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New and Updated Convex Shape Models of Asteroids Based on Optical Data from a Large Collaboration Network

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New and Updated Convex Shape Models of Asteroids Based on Optical Data from a Large Collaboration Network A&A 586, A108 (2016) Astronomy DOI: 10.1051/0004-6361/201527441 & c ESO 2016 Astrophysics New and updated convex shape models of asteroids based on optical data from a large collaboration network J. Hanuš1,2,J.Durechˇ 3, D. A. Oszkiewicz4,R.Behrend5,B.Carry2,M.Delbo2,O.Adam6, V. Afonina7, R. Anquetin8,45, P. Antonini9, L. Arnold6,M.Audejean10,P.Aurard6, M. Bachschmidt6, B. Baduel6,E.Barbotin11, P. Barroy8,45, P. Baudouin12,L.Berard6,N.Berger13, L. Bernasconi14, J-G. Bosch15,S.Bouley8,45, I. Bozhinova16, J. Brinsfield17,L.Brunetto18,G.Canaud8,45,J.Caron19,20, F. Carrier21, G. Casalnuovo22,S.Casulli23,M.Cerda24, L. Chalamet86, S. Charbonnel25, B. Chinaglia22,A.Cikota26,F.Colas8,45, J.-F. Coliac27, A. Collet6,J.Coloma28,29, M. Conjat2,E.Conseil30,R.Costa28,31,R.Crippa32, M. Cristofanelli33, Y. Damerdji87, A. Debackère86, A. Decock34, Q. Déhais36, T. Déléage35,S.Delmelle34, C. Demeautis37,M.Dró˙zd˙z38, G. Dubos8,45, T. Dulcamara6, M. Dumont34, R. Durkee39, R. Dymock40, A. Escalante del Valle85, N. Esseiva41, R. Esseiva41, M. Esteban24,42, T. Fauchez34, M. Fauerbach43,M.Fauvaud44,45,S.Fauvaud8,44,45,E.Forné28,46,†, C. Fournel86,D.Fradet8,45, J. Garlitz47, O. Gerteis6, C. Gillier48, M. Gillon34, R. Giraud34, J.-P. Godard8,45,R.Goncalves49, Hiroko Hamanowa50, Hiromi Hamanowa50,K.Hay16, S. Hellmich51,S.Heterier52,53, D. Higgins54,R.Hirsch4, G. Hodosan16,M.Hren26, A. Hygate16, N. Innocent6, H. Jacquinot55,S.Jawahar56, E. Jehin34, L. Jerosimic26,A.Klotz6,57,58,W.Koff59, P. Korlevic26, E. Kosturkiewicz4,38,88,P.Krafft6, Y. Krugly60, F. Kugel19,O.Labrevoir6, J. Lecacheux8,45, M. Lehký61, A. Leroy8,45,62,63, B. Lesquerbault6, M. J. Lopez-Gonzales64,M.Lutz6, B. Mallecot8,45, J. Manfroid34, F. Manzini32, A. Marciniak4, A. Martin65,66, B. Modave6, R. Montaigut8,45,48,63, J. Montier52,53, E. Morelle27, B. Morton16, S. Mottola51,R.Naves67,J.Nomen26,J.Oey68,W.Ogłoza38, M. Paiella33, H. Pallares28,69,A.Peyrot58, F. Pilcher70, J.-F. Pirenne6, P. Piron6,M.Polinska´ 4, M. Polotto6, R. Poncy71,J.P.Previt53,F.Reignier72,D.Renauld6, D. Ricci34, F. Richard8,45, C. Rinner73, V. Risoldi33, D. Robilliard53,D.Romeuf74, G. Rousseau75,R.Roy76, J. Ruthroff77, P. A. Salom 24,42,L.Salvador6, S. Sanchez26, T. Santana-Ros4,A.Scholz16,G.Séné6,B.Skiff78, K. Sobkowiak4, P. Sogorb79,F.Soldán80, A. Spiridakis35,E.Splanska6,S.Sposetti81, D. Starkey82, R. Stephens83, A. Stiepen34, R. Stoss26, J. Strajnic6,J.-P.Teng58, G. Tumolo84, A. Vagnozzi33,B.Vanoutryve6, J. M. Vugnon8,45,B.D.Warner83, M. Waucomont6, O. Wertz34, M. Winiarski38,†,andM.Wolf3 (Affiliations can be found after the references) Received 24 September 2015 / Accepted 22 October 2015 ABSTRACT 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 in combination 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 submit their 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 orbital deflections 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. Key words. minor planets, asteroids: general – techniques: photometric – methods: observational – methods: numerical † Deceased. Article published by EDP Sciences A108, page 1 of 24 A&A 586, A108 (2016) 1. Introduction and collisional dynamical evolution (Kryszczynska´ 2013; Hanuš et al. 2013a); (v) the larger dispersion of spin-axis directions of Asteroid modeling efforts in the last decade resulted in an ex- smaller (D 50 km) prograde than retrograde asteroids suggests tensive dataset of almost 400 convex shape models and rotation that spin states of prograde rotators are affected by resonances states (see the review by Durechˇ et al. 2015a). The major- (Hanuš et al. 2013c); or (vi) the disruption of asteroid pairs4 was ity of these models was determined by the lightcurve inver- most likely the outcome of the YORP effect that spun up the sion method (LI) developed by Kaasalainen & Torppa (2001) original asteroid (Polishook 2014). and Kaasalainen et al. (2001). About 100 models are based on With the use of convex shape models in combination with as- disk-integrated, dense-in-time optical data (e.g., Torppa et al. teroidal stellar occultations and disk-resolved images obtained 2003; Slivan et al. 2003; Michałowski et al. 2005; Marciniak by space telescopes or ground-based telescopes equipped with et al. 2009, 2011). Combining dense-in-time data with sparse-in- adaptive optics (AO) systems, the size of the model can be con- time measurements from large sky surveys, or using only sparse- strained, making it possible to determine the asteroid volume. in-time data, increased the number of available shape models by Even when the object is considerably nonconvex, the scaled con- a factor of 4 (Durechˇ et al. 2009; Hanuš et al. 2011, 2013a,c). vex model from occultations and AO data tends to compensate Future data from Gaia, Panoramic Survey Telescope and Rapid by average fitting to the disk-resolved data. As a result, the over- Response System (PanSTARRS), and Large Synoptic Survey estimation of the volume is smaller than would correspond to the Telescope (LSST) should result in an increase of shape mod- convex hull. The volume can then provide, in combination with els by an order of at least one magnitude (Durechˇ et al. 2005). mass estimates, realistic values of bulk densities (Durechˇ et al. The methods that will be used for analysis of these future data 2011; Hanuš et al. 2013b). of unprecedented amount and quality, by the means of complex The mass is one of the most challenging parameters to mea- shape modeling, are similar to those applied here and developed sure for an asteroid. Mass estimates are now available for 280 as- within the scope of our recent studies. teroids, but only 113 of these are more precise than 20% (Carry Most asteroid shape models derived by the LI method and 2012; Scheeres et al. 2015). However, the situation is expected their optical data are available in the Database of Asteroid to improve significantly in the near future. The observations of the ESA Gaia astrometric satellite will provide masses accurate Models from Inversion Techniques (DAMIT1; Durechˇ et al. to better than 50% for ≈150 asteroids (and for ≈50 with an ac- 2010). curacy better than 10%; Mouret et al. 2007, 2008) by the orbit We would like to emphasize and acknowledge that the shape deflection method. The advantage of the masses determined by modeling stands on the shoulders of hundreds of observers, often Gaia is in the uniqueness of the mission: we should obtain a amateurs, who regularly obtain photometric data with their small comprehensive sample with well-described biases (e.g., the cur- and mid-sized telescopes. These observations have significantly rent mass estimates are currently strongly biased toward the in- contributed to the great progress of the shape modeling field in ner main belt). the last decade. Although there is much more sparse than dense To maximize the possible outcome by means of density de- data available, the latter will always remain important because terminations, we focus on determination of shape models for as- their much higher photometric accuracy and rotation coverage teroids for which accurate mass estimates are available or will leads to higher quality shape models. This is a typical example most likely be determined by Gaia. Moreover, it is also impor- of the great interaction between the professional and amateur tant to update shape models for such asteroids using recently community (Mousis et al. 2014). obtained optical data. By doing this, we can provide better con- Knowing the rotational parameters and shapes of asteroids straints on the rotational phase (i.e., on the asteroid orientation, is very important for numerous applications. The large amount which is important for scaling the size) of these asteroids due to of currently known asteroid models already provided a deep the improvement of the rotation period, and more accurate rota- insight into physical properties of main-belt asteroids (MBAs) tion state and shape parameters. and large collisional families: (i) an excess of prograde rotators Convex models, together with thermal infrared observations, within (MBAs) larger than ∼50 km in diameter, predicted by nu- have also been used as inputs for thermophysical modeling, merical simulations (Johansen & Lacerda 2010), was confirmed enabling the determination of geometric visible albedo, size, by Kryszczynska´ et al.
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