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:  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: 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: 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: 487 Venetia
Content:  Venetia orbits the Sun in the middle main-belt at a distance of 2.4–2.9 AU once every 4 years and 4 months (1,593 days). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins in 1913, at the Collegio Romano Observatory (531) in Italy, approximately 17 months after its official discovery observation at Heidelberg.
Title: VB 10
Content:  In May 2009, astronomers from NASA's Jet Propulsion Laboratory, Pasadena, California, announced that they had found evidence of a planet orbiting VB 10, which they designated VB 10b. The 200 in Hale telescope at the Palomar Observatory was used to detect evidence of this planet using the astrometry method. The new planet was claimed to have a mass 6 times that of Jupiter and an orbital period of 270 days. However, subsequent studies using Doppler spectroscopy failed to detect the radial velocity variations that would be expected if such a planet was orbiting this small star. The claimants of VB 10b note that these Doppler measurements only rule out planets more massive than 3 times the mass of Jupiter, but this limit is only half the reported best-fit mass of the planet as originally claimed. The claims for this planet thus fall into a long history of claimed astrometric extrasolar planet detections that were subsequently refuted. By 2016, it was suspected that the asymmetric debris disk signal was mistaken for the long-period planet.
Title: HD 103774
Content:  This star has been under observation as part of a survey using the HARPS spectrogram for a period of 7.5 years. In 2012, the detection of an exoplanetary companion using the radial velocity method was announced. This result was published in January 2013. The object is orbiting close to the host star at a distance of 0.07 AU with a period of just 5.9 days and an eccentricity (ovalness) of 0.09. As the inclination of the orbital plane is unknown, only a lower limit on the mass can be determined; this lower bound is about equal to the mass of Saturn. There is marginal evidence for an infrared excess at a wavelength of 12 μm, indicating the likely grain size. More measurements are needed to confirm this signal.
Title: HD 219077
Content:  From 1998 to 2012, the star was placed under observation using the CORALIE echelle spectrograph at La Silla Observatory. In 2012, the presence of a long-period, wide-orbiting planet was deduced through radial velocity variations. This discovery was published in November of the same year. The estimated mass of the planet is at least ten times that of Jupiter. The discoverers noted that HD 219077 b is among the "three most eccentric planets with a period larger than 5 years" – along with HD 98649 b and HD 166724 b, also found with CORALIE. The reason for this eccentricity is unknown. They submitted HD 219077 b as a candidate for direct imaging, once it gets out to 11.0 AU at apoastron with 375 milliarcseconds of angular separation as seen from Earth.

Question: Verify the following claims with "True" or "False": Indeed. The orbital period of 1097 Vicia is 135589000.0.
Answer: True