Title: 1097 Vicia
Content:  In November 2010, a rotational lightcurve of Vicia was obtained from photometric observations by Gordon Gartrelle at the University of North Dakota (730) and at the Badlands Observatory in North Dakota, United States. Analysis of the fragmentary lightcurve gave a rotation period of 26.5 hours with a brightness variation of 0.08 magnitude, indicative for a spherical rather than irregular and elongated shape (U=1). As of 2017, however, no other lightcurve has been obtained and Vicias rotation period has not yet been secured.
Title: 1030 Vitja
Content:  In July 2007, a rotational lightcurve of Vitja was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 5.7014 hours and a brightness variation of 0.18 magnitude (U=3-). Another observation by Andrea Ferrero at the Bigmuskie Observatory in Italy showed a period of 6.332 with an amplitude of 0.21 (U=2).
Title: 1097 Vicia
Content:  Vicia spectral type has not been determined. Asteroids in the central main belt with a semi-major axis between 2.6 and 2.7 AU, are located in a transitional region where both stony and carbonaceous asteroids are frequent and generic assumptions are difficult.
Title: 1097 Vicia
Content:  Vicia was discovered by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany on 11 August 1928. On 15 and 22 August, the asteroid was independently discovered by Soviet astronomer Pelageya Shajn at Simeiz Observatory on the Crimean peninsula, and by English astronomer Harry Edwin Wood at the Johannesburg Observatory in South Africa, respectively. However, the Minor Planet Center only recognizes the first discoverer. The asteroid was first identified as at Heidelberg in May 1907. The body's observation arc begins at Heidelberg in August 1928, six nights after its official discovery observation.
Title: Vega
Content:  Vega has a rotation period of 12.5 hours. When the radius of Vega was measured to high accuracy with an interferometer, it resulted in an unexpectedly large estimated value of 2.73 ± 0.01 times the radius of the Sun. This is 60% larger than the radius of the star Sirius, while stellar models indicated it should only be about 12% larger. However, this discrepancy can be explained if Vega is a rapidly rotating star that is being viewed from the direction of its pole of rotation. Observations by the CHARA array in 2005–06 confirmed this deduction. The pole of Vega—its axis of rotation—is inclined no more than 
Title: 1197 Rhodesia
Content:  In December 2017, a rotational lightcurve of Rhodesia was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Tempe, Arizona. Lightcurve analysis gave a rotation period of 16.06 hours with a brightness variation of 0.27 magnitude (U=3-). This result refines previous period determinations of 15.89 and 16.062 hours by Richard Binzel (1984) and Laurent Bernasconi (2005), respectively (U=2/2).
Title: 917 Lyka
Content:  In January 2005, a rotational lightcurve of Lyka was obtained from photometric observations by Matthieu Conjat. Lightcurve analysis gave a well-defined rotation period of 7.867 hours with a low brightness variation of 0.17 magnitude, indicative of a rather spherical shape (U=3). In October 2018, the period was confirmed by Laurent Bernasconi (7.884 h) and by Alfonso Carreño of OBAS (7.889 h) with amplitudes of 0.12 and 0.26, respectively (U=3/3).
Title: 4962 Vecherka
Content:  In August 2015, a rotational lightcurve of Vecherka was obtained from photometric observations by a collaboration of Bulgarian astronomers. Lightcurve analysis gave a long rotation period of 336 hours with a brightness variation of 1.08 magnitude (U=2), indicating that the body's shape is irregular and elongated rather than spherical. This long period makes Vecherka a slow rotator, which ranks among the Top 200 slowest ones known to exists.
Title: 1310 Villigera
Content:  In October 2001, a first rotational lightcurve of Villigera was obtained by astronomer Robert Koff at Thornton Observatory (713) in Colorado. Light curve analysis gave a well-defined rotation period of 7.830 hours with a brightness variation of 0.39 magnitude (U=3). Photometric observations by astronomers René Roy, Raoul Behrend and Pierre Antonini in February 2006, gave a concurring period of 7.834 hours and an amplitude of 0.36 magnitude (U=3). In 2016, a modeled lightcurves using photometric data from various sources, rendered an identical period of 7.830 and a spin axis of (3.0°, 63°) in ecliptic coordinates.
Title: 759 Vinifera
Content:  In September 2002, a rotational lightcurve of Vinifera was obtained from photometric observations by Maurice Clark at the Goodsell Observatory in Minnesota. Lightcurve analysis gave a well-defined rotation period of 14.229 hours with a brightness variation of 0.36 magnitude (U=3). Other observation by Jean-Gabriel Bosch, Jacques Michelet and René Roy (2002), Brian Uzpen and Steven Kipp (2002), as well as René Roy and Eric Barbotin (2019), gave nearly identical periods of 14.212, 14.234 and 14.211 hours with an amplitude of 0.4, 0.4 and 0.36 magnitude, respectively (U=3/3/3).

Question: Verify the following claims with "True" or "False": Indeed, the rotation period of 1097 Vicia is 35804.16.
Answer: False