The EURONEAR Lightcurve Survey of Near Earth Asteroids
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This data paper presents lightcurves of 101 near Earth asteroids (NEAs) observed mostly between 2014 and 2017 as part of the EURONEAR photometric survey using 11 telescopes with diameters between 0.4 and 4.2 m located in Spain, Chile, Slovakia and Romania. Most targets had no published data at the time of observing, but some objects were observed in the same period mainly by B. Warner, allowing us to confirm or improve the existing results. To plan the runs and select the targets, we developed the public Long Planning tool in PHP. For preliminary data reduction and rapid follow-up planning we developed the LiDAS pipeline in Python and IRAF. For final data reduction, flux calibration, night linkage and Fourier fitting, we used mainly MPO Canopus. Periods of 18 targets are presented for the first time, and we could solve or constrain rotation for 16 of them. We secured periods for 45 targets (\(U\sim 3\)), found candidate periods for other 16 targets (\(U\sim 2\)), and we propose tentative periods for other 32 targets (\(U\sim 1\)). We observed 7 known or candidate binary NEAs, fiting 3 of them (2102 Tantalus, 5143 Heracles and 68348). We observed 8 known or candidate tumbling NEAs, deriving primary periods for 3 objects (9400, 242708 and 470510). We evidenced rapid oscillations (few minutes) and could fit fast tentative periods TP2 for 5 large newly suggested tumbling or binary candidates (27346, 112985, 285625, 377732, 408980), probably discovering at least one new binary NEA (2011 WO41). We resolved periods of 4 special objects which include two proposed space mission targets (163249 and 101955 Bennu), one very fast rotator NEA discovered by EURONEAR (2014 NL52) and the “Halloween asteroid” (2015 TB145). Using Mercator in simultaneous 3 band MAIA imaging, we could evidence for the first time clear variation in the color lightcurves of 10 NEAs. The periods derived from the g–r color lightcurves are found to match individual band period fits for 4 NEAs (27346, 86067, 112985 and 275976).
KeywordsNear Earth asteroids Lightcurves Rotation periods Binary asteroids Tumbling asteroids
Thanks are due to P. Pravec (Ondřejov Observatory, Czech Republic) for his Asteroid Light Curve (ALC) software used in the data analysis in Modra and for help with fast data transfer of the Danish images. Many thanks are due to Brian Warner for his prompt answers regarding the use of his excellent software MPO Canopus (http://www.minorplanetobserver.com/MPOSoftware/MPOCanopus.htm). The data reduction at Modra was carried out using MaxIm DL (http://diffractionlimited.com/product/maxim-dl) and Astrometrica (http://www.astrometrica.at) software and CMC14 star catallogue (Dymock and Miles 2009). This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. The original description of the VizieR service was published by Ochsenbein et al. (2000). The Isaac Newton Telescope (INT) and William Herschel Telescope (WHT) are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. The INT data was acquired by O. Vaduvescu, ING students and collaborators during the Dutch observing runs W14BN008 and W15BN004, some IAC and ING service programs. Part of the work was based on observations made by O. Vaduvescu and students (run 83-Mercator4) with the Mercator Telescope, operated by the Flemish Community on the island of La Palma at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. The Bennu data was secured by J. Licandro based on service observations (program SW2011a31) acquired with the William Herschel Telescope (WHT). The data collected at Cerro Tololo (CTIO 0.9 m) and La Silla (Danish 1.5 m) was based on the Chilean observing time granted to E. Unda-Sanzana (CNTAC program CN2014B-47), while the Caisey SON data was obtained via collaboration between the Universidad de Antofagasta and the SON program owners. The private remote facility IAO-T35 is owned by A. Aznar in the Spanish province of Valencia. All other accessed facilities, namely Buc-T50, Mod-T60, OT-IAC80 and OSN-T90 are owned by public institutions to which the co-authors are affiliated. J. Licandro and M. Serra-Ricart acknowledge support from the project AYA2015-67772-R (MINECO, Spanish Ministry of Economy and Competitiveness). This research was partially based on observations carried out at the Observatorio de Sierra Nevada (OSN) operated by Instituto de Astrofísica de Andalucía (CSIC). P. Santos-Sanz would like to acknowledge financial support by the European Union’s Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378, the Spanish grant AYA-2014-56637-C2-1-P and the Proyecto de Excelencia de la Junta de Andalucá J.A. 2012-FQM1776. The work at Modra was supported by the Slovak Grant Agency for Science VEGA, Grant 1/0911/17. N. Peixinho acknowledges funding by the Gemini-Conicyt Fund, allocated to project No. 32120036 and by the Portuguese FCT—Foundation for Science and Technology and the European Social Fund (ref: SFRH/BGCT/113686/2015). CITEUC is funded by National Funds through FCT—Foundation for Science and Technology (project: UID/Multi/00611/2013) and FEDER—European Regional Development Fund through COMPETE 2020—Operational Programme Competitiveness and Inter- nationalisation (project: POCI-01-0145-FEDER-006922). R. Toma acknowledges funding her La Palma trip to Armagh Observatory, which is core funded by the Northern Ireland Government. The work of M. Popescu was supported by a grant of from Campus Atlantico Tricontinental run by the Univesidad de Las Palmas de Gran Canaria and Universidad de La Laguna, under Programa Talento Tricontinental 2014 (http://www.ceicanarias.com). Thanks to P. Rodriguez-Gil for serving as IAC CAT observer to acquire data for target 143409 with the ORM-INT. Four Chilean students assisted on training to the SON remote observations (J. P. Colque Saavedra, G. Aravena, A. Herrera and Y. Gomez), and two ING students attended one night training which included some ORM-INT observations (L. Peralta and P. Sowicka). The training in La Palma of the Romanian amateur Radu Cornea was made possible with the support of the Isaac Newton Group in the preparation of the long observing run (5 months) in Tenerife which was sponsored by the following private entities from Sibiu, Romania: Cotidianul Sibiu 100%, the companies Mainetti, Banca Comerciala Carpatica, Farmacia alphaMed, Policlinica ASTRA, SIMPA, Biotechnik, Fritzmeier, Euroconf, Docs Softmedical and Mitropolia Ardealului. Acknowledgements are due to the two anonymous referees whose comments improved our paper.
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