Title: 1101 Clematis
Content:  Clematis is a member of the Alauda family (902), a large family of typically "bright" carbonaceous asteroids and named after its parent body, 702 Alauda. According to a different study, this object is also the namesake of the Clematis family, a small family of 5–16 asteroids hence they may have arisen from the same collisional event. All members have a relatively high orbital inclination. It orbits the Sun in the outermost asteroid belt at a distance of 3.0–3.5 AU once every 5 years and 10 months (2,120 days; semi-major axis of 3.23 AU). Its orbit has an eccentricity of 0.08 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins with its observation as at Goethe Link Observatory in October 1963, more than 35 years after its official discovery observation at Heidelberg.
Title: 1101 Clematis
Content:  1101 Clematis is an Alauda asteroid from the outermost regions of the asteroid belt, approximately 37 kilometers in diameter. It was discovered on 22 September 1928, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany, and assigned the provisional designation. It was named for the flowering plant Clematis. The presumably carbonaceous asteroid has a relatively long rotation period of 34.3 hours.
Title: 1101 Clematis
Content:  In September 2009, a rotational lightcurve of Clematis was obtained from photometric observations by American astronomers Brian Warner at the Palmer Divide Observatory, Colorado, and by Robert Stephens at GMARS (G79, California. Lightcurve analysis gave a synodic rotation period of 34.3 hours with a brightness amplitude of 0.16 magnitude (U=2), which significantly differs from previously reported periods of 6 to 12.68 hours (U=1/2/2/2). While not being a slow rotator, Clematis has a much longer period than that known for most other asteroids, and its small amplitude is indicative for a rather spheroidal shape.
Title: 1101 Clematis
Content:  Clematis is an assumed carbonaceous C-type asteroids, while the overall spectral type for members of the Alauda family is that of a somewhat brighter B-type.
Title: 1101 Clematis
Content:  This minor planet was named after the flowering plant Clematis, a genus within the Ranunculaceae (buttercup or crowfoot family). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H n.a.).
Title: 179 Klytaemnestra
Content:  Photometric observations of this asteroid at the Oakley Observatory in Terre Haute, Indiana, during 2006 gave a light curve with a period of 11.13 ± 0.02 hours and a brightness variation of 0.55 ± 0.02 in magnitude (U=2). A better rated lightcurve, already obtained by Alan Harris in October 1979, gave a period of 11.173 hours with an amplitude of 0.35 (U=3). A modeled lightcurve using photometric data from a larger international collaboration was published in 2016. It gave a period of 11.17342 hours, identical to the 1979-observations by Harris, as well as two spin axes at (65.0°, −6.0°) and (248.0°, −9.0°) in ecliptic coordinates (λ,&thinsp;β).
Title: 19763 Klimesh
Content:  Klimesh is a slow rotator, as it has a rotation period of 101 hours with a brightness variation of 0.67 magnitude. The photometric observations were made by Czech astronomer Petr Pravec at the Ondřejov Observatory during the asteroid's 2011-opposition (U=2). The result supersedes a period of 4.4 hours with an amplitude of 0.12, obtained from a fragmentary lightcurve by Italian astronomer Silvano Casulli (U=1).
Title: 1092 Lilium
Content:  Lilium 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 2.7–3.1 AU once every 4 years and 11 months (1,804 days). Its orbit has an eccentricity of 0.08 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins with a precovery image taken at the Lowell Observatory in July 1906, almost 18 years prior to its official discovery observation at Heidelberg.
Title: 957 Camelia
Content:  Camelia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.2 AU once every 5 years (1,826 days; semi-major axis of 2.92 AU). Its orbit has an eccentricity of 0.08 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 4 October 1926, five years after its official discovery observation.
Title: 117 Lomia
Content:  Lomia (minor planet designation: 117 Lomia) is a large main-belt asteroid that has a nearly circular orbit; the orbital eccentricity is 0.029. It was discovered by French astronomer Alphonse Borrelly on September 12, 1871, from the Marseilles Observatory. The preliminary orbital elements were published in the following year by German astronomer Friedrich Tietjen. The reason for the name is uncertain, but Lutz D. Schmadel believes it is most likely a misspelling of Lamia, the female demon of Greek mythology (the asteroid 248 Lameia is also named after this figure). Photometric observations of this asteroid in 1985 gave a light curve with a period of 9.127 hours and a brightness variation of 0.29 in magnitude. The curve is symmetrical with a single maxima and minima. This object has a spectrum that matches an XC classification; occupying the transition range between an X-type and a C-type asteroid. It has an estimated cross-section diameter of ~148 km. Eight occultations of stars by Lomia have so far been observed, between 2000 and 2018. Four of these events provided two or more chords across the asteroid, including a four-chord event in 2003.

Question: Verify the following claims with "True" or "False": With a mass of 5.7 kgs, 1101 Clematis, has an orbital period of 183309000.0 and an epoch on 31 December 2006.
Answer: True