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: (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: 732 Tjilaki
Content:   In February 1996, a rotational lightcurve of Tjilaki was obtained from photometric observations over ten nights by European astronomers using the Dutch 0.9-metre Telescope and the Bochum 0.61-metre Telescope at La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of 12.34 hours with a brightness variation of 0.19 magnitude (U=3−). In May 2012, astronomers at the Palomar Transient Factory measured a period of 12.277 hours (U=2). Additional observations were made by the TESS-team in January 2019, and by amateur astronomers Axel Martin and Rui Goncalves in May 2020, reporting a concurring period of (12.329) and (12.322) hours with an amplitude of (0.16) and (0.287) magnitude, respectively (U=2/n.a.). In 2016, a modeled lightcurve gave a concurring sidereal period of 12.341 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, 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 (160.0°, 23.0°) and (353.0°, 24.0°) 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: (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: 894 Erda
Content:  In June 2006, a rotational lightcurve of Erda was obtained from photometric observations by David Higgins at Hunters Hill Observatory, Australia, and by Rui Gonçalves at Linhaceira Observatory in Portugal. Lightcurve analysis gave a well-defined rotation period of 4.69 hours with a brightness variation of 0.27 magnitude, significantly higher than previous observations had measured (U=3). The observers also found no indication of a previously speculated companion. The result supersedes observations from July 2001, when both Robert Stephens and Laurent Bernasconi determined a period of 4.69 and 4.69 hours with an amplitude of 0.05 and 0.06 magnitude, respectively.
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: 1251 Hedera
Content:  Modeled photometric data from the Lowell Photometric Database (LPD) and the robotic BlueEye600 Observatory, gave a concurring period of 19.9020 hours, Both studies determined two spin axes of (124.0°, −70.0°) and (266.0°, −62.0°), as well as (271.0°, −53.0°) and (115.0°, −62.0°) in ecliptic coordinates (λ, β).
Title: 1094 Siberia
Content:  In December 2006, a first rotational lightcurve of Siberia was obtained from photometric observations by astronomers from New Zealand and Australia. Lightcurve analysis gave a rotation period of 21.15 hours with a brightness amplitude of 0.45 magnitude, indicating a non-spherical shape (U=2). While not being a slow rotator, Siberia has a longer than average rotation period, especially for its size.
Title: 2006 HH123
Content:  , also written as 2006 HH123, was a misidentified nonexistent object that had a short 1 day observation arc. It was formerly thought to be a lost object with an assumed eccentricity of 0.46. If it had been a scattered-disc object it would have had an absolute magnitude of 5.2, and been a possible dwarf planet. The preliminary orbital elements (as displayed in the infobox to the right) were calculated using only three observations over a period of one day; hence its orbit was very poorly known and it quickly became lost. Of the three discovery images, the first one is an unidentified object, the second one was identified as the main-belt asteroid, and the third image shows nothing at the measured position. The three observations of were deleted on 6 November 2014, and the provisional designation  is no longer listed in the Minor Planet Center database.

Question: Verify the following claims with "True" or "False": it has an epoch date of 2006.12.31 and rotation period of 93736.8.
Answer: False