Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Full list of authors: Marciniak, A.; Ďurech, J.; Alí-Lagoa, V.; Ogłoza, W.; Szakáts, R.; Müller, T. G.; Molnár, L.; Pál, A.; Monteiro, F.; Arcoverde, P.; Behrend, R.; Benkhaldoun, Z.; Bernasconi, L.; Bosch, J.; Brincat, S.; Brunetto, L.; Butkiewicz-Bąk, M.; Del Freo, F.; Duffard, R.; Evangelista-Santana, M.; Farroni, G.; Fauvaud, S.; Fauvaud, M.; Ferrais, M.; Geier, S.; Golonka, J.; Grice, J.; Hirsch, R.; Horbowicz, J.; Jehin, E.; Julien, P.; Kalup, Cs.; Kamiński, K.; Kamińska, M. K.; Kankiewicz, P.; Kecskeméthy, V.; Kim, D. -H.; Kim, M. -J.; Konstanciak, I.; Krajewski, J.; Kudak, V.; Kulczak, P.; Kundera, T.; Lazzaro, D.; Manzini, F.; Medeiros, H.; Michimani-Garcia, J.; Morales, N.; Nadolny, J.; Oszkiewicz, D.; Pakštienė, E.; Pawłowski, M.; Perig, V.; Pilcher, F.; Pinel, P.; Podlewska-Gaca, E.; Polakis, T.; Richard, F.; Rodrigues, T.; Rondón, E.; Roy, R.; Sanabria, J. J.; Santana-Ros, T.; Skiff, B.; Skrzypek, J.; Sobkowiak, K.; Sonbas, E.; Stachowski, G.; Strajnic, J.; Trela, P.; Tychoniec, Ł.; Urakawa, S.; Verebelyi, E.; Wagrez, K.; Żejmo, M.; Żukowski, K.
Context. Recent results for asteroid rotation periods from the TESS mission showed how strongly previous studies have underestimated the number of slow rotators, revealing the importance of studying those targets. For most slowly rotating asteroids (those with P > 12 h), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. Also, it is still unclear whether signatures of different surface material properties can be seen in thermal inertia determined from mid-infrared thermal flux fitting. Aims. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. Our goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Methods. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS spacecrafts. In addition to data in the visible range, we also use thermal data from infrared space observatories (mainly IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model. This novel method has so far been applied to only a few targets, and therefore in this work we further validate the method itself. Results. We present the models of 16 slow rotators, including two updated models. All provide good fits to both thermal and visible data.The obtained sizes are on average accurate at the 5% precision level, with diameters found to be in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 h, and the thermal inertia covers a wide range of values, from 2 to
This work was was initiated with the support from the National Science Centre, Poland, through grant no. 2014/13/D/ST9/01818; and from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378 (SBNAF). The work of J.D. was supported by the grant 20-08218S of the Czech Science Foundation. A.P. and R.S. have been supported by the K-125015 grant of the National Research, Development and Innovation Office (NKFIH), Hungary. This project has been supported by the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences. This project has been supported by the GINOP-2.3.2-15-2016-00003 grant of the Hungarian National Research, Development and Innovation Office (NKFIH). L.M. was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has received funding from the LP2018-7/2020 Lendulet grant of the Hungarian Academy of Sciences. The work of T.S.-R. was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). E. P. acknowledges the Europlanet 2024 RI project funded by the European Union's Horizon 2020 Research and Innovation Programme (Grant agreement No. 871149). This article is based on observations obtained at the Observatorio Astronomico do Sertao de Itaparica (OASI, Itacuruba) of the Observatorio Nacional, Brazil. F.M. would like to thank the financial support given by FAPERJ (Process E-26/201.877/2020). E.R., P.A., H.M., M.E. and J.M. would like to thank CNPq and CAPES (Brazilian agencies) for their support through diverse fellowships. Support by CNPq (Process 305409/2016-6) and FAPERJ (Process E-26/202.841/2017) is acknowledged by D.L. The Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and operated by the Institute for Space Studies of Catalonia (IEEC). This article is based on observations made in the Observatorios de Canarias del IAC with the 0.82 m IAC80 telescope operated on the island of Tenerife by the Instituto de Astrofisica de Canarias (IAC) in the Observatorio del Teide. This article is based on observations made with the SARA telescopes (Southeastern Association for Research in Astronomy), whose nodes are located at the Observatorios de Canarias del IAC on the island of La Palma in the Observatorio del Roque de los Muchachos; Kitt Peak, AZ under the auspices of the National Optical Astronomy Observatory (NOAO); and Cerro Tololo Inter-American Observatory (CTIO) in La Serena, Chile. This project uses data from the SuperWASP archive. The WASP project is currently funded and operated by Warwick University and Keele University, and was originally set up by Queen's University Belfast, the Universities of Keele, St. Andrews, and Leicester, the Open University, the Isaac Newton Group, the Instituto de Astrofisica de Canarias, the South African Astronomical Observatory, and by STFC. TRAPPIST-South is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E. Jehin is FNRS Senior Research Associate. Funding for the Kepler and K2 missions are provided by the NASA Science Mission Directorate. The data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Data from Pic du Midi Observatory have been obtained with the 0.6-m telescope, a facility operated by Observatoire Midi Pyrenees and Association T60, an amateur association. We acknowledge the contributions of the occultation observers who have provided the observations in the dataset. Most of those observers are affiliated with one or more of: European Asteroidal Occultation Network (EAON), International Occultation Timing Association (IOTA), International Occultation Timing Association European Section (IOTA/ES), Japanese Occultation Information Network (JOIN), and Trans Tasman Occultation Alliance (TTOA).
With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.