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: (5645) 1990 SP
Content:  The asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.
Title: 2005 RH52
Content:   belongs to a small group of detached objects with perihelion distances of 30 AU or more, and semi-major axes of 150 AU or more. Such extreme trans-Neptunian objects (ETNOs) can not reach such orbits without some perturbing object, which lead to the speculation of Planet Nine. It orbits the Sun at a distance of 39–270 AU once every 1923 years and 10 months (702,689 days; semi-major axis of 154.68 AU). Its orbit has an eccentricity of 0.75 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its first official observation at Mauna Kea in September 2005.
Title: (505478) 2013 UT15
Content:  With a semi-major axis of 196 AU, orbits the Sun at a distance of 43.9–348 AU once every 2,742 years. Its orbit has an eccentricity of 0.78 and an inclination of 11° with respect to the ecliptic. It has a similar orbit to, except for a smaller inclination. belongs to a small number of detached objects with perihelion distances of 30 AU or more, and semi-major axes of 150 AU or more. Such objects can not reach such orbits without some perturbing object, which lead to the speculation of planet nine.
Title: (55638) 2002 VE95
Content:  The rotation period of  is poorly defined and has ambiguous results with multiple alternative period solutions in between 4.90 and 10 hours. In December 2002, a rotational lightcurve of this object was obtained from photometric observations by astromomers from the Sierra Nevada Observatory in Spain. Lightcurve analysis gave a poorly defined period of 6.76 hours with a brightness variation of 0.08 magnitude (U=1+). Two years later in December 2004, it was revisited by the same astronomers, obtaining another poorly defined period of 9.97 hours with an amplitude of 0.05 magnitude (U=1+). Other observations by Sheppard only determined an amplitude of less than 0.06 magnitude (U=1).
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: 952 Caia
Content:  Two photoelectric lightcurve observations from 1980 rendered a rotation period of 7.50 and 7.51 hours (U=2/2), while a more recent light-curve analysis in 2004 gave a period of 3.795 hours (or half the previously determined period) with a very low brightness variation of 0.03 in magnitude (U=2), which typically indicates a nearly spheroidal shape.
Title: 3915 Fukushima
Content:  Several high-quality rotational lightcurves were obtained from photometric observations since 2003. An observation by Brian Warner at the U.S. Palmer Divide Observatory in Colorado rendered a rotation period of 9.418 hours with a high brightness variation of 0.67 in magnitude (U=3), indicating that the body has a non-spherical shape. This observation concurs with another measurement taken at the Oakley Observatory that rendered a period of 9.41 and an amplitude of 0.50 mag (U=3), superseding a less accurate lightcurve produced by the PDS of 8.40 hours (U=2). In 2011, an observation by René Roy gave another concurring period of 9.418 hours and an amplitude of 0.79 mag (U=3). On 16 December 2012, the asteroid occulted the star HIP 4315 over parts of Europe and North America. At the time the body's brightness was 16.3 in magnitude (mag) and that of the star was 8.5 mag.
Title: (39546) 1992 DT5
Content:  In September 2013, a rotational lightcurve for this asteroid was obtained from photometric observations in the R-band at the Palomar Transient Factory in California. It gave an exceptionally long rotation period of 1167 hours with an estimated error margin of ±100 hours. According to the Light Curve Data Base (LCDB), it is the 8th slowest rotating minor planet known to exist. Due to its high brightness amplitude of 0.80 magnitude, the body has a likely elongated shape (U=2).
Title: (585310) 2017 YZ1
Content:   is a member of the Apollo asteroids, which cross the orbit of Earth. Apollo's are the largest group of near-Earth objects with nearly 10 thousand known objects. It orbits the Sun at a distance of 0.88–1.77 AU once every 18 months (558 days; semi-major axis of 1.33 AU). Its orbit has an eccentricity of 0.33 and an inclination of 21° with respect to the ecliptic.

Question: Verify the following claims with "True" or "False": They have a rotation period of 95040 and an apoapsis of 511592000.0 km.
Answer: True