Rotational properties of the binary and non-binary populations in the trans-Neptunian belt

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Volume 569 (September 2014)

A&A, 569 (2014) A3

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Issue		A&A Volume 569, September 2014


Article Number		A3
Number of page(s)		20
Section		Planets and planetary systems
DOI		https://doi.org/10.1051/0004-6361/201423567
Published online		08 September 2014

Online material

Appendix A

	Fig. A.1 Lomb-normalized spectral power versus frequency in cycles/day for Varda: the Lomb periodogram of our data sets shows that one highest peak is located at 5.91 h (4.06 cycles/day) and the two largest aliases are at 7.87 h (3.04 cycles/day) and at 4.76 h (5.04 cycles/day).
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	Fig. A.2 Varda light curve: rotational phase curve for Varda obtained by using a spin period of 5.91 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates.
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	Fig. A.3 Lomb-normalized spectral power versus frequency in cycles/day for Salacia: the Lomb periodogram shows one main peak located at 3.69 cycles/day (6.5 h) and one alias at 2.71 cycles/day (8.86 h).
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	Fig. A.4 Salacia light curve: rotational phase curve for Salacia obtained by using a spin period of 6.5 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates.
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	Fig. A.5 Lomb-normalized spectral power versus frequency in cycles/day for 2007 UK₁₂₆: the Lomb periodogram shows one peak with the highest spectral power located at 11.04 h (2.17 cycles/day), and several aliases located at 14.30 h (1.68 cycles/day) and at 20.25 h (1.19 cycles/day).
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	Fig. A.6 2007 UK₁₂₆ light curve: rotational phase curve for 2007 UK₁₂₆ obtained by using a spin period of 11.05 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates.
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	Fig. A.7 Lomb-normalized spectral power versus frequency in cycles/day for Huya: the Lomb periodogram shows one main peak located at 5.28 h (4.55 cycles/day), and three aliases located at 6.63 h (3.62 cycles/day), at 4.31 h (5.57 cycles/day), and at 9.15 h (2.62 cycles/day).
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	Fig. A.8 Huya light curve: rotational phase curve for Huya obtained by using a spin period of 5.28 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates.
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Table A.1

Dates (UT-dates, format MM/DD/YYYY), heliocentric (r_h), and geocentric (Δ) distances, and phase angle (α).

Table A.2

Short-term variability of BTNOs.

Table A.3

Density, size, and albedo from this work and from the literature.

Table A.4

System names, Love number of the primary (k_primary), primary and satellite densities (ρ_primary and ρ_satellite), initial rotational rate of the primary (T₀), mean orbital angular velocity (n), and orbital semimajor axis (a).

Table A.5

System names, secondary-to-primary mass ratio (q), semi-major axis (a), eccentricity (e), primary radius (R_p), rotational period of the primary and its critical rotational period (P_p, and P_c), and the λ shape parameter of the primary (λ_p) and satellite.

© ESO, 2014

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