Table B.2: Same as Table B.1 for the non-dwarf luminosity classes. The reference abbreviations are appended with "g'' for a giant scale, "sg'' for a subgiant scale and "i'' for an intermediate scale. See Table 2 for further details. Again temperatures are given in [K].
Spectral type bessell79g1 djn87sg2 djn87g3 perrin98g4 luhman03i5 luhman99g6
G0   5640 5470      
G1            
G2   5460 5300      
G3            
G4   5280 5130      
G5            
G6            
G7 5000          
G8   4940 4800 4930    
G9            
K0 4750 4780 4660 4790    
K1   4620 4510 4610    
K2 4500     4450    
K3 4250 4340 4260 4270    
K4   4210 4150 4095    
K5 4000 4080 4050 3980    
K6            
K7   3870 3870      
K7-M0            
K9   3700 3740      
M0   3630 3690 3895    
M0.5            
M 1   3510 3600 3810 3705 3800
M 1.5   3460 3560      
M 2 3750 3410 3540 3730 3560 3700
M 2.5            
M 3   3340 3480 3640 3415 3590
M 3.5            
M 4   3280 3440 3560 3270 3480
M 4.5 3500          
M 5   3220 3380 3420 3125 3370
M 5.5            
M 6 3250 3150 3330 3243 2990 3250
M 6.5   3110 3300      
M 7   3070 3270 3087 2880 3100
M 7.5            
M 8   2990 3240 2806 2710 2800
M 9   2920 3270   2400 2650
1 bessell79g = Bessell (1979); 2 djn87sg = de Jager & Nieuwenhuijzen (1987); 3 djn87g = de Jager & Nieuwenhuijzen (1987); 4 perrin98g = Perrin et al. (1998); 5 luhman03i = Luhman et al. (2003); 6 luhman99g = Luhman (1999).

Source LaTeX | All tables | In the text

Article Contents
1 Introduction
2 A new method - extending the approach of White et al. (1999)
3 Application to known eclipsing binaries
4 Summary and conclusions
References
Online Material
Appendix A: Derivation of intrinsic scale errors
Appendix B: Conversion tables
List of tables
List of figures