Title: HD 173416 b
Content:  HD 173416 b is an extrasolar planet located approximately 440 light years away in the constellation of Lyra, orbiting the 6th magnitude G-type giant star HD 173416. This is planet has at least 2.7 times the mass of Jupiter and was discovered on January 10, 2009 by Liu et al. HD 173416 b orbits at 1.16 AU from the star. However, despite the fact that the planet orbits 16% further from the star than Earth does from the Sun, it has orbital period of only 323.6 days, compared to 365.25 days for Earth. This inverse relationship is caused by the parent star having twice the mass of our Sun, which increases the strength of its gravitational field. This evidence implies that when this star was on the main sequence, it was an A-type star. The planet HD 173416 b is named Wangshu (望舒). The name was selected in the NameExoWorlds campaign by Nanjing, during the 100th anniversary of the IAU. Wangshu is the goddess who drives for the Moon and also represents the Moon in Chinese mythology.
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: Epsilon Eridani b
Content:  Similar updated findings were published in a paper in July 2021, determining a minimum mass of 0.651 that of jupiter, with the planet's semi-major axis at 3.5 AU orbiting with an eccentricity of 0.044. Using astrometric velocity data taken from the U.S. Naval Observatory Robotic Astrometric Telescope (URAT) combined with previously collected data from the Hipparcos mission, and the newer Gaia EDR3 data release, a group of scientists at the United States Naval Observatory believe they have, with high formal confidence levels, confirmed the presence of a long-period exoplanet orbiting Epsilon Eridani. , both the Extrasolar Planets Encyclopaedia and the NASA Exoplanet Archive list the planet as 'confirmed'.
Title: JPL Horizons On-Line Ephemeris System
Content:  modern, highly accurate measurements of planetary positions. Since August 2013, Horizons has been using ephemeris DE431. During the week of 12 April 2021, the Horizons ephemeris system was updated to replace the DE430/431 planetary ephemeris, used since 2013, with the new DE440/441 solution. The new DE440/441 general-purpose planetary solution includes seven additional years of ground and space-based astrometric data, data calibrations, and dynamical model improvements, most significantly involving Jupiter, Saturn, Pluto, and the Kuiper Belt. Inclusion of 30 new Kuiper-belt masses, and the Kuiper Belt ring mass, results in a time-varying shift of ~100 km in DE441's barycenter relative to DE431. In September 2021 JPL started transitioning from common gateway interface (CGI) to application programming interface (API).
Title: HD 175167
Content:  It is radiating 2.9 times the Sun's luminosity from its photosphere at an effective temperature of 5,635 K. A Jovian planetary companion was discovered in 2010 by a team of the Magellan Planet Search Program, led by Pamela Arriagada. Designated HD 175167 b, their Doppler velocity data (taken over a five year period) indicates the planet has an orbital period of 1290 days at a distance of 2.40 AU from the host star with an eccentricity (ovalness) of 0.54. Since the inclination of the orbital plane is unknown, it is only possible to deduce a lower bound on the planet's mass. It is at least 7.8 times as massive as Jupiter. In a 2013 paper, Robert A. Wittenmyer and colleagues reviewed the data of this and many other systems with one or two planets for possible additional planets, but were unable to find any evidence of any.
Title: Epsilon Eridani b
Content:  The planet's existence was suspected by a Canadian team led by Bruce Campbell and Gordon Walker in the early 1990s, but their observations were not definitive enough to make a solid discovery. Its formal discovery was announced on August 7, 2000, by a team led by Artie Hatzes. The discoverers gave its mass as 1.2 ± 0.33 times that of Jupiter, with a mean distance of 3.4 AU from the star. Observers, including Geoffrey Marcy, suggested that more information on the star's Doppler noise behaviour created by its large and varying magnetic field was needed before the planet could be confirmed. In 2006, the Hubble Space Telescope made astrometric 
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.
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 17156 b
Content:  HD 17156 b, named Mulchatna by the IAU, is an extrasolar planet approximately 255 light-years away in the constellation of Cassiopeia. The planet was discovered orbiting the yellow subgiant star HD 17156 in April 2007. The planet is classified as a relatively cool hot Jupiter planet slightly smaller than Jupiter but slightly larger than Saturn. This highly-eccentric three-week orbit takes it approximately 0.0523 AU of the star at periastron before swinging out to approximately 0.2665 AU at apastron. Its eccentricity is about the same as 16 Cygni Bb, a so-called "eccentric Jupiter". Until 2009, HD 17156 b was the transiting planet with the longest orbital period.
Title: Nibiru cataclysm
Content:  In March 2014, astronomers Chad Trujillo and Scott Sheppard published a paper in Nature arguing that the apparent clustering of the arguments of perihelion of distant trans-Neptunian objects suggested the existence of a large trans-Neptunian planet. On January 20, 2016, Mike Brown and Konstantin Batygin announced that they had corroborated Trujillo and Sheppard's findings, and that they believed the planet, which they dubbed "Planet Nine", would have a mass roughly ten times that of Earth, and a semimajor axis of approximately 400–1500 AU (60–225 billion km). Believers in Nibiru and the Nibiru cataclysm immediately argued that this constituted evidence for their claims. However, astronomers pointed out that this planet, if it exists, would have a perihelion (closest approach to the Sun) of roughly 

Question: Verify the following claims with "True" or "False": The epoch of a planet was on the 31st of July 2016 and its periapsis is 445895000000.0.
Answer: True