Title: 1101 Clematis
Content:  1101 Clematis is an Alauda asteroid from the outermost regions of the asteroid belt, approximately 37 kilometers in diameter. It was discovered on 22 September 1928, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany, and assigned the provisional designation. It was named for the flowering plant Clematis. The presumably carbonaceous asteroid has a relatively long rotation period of 34.3 hours.
Title: 1101 Clematis
Content:  Clematis is a member of the Alauda family (902), a large family of typically "bright" carbonaceous asteroids and named after its parent body, 702 Alauda. According to a different study, this object is also the namesake of the Clematis family, a small family of 5–16 asteroids hence they may have arisen from the same collisional event. All members have a relatively high orbital inclination. It orbits the Sun in the outermost asteroid belt at a distance of 3.0–3.5 AU once every 5 years and 10 months (2,120 days; semi-major axis of 3.23 AU). Its orbit has an eccentricity of 0.08 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins with its observation as at Goethe Link Observatory in October 1963, more than 35 years after its official discovery observation at Heidelberg.
Title: 1101 Clematis
Content:  Clematis is an assumed carbonaceous C-type asteroids, while the overall spectral type for members of the Alauda family is that of a somewhat brighter B-type.
Title: 1101 Clematis
Content:  This minor planet was named after the flowering plant Clematis, a genus within the Ranunculaceae (buttercup or crowfoot family). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H n.a.).
Title: 11P/Tempel–Swift–LINEAR
Content:  11P/Tempel–Swift–LINEAR is a periodic Jupiter-family comet in the Solar System. Ernst Wilhelm Leberecht Tempel (Marseille) originally discovered the comet on November 27, 1869, it was later observed by Lewis Swift (Warner Observatory) on October 11, 1880, and realised to be the same comet. After 1908 the comet became an unobservable lost comet, but on December 7, 2001, an object was found by the Lincoln Near-Earth Asteroid Research (LINEAR) program, and confirmed by previous images from September 10 and October 17 as being the same comet. The comet was not observed during the 2008 unfavorable apparition because the perihelion passage occurred when the comet was on the far side of the Sun. The comet was observed during the 2014 and 2020 apparitions.
Title: 2010 BK118
Content:   (also written 2010 BK118) is a centaur roughly 20–60 km in diameter. It is on a retrograde cometary orbit. It has a barycentric semi-major axis (average distance from the Sun) of ~400 AU. came to perihelion in April 2012 at a distance of 6.1 AU from the Sun (outside the orbit of Jupiter). It has a Jupiter-MOID of 1.1 AU. , it is 11 AU from the Sun. It will not be 50 AU from the Sun until 2043. After leaving the planetary region of the Solar System, will have a barycentric aphelion of 791 AU with an orbital period of 8000 years.
Title: 3034 Climenhaga
Content:  Climenhaga is a member of the Flora family, one of the largest families of stony asteroids in the main belt. It orbits the Sun in the inner main-belt at a distance of 1.8–2.8 AU once every 3 years and 6 months (1,294 days). Its orbit has an eccentricity of 0.21 and an inclination of 5° with respect to the ecliptic. The asteroid's observation arc begins with its official discovery observation at Heidelberg, as no precoveries were taken, and no prior identifications were made.
Title: 1140 Crimea
Content:  Crimea is a S-type asteroid in both the Tholen and SMASS taxonomic scheme. It orbits the Sun in the central main-belt at a distance of 2.5–3.1 AU once every 4 years and 7 months (1,685 days). Its orbit has an eccentricity of 0.11 and an inclination of 14° with respect to the ecliptic. First identified as at Simeiz in 1922, the body's observation arc begins at Uccle in 1935, or 16 years after its official discovery observation at Simeiz.
Title: Apsis
Content:  Orbital elements such as the time of perihelion passage are defined at the epoch chosen using an unperturbed two-body solution that does not account for the n-body problem. To get an accurate time of perihelion passage you need to use an epoch close to the perihelion passage. For example, using an epoch of 1996, Comet Hale–Bopp shows perihelion on 1 April 1997. Using an epoch of 2008 shows a less accurate perihelion date of 30 March 1997. Short-period comets can be even more sensitive to the epoch selected. Using an epoch of 2005 shows 101P/Chernykh coming to perihelion on 25 December 2005, but using an epoch of 2012 produces a less accurate unperturbed perihelion date of 20 January 2006. Numerical integration shows dwarf planet Eris will come to perihelion around December 2257. Using an epoch of 2021, which is 236 years early, less accurately shows Eris coming to perihelion is 2260. 4 Vesta comes to perihelion on 26 December 2021, but using a two-body solution at an epoch of July 2021 less accurately shows Vesta coming to perihelion on 25 December 2021.
Title: 104 Klymene
Content:  Klymene (minor planet designation: 104 Klymene) is a large, dark Themistian asteroid that was discovered by J. C. Watson on September 13, 1868, and named after one of the many Clymenes in Greek mythology. It is orbiting the Sun with a period of 5.60 years and an eccentricity of 0.16. The orbital plane is inclined by 2.8° to the plane of the ecliptic. It is classified as a C-type asteroid, indicating it probably has a carbonaceous composition. The spectra indicates the presence of aqueous-altered minerals on the surface based upon a sharp feature at a wavelength of 3 μm, and, as of 2015, is the only member of the Themis family found to show this absorption. Based upon measurements made using adaptive optics at the W. M. Keck Observatory, this object may have a bi-lobed shape with a length of 163 ± 3 km and width of 103 ± 5 km, for an average dimension of 133 km. This asteroid is located near the region of the Themis family but itself considered a background asteroid using HCM-analysis. It is listed as a member of the Hecuba group of asteroids that orbit near the 2:1 mean-motion resonance with Jupiter.

Question: Verify the following claims with "True" or "False": The epoch of 1101 Clematis was on the 31st of July 2016 and its periapsis is 445895000000.0.
Answer: True