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: (391211) 2006 HZ51
Content:  As of 2018, n rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remains unknown.
Title: (89830) 2002 CE
Content:  In October 2004, a rotational lightcurve of was obtained from photometric observations by Czech astronomer Petr Pravec at the Ondřejov Observatory. Lightcurve analysis gave a rotation period of 2.6149 hours with a low brightness amplitude of 0.09 magnitude (U=2-). Several longer periods are also possible.
Title: 1140 Crimea
Content:  In April 2005, a rotational lightcurve of Crimea was obtained by American astronomer Robert Stephens at Santana Observatory in California. Lightcurve analysis gave a well-defined rotation period of 9.77 hours with a brightness variation of 0.30 magnitude (U=3). Photometric observations by amateur astronomers Federico Manzini and Pierre Antonini in March 2014, gave a concurring period of 9.784 hours with an amplitude of 0.23 magnitude (U=2). In addition, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue and other sources gave a period 9.7869 hours, as well as a spin axis of (12.0°, -73.0°) in ecliptic coordinates (U=n.a.).
Title: (481394) 2006 SF6
Content:  In September 2018, a rotational lightcurve of  was obtained from photometric observations by Brian Warner and Robert Stephens at the Center for Solar System Studies in California. Lightcurve analysis gave a rotation period of 11.517 hours with a very high brightness amplitude of 0.97 magnitude (U=3), indicative of a highly elongated non-spherical shape. The two photometrists revisited the object in October 2019 and obtained a similar result of 11.495 hours with an even higher magnitude of 1.07 (U=3-).
Title: (65407) 2002 RP120
Content:  In October 2010, a rotational lightcurve of  was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 200 hours with a brightness amplitude of 0.6 magnitude, indicative of an elongated, non-spherical shape (U=2). With a rotation period above 100 hours, it is a typical slow rotator.
Title: 986 Amelia
Content:  In October 2000, a rotational lightcurve of Amelia was obtained from photometric observations by American amateur astronomer Robert A. Koff at the Thornton Observatory in Colorado. Lightcurve analysis gave a well-defined rotation period of 9.52 hours with a brightness amplitude of 0.43 magnitude (U=3). In December 2006, a concurring period determination of 0.396533 d was made by astronomers Raymond Poncy, Enric Forné, Hiromi Hamanowa, Hiroko Hamanowa and Hilari Pallarés (U=3). In 2016, a modeled lightcurves using photometric data from various sources, rendered a concurring sidereal period of 9.519 h and two spin axes of (80.0°, 30.0°) and (282.0°, 30.0°) in ecliptic coordinates.
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: 920 Rogeria
Content:   In October 2010, a rotational lightcurve of Rogeria was obtained from photometric observations by Thomas A. Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of 12.244 hours with a brightness variation of 0.31 magnitude (U=3−). A tentative period determination of 9.05 hours with an amplitude of 0.21 magnitude was made by French amateur French astronomer René Roy in July 2012 (U=2−). Another observation by Petr Pravec and Peter Kušnirák at Ondřejov Observatory in June 2007 gave a period of 8.09 hours (U=2−). In 2016, a modeled lightcurve gave a concurring sidereal period of 12.575 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys. The study also determined two spin axes of (238.0°, −15.0°) and (47.0°, −35.0°) in ecliptic coordinates (λ,&thinsp;β).
Title: (5645) 1990 SP
Content:  In April 2002, Czech astronomer Petr Pravec obtained a rotational lightcurve from a photometric observations, which gave a relatively long period of 30.39 hours with a brightness variation of 0.7 in magnitude (U=2). The observations have also shown that the body is most likely in a tumbling motion.

Question: Verify the following claims with "True" or "False": It has a rotation period of 95040.0 and its epoch on 2006.12.31.
Answer: True