the 9.9 day period was undetectable, and instead proposed, using both datasets, that an exoplanet orbiting the star with a period of either 12.95 or 1.08 days, much more probably 12.95 as 1-day-period exoplanets seem to be rare in systems. This would give the planet a minimum mass of 2.99 
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: 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 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 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: 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.

Question: Verify the following claims with "True" or "False": A planet has a mass of 9.8 kgs, the epoch date 2006.12.31, and an orbital period of 135589000.0.
Answer: True