107 CAMILLA

'107 Camilla' is one of the largest main belt asteroids. It orbits within the Cybele Group, beyond most of the main belt asteroids. It has a very dark surface and primitive carbonaceous composition. It was discovered by N. R. Pogson on November 17, 1868 and named after Camilla, Queen of the Volsci in Roman mythology. Lightcurve analysis indicates that Camilla's pole most likely points towards ecliptic coordinates (β, λ) = (+51°, 72°) with a 10° uncertainty , which gives it an axial tilt of 29°. Contents Satellite (S/2001 (107) I) External links References Satellite (S/2001 (107) I)

On 1 March, 2001, a satellite of Camilla was found by A. Storrs, F. Vilas, R. Landis, E. Wells, C. Woods, B. Zellner, and M. Gaffey using the Hubble Space Telescope [1]. It has been designated 'S/2001 (107) 1' but has not yet received an official name. Later observations in September 2005 with the VLT allowed the determination of an orbit . Apart from data in infobox, the inclination was found to be 3 ± 1° with respect to an axis pointing towards (β, λ) = (+55°, 75°) . Given the ~10° uncertainty in the actual rotational axis of Camilla, one can say that the orbit's inclination is less than 10°. The satellite is estimated to measure about 11 km in diameter . Assuming a similar density to the primary, this would give it an approximate mass of ~1.5 kg. It has a similar colour to the primary .

External links

★ Data on (87) Sylvia from Johnston's archive (maintained by W. R. Johnston)

★ ''Hubble Finds New Asteroid Moon'' (SpaceDaily.com, 21-03-2001), includes discovery image.

★ ''107 Camilla and S/2001 (107) 1'', orbit data website maintained by F. Marchis. Includes orbit diagrams.

References

1. IAUC 7599
2. IAUC 7599
3. Assuming a similar density to the primary.
4. Supplemental IRAS Minor Planet Survey
5. ''Shapes and rotational properties of thirty asteroids from photometric data'', J. Torppa et al, , , Icarus, 2003
6. ''Shape, size and multiplicity of main-belt asteroids I. Keck Adaptive Optics survey'', F. Marchis et al, , , Icarus, 2006
7. Axis ratios (rounded to nearest 5 km) based on lightcurve analysis of Torppa et al (2003), however taking IRAS mean diameter is inconsistent with the maximum value of the short axis obtained in Marchis et al (2006). Hence, presumably IRAS measurements were taken of a large face. Therefore, anchoring absolute size by reuqiring the shortest axis to be no larger than the maximum allowed by Marchis et al (2006).
8. ''107 Camilla and S/2001 (107) 1'', F. Marchis
9. Error estimate derived from consideration of $M\; propto\; a^3/P^2$ and given errors in ''a'' and ''P''. See propagation of uncertainty.
10. PDS spectral class data