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Table 3

Parameters of the spin models of the five targets studied here, and the uncertainty values.

Sidereal Pole 1 Pole 2 RMSD Observing span N app N lc Method
period [hours] λ p β p λ p β p [mag] (years)

(159) Aemilia
24.4787 139° + 68° 348° + 59° 0.014 1981–2015 6 45 convex LI
± 0.0001 ± 18° ± 8° ± 18° ± 6°
24.4787 139° + 66° 349° + 63° 0.014 ′′ ′′ ′′ SAGE
± 0.0001 ± 7° ± 5° ± 7° ± 6°
(227) Philosophia
26.4614 95° + 19° 272° − 1° 0.011 2006–2016 5 97 convex LI
± 0.0001 ± 5° ± 4° ± 6° ± 2°
26.4612 97° + 16° 271° 0.009 ′′ ′′ ′′ SAGE
± 0.0003 ± 5° ± 5° ± 5° ± 5°
(329) Svea
22.7670 33° + 51° 0.010 1986–2016 6 60 convex LI
± 0.0001 ± 15° ± 10°
22.7671 21 ° +47 ° 0.011 ′′ ′′ ′′ SAGE
± 0.0002 ± 7° ± 5°
(478) Tergeste
16.10308 − 42° 216° − 56° 0.011 1980–2016 6 48 convex LI
± 0.00003 ± 2° ± 3° ± 6° ± 4°
16.10312 − 43° 218 ° 0.011 ′′ ′′ ′′ SAGE
± 0.00003 ± 6° ± 5° ± 9° ± 7°
(487) Venetia
13.34133 78° + 3° 252° + 3° 0.012 1984–2015 8 34 convex LI
± 0.00001 ± 7° ± 10° ± 8° ± 12°
13.34133 70° + 8° 255 ° +8 ° 0.011 ′′ ′′ ′′ SAGE
± 0.00002 ± 6° ± 11° ± 5° ± 10°

Notes. Column 1 gives the sidereal period of rotation; Cols. 2–5 give two sets of pole J2000.0 longitude and latitude; Col. 6 gives the rms deviations of the model lightcurves from the data; Cols. 7–9 give the photometric dataset parameters (observing span, number of apparitions, and individual lightcurve fragments). The last column contains the name of the lightcurve inversion (LI) method. The preferred pole solutions are shown in bold. The second pole solution of (329) Svea, though possible in the lightcurve inversion, was clearly rejected by occultation fitting.

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