Title: 580 Selene
Content:  Selene (minor planet designation: 580 Selene) is a minor planet orbiting the Sun in the asteroid belt. The name Selene is that of an ancient Greek goddess of the Moon. The name may have been inspired by the asteroid's provisional designation 1905 SE. This body orbits the Sun nearly midway between the orbits of Mars and Jupiter. The orbital eccentricity is slightly lower than that of Mars. Based on its light curve, Selene has an estimated rotation period of 0.3947±0.0004 days, or just under 9.5 hours. During each rotation, the apparent magnitude varies by 0.27. The approximate diameter of this asteroid is 46 km. (Some sources list a diameter of up to 56 km.) The albedo is about 7%, comparable to that of the Earth's Moon.
Title: 956 Elisa
Content:  In July 2008, a rotational lightcurve of Elisa was obtained from photometric observations by Matthieu Conjat at Nice Observatory in France. Lightcurve analysis gave a well-defined rotation period of 16.492 hours with a brightness variation of 0.36 magnitude (U=3). During the same opposition, Vladimir Benishek at Belgrade Observatory and Lucy Lim with the Spitzer-team determined a period for this asteroid of 16.508 and 16.494 hours with an amplitude of 0.37 and 0.35 magnitude, respectively (U=3/3–).
Title: 1374 Isora
Content:  In January 2014, a rotational light-curve of Isora was obtained by American astronomer Robert D. Stephens at the Center for Solar System Studies (CS3) in California. Light-curve analysis gave a longer than average rotation period of 36.699 hours with a brightness variation of 0.12 magnitude (U=2+). However, a second period solution of 18.35 hours is also possible. The result supersedes photometric observations taken by Wiesław Z. Wiśniewski in 1989, which rendered a fragmentary light-curve with a period of 8 hours (U=1). The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a diameter of 5.48 kilometers using an absolute magnitude of 13.67.
Title: 5331 Erimomisaki
Content:  In December 2007, two rotational lightcurve of Erimomisaki were obtained from photometric observations by international collaboration between astronomers Silvano Casulli, Russel Durkee, Caleb Boe, Fiona Vincent and David Higgins. Lightcurve analysis gave a longer-than-average rotation period of 24.233 and 24.26 hours with a brightness amplitude of 0.42 and 0.27 magnitude, respectively (U=2/3-). CALL adopts the longer period as its best result. While not being a slow rotator, Erimomisaki period is longer than that of most other asteroids, which have spin rates between 2 and 20 hours.
Title: 919 Ilsebill
Content:  In October 2010, a rotational lightcurve of Ilsebill was obtained from photometric observations by Zachary Pligge, Ben Hall and Richard Ditteon at the U.S. Oakley Observatory in Indiana. Lightcurve analysis gave a well-defined rotation period of 5.033 hours with a brightness variation of 0.25 magnitude (U=3). In September 2010, a similar, though lower rated period of 5.034 hours with an amplitude of 0.24 was determined by astronomers at the Palomar Transient Factory in California (U=2). A modeled lightcurve using photometric data from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) was published in 2018. It gave a concurring sidereal period of 5.033 hours and includes a partial spin axis at (β1 = −53.0°) in ecliptic coordinates (λ,&thinsp;β).
Title: 2074 Shoemaker
Content:  In October 2003, photometric observations of Shoemaker by Robert D. Stephens gave a long rotation period of 57.02 hours. After re-measuring the images with newer software and calibration techniques, two mutual occultation and eclipsing events were found, indicating that Shoemaker might be a synchronous binary asteroid with a minor-planet moon orbiting it every 55 hours. Observations in 2010, were difficult due to incomplete coverage and gave an orbital period of 27.39 hours for the secondary. Observations by astronomers at Etscorn Campus Observatory (719) in 2015, did not mention any mutual events. In June 2017, Warner measured a rotation period of 2.533 hours and an orbital period for the secondary of 44.28 hours at his CS3-Palmer Divide Station in California. The binary nature of Shoemaker remains unconfirmed.
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: 957 Camelia
Content:  In August 2000, a rotational lightcurve of Camelia was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado. The originally published lightcurve analysis gave a wrong rotation period of 5.391 hours with a brightness variation of 0.32 magnitude (U=0). In July 2010, and with the availability of improved analysis tools and techniques along with the experience gained over more than a decade, Warner reviewed and recalibrated the original data set and determined a period of at least 150 hours with an amplitude of more than 0.3 (U=1+). With such a long period, Camelia is a slow rotator. While the slowest rotators have periods above 1000 hours, the vast majority of asteroids have a much shorter rotation period of 2.2 to 20 hours.
Title: 1079 Mimosa
Content:  Several fragmentary rotational lightcurves of Mimosa have been obtained from photometric observations since 1983. Lightcurve analysis gave a consolidated rotation period of 64.6 hours with a brightness amplitude between 0.07 and 0.13 magnitude (U=2-). While not being a slow rotator, this is a notably longer-than average period as most asteroids take less than 20 hours to complete a full rotation. However, the period is based on a fragmentary lightcurve and still may change significantly. As of 2017, no secure period has been obtained.
Title: (162058) 1997 AE12
Content:  The most unusual feature of, however, is its exceptionally slow rotation period of 1,880 hours, or approximately 11 weeks (U=2). It holds the record for being the slowest-rotating asteroid discovered so far. Its precise period with a smaller error margin still needs to be determined. The lightcurve also showed a high brightness variation of at least 0.6 magnitude, which is indicative for a non-spherical shape. The asteroid may also be in a tumbling motion, but observations are not sufficient to determine any non-principal axis rotation. Like other slowly-rotating asteroids such as 912 Maritima, it is possible that the extremely long period of this asteroid is caused by YORP radiation pressure slowing down the asteroid's rotation. This is especially likely considering that has a very low albedo, which would allow it to absorb more radiant energy from the Sun. Furthermore, the YORP effect has also been observed on other Q-type asteroids such as 1862 Apollo.

Question: Verify the following claims with "True" or "False": 190 Ismene has a rotation period of 95040.0 and an apoapsis of 511592000.0 km.
Answer: False