Adaptive optics observations of asteroid (216) Kleopatra

Hestroffer, Daniel; Marchis, Franck; Fusco, Thierry; Berthier, J.

doi:10.1051/0004-6361:20021094

Cited by 19 publications

(17 citation statements)

References 15 publications

(24 reference statements)

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“…• , β = 23 • , which had been confirmed by Hestroffer et al (2002b) with the adaptive optics technique. Model shapes and scattering functions are mentioned in the following sections.…”

Section: Lightcurve Simulationsmentioning

confidence: 57%

“…The two observations by the radar and interferometric techniques indicated that (216) Kleopatra had a shape with two components in contact, but Hestroffer et al (2002b) suggested that the two bodies could be separated by analyzing data from an adaptive optics system, ADONIS, installed on the 3.6 m ESO telescope, using the MISTRAL deconvolution technique. Binary model-Roche Binary Equal-sized binary asteroids in the size range of 100 km could be formed by catastrophic collisions (Farinella et al, 1982).…”

Section: Lightcurve Simulationsmentioning

confidence: 99%

“…Ostro et al (2000) estimated the dimensions of (216) ponents are so close as to be in contact; that is, the binary system is almost at the Roche limit. Hestroffer et al (2002b) have reported that the flux ratio of the primary to the secondary was F = 0.81 ± 0.03. The flux ratio of the model by Cellino et al (1985) at the time of Hestroffer et al (2002b) observations varied between 0.79-0.84 during one rotation, which is consistent with the observations.…”

Section: Roche Binary Modelmentioning

confidence: 99%

“…Both models indicated that (216) Kleopatra had a shape with two components in contact. On the other hand, Hestroffer et al (2002b) suggested that the two bodies could possibly be resolved with an adaptive optics observations in 1999.…”

Section: Introductionmentioning

confidence: 99%

“…We have performed simultaneous observations of (216) Kleopatra by both photometric and polarimetric techniques using the HBS spectro-photo-polarimeter at Dodaira Observatory (Kawabata et al, 1999), Astronomical Observatory of Japan in November 1999, when the adaptive optics observations were done by Hestroffer et al (2002b). It is well known that some asteroids have correlations between variations of photometric magnitude and polarization due to the changes in surface albedos (Dollfus et al, 1989;Nakayama et al, 2000 and others).…”

Section: Introductionmentioning

confidence: 99%

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Photometric and polarimetric observations and model simulations of (216) Kleopatra

et al. 2014

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We performed photometric and polarimetric observations, on November 8 and 9, 1999, of an M-type main belt asteroid, (216) Kleopatra by using the HBS spectropolarimeter installed at Dodaira observatory, National Astronomical Observatory of Japan (NAOJ). Photometric amplitude of lightcurve in the V band was 0.12 mag, and the averaged degree of polarization was −1.01±0.1%. It seems that the polarimetric data might also show a slight change in the degree of polarization (∼0.2%) at the second minimum of the photometric lightcurve, but we could not confirm that the feature was real because of the large errors of data. With the assumption that the surface is uniform, we have carried out lightcurve simulations based on shape models by Ostro et al. (2000), Tanga et al. (2001) and Roche binary (Cellino et al., 1985). The results of simulations were compared to the configurations of lightcurves which had been obtained at different 4 geometric positions (1980, 1982, 1987 and 1999). The model by Cellino et al. (1985) reproduced almost all the data points without the 1987 observations within ∼0.05 mag., which is the best result among the 3 models. The model by Tanga et al. (2001) well reproduced the lightcurves, but failed in reproducing the 1982 amplitude (difference diff ∼ 0.2 mag.). We also confirmed that the model by Ostro et al. (2000) could not explain the observed lightcurves.

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“…• , β = 23 • , which had been confirmed by Hestroffer et al (2002b) with the adaptive optics technique. Model shapes and scattering functions are mentioned in the following sections.…”

Section: Lightcurve Simulationsmentioning

confidence: 57%

Section: Lightcurve Simulationsmentioning

confidence: 99%