New and updated convex shape models of asteroids based on optical data from a large collaboration network

Hanuš, J. and Ďurech, J. and Oszkiewicz, D. A. and Behrend, R. and Carry, B. and Delbo, M. and Adam, O. and Afonina, V. and Anquetin, R. and Antonini, P. and Arnold, L. and Audejean, M. and Aurard, P. and Bachschmidt, M. and Baduel, B. and Barbotin, E. and Barroy, P. and Baudouin, P. and Berard, L. and Berger, N. and Bernasconi, L. and Bosch, J. G. and Bouley, S. and Bozhinova, I. and Brinsfield, J. and Brunetto, L. and Canaud, G. and Caron, J. and Carrier, F. and Casalnuovo, G. and Casulli, S. and Cerda, M. and Chalamet, L. and Charbonnel, S. and Chinaglia, B. and Cikota, A. and Colas, F. and Coliac, J. -F. and Collet, A. and Coloma, J. and Conjat, M. and Conseil, E. and Costa, R. and Crippa, R. and Cristofanelli, M. and Damerdji, Y. and Debackère, A. and Decock, A. and Déhais, Q. and Déléage, T. and Delmelle, S. and Demeautis, C. and Dróżdż, M. and Dubos, G. and Dulcamara, T. and Dumont, M. and Durkee, R. and Dymock, R. and Escalante Del Valle, A. and Esseiva, N. and Esseiva, R. and Esteban, M. and Fauchez, T. and Fauerbach, M. and Fauvaud, M. and Fauvaud, S. and Forné, E. and Fournel, C. and Fradet, D. and Garlitz, J. and Gerteis, O. and Gillier, C. and Gillon, M. and Giraud, R. and Godard, J. -P. and Goncalves, R. and Hamanowa, Hiroko and Hamanowa, Hiromi and Hay, K. and Hellmich, S. and Heterier, S. and Higgins, D. and Hirsch, R. and Hodosan, G. and Hren, M. and Hygate, A. and Innocent, N. and Jacquinot, H. and Jawahar, S. and Jehin, E. and Jerosimic, L. and Klotz, A. and Koff, W. and Korlevic, P. and Kosturkiewicz, E. and Krafft, P. and Krugly, Y. and Kugel, F. and Labrevoir, O. and Lecacheux, J. and Lehký, M. and Leroy, A. and Lesquerbault, B. and Lopez-Gonzales, M. J. and Lutz, M. and Mallecot, B. and Manfroid, J. and Manzini, F. and Marciniak, A. and Martin, A. and Modave, B. and Montaigut, R. and Montier, J. and Morelle, E. and Morton, B. and Mottola, S. and Naves, R. and Nomen, J. and Oey, J. and Ogłoza, W. and Paiella, M. and Pallares, H. and Peyrot, A. and Pilcher, F. and Pirenne, J. -F. and Piron, P. and Polińska, M. and Polotto, M. and Poncy, R. and Previt, J. P. and Reignier, F. and Renauld, D. and Ricci, D. and Richard, F. and Rinner, C. and Risoldi, V. and Robilliard, D. and Romeuf, D. and Rousseau, G. and Roy, R. and Ruthroff, J. and Salom, P. A. and Salvador, L. and Sanchez, S. and Santana-Ros, T. and Scholz, A. and Séné, G. and Skiff, B. and Sobkowiak, K. and Sogorb, P. and Soldán, F. and Spiridakis, A. and Splanska, E. and Sposetti, S. and Starkey, D. and Stephens, R. and Stiepen, A. and Stoss, R. and Strajnic, J. and Teng, J. -P. and Tumolo, G. and Vagnozzi, A. and Vanoutryve, B. and Vugnon, J. M. and Warner, B. D. and Waucomont, M. and Wertz, O. and Winiarski, M. and Wolf, M. (2016) New and updated convex shape models of asteroids based on optical data from a large collaboration network. Astronomy and Astrophysics, 586. A108. ISSN 0004-6361

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    Context. Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. These efforts already provided deep insight into physical properties of main-belt asteroids or large collisional families. Going into finer detail (e.g., smaller collisional families, asteroids with sizes 20 km) requires knowledge of physical parameters of more objects. Aims. We aim to increase the number of asteroid shape models and rotation states. Such results provide important input for further studies, such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides bulk density estimates incombination with known masses, but also constrains theoretical collisional and evolutional models of the solar system. Methods. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as input for the convex inversion method, and derive 3D shape models of asteroids together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that 100 observers who submittheir optical data to publicly available databases. Results. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature, or for which masses will most likely be determined from their gravitational influence on smaller bodies whose orbitaldeflections will be observed by the ESA Gaia astrometric mission. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and three near-Earth asteroids. The shape model revisions and determinations were enabled by using additional optical data from recent apparitions for shape optimization.

    ORCID iDs

    Hanuš, J., Ďurech, J., Oszkiewicz, D. A., Behrend, R., Carry, B., Delbo, M., Adam, O., Afonina, V., Anquetin, R., Antonini, P., Arnold, L., Audejean, M., Aurard, P., Bachschmidt, M., Baduel, B., Barbotin, E., Barroy, P., Baudouin, P., Berard, L., Berger, N., Bernasconi, L., Bosch, J. G., Bouley, S., Bozhinova, I., Brinsfield, J., Brunetto, L., Canaud, G., Caron, J., Carrier, F., Casalnuovo, G., Casulli, S., Cerda, M., Chalamet, L., Charbonnel, S., Chinaglia, B., Cikota, A., Colas, F., Coliac, J. -F., Collet, A., Coloma, J., Conjat, M., Conseil, E., Costa, R., Crippa, R., Cristofanelli, M., Damerdji, Y., Debackère, A., Decock, A., Déhais, Q., Déléage, T., Delmelle, S., Demeautis, C., Dróżdż, M., Dubos, G., Dulcamara, T., Dumont, M., Durkee, R., Dymock, R., Escalante Del Valle, A., Esseiva, N., Esseiva, R., Esteban, M., Fauchez, T., Fauerbach, M., Fauvaud, M., Fauvaud, S., Forné, E., Fournel, C., Fradet, D., Garlitz, J., Gerteis, O., Gillier, C., Gillon, M., Giraud, R., Godard, J. -P., Goncalves, R., Hamanowa, Hiroko, Hamanowa, Hiromi, Hay, K., Hellmich, S., Heterier, S., Higgins, D., Hirsch, R., Hodosan, G., Hren, M., Hygate, A., Innocent, N., Jacquinot, H., Jawahar, S. ORCID logoORCID:, Jehin, E., Jerosimic, L., Klotz, A., Koff, W., Korlevic, P., Kosturkiewicz, E., Krafft, P., Krugly, Y., Kugel, F., Labrevoir, O., Lecacheux, J., Lehký, M., Leroy, A., Lesquerbault, B., Lopez-Gonzales, M. J., Lutz, M., Mallecot, B., Manfroid, J., Manzini, F., Marciniak, A., Martin, A., Modave, B., Montaigut, R., Montier, J., Morelle, E., Morton, B., Mottola, S., Naves, R., Nomen, J., Oey, J., Ogłoza, W., Paiella, M., Pallares, H., Peyrot, A., Pilcher, F., Pirenne, J. -F., Piron, P., Polińska, M., Polotto, M., Poncy, R., Previt, J. P., Reignier, F., Renauld, D., Ricci, D., Richard, F., Rinner, C., Risoldi, V., Robilliard, D., Romeuf, D., Rousseau, G., Roy, R., Ruthroff, J., Salom, P. A., Salvador, L., Sanchez, S., Santana-Ros, T., Scholz, A., Séné, G., Skiff, B., Sobkowiak, K., Sogorb, P., Soldán, F., Spiridakis, A., Splanska, E., Sposetti, S., Starkey, D., Stephens, R., Stiepen, A., Stoss, R., Strajnic, J., Teng, J. -P., Tumolo, G., Vagnozzi, A., Vanoutryve, B., Vugnon, J. M., Warner, B. D., Waucomont, M., Wertz, O., Winiarski, M. and Wolf, M.;