Photometry and models of selected main belt asteroids - V. 73 Klytia, 377 Campania, and 378 Holmia (original) (raw)

A&A 478, 559-565 (2008)

V. 73 Klytia, 377 Campania, and 378 Holmia

1, T. Michałowski1, M. Kaasalainen2, A. Kryszczyńska1, T. Kwiatkowski1, R. Hirsch1, K. Kamiński1, M. Fagas1, M. Polińska1, F. P. Velichko3, M. J. Michałowski4, C. Snodgrass5, R. Behrend6 and L. Bernasconi7

1 Astronomical Observatory, Adam Mickiewicz University, Słoneczna 36, 60-286 Poznań, Poland e-mail: aniab@lab.astro.amu.edu.pl
2 Department of Mathematics and Statistics, University of Helsinki, PO Box 68, 00014 Helsinki, Finland
3 Institute of Astronomy, Karazin Kharkiv National University, Sums'ka 35, 61022 Kharkiv, Ukraine
4 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
5 European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
6 Geneva Observatory, 1290 Sauverny, Switzerland
7 Les Engarouines Observatory, 84570 Mallemort-du-Comtat, France

Received: 26 October 2007
Accepted: 20 November 2007

Abstract

We present photometric observations of three asteroids: 73 Klytia, 377 Campania, and 378 Holmia, together with their spin and shape models. The models were constructed with the lightcurve inversion method, using all available lightcurves of these objects. In the case of Campania, the long persisting doubts about its rotational period have been resolved. Various authors state periods between 8.48 and 16 h, while the period we determined is $11.664401 \pm 0.000010$ h.

Key words: techniques: photometric / minor planets, asteroids