Opposition polarimetry and photometry of S- and E-type asteroids

Belskaya, I. N.; Shevchenko, V. G.; Kiselev, N. N.; Krugly, Yu. N.; Shakhovskoy, N. M.; Efimov, Yurij S; Gaftonyuk, N. M.; Cellino, A.; Gil-Hutton, R.

doi:10.1016/j.icarus.2003.09.005

Cited by 43 publications

(34 citation statements)

References 25 publications

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“…(2867) Steins is an E-type, a type of asteroid that generally presents a strong opposition effect (Belskaya et al, 2003). This body was one of the Rosetta asteroid targets and was observed with the OSIRIS camera in similar conditions to (21) Lutetia, having a phase angle that ranged from 0.36 to 141 degrees and varying pixel resolution.…”

Section: Discussionmentioning

confidence: 99%

Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Hasselmann

Fornasier

Leyrat

et al. 2016

Icarus

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ABSTRACT. (21) Lutetia has been visited by Rosetta mission on July 2010 and observed with a phase angle ranging from 0.15 to 156.8 degrees. The Baetica region, located at the north pole has been extensively observed by OSIRIS cameras system. Baetica encompass a region called North Pole Crater Cluster (NPCC), shows a cluster of superposed craters which presents signs of variegation at the small phase angle images. For studying the location, we used 187 images distributed throughout 14 filter recorded by the NAC (Narrow Angle Camera) and WAC (Wide Angle Camera) of the OSIRIS system on-board Rosetta taken during the fly-by. Then, we photometrically modeled the region using Minnaert diskfunction and Akimov phase function to obtain a resolved spectral slope map at phase angles of 5 • and 20 • . We observed a dicothomy between Gallicum and Danuvius-Sarnus Labes in the NPCC, but no significant phase reddening (−0.04 ± 0.045% · microns −1 deg −1 ). In the next step, we applied the Hapke (2008Hapke ( ,2012 model for the NAC F82+F22 (649.2 nm), WAC F13 (375 nm) and WAC F17 (631.6 nm) and we obtained normal albedo maps and Hapke parameter maps for NAC F82+F22. On Baetica, at 649.2 nm, the geometric albedo is 0.205 ± 0.005, the average single-scattering albedo is 0.181 ± 0.005, the average asymmetric factor is −0.342 ± 0.003, the average shadow-hiding opposition effect amplitude and width are 0.824 ± 0.002 and 0.040 ± 0.0007, the average roughness slope is 11.45 • ± 3 • and the average porosity is 0.85 ± 0.002. We are unable to confirm the presence of coherent-backscattering mechanism. In the NPCC, the normal albedo variegation among the craters walls reach 8% brighter for Gallicum Labes and 2% fainter for Danuvius Labes. The Hapke parameter maps also show a dicothomy at the opposition effect coefficients, single-scattering albedo and asymmetric factor, that may be attributed to the maturation degree of the regolith or to compositonal variation. In addition, we compared the Hapke (2008Hapke ( , 2012 and Hapke (1993) parameters with laboratory samples and other small-solar system bodies visited by space missions.

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Section: Discussionmentioning

confidence: 99%

Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Hasselmann

Fornasier

Leyrat

et al. 2016

Icarus

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“…6). Recently, it was shown that observed F-type Belskaya et al (2003Belskaya et al ( , 2005, Chernova et al (1994), Lupishko et al (1994), andCellino et al (2005). asteroids are characterized by substantially smaller depths of the negative polarization branch, as compared to other low albedo asteroids. In addition, they have unusually small inversion angles (Belskaya et al 2005).…”

Section: Low Albedo Asteroidsmentioning

confidence: 96%

Polarimetric survey of asteroids with the Asiago telescope

Fornasier¹,

Belskaya²,

Shkuratov³

et al. 2006

A&A

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Aims. We present the first results of an asteroid photo-polarimetry program started at Asiago-Cima Ekar Observatory. The aim of our survey is to estimate diversity in polarimetric properties of asteroids belonging to different taxonomic and dynamical classes. Methods. The data were obtained with the polarization analyser placed inside the Faint Object Spectrographic Camera (AFOSC) of the 1.8 m telescope. This instrument allows simultaneous measurements of the two first Stokes parameters without any λ/2 retarding plate. Results. Our survey began in 2002, and up to now we have obtained data on a sample of 36 asteroids; most of them are being investigated with the polarimetric technique for the first time. Combining our data with those already available in literature, we present an estimate of the inversion angle for 7 asteroids in this paper. Furthermore, we present the polarimetric measurements of the rare asteroid classes belonging to the A and D types and a detailed VRI observations at extremely small phase angles of the low albedo asteroid 1021 Flammario

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“…It is also worth to be mentioned here that in dark asteroids the usual correlation between the angular parameters of the opposition effects in brightness and polarization of relatively high-albedo objects was not found (e.g., Belskaya et al, 2003). This can be explained not only by the increase of the shadow hiding contribution to the opposition brightening for the objects with low albedo, but also by the strengthening in the field inhomogeneity close to the particles.…”

Section: Opposition Effects: the Results Of The Manifestation Of Diffementioning

confidence: 79%