Abstract
Here we present the results of visible range light curve observations of ten Centaurs using the Kepler Space Telescope in the framework of the K2 mission. Well defined periodic light curves are obtained in six cases allowing us to derive rotational periods, a notable increase in the number of Centaurs with known rotational properties.The low amplitude light curves of (471931) 2013 PH44 and (250112) 2002 KY14 can be explained either by albedo variegations, binarity or elongated shape. (353222) 2009 YD7 and (514312) 2016 AE193 could be rotating elongated objects, while 2017 CX33 and 2012 VU85 are the most promising binary candidates due to their slow rotations and higher light curve amplitudes. (463368) 2012 VU85 has the longest rotation period, P = 56.2 h observed among Centaurs. The P > 20 h rotation periods obtained for the two potential binaries underlines the importance of long, uninterrupted time series photometry of solar system targets that can suitably be performed only from spacecraft, like the Kepler in the K2 mission, and the currently running TESS mission.
Highlights
Centaurs are small solar system objects on non-resonant, giant planet crossing orbits (Gladman et al, 2008), which leads to frequent en counters with the giant planets and results in short dynamical lifetimes
In this paper we report on observations of ten Centaurs: (250112) 2002 KY14, (353222) 2009 YD7, 2010 GX34, 2010 JJ124, (499522) 2010 PL66, (463368) 2012 VU85, (471931) 2013 PH44, (472760) 2015 FZ117, (514312) 2016 AE193, and (523798) 2017 CX33,1 observed with Kepler in the K2 campaigns
As demon strated in Molna r et al (2018) the best fit frequencies obtained with this method are identical to the results of Lomb–Scargle periodogram or fast Fourier transform analyses, with a notably smaller general uncertainty in the residuals
Summary
Centaurs are small solar system objects on non-resonant, giant planet crossing orbits (Gladman et al, 2008), which leads to frequent en counters with the giant planets and results in short dynamical lifetimes. These studies were carried out in the course of systematic programs in the K2 mission, aimed at obtaining light curves of solar system targets, including main belt asteroids (Szabo et al, 2015, 2016; Berthier et al, 2016; Moln ar et al, 2018), Jovian Trojans (Ryan et al, 2017; Szabo et al, 2017), transneptunian objects (P al et al, 2015a, 2015b, 2016; Benecchi et al, 2018) and irregular moons of giant planets (Kiss et al, 2016; Farkas-Taka cs et al, 2017) These observations pro vided continuous light curves which had significantly longer time-spans (up to 80 d) than ground-based measurements and could break the ambiguity of rotational periods caused by daily aliases. As demon strated in Molna r et al (2018) the best fit frequencies obtained with this method are identical to the results of Lomb–Scargle periodogram or fast Fourier transform analyses, with a notably smaller general uncertainty in the residuals
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