Table 7
Adopted physical properties in comparison with previous works.
| This work | Previous work | ||||||
| Target | D (km) | p V | λdetect (μm) | D (km) | p V | Reference | |
|
|
|||||||
| 119951 (2002 KX14) | 455 ± 27 |
|
24, 71 |
|
|
Brucker et al. (2009) | |
| (2001 XR254) | B |
|
|
(binary) | 130–208a | 0.09–0.23 | 34 |
| 275809 (2001 QY297) | B |
|
|
(binary) | 128–200a | 0.13–0.32 | 34 |
| (2001 RZ143) | B |
|
|
24 | <160 | >0.23 | Brucker et al. (2009) |
| 79360 Sila | B | 343 ± 42 |
|
70, 160 | 250–420 | 0.06–0.14 | Müller et al. (2010) |
| 88611 Teharonhiawako | B |
|
|
(binary) | 114–180a | 0.13–0.32 | 34 |
| 138537 (2000 OK67) |
|
|
24 | <160 | >0.16 | Brucker et al. (2009) | |
| 148780 Altjira | B |
|
|
24 | <200 | >0.10 | Brucker et al. (2009) |
| (binary) | 128–200a | 0.06–0.14 | 34 | ||||
| (2002 KW14) |
|
|
71 | <360 | >0.05 | Brucker et al. (2009) | |
| (2001 KA77) |
|
|
24, 71 |
|
|
Brucker et al. (2009) | |
| 19521 Chaos |
|
|
1200 | <742 | >0.033 | 1 | |
| (2002 MS4) | 934 ± 47 |
|
24, 71 | 730 ± 120 |
|
Brucker et al. (2009) | |
| 90568 (2004 GV9) | 680 ± 34 |
|
24, 71 |
|
|
Brucker et al. (2009) | |
| 120347 Salacia | B | 901 ± 45 | 0.0439 ± 0.0044 | (binary) | 720–1140a | 0.01–0.03 | 34 |
| 24, 71 | 954 ± 80 |
|
85 | ||||
|
|
|||||||
| (2001 QD298) | ... | 24, 71 |
|
|
Brucker et al. (2009) | ||
| (1996 TS66) | ... | 24, 71 |
|
|
Brucker et al. (2009) | ||
| 50000 Quaoar | B | ... | 24, 71, (direct) | 890 ± 70a | 0.18 ± 0.04 | Fraser & Brown (2010) | |
| (2002 GJ32) | ... | 24, 71 |
|
|
Brucker et al. (2009) | ||
| 20000 Varuna | ... | 71 |
|
|
Brucker et al. (2009) | ||
| 55637 (2002 UX25) | B | ... | 24, 71 |
|
|
Stansberry et al. (2008) | |
| 55636 (2002 TX300) | ... | (occultation) | 286 ± 10 |
|
23 | ||
| 55565 (2002 AW197) | ... | 24, 71 | 740 ± 100 |
|
Brucker et al. (2009) | ||
Notes. Binary systems are indicated by “B”. Column λdetect lists the wavelengths used in the reference for radiometric diameters. If no radiometric result is available then binary system mass is used to give the diameter of the primary component assuming equal albedos. The second part of this table lists all other classical TNOs with radiometric or other reliable size estimates. The size of 50000 Quaoar is derived from both Spitzer and from direct imaging by Hubble. All targets in the lower part are dynamically hot.
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