Table 6
Mean differences and standard deviations between stellar parameters presented in this work and derived by other authors.
| Reference | Number | ΔTeff ± σ | Δlog g ± σ | Δ[Fe/H] ± σ | ΔR ± σ | ΔRV ± σ | Remarks |
| of stars | [K] | [cm s-2] | [R⊙] | [km s-1] | |||
|
|
|||||||
| Adamów et al. (in prep.) | 332 | 48 ± 224 | − | − | − | − | (†) |
| Alonso et al. (2000) | 332 | − | − | − | −2.2 ± 5.8 | − | (†) |
| Baines et al. (2009) | 1 | −178 | − | − | −0.7 | − | |
| Baines et al. (2010) spectroscopy | 1 | −179 | −0.34 | −0.10 | −5.2 | − | |
| Baines et al. (2010) interferometry | 1 | −78 | − | − | −3.1 | − | |
| Balachandran et al. (1988) | 1 | − | − | −0.32 | − | − | |
| Bartkevičius & Sperauskas (1999) | 1 | − | − | − | − | 0.113 | |
| Blackwell & Lynas-Gray (1998) | 1 | 22 | − | − | − | − | |
| Bordé et al. (2002) | 1 | −57 | −0.74 | − | − | − | |
| Brown et al. (1989) | 2 | 103 ± 129 | 0.26 ± 0.42 | −0.14 ± 0.10 | − | − | (†) |
| de Medeiros & Mayor (1999) | 4 | − | − | − | − | 0.178 ± 0.169 | (†,*) |
| Duflot et al. (1995) | 5 | − | − | − | − | −0.405 ± 1.810 | (†,*) |
| Famaey et al. (2005) | 19 | − | − | − | − | 0.163 ± 0.834 | (†,*) |
| Gontcharov (2006) | 21 | − | − | − | − | 0.422 ± 1.475 | (†,*) |
| Hekker & Meléndez (2007) | 1 | −184 | −0.74 | −0.11 | − | − | |
| Luck (1991) | 1 | 448 | 2.14 | −0.01 | − | − | |
| Luck & Heiter (2007) | 1 | −120 | −0.13 | −0.05 | − | − | |
| McWilliam (1990) | 3 | −10 ± 176 | 0.05 ± 0.84 | 0.06 ± 0.09 | − | − | (†) |
| Nidever et al. (2002) | 1 | − | − | − | − | −0.647 | |
| Nordgren et al. (1999) | 1 | − | − | − | 0.8 | − | |
| Pasinetti Fracassini et al. (2001) | 4 | − | − | − | 1.4 ± 6.1 | − | (†) |
| Ramírez & Meléndez (2005) | 1 | −42 | − | −0.03 | − | − | |
| Soubiran et al. (2008) | 5 | − | − | 0.00 ± 0.12 | − | − | (†) |
| Taylor (1999) | 4 | 408 | − | −0.02 ± 0.06 | − | − | (†) |
| van Belle & von Braun (2009) | 1 | −266 | − | − | 4.9 | − | |
Notes.
The value after the plus-minus sign is standard deviation (if number of stars to compare is >1).
The difference and scatter value obtained, with the exception of discrepant stars (see Sect. 9.1 and Fig. 16 for details).
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