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Table 1

Dataset.

Object Dyn. cl. D, km p V Reference ΔHV m × 1018, kg ρb, g/cm3
2001 QY297 CC 229 0.152 Vilenius et al. (2014) 0.2 4.105±0.038 a 0.92
2001 XR254 CC 221 0.136 Vilenius et al. (2014) 0.43 4.055±0.065 a 1.00
Borasisi CC 163 0.236 Vilenius et al. (2014) 0.45 3.433±0.027 a 2.1
Teharonhiawako CC 220 0.145 Vilenius et al. (2014) 0.7 2.445±0.032 a 0.60
2005 EF298 CC 174 0.16 Vilenius et al. (2012) 0.59 2.2±0.1 b 1.10
Sila-Nunam CC 343 ±42 0.090 Vilenius et al. (2012) 0.12 10.84± 0.22 c 0.72±0.28
2001 RZ143 CC 140 0.191 Vilenius et al. (2012) 0.4 – –
2003 QA91 CC 260 0.130 Vilenius et al. (2014) 0.1 – –
2003 QR91 CC 280 0.054 Vilenius et al. (2014) 0.2 – –
2003 WU188 CC <220 >0.15 Vilenius et al. (2014) 0.7 – –
2002 VT130 CC 324 0.097 Mommert (2013) 0.44 – –
Makemake k HC 1440±9 0.77±0.03 Ortiz et al. (2012) 7.8 2600±500k 1.7±0.36
Salacia HC 901±45 0.044 ±0.004 Fornasier et al. (2013) 2.36 436±11 d 1.29±0.23
Haumea l HC 1240 0.804 Fornasier et al. (2013) 2.98 4030±40 e 2.55
Altjira HC 331 0.043 Vilenius et al. (2014) 0.23 3.99±0.067 a 0.30
Varda HC 792 0.102 Vilenius et al. (2014) 1.45 265±3.9 b 1.27
Quaoarm HC 1110±5 0.109 ± 0.007 Braga-Ribas et al. (2013) 5.6 1400±210 f 1.99±0.46
2002 UX25 HC 697 0.107 Fornasier et al. (2013) 2.5 125±3 g 0.79±0.10
2001 QC298 HC 303 0.061 Vilenius et al. (2014) 0.44 11.88±0.14 a 1.14
Orcus Plu 958±23 0.231 Fornasier et al. (2013) 2.61 636±3.3 a 1.53
1999 TC36 Plu 393 0.079 Mommert et al. (2012) 2.21 12.8±0.06 h 0.62
2003 AZ84 Plu 727 0.107 Mommert et al. (2012) 5 – –
Huya Plu 458 ±9 0.083 ±0.004 Fornasier et al. (2013) 1.56 – –
2002 WC19 Res 348±45 0.167 Lellouch et al. (2013) 3.1 77±5 b 3.47±1.7
1998 SM165 Res 291 0.083 Lellouch et al. (2013) 2.69 6.89±0.01 a 0.59
Typhon SDO 185± 7 0.044 ± 0.003 Santos-Sanz et al. (2012) 1.3 0.87±0.03 d 0.33±0.05
Ceto SDO 281±11 0.056 ±0.006 Santos-Sanz et al. (2012) 0.58 5.41±0.42 i 0.64±0.13
Erisn Det 2260±50 0.96 Sicardy et al. (2011) 6.7 16700±200 j 2.75±0.22
1995 TL8 Det 244 0.231 Lellouch et al. (2013) 1.7 – –
2007 UK126 n Det 614±15 0.15 Schindler et al. (2017) 3.79 – –

Notes. Diameter D and albedo pV are obtained by applying the hybrid STM or NEATM (Harris 1998; Lebofsky et al. 1986; Stansberry et al. 2008) to the fluxes measured by Herschel (and Spitzer when are available) for all objects, unless otherwise indicated. Dyn. cl. means dynamical classification: CC denotes cold classicals, HC denotes hot classicals, Plu denotes plutinos, Res denotes resonant objects, SDO denotes scatered disc objects, and Det denoted detached objects. Magnitude difference between the primary and secondary, ΔHV, is from Grundy’s tables on webpage2. The triple systems Haumea and 1999 TC36 are also considered here as binaries: the magnitude difference between the primary and the most distant satellite is used. Bulk density ρb is calculated in this work, unless otherwise indicated (see text). System mass, m, is from literature.

(b)

Grundy’s tables on webpage2;

(k)

Size and albedo were obtained from stellar occultation. The effective diameter D is derived with D1 = 1430 ± 14 km (Ortiz et al. 2012) and D2 = 175 ± 75 km (Parker et al. 2016).

(l)

Bulk density is from Lacerda & Jewitt (2007), calculated with assumption of Jacobi triaxial ellipsoid form.

(m)

Size and albedo were obtained from stellar occultation. Bulk density is from Braga-Ribas et al. (2013), calculated with assumption of Maclaurin spheroid form.

(n)

Size and albedo were obtained from stellar occultation.

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