Title: 251 Sophia
Content:  In December 2000, a rotational lightcurve of Sophia was obtained from photometric observations by Bill Holliday in New Braunfels, Texas. Lightcurve analysis gave a well-defined rotation period of 20.216 hours with a brightness variation of 0.3 magnitude (U=3). Between 2005 and 2013, additional observations by French amateur astronomers Laurent Bernasconi, Etienne Morelle and René Roy gave a tentative period of 20.28 hours with an amplitude between 0.25 and 0.61 (U=2/2/2). Modeled lightcurves by Josef Ďurech and Josef Hanuš, using photometric data including from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) were published in 2018. It gave a concurring sidereal period of 20.222 and 20.222 hours, respectively. Hanuš also gave two spin axes at (235.0°, −52.0°) and (47.0°, 84.0°) in ecliptic coordinates (λ,&thinsp;β).
Title: 1102 Pepita
Content:  Three rotational lightcurves of Pepita were obtained from photometric observations by astronomers Hilari Pallares and Enric Forné (2006, U=2), Pierre Antonini and René Roy (2007, U=3), as well as by Robert Stephens (2007, U=3). The consolidated lightcurve gave a well-defined rotation period of 5.1054 hours with a brightness amplitude between 0.31 and 0.36 magnitude. In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue and other sources gave a concurring sidereal period 5.10532 hours, as well as two spin axes of (25.0°, −34.0°) and (231.0°, −30.0°) in ecliptic coordinates (λ, β).
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: 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: 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: 1291 Phryne
Content:  In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a period 5.58414 hours, as well as two spin axis of (106.0°, 35.0°) and (277.0°, 59.0°) in ecliptic coordinates (λ, β). In 2017, a new study of the same international collaboration about the rotational states of Eoan asteroids gave a revised shape model with a period of 5.584139 hours and two spin axis of (109.0°, 33.0°) and (281.0°, 56.0°).
Title: 4867 Polites
Content:  In August 2010, a rotational lightcurve of Polites was obtained from photometric observations over five nights by Linda French at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a tentative rotation period of 9.21 hours with a low brightness variation of 0.09 magnitude (U=2-). Follow-up observations on a yearly basis by Robert D. Stephens and Daniel Coley at the Center for Solar System Studies gave several lightcurves during 2013–2018. The best-rated one from January 2016 gave a period of 11.235 hours and an amplitude of 0.15 magnitude (U=3).
Title: 2892 Filipenko
Content:  In November 2004, a rotational lightcurve of Filipenko was obtained from photometric observations by Robert D. Stephens at the Santana Observatory (646), California, and gave a well-defined rotation period of 14 hours with a brightness variation of 0.21 magnitude (U=3).
Title: 5145 Pholus
Content:  In March 2005, a rotational lightcurve of Pholus was obtained from photometric observations by Tegler using the VATT at Mount Graham. Lightcurve analysis gave a rotation period of 9.980 hours with a brightness amplitude of 0.60 magnitude (U=3-). Alternative period determinations were also conducted by Hoffmann, Franham and Buie with concurring results of 9.977, 9.982 and 9.983 hours, respectively (U=3/3/3).
Title: 2099 Öpik
Content:  In 2005, a photometric lightcurve analysis by several astronomers including Pierre Antonini, rendered a rotation period of 6.443 hours and with a brightness amplitude of 0.21 in magnitude (U=2), superseding the results of an observation from the 1990s that gave a longer period of 9.3 hours (U=2).

Question: Verify the following claims with "True" or "False": 201 Penelope, has a rotation period of 95040.0, and its epoch date is 2006.12.31.
Answer: False