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: 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: 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: 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:  This minor planet was named after the flowering plant Vicia, member of the Fabaceae (legume family). It is commonly known as vetches. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 103).
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: 1030 Vitja
Content:  Vitja is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.5 AU once every 5 years and 6 months (2,014 days; semi-major axis of 3.12 AU). Its orbit has an eccentricity of 0.12 and an inclination of 15° with respect to the ecliptic. The asteroid's first recorded observation was made a week after its official discovery at Heidelberg Observatory in June 1924, while its observation arc begins more than seven years later at Lowell Observatory in October 1931.
Title: 807 Ceraskia
Content:   In October 2017, a rotational lightcurve of Ceraskia was obtained from photometric observations by Matthieu Conjat at Nice Observatory in France. Lightcurve analysis gave a well-defined rotation period of 7.368 hours with a brightness variation of 0.39 magnitude (U=3). The result supersedes previous observations by Richard Binzel in April 1983 and by astronomers at the Palomar Transient Factory in California on October 2012, which gave a period of 7.4 and 7.375 hours with an amplitude of 0.25 and 0.49 magnitude, respectively (U=2/2). Lightcurve inversion also modeled the body's shape and poles. In 2013, modelling by an international study using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory and the Catalina Sky Survey gave a concurring sidereal period of 7.374 hours and two spin axes of (325.0°, 23.0°) and (132.0°, 26.0°) in ecliptic coordinates (λ,&thinsp;β). The body's very elongated shape had already been indicated by the relatively high brightness variation measured during the direct photometric observations.
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: 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 

Question: Verify the following claims with "True" or "False": 1097 Vicia does have a rotation period of 9058.32.
Answer: False