Title: (13366) 1998 US24
Content:  In August 2015, a first rotational lightcurve of  was obtained from photometric observations by the Kepler space telescope during its K2 mission. Lightcurve analysis gave a rotation period of 400 hours with a brightness variation of 0.23 magnitude (U=2-). One month later, a second, lower-rated lightcurve by Kepler determined an alternative period of 522 hours with an amplitude of 0.20 (U=1+). As of 2018, no secure period of this slow rotator has yet been obtained.
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: (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: (21601) 1998 XO89
Content:  In April 2013, a rotational lightcurve of  was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies (CS3) in California. Lightcurve analysis gave a rotation period of 12.65 hours and a brightness variation of 0.30 magnitude (U=2+). Observations by his college Brian Warner at CS3 in July 2017, gave a similar period of 12.530 hours with an amplitude of 0.25 magnitude (U=2+).
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: (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: (10115) 1992 SK
Content:  Several rotational lightcurves form photometric observations have been obtained for this body. In 1999, Czech astronomer Petr Pravec constructed a lightcurve, that rendered a rotation period of 7.328 hours and a brightness variation of 0.72 in magnitude (U=n/a). In March 2006, observations by astronomer David Polishook from the ground-based Wise Observatory, Israel, gave a rotation period of 7.31 and amplitude of 0.70 mag (U=2), and in November 2011, American astronomer Brian Warner at the Palmer Divide Observatory, Colorado, obtained the first well-defined period of 7.323 hours with an amplitude of 0.50 mag (U=3).
Title: (5646) 1990 TR
Content:  In December 2012, the so far best rated rotational lightcurve was obtained by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 3.1999 hours with a brightness variation of 0.12 magnitude (U=3). Photometric observations also gave a period of 19.47 hours for a probable asteroid moon, with a measured diameter-ratio of 0.18, which translates into a diameter of 400 meters for its moon.
Title: 2016 DV1
Content:  In March 2016, a rotational lightcurve of  was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station at the Center for Solar System Studies in California. Lightcurve analysis gave a well-defined rotation period of 0.084 hours (or 302.9 seconds) with a high brightness variation of 0.56 in magnitude, indicative of an irregular shape (U=3). On the following night, European astronomers Siegfried Eggl, William Thuillot, Maria Kudryashova, and Raoul Behrend determined a similar period of 0.084 hours (or 303.7 seconds) and an even higher amplitude of 1.02 magnitude.(U=3).
Title: 1508 Kemi
Content:  In 2016, an international study modeled a lightcurve with a concurring period of 9.19182 hours. It also determined two spin axis at (352.0°, 72.0°) and (166.0°, 73.0°) in ecliptic coordinates (λ, β).

Question: Verify the following claims with "True" or "False": well its rotation period is 95040 and its epoch is on 13 January 2016.
Answer: True