Table 1 Best spin and pole solutions of 1998 KY26 obtained with the convex and SAGE modelling techniques, ordered by goodness of fit

From: Hayabusa2 extended mission target asteroid 1998 KY26 is smaller and rotating faster than previously known

Solution

λ (°)

β (°)

Spin period (min)

rms-value

Convex#1

29 ± 7 ( ± 1)

− 41 ± 7 ( ± 2)

5.3515986 ± 0.00018 ( ± 0.0000003)

0.106

Convex#2

208 ± 14 ( ± 1)

37 ± 7 ( ± 2)

5.3512902 ± 0.00036 ( ± 0.0000003)

0.108

Convex#3

225 ± 3 ( ± 1)

− 38 ± 6 ( ± 2)

5.3516346 ± 0.00018 ( ± 0.0000003)

0.113

Convex#4

287 ± 13 ( ± 1)

31 ± 20 ( ± 1)

5.3513970 ± 0.00012 ( ± 0.0000003)

0.117

SAGE#1

\(3{6}_{-5}^{+6}\)

\(-4{4}_{-10}^{+12}\)

5.3516 ± 0.0001

0.106

SAGE#2

\(23{2}_{-7}^{+6}\)

\(-4{4}_{-9}^{+22}\)

\(5.351{6}_{-0.0002}^{+0.0028}\)

0.107

SAGE#3

\(4{7}_{-4}^{+8}\)

\(3{7}_{-17}^{+14}\)

\(5.351{3}_{-0.0002}^{+0.0001}\)

0.111

SAGE#4

\(26{2}_{-12}^{+13}\)

\(6{1}_{-17}^{+26}\)

\(5.351{3}_{-0.0058}^{+0.0028}\)

0.114

  1. The convex solutions include two uncertainties: the ones next to the parameter values refer to the full range of plausible periods and the ones in parentheses refer to Markov chain Monte Carlo (MCMC) 1-σ values for a period fixed to the best solution given. The latter uncertainty for the period refers to the approximate interval between plausible discrete periods allowed by the photometric data.
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