Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-24T19:49:38.585Z Has data issue: false hasContentIssue false
  • English
  • Français

Occultation by (22) Kalliope and its satellite Linus

Published online by Cambridge University Press:  01 October 2007

M. Sôma ,
T. Hayamizu ,
K. Miyashita ,
T. Setoguchi  and
T. Hirose
M. Sôma
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan email: [email protected]
T. Hayamizu
Affiliation:
Sendai Space Hall, Satsumasendai City, Kagoshima Pref. 895-0005, Japan email: [email protected]
K. Miyashita
Affiliation:
Chikuhoku Junior High School, Omi Village, Higashi-Chikuma Gun, Nagano Pref. 399-7701, Japan email: [email protected]
T. Setoguchi
Affiliation:
Japanese Occultation Information Network, c/o Kagoshima Hi-tech College, Kagoshima City, Kagoshima Pref. 891-0141, Japan email: [email protected]
T. Hirose
Affiliation:
International Occultation Timing Association, 1-13, Shimomaruko 1-chome, Ota Ku, Tokyo 146-0092, Japan email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The occultation of a 9.1 magnitude star by asteroid (22) Kalliope and its satellite Linus was successfully observed in Japan in 2006 November 7.826 UT. This was the first definite observation of an occultation of a satellite of an asteroid that was discovered previously by other means. As a result the position of the satellite relative to Kalliope was obtained to be d = 0.246 ± 0.011 (arcsec), and P = 313.8 ± 2.7 (deg), where d is the angular distance and P is the position angle. The derived size for Kalliope is (209 ± 40)km × (136 ± 26)km (with the major axis in position angle of (8 ± 17) deg), and that for Linus is (33 ± 3) km. From the observations, the occulted star is also found to be a close double star whose separation is about 0.7 mas in position angle of about 300 deg, and the magnitudes of the components are found to be almost the same (~9.9 mag).

Keywords

occultationsminor planetsasteroidsbinaries: close
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S248: A Giant Step: from Milli- to Micro-arcsecond Astrometry , October 2007 , pp. 130 - 131
Copyright
Copyright © International Astronomical Union 2008