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Table 1

Best-fitting values of size (D) and beaming parameter (η) and corresponding visible geometric albedos (pV) for all our objects.

Object H G D (km) p V η n W2 n W3 n W4 r (au) Δ (au) α (degree) MJD

00132 9.38 0.15 50.13 0.124 0.92 0 15 15 3.30812 3.14966 17.88688 55 395.8002
00323 9.73 0.15 29.23 0.265 0.94 0 15 15 2.77473 2.50662 21.25193 55 321.6229
00391 10.80 0.15 17.33 0.282 0.91 0 11 11 2.76976 2.58080 20.89958 55 244.0457
00391 10.80 0.15 19.66 0.219 1.01 0 12 12 2.28260 1.96104 26.29792 55 409.9965
00512 10.68 0.15 18.70 0.270 1.03 0 14 14 2.18148 1.94928 27.23824 55 284.5366
00699 11.72 0.15 12.19 0.244 1.02 0 14 13 3.66612 3.43622 15.92318 55 325.3199
01009 13.90 0.15 6.47 0.116 1.26 0 7 5 3.04221 2.85917 18.86819 55 217.0517
01011 12.74 0.15 7.56 0.248 1.19 0 9 9 2.56987 2.36658 22.80497 55 276.0682
01131 12.90 0.15 6.53 0.287 1.13 0 16 16 2.17259 1.83759 26.90384 55 243.0204
01139 12.51 0.15 8.24 0.258 0.90 0 22 11 2.24136 1.97573 26.69370 55 285.0652

Notes. Absolute magnitude and slope parameters (H, G) were retrieved from the Minor Planet Center. W1 through W4 indicate the number of observations used in each WISE band. When η could not be fitted, we show the negative value of the default η that we used. We took the geometry of observation for each epoch from the Miriade Ephemeris Generator. “MJD” refers to the modified Julian Date of the first observation, whereas r, Δ and α are the average values of heliocentric and geocentric distances and phase angle of each group of epochs. Minimum relative errors of 10%, 15%, and 20% should be considered for D, η, and pV when η could be fitted to at least five measurements in bands W3 and W4. Otherwise, the minimum errors for the diameters would be 20% and 40% for the albedos (see Nugent et al. 2016). Here we provide a small set of results to illustrate the format of the full table, which can be downloaded from the CDS.

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