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Table 3

Individual absolute magnitudes (Hmag) and Herschel flux densities (F70, F100 and F160), diameter (D), albedo (pv), and beaming parameter (η) of the Centaur sample.

Herschel sample
Target H mag F 24 F 71 F 70 F 100 F 160 D p v η
(mag) (mJy) (mJy) (mJy) (mJy) (mJy) (km) %
2002 GZ32 7.37 ± 0.10(a) 9.88 ± 0.31 44.49 ± 2.91 54.48 ± 1.80 41.16 ± 1.94 20.26 ± 2.17 237 3.7 0.97
2002 KY14 10.37 ± 0.07(b) ..... ..... 23.43 ± 1.20 14.81 ± 0.92 6.76 ± 1.29 47 5.7 1.20
2003 CO1 9.07 ± 0.05(c) 21.12 ± 0.68 34.02 ± 3.60 34.51 ± 1.45 23.73 ± 2.11 11.28 ± 1.63 94 4.9 1.23
2003 WL7 8.75 ± 0.16(d) 7.08 ± 0.21 20.95 ± 1.54 22.18 ± 1.30 15.07 ± 1.16 < 3.04 105 5.3 1.02
2005 RO43 7.34 ± 0.51(e) 0.81 ± 0.03 ..... 11.30 ± 0.93 12.69 ± 1.24 5.77 ± 2.48 194 5.6 1.12
2005 UJ438 11.14 ± 0.32(f) 8.05 ± 0.24 4.71 ± 0.96 5.02 ± 0.72 3.38 ± 0.89 2.78 ± 1.56 16 25.6 0.34
2006 SX368 9.45 ± 0.11(g) 15.09 ± 0.48 26.65 ± 2.40 25.00 ± 1.12 15.63 ± 1.21 10.71 ± 1.94 76 5.2 0.87
2008 FC76 9.44 ± 0.10(h) ..... ..... 26.79 ± 1.43 15.58 ± 1.72 5.00 ± 1.65 68 6.7 1.20
Amycus 8.27 ± 0.11(i) 6.19 ± 0.20 14.74 ± 1.93 17.02 ± 0.82 10.31 ± 0.91 6.53 ± 3.16 104 8.3 1.00
Asbolus(7) 9.13 ± 0.25(j) 73.52 ± 2.24 85.70 ± 9.56 8.51 ± 1.62 <2.07 <2.99 85 5.6 0.97
Bienor 7.57 ± 0.34(k) 3.51 ± 0.11 28.81 ± 4.77 37.51 ± 1.42 26.67 ± 1.36 14.45 ± 4.92 198 4.3 1.58
Echeclus(1) 9.78 ± 0.14(l) 4.91 ± 0.15 16.36 ± 4.86 42.15 ± 1.50 26.93 ± 2.17 16.55 ± 2.11 65 5.3 0.87
Echeclus(2) 9.78 ± 0.14(l) 20.15 ± 0.61 ..... 42.15 ± 1.50 26.93 ± 2.17 16.55 ± 2.11 63 5.5 0.81
Echeclus 64.6 5.2 0.86
Hylonome(3) 9.51 ± 0.08(m) 0.51 ± 0.08 <4.798 2.76 ± 0.96 2.06 ± 1.09 4.06 ± 2.45 77
Hylonome(4) 9.51 ± 0.08(m) 0.44 ± 0.03 ..... 2.76 ± 0.96 2.06 ± 1.09 4.06 ± 2.45 77
Hylonome 74 5.1 1.29
Okyrhoe 11.07 ± 0.10(n) 28.89 ± 0.89 37.53 ± 5.07 30.34 ± 1.80 14.82 ± 2.50 10.02 ± 3.64 35 5.6 0.71
Pholus(5) 7.68 ± 0.28(o) 3.13 ± 0.13 15.63 ± 7.11 4.83 ± 0.99 3.21 ± 1.86 <3.91 99 15.5 0.77
Pholus(6) 7.68 ± 0.28(o) 0.95 ± 0.10 <5.220 4.83 ± 0.99 3.21 ± 1.86 <3.91
Thereus(8) 9.40 ± 0.16(p) 23.60 ± 0.73 43.90 ± 5.44 17.39 ± 1.22 9.68 ± 1.08 4.46 ± 2.05 62 8.3 0.87
Spitzer sample re-analyzed targets
Target H mag F 24 F 71 F 70 F 100 F 160 D p v η
(mag) (mJy) (mJy) (mJy) (mJy) (mJy) (km) %
Nessus 9.51 ± 0.22 (s) 0.38 ± 0.09 ..... ..... ..... ..... 57 8.6 1.20
Elatus/2004 8.59 ± 0.12 <5.97 ..... ..... .....
Elatus/2005 10.40 ± 0.09 (t) 6.05 ± 0.20 10.68 ± 4.30 ..... ..... ..... 49.8 4.9 1.20
Cyllarus 9.02 ± 0.15 (v) 0.21 ± 0.11 ..... ..... ..... ..... 56 13.9 1.20
2001 BL41 11.34 ± 0.21 (w) 4.90 ± 0.15 ..... ..... ..... ..... 34.6 4.3 1.20
Crantor 9.03 ± 0.16 (w) 2.26 ± 0.08 <6.31 ..... ..... ..... 59 12.1 1.20
2001 SQ73 9.15 ± 0.11 (q) 1.81 ± 0.06 ..... ..... ..... ..... 90 4.8 1.20
2002 VR130 11.26 ± 0.39 (r) 0.27 ± 0.02 ..... ..... ..... ..... 24.4 9.3 1.20
2004 QQ26 9.53 ± 0.36 (r) 0.63 ± 0.02 ..... ..... ..... ..... 79 ± 19 4.4 1.20
2000 GM137 14.36 ± 0.38 (r) 0.75 ± 0.03 ..... ..... ..... ..... 8.6 ± 1.5 4.3 1.20

Notes. Color-corrected Spitzer flux densities (F24 and F71) of previously published targets and four unpublished targets. The object 29P is excluded from this table because we used the values published in Stansberry et al. (2008). All the used Hmag also consider the amplitude of the light-curve adding quadratically the 88% of half the amplitude to each uncertainty (when amplitude is unknown we assumed an amplitude of 0.2 mag – (Vilenius et al. 2012). For some of the objects this variation is significant, about 0.3–0.4 mag (e.g. Pholus and Asbolus). The MIPS and PACS data have been taken at very different epochs, hence have substantially different observing geometries.

Reference. (1) MIPS AORKEY 8808960; (2) MIPS AORKEY 26034432; (3) MIPS AORKEY 9038080; (4) MIPS AORKEY 12659968; (5) MIPS AORKEY 9040896; (6) MIPS AORKEY 12661760; (7) MIPS AORKEY 12660480; (8) MIPS AORKEY 9044480 (a) Rabinowitz et al. (2007); Romanishin & Tegler (2005); Doressoundiram et al. (2005); (b) Perna et al. (2010); (c) Perna et al. (2013); (d) Perna et al. (2013); (e) Herschel Database, Delsanti (priv. comm. 2013); (f) Perna et al. (2013); (g) Perna & Dotto (unpublished); (h) Perna et al. (2010) and Perna & Dotto (unpublished); (i) Perna et al. (2010); (j) Rabinowitz et al. (2007); Romanishin & Tegler (2005); (k) Rabinowitz et al. (2007); Romanishin & Tegler (2005); Doressoundiram et al. (2005); (l) Delsanti & Vilenius (priv. comm. 2013); (m) Romanishin & Tegler (2005); Doressoundiram et al. (2005); (n) Romanishin & Tegler (2005); Perna et al. (2010); Doressoundiram et al. (2005); (o) Romanishin & Tegler (2005); Perna et al. (2010); (p) Rabinowitz et al. (2007); Romanishin & Tegler (2005); (q) Tegler et al. (2003); Santos-Sanz et al. (2009); (r) from MPC R-band data (7–24 data points/target) using average V − R = 0.57 ± 0.13 for Centaurs from MBOSS-2 Hainaut et al. (2012) and average β = 0.09 ± 0.04 from Perna et al. (2013); (s) Photometric data (N = 1) from Romanishin et al. (1997) with new βV fit from MPC/Steward observatory data (N = 34); (t) Belskaya et al. (2003) and V − R color; (v) Tegler et al. (2003); Delsanti et al. (2001); Doressoundiram et al. (2002); Boehnhardt et al. (2001) new slope coefficient fit β = 0.141 ± 0.073; (w) Bauer et al. (2003); Tegler et al. (2003); Doressoundiram et al. (2005); Fornasier et al. (2004); DeMeoet al. (2009), default β = 0.09 ± 0.04; (w) Tegler et al. (2003), default β = 0.09 ± 0.04.

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