Title: (5604) 1992 FE
Content:  (327 days) | mean_anomaly   = 286.36° | mean_motion    = {{Deg2DMS|1.1011|sup=ms}} / day | inclination    = 4.7136° | asc_node       = 311.96° | arg_peri       = 82.586° | moid           = 0.0332 AU{{·}}12.9 LD | venus_moid     = 0.0059 AU | mean_diameter   = 550 m  | rotation        = {{Convert|5.3375|h|d|abbr=on|lk=on}}} | albedo         = 0.48 | abs_magnitude  = 17.1 }} (5604) 1992 FE is an Aten-type near-Earth minor planet. It was discovered by Robert H. McNaught at the Siding Spring Observatory in Canberra, Australia, on March 26, 1992. The asteroid is 550 m in diameter. The asteroid has a Venus minimum orbit intersection distance (Venus–MOID) of 0.0059 AU. On April 7, 2015 the asteroid passed 0.00717 AU from Venus.
Title: (53319) 1999 JM8
Content:  Radar imaging by Goldstone and Arecibo observatories revealed that has an unusually slow and possibly chaotic rotation period, similar to that of asteroid 4179 Toutatis. In July 1999, a rotational lightcurve of was obtained from photometric observations. It gave a period of 136 hours with a brightness amplitude of 0.7 magnitude (U=2), and suggested that the body is in a non-principal axis rotation, commonly known as tumbling.
Title: (416151) 2002 RQ25
Content:  orbits the Sun at a distance of 0.8–1.5 AU once every 1 years and 2 months (428 days). Its orbit has an eccentricity of 0.31 and an inclination of 5° with respect to the ecliptic. The asteroid's minimum orbit intersection distance with Earth is 0.0499 AU, which is currently exactly at the threshold limit of 0.05 AU (or about 19.5 lunar distances) to make it a potentially hazardous object.
Title: 2101 Adonis
Content:  The near-Earth object orbits the Sun at a distance of 0.4–3.3 AU once every 2 years and 7 months (937 days; semi-major axis of 1.87 AU). Its orbit has an eccentricity of 0.76 and an inclination of 1° with respect to the ecliptic. Adonis was one of the first near-Earth objects ever to be discovered. It was also the second known Apollo asteroid after 1862 Apollo, the group's namesake discovered four years earlier in 1932.
Title: 2MASS J12195156+3128497
Content:  2MASS J12195156+3128497 (abbreviated to 2MASS J1219+3128) is a rapidly-rotating brown dwarf of spectral class L8, located in the constellation Coma Berenices about 66 light-years from Earth. With a photometrically measured rotation period of 1.14 hours, it is one of the fastest-rotating known brown dwarfs announced by a team of astronomers led by Megan E. Tannock in March 2021. With a rotational velocity of about 80 km/s, it is approaching the predicted rotational speed limit beyond which it would break apart due to centripetal forces. As a consequence of its rapid rotation, the brown dwarf is slightly flattened at its poles to a similar degree as Saturn, the most oblate planet in the Solar System. Its rapid rotation may enable strong auroral radio emissions via particle interactions in its magnetic field, as observed in other known rapidly-rotating brown dwarfs.
Title: 5751 Zao
Content:  Zao has been observed by several groups to determine its rotational period. Its light curve was observed by Pravec, et al. between 1992 and 1995 with the intention of determining its rotational period. From its nearly constant brightness it was determined that the asteroid is roughly spherical and has a rotational period of ≥ 21.7 hr. Another group led by Wisniewski conducted an approximately 5 hour observation and were unable to conclude a rotational period. Zao was again observed in 2001 by Delbó, et al. using the Keck telescope. They were able to determine the asteroid's albedo of 0.36 and re-classify the asteroid from X-type to E-type. Using the asteroid's albedo and the Near Earth Asteroid Thermal Model (NEATM) the asteroid's diameter was estimated to be 2.3 km. Further study of the asteroid by the Ondrejov Asteroid Photometry Project concludes that a rotational period of 76 hours is consistent with earlier measurements.
Title: (84522) 2002 TC302
Content:  0.04 mag. However, this short rotation period was most likely an alias due to a bias for shorter and more easily discernable shorter periods. is highly oblate, and Ortiz et al. suggest a longer rotation period estimate of 56.1 hours. An occultation of a 15.3 magnitude star by on 28 January 2018 over Europe suggests that it has highly oblate shape with dimensions of 543.2 × 459.5 km and a projected axial ratio of a/c=1.18. The area equivalent diameter of is 499.6 km. On 11 November 2021, an occultation across North America and Europe detected an oblate shape of 530 km (mean 499 km), in strong agreement with the 2018 occultation results. No satellites were detected.
Title: (459883) 2014 JX55
Content:  The object remained listed as an inner heliospheric asteroid for several years, until identifications with and  and a subsequent improvement of the orbital uncertainty completely overturned previous calculations. is now a secured central main-belt asteroid orbiting the Sun at a distance of 2.2–3.1 AU once every 4 years and 3 months (1,555 days; semi-major axis of 2.63 AU). Its orbit has an eccentricity of 0.17 and an inclination of 32° with respect to the ecliptic.
Title: 514107 Kaʻepaokaʻawela
Content:   Kaʻepaokaʻawela orbits the Sun at a distance of 3.2–7.1 AU once every 11 years and 8 months (4,256 days; semi-major axis of 5.14 AU). Its orbit has an eccentricity of 0.38 and an inclination of 163° with respect to the ecliptic. Its period is close to the 11.86-year period of Jupiter. During one Jovian year, Jupiter moves 360° around the sun whereas Kaʻepaokaʻawela moves 366.3° in the opposite direction. The eccentricity of its orbit allows it to alternately pass inside and outside of Jupiter's orbit at its closest approaches of 176 million kilometers. Each time it passes near Jupiter its 
Title: 1441 Bolyai
Content:  Bolyai orbits the Sun in the central main-belt at a distance of 2.0–3.3 AU once every 4 years and 3 months (1,559 days). Its orbit has an eccentricity of 0.24 and an inclination of 14° with respect to the ecliptic. Bolyais observation arc begins the night following its official discovery observation in 1937, as no precoveries were taken, and no prior identifications were made.

Question: Verify the following claims with "True" or "False": And it has a rotation period of 48240.0 and an apoapsis of 511592000.0 km.
Answer: False