Adopted distance estimates
Object | Parallax, mas | Distance, pc | Distance, ly | Distance, Pm | Source | ||
---|---|---|---|---|---|---|---|
Systems with a G-type subgiant star as primary member. | |||||||
Delta Pavonis | 163.71±0.17 | 6.108±0.006 | 19.923±0.021 | 188.48±0.2 | van Leeuwen (2007)[1] | ||
Systems with an A-type main-sequence star as primary member. | |||||||
Altair | 194.95±0.57 | 5.13±0.015 | 16.73±0.05 | 158.3±0.5 | van Leeuwen (2007)[2] | ||
Systems with a G-type main-sequence star (yellow dwarf) as primary member. | |||||||
Sigma Draconis | 173.77±0.18 | 5.755±0.006 | 18.769±0.019 | 177.57±0.18 | van Leeuwen (2007)[3] | ||
Eta Cassiopeiae | 167.98±0.48 | 5.953±0.017 | 19.42±0.06 | 183.7±0.5 | van Leeuwen (2007)[4] | ||
82 G. Eridani | 165.47±0.19 | 6.043±0.007 | 19.711±0.023 | 186.48±0.21 | van Leeuwen (2007)[5] | ||
Systems with a K-type main-sequence star (orange dwarf) as primary member. | |||||||
Groombridge 1618 | 205.21±0.54 | 4.873±0.013 | 15.89±0.04 | 150.4±0.4 | van Leeuwen (2007)[6] | ||
40 Eridani | 200.62±0.23 | 4.985±0.006 | 16.257±0.019 | 153.81±0.18 | van Leeuwen (2007)[7] | ||
70 Ophiuchi | 196.72±0.83 | 5.083+0.022 −0.021 |
16.58±0.07 | 156.9±0.7 | van Leeuwen (2007)[8] | ||
Gliese 570 | 171.22±0.94 | 5.84±0.03 | 19.05+0.11 −0.1 |
180.2±1 | van Leeuwen (2007) (A)[9] | ||
36 Ophiuchi | 168.54±0.54 | 5.933±0.019 | 19.35±0.06 | 183.1±0.6 | van Leeuwen (2007) (AB)[10] | ||
HR 7703 | 166.25±0.27 | 6.015±0.01 | 19.62±0.03 | 185.6±0.3 | van Leeuwen (2007)[11] | ||
Systems with an M-type main-sequence star (red dwarf) as primary member. | |||||||
Gliese 876 | 214.6±0.2 | 4.66±0.004 | 15.198±0.014 | 143.79±0.13 | Benedict et al. (2002)[12] | ||
GJ 1002 | 212.8±3.3 | 4.7±0.07 | 15.33+0.24 −0.23 |
145+2.3 −2.2 |
Gliese & Jahreiß (1991)[13] | ||
LHS 288 | 208.95±2.73 | 4.79±0.06 | 15.61+0.21 −0.2 |
147.7+2 −1.9 |
Henry et al. (2006)[14] | ||
Gliese 412 | 206.27±1.00 | 4.848+0.024 −0.023 |
15.81±0.08 | 149.6±0.7 | van Leeuwen (2007)[15] | ||
AD Leonis | 203.9±2.8 | 4.9±0.07 | 16±0.22 | 151.3+2.1 −2 |
Gliese & Jahreiß (1991)[16] | ||
Gliese 832 | 201.87±1.01 | 4.954±0.025 | 16.16±0.08 | 152.9±0.8 | van Leeuwen (2007)[17] | ||
EV Lacertae | 199.3±0.93 | 5.018+0.024 −0.023 |
16.37±0.08 | 154.8±0.7 | Gatewood et al. (1993)[18] | ||
Gliese 682 | 196.90±2.15 | 5.08+0.06 −0.05 |
16.56±0.18 | 156.7±1.7 | van Leeuwen (2007)[19] | ||
G 9-38 | 191.3±2.5 | 5.23±0.07 | 17.05+0.23 −0.22 |
161.3±2.1 | Gliese & Jahreiß (1991)[20] | ||
GJ 3379 | 190.93±1.89 | 5.24±0.05 | 17.08±0.17 | 161.6±1.6 | Henry et al. (2006)[14] | ||
LHS 1723 | 187.92±1.26 | 5.32±0.04 | 17.36±0.12 | 164.2±1.1 | Henry et al. (2006)[14] | ||
Gliese 445 | 185.48±1.43 | 5.39±0.04 | 17.58+0.14 −0.13 |
166.4±1.3 | Perryman et al. (1997) (Hipparcos)[21] | ||
GJ 526 | 184.00±1.07 | 5.435+0.032 −0.031 |
17.73±0.1 | 167.7±1 | Gatewood (2008)[22] | ||
Stein 2051 | 180.6±0.8 | 5.537+0.025 −0.024 |
18.06±0.08 | 170.9±0.8 | van Altena et al. (1995)[23] | ||
Gliese 251 | 179.01±1.60 | 5.59±0.05 | 18.22±0.16 | 172.4+1.6 −1.5 |
van Leeuwen (2007)[24] | ||
Gliese 205 | 176.77±1.18 | 5.66±0.04 | 18.45±0.12 | 174.6±1.2 | van Leeuwen (2007)[25] | ||
LP 816-60 | 175.03±3.40 | 5.71±0.11 | 18.6±0.4 | 176.3+3.5 −3.4 |
van Leeuwen (2007)[26] | ||
Gliese 229 | 173.81±0.99 | 5.75±0.03 | 18.77±0.11 | 177.5±1 | van Leeuwen (2007)[27] | ||
Gliese 693 | 172.08±2.22 | 5.81+0.08 −0.07 |
18.95+0.25 −0.24 |
179.3±2.3 | Perryman et al. (1997) (Hipparcos)[28] | ||
Ross 47 | 171.72±1.06 | 5.82±0.04 | 18.99±0.12 | 179.7±1.1 | Gatewood (2008)[22] | ||
Gliese 752 | 171.2±0.7 | 5.841±0.024 | 19.05±0.08 | 180.2±0.7 | van Altena et al. (1995)[29] | ||
Gliese 754 | 169.03±1.55 | 5.92±0.05 | 19.3±0.18 | 182.6±1.7 | Jao et al. (2005)[30] | ||
TYC 3980-1081-1 | 5.93±1.32 | 19.3±4.3 | 183±40.7 | Finch et al. (2014)[31] | |||
Gliese 588 | 168.66±1.30 | 5.93±0.05 | 19.34±0.15 | 183±1.4 | van Leeuwen (2007)[32] | ||
YZ Canis Minoris | 167.88±2.31 | 5.96±0.08 | 19.43+0.27 −0.26 |
183.8+2.6 −2.5 |
van Leeuwen (2007)[33] | ||
Gliese 908 | 167.29±1.23 | 5.98±0.04 | 19.5±0.14 | 184.5+1.4 −1.3 |
van Leeuwen (2007)[34] | ||
GJ 1005 | 166.6±0.8[nb 1] | 6.002±0.029 | 19.58±0.09 | 185.2±0.9 | Hershey & Taff (1998)[35] | ||
2MASS J05332802-4257205 | ~ 6 | ~ 19.6 | ~ 185.1 | Riaz et al. (2006)[36] | |||
2MASS J18450079-1409036 | ~ 6[nb 2] | ~ 19.6 | ~ 185.1 | Riaz et al. (2006)[36] | |||
Scholz's star | 166±28 | 6+1.2 −0.9 |
19.6+4 −2.8 |
185.9+37.7 −26.8 |
Burgasser et al. (2015)[37] | ||
Gliese 268 | 165.2±2.1 | 6.05±0.08 | 19.74±0.25 | 186.8+2.4 −2.3 |
van Altena et al. (1995)[38] | ||
Systems with a white dwarf star as primary member. | |||||||
LP 145-141 | 215.80±1.25 | 4.634±0.027 | 15.11±0.09 | 143±0.8 | Subasavage et al. (2009)[39] | ||
G 240-72 | 164.7±2.4 | 6.07±0.09 | 19.8+0.29 −0.28 |
187.4+2.8 −2.7 |
van Altena et al. (1995)[40] | ||
Systems with an M-type brown dwarf as primary member. | |||||||
2MASS 1835+3259 | 176.5±0.5 | 5.666±0.016 | 18.48±0.05 | 174.8±0.5 | Reid et al. (2003)[41] | ||
Systems with an L-type brown dwarf as primary member. | |||||||
DEN 0255-4700 | 201.37±3.89 | 4.97+0.1 −0.09 |
16.2+0.32 −0.31 |
153.2+3 −2.9 |
Costa et al. (2006)[42] | ||
Systems with a T-type brown dwarf as primary member. | |||||||
DENIS J081730.0-615520 | 203±13 | 4.93+0.34 −0.3 |
16.1+1.1 −1 |
152+10.4 −9.1 |
Artigau et al. (2010)[43] | ||
WISE J0521+1025 | 5.0±1.3 | 16.3±4.2 | 154.3±40.1 | Bihain et al. (2013)[44] | |||
2MASS 0939-2448 | 187.3±4.6 | 5.34±0.13 | 17.4±0.4 | 164.7+4.1 −3.9 |
Burgasser et al. (2008)[45] | ||
WISEPA J174124.26+255319.5 | 180±15[nb 3] | 5.6+0.5 −0.4 |
18.1+1.6 −1.4 |
171.4+15.6 −13.2 |
Dupuy & Kraus (2013)[46] | ||
2MASS J11145133-2618235 | 179.2±1.4 | 5.58±0.04 | 18.2±0.14 | 172.2+1.4 −1.3 |
Dupuy & Liu (2012)[47] | ||
2MASS J04151954-0935066 | 175.2±1.7 | 5.71+0.06 −0.05 |
18.62±0.18 | 176.1±1.7 | Dupuy & Liu (2012)[47] | ||
WISE J2000+3629 | 5.95±2.05[nb 4] | 19.4±6.7 | 183.6±63.3 | Cushing et al. (2014)[48] | |||
2MASSI J0937347+293142 | 163.39±1.76 | 6.12±0.07 | 19.96+0.22 −0.21 |
188.9+2.1 −2 |
Schilbach et al. (2009)[49] | ||
Systems with a Y-type brown dwarf as primary member. | |||||||
WISE 1639-6847 | 202.3±3.1 | 4.94+0.08 −0.07 |
16.12+0.25 −0.24 |
152.5+2.4 −2.3 |
Tinney et al. (2014)[50] | ||
WISE 0359−5401 | 145±39[nb 5] | 5.9+1.3 −0.8 |
19.2+4.2 −2.6 |
182.1+40.1 −24.7 |
Marsh et al. (2013)[51] | ||
Systems with a Y-type sub-brown dwarf or a Y-type rogue planet as primary member. | |||||||
WISE 1541−2250 | 175.1±4.4 | 5.71+0.15 −0.14 |
18.6±0.5 | 176.2+4.5 −4.3 |
Tinney et al. (2014)[50] | ||
Non-trigonometric distance estimates are marked in italic. For other distance estimates see articles on these objects. |
See also
|
References
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Notes
- ^ Absolute parallax, but error of parallax taken from relative parallax. Error of absolute parallax should be larger — at least, larger than error of RECONS' weighted parallax 0.90 mas.
- ^ Same estimates for both stars.
- ^ Relative parallax.
- ^ In the article: 3.9−8.0 pc.
- ^ In this parallax and distance estimates the most probable distance value does not equal to inverse maximum likelihood parallax value, as would be in the case of exact parallax and distance values. This is due to the fact that Marsh et al. used a more sophisticated method of converting maximum likelihood parallaxes into most probable distances, that uses also some prior information, and not just the calculation of the inverse value. (The method description see in Marsh et al. (2013), Section 4).