# "A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence" # http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt # Eric Mamajek # Version 2022.04.16 # # Much of the original content of this table was incorporated into # Table 5 of Pecaut & Mamajek (2013, ApJS, 208, 9; # http://adsabs.harvard.edu/abs/2013ApJS..208....9P), so that # reference should be cited until an updated version of the table is # published. Parts of this table for A/F/G stars also appeared in # Table 3 of Pecaut, Mamajek, & Bubar (2012, ApJ 756, 154). For # example, Table 5 of Pecaut & Mamajek did not include the absolute # magnitude and luminosity estimates, nor the properties of dwarfs of # types L, T, Y, or O3-O8. # The author's notes on standard stars and mean parameters for stars # for each dwarf spectral type can be found in the directory at: # http://www.pas.rochester.edu/~emamajek/spt/. See further notes and # caveats after the table. Colors are based on Johnson UBV, Tycho # BtVt, Cousins RcIc, Gaia DR2 G/Bp/Rp, Sloan izY, 2MASS JHKs, # MKO JK (for Y dwarfs), WISE W1/W2/W3/W4 photometry. # G-V color is Gaia DR2 G - Johnson V. # #SpT Teff logT BCv logL Mbol R_Rsun Mv B-V Bt-Vt G-V Bp-Rp G-Rp M_G b-y U-B V-Rc V-Ic V-Ks J-H H-Ks M_J M_Ks Ks-W1 W1-W2 W1-W3 W1-W4 g-r i-z z-Y Msun #SpT O3V 44900 4.652 -4.01 5.82 -9.81 13.43 -5.80 -0.330 ... ... ... ... ... ..... -1.175 ... ..... ..... ..... ..... .... .... ... ... ... ... ... ... ... 59 O3V O4V 42900 4.632 -3.89 5.65 -9.39 12.13 -5.50 -0.326 ... ... ... ... ... ..... -1.160 ... ..... ..... ..... ..... .... .... ... ... ... ... ... ... ... 48 O4V O5V 41400 4.617 -3.76 5.54 -9.11 11.45 -5.35 -0.323 ... ... ... ... ... -0.133 -1.150 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 43 O5V O5.5V 40500 4.607 -3.67 5.44 -8.87 10.71 -5.20 -0.322 ... ... ... ... ... -0.133 -1.145 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 38 O5.5V O6V 39500 4.597 -3.57 5.36 -8.67 10.27 -5.10 -0.321 ... ... ... ... ... -0.132 -1.140 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 35 O6V O6.5V 38300 4.583 -3.49 5.27 -8.44 9.82 -4.95 -0.319 ... ... ... ... ... -0.131 -1.135 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 31 O6.5V O7V 37100 4.569 -3.41 5.18 -8.21 9.42 -4.80 -0.318 ... ... ... ... ... -0.130 -1.130 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 28 O7V O7.5V 36100 4.558 -3.33 5.09 -7.98 8.95 -4.65 -0.317 ... ... ... ... ... -0.130 -1.125 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 26 O7.5V O8V 35100 4.545 -3.24 4.99 -7.74 8.47 -4.50 -0.315 ... ... ... ... ... -0.129 -1.120 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 23.6 O8V O8.5V 34300 4.535 -3.18 4.91 -7.53 8.06 -4.35 -0.314 ... ... ... ... ... -0.128 -1.115 ... ..... ..... ..... ..... .... .... ... ... ... ... -0.620 ... ... 21.9 O8.5V O9V 33300 4.522 -3.11 4.82 -7.31 7.72 -4.20 -0.312 ... ... ... ... ... -0.127 -1.110 ... -0.369 -1.000 -0.164 -0.071 -3.44 -3.20 ... ... ... ... -0.620 ... ... 20.2 O9V O9.5V 31900 4.504 -3.01 4.72 -7.06 7.50 -4.05 -0.307 ... ... ... ... ... -0.125 -1.090 ... -0.361 -0.977 -0.161 -0.069 -3.30 -3.073 ... ... ... ... -0.605 ... ... 18.7 O9.5V B0V 31400 4.497 -2.99 4.65 -6.89 7.16 -3.90 -0.301 ... ... ... ... ... -0.122 -1.070 ... -0.355 -0.958 -0.159 -0.067 -3.17 -2.942 0.016 ... ... ... -0.590 ... ... 17.7 B0V B0.5V 29000 4.462 -2.83 4.43 -6.33 6.48 -3.50 -0.289 ... ... ... ... ... -0.120 -1.030 ... -0.338 -0.913 -0.153 -0.063 -2.80 -2.587 0.017 ... ... ... -0.540 ... ... 14.8 B0.5V B1V 26000 4.415 -2.58 4.13 -5.58 5.71 -3.00 -0.278 ... ... ... ... ... -0.113 -0.995 -0.115 -0.325 -0.874 -0.148 -0.059 -2.33 -2.126 0.018 ... ... ... -0.490 ... ... 11.8 B1V B1.5V 24500 4.389 -2.44 3.91 -5.04 5.02 -2.60 -0.252 -0.274 -0.021 ... ... ... -0.103 -0.910 -0.114 -0.281 -0.752 -0.132 -0.047 -2.03 -1.848 0.021 ... ... ... -0.483 ... ... 9.9 B1.5V B2V 20600 4.314 -2.03 3.43 -3.83 4.06 -1.80 -0.215 -0.219 -0.008 ... ... ... -0.094 -0.790 -0.094 -0.230 -0.602 -0.113 -0.032 -1.34 -1.198 0.023 ... ... ... -0.475 ... ... 7.3 B2V B2.5V 18500 4.267 -1.77 3.20 -3.27 3.89 -1.50 -0.198 -0.206 -0.003 ... ... ... -0.087 -0.732 -0.087 -0.210 -0.544 -0.105 -0.026 -1.09 -0.956 0.025 ... ... ... -0.468 ... ... 6.1 B2.5V B3V 17000 4.230 -1.54 2.99 -2.74 3.61 -1.20 -0.178 -0.184 0.001 ... ... -1.19 -0.083 -0.673 -0.080 -0.192 -0.492 -0.098 -0.021 -0.83 -0.708 0.026 ... ... ... -0.460 ... ... 5.4 B3V B4V 16400 4.215 -1.49 2.89 -2.49 3.46 -1.00 -0.165 -0.170 0.004 ... ... -0.99 -0.078 -0.619 -0.074 -0.176 -0.447 -0.092 -0.016 -0.66 -0.553 0.028 ... ... ... -0.437 ... ... 5.1 B4V B5V 15700 4.196 -1.34 2.77 -2.19 3.36 -0.85 -0.156 -0.160 0.007 ... ... -0.84 -0.072 -0.581 -0.070 -0.165 -0.380 -0.084 -0.010 -0.54 -0.376 0.029 -0.045 -0.117 -0.070 -0.413 ... ... 4.7 B5V B6V 14500 4.161 -1.13 2.57 -1.68 3.27 -0.55 -0.140 -0.142 0.010 ... ... -0.54 -0.066 -0.504 -0.062 -0.145 -0.358 -0.081 -0.007 -0.28 -0.192 0.030 -0.045 -0.117 -0.070 -0.390 ... ... 4.3 B6V B7V 14000 4.146 -1.05 2.48 -1.45 2.94 -0.40 -0.128 -0.129 0.012 ... ... -0.39 -0.062 -0.459 -0.058 -0.133 -0.325 -0.077 -0.004 -0.16 -0.075 0.031 -0.045 -0.117 -0.070 -0.360 ... ... 3.92 B7V B8V 12300 4.090 -0.73 2.19 -0.73 2.86 0.00 -0.109 -0.107 0.016 ... ... -0.01 -0.045 -0.364 -0.048 -0.108 -0.254 -0.067 0.003 0.19 0.254 0.033 -0.046 -0.116 -0.067 -0.330 ... ... 3.38 B8V B9V 10700 4.029 -0.42 1.86 0.08 2.49 0.50 -0.070 -0.063 0.018 -0.120 -0.036 0.515 -0.029 -0.200 -0.028 -0.061 -0.121 -0.050 0.016 0.59 0.621 0.038 -0.063 -0.104 -0.054 -0.280 ... ... 2.75 B9V B9.5V 10400 4.017 -0.36 1.80 0.24 2.45 0.60 -0.050 -0.040 0.017 -0.087 -0.016 0.615 -0.021 -0.130 -0.017 -0.035 -0.048 -0.044 0.021 0.63 0.648 0.040 -0.044 -0.091 -0.043 -0.265 ... ... 2.68 B9.5V A0V 9700 3.987 -0.21 1.58 0.78 2.193 0.99 0.000 0.013 0.015 -0.037 -0.020 1.00 0.000 -0.005 0.001 0.004 0.041 -0.032 0.028 0.95 0.949 0.042 -0.041 -0.074 -0.022 -0.250 ... ... 2.18 A0V A1V 9300 3.968 -0.14 1.49 1.02 2.136 1.16 0.035 0.056 0.01 0.005 0.032 1.16 0.017 0.033 0.019 0.044 0.090 -0.025 0.030 1.08 1.07 0.043 -0.036 -0.068 -0.023 -0.210 ... ... 2.05 A1V A2V 8800 3.944 -0.07 1.38 1.28 2.117 1.35 0.070 0.091 0.00 0.068 0.050 1.345 0.038 0.063 0.042 0.091 0.178 -0.012 0.034 1.19 1.172 0.044 -0.034 -0.067 -0.029 -0.170 ... ... 1.98 A2V A3V 8600 3.934 -0.04 1.23 1.66 1.861 1.70 0.100 0.109 -0.005 0.110 0.092 1.69 0.055 0.077 0.050 0.108 0.253 0.003 0.035 1.49 1.447 0.045 -0.033 -0.066 -0.029 -0.140 ... ... 1.86 A3V A4V 8250 3.917 -0.02 1.13 1.92 1.794 1.94 0.140 0.166 -0.01 0.166 0.113 1.92 0.071 0.097 0.078 0.164 0.353 0.022 0.037 1.65 1.587 0.046 -0.031 -0.059 -0.021 -0.090 ... ... 1.93 A4V A5V 8100 3.908 0.00 1.09 2.01 1.785 2.01 0.160 0.185 -0.015 0.194 0.130 1.98 0.090 0.100 0.089 0.186 0.403 0.031 0.038 1.68 1.607 0.046 -0.030 -0.058 -0.021 -0.070 ... ... 1.88 A5V A6V 7910 3.898 0.005 1.05 2.13 1.775 2.12 0.185 0.194 -0.02 0.222 0.152 2.09 0.099 0.098 0.094 0.197 0.465 0.043 0.039 1.74 1.655 0.046 -0.030 -0.057 -0.018 -0.050 ... ... 1.83 A6V A7V 7760 3.890 0.01 1.00 2.24 1.750 2.23 0.210 0.233 -0.03 0.263 0.173 2.19 0.107 0.091 0.117 0.242 0.528 0.055 0.040 1.80 1.702 0.047 -0.030 -0.056 -0.017 -0.020 ... ... 1.77 A7V A8V 7590 3.880 0.02 0.96 2.34 1.747 2.32 0.250 0.274 -0.04 0.320 0.204 2.27 0.132 0.082 0.140 0.288 0.601 0.070 0.042 1.81 1.694 0.048 -0.028 -0.055 -0.009 0.030 ... ... 1.81 A8V A9V 7400 3.869 0.02 0.92 2.45 1.747 2.43 0.270 0.279 -0.05 0.327 0.207 2.37 0.145 0.080 0.143 0.294 0.674 0.086 0.044 1.89 1.756 0.048 -0.028 -0.055 -0.007 0.060 ... ... 1.75 A9V F0V 7220 3.859 0.01 0.86 2.58 1.728 2.57 0.295 0.317 -0.06 0.377 0.230 2.51 0.158 0.053 0.166 0.339 0.734 0.096 0.045 1.98 1.836 0.049 -0.026 -0.050 0.003 0.100 ... ... 1.61 F0V F1V 7020 3.846 0.005 0.79 2.77 1.679 2.76 0.330 0.350 -0.07 0.434 0.252 2.69 0.204 0.021 0.190 0.385 0.819 0.117 0.047 2.11 1.941 0.050 -0.026 -0.047 0.009 0.140 ... ... 1.50 F1V F2V 6820 3.834 -0.005 0.71 2.97 1.622 2.97 0.370 0.390 -0.08 0.490 0.279 2.89 0.250 -0.008 0.213 0.432 0.925 0.140 0.050 2.24 2.045 0.051 -0.027 -0.046 0.011 0.190 ... ... 1.46 F2V F3V 6750 3.829 -0.01 0.67 3.07 1.578 3.08 0.390 0.405 -0.09 0.518 0.293 2.99 0.263 -0.016 0.222 0.449 0.964 0.148 0.051 2.32 2.116 0.051 -0.028 -0.046 0.008 0.210 ... ... 1.44 F3V F4V 6670 3.824 -0.015 0.62 3.19 1.533 3.20 0.410 0.428 -0.10 0.546 0.307 3.10 0.277 -0.026 0.236 0.476 1.012 0.159 0.052 2.40 2.188 0.052 -0.029 -0.046 0.000 0.240 ... ... 1.38 F4V F5V 6550 3.816 -0.02 0.56 3.35 1.473 3.37 0.440 0.455 -0.11 0.587 0.329 3.26 0.290 -0.029 0.252 0.506 1.079 0.173 0.054 2.52 2.291 0.052 -0.030 -0.045 -0.004 0.280 ... ... 1.33 F5V F6V 6350 3.803 -0.03 0.43 3.66 1.359 3.69 0.486 0.504 -0.13 0.640 0.356 3.56 0.317 -0.021 0.276 0.553 1.190 0.199 0.057 2.76 2.50 0.054 -0.033 -0.045 -0.012 0.290 ... ... 1.25 F6V F7V 6280 3.798 -0.035 0.39 3.77 1.324 3.80 0.500 0.534 -0.14 0.670 0.372 3.66 0.332 -0.012 0.290 0.579 1.221 0.213 0.060 2.85 2.579 0.055 -0.036 -0.045 -0.013 0.320 ... ... 1.21 F7V F8V 6180 3.791 -0.04 0.29 4.01 1.221 4.05 0.530 0.558 -0.15 0.694 0.385 3.90 0.350 0.001 0.300 0.599 1.290 0.225 0.061 3.05 2.76 0.056 -0.039 -0.044 -0.016 0.360 ... ... 1.18 F8V F9V 6050 3.782 -0.05 0.22 4.20 1.167 4.25 0.560 0.587 -0.145 0.719 0.399 4.105 0.378 0.014 0.312 0.620 1.335 0.236 0.063 3.21 2.915 0.057 -0.041 -0.044 -0.014 0.380 ... ... 1.13 F9V F9.5V 5990 3.777 -0.06 0.18 4.29 1.142 4.35 0.580 0.615 -0.155 0.767 0.431 4.195 ... 0.033 0.323 0.640 1.403 0.249 0.065 3.26 2.947 0.057 -0.042 -0.043 -0.012 0.390 ... ... 1.08 F9.5V G0V 5930 3.773 -0.065 0.13 4.42 1.100 4.48 0.595 0.650 -0.155 0.784 0.439 4.325 ... 0.057 0.341 0.673 1.437 0.262 0.067 3.37 3.043 0.058 -0.043 -0.043 -0.010 0.420 ... ... 1.06 G0V G1V 5860 3.768 -0.073 0.08 4.55 1.060 4.62 0.622 0.661 -0.158 0.803 0.448 4.462 ... 0.067 0.340 0.672 1.500 0.279 0.070 3.47 3.120 0.060 -0.044 -0.042 -0.010 0.450 ... ... 1.03 G1V G2V 5770 3.761 -0.085 0.01 4.72 1.012 4.80 0.650 0.724 -0.165 0.823 0.459 4.635 ... 0.133 0.363 0.713 1.564 0.293 0.073 3.60 3.236 0.061 -0.050 -0.040 -0.016 0.476 ... ... 1.00 G2V G3V 5720 3.757 -0.095 -0.01 4.78 1.002 4.87 0.660 0.739 -0.167 0.832 0.464 4.703 ... 0.152 0.368 0.722 1.588 0.299 0.074 3.66 3.282 0.061 -0.050 -0.040 -0.014 0.480 ... ... 0.99 G3V G4V 5680 3.754 -0.10 -0.04 4.83 0.991 4.93 0.670 0.757 -0.173 0.841 0.468 4.757 ... 0.175 0.374 0.733 1.611 0.304 0.075 3.70 3.319 0.062 -0.052 -0.041 -0.014 0.490 ... ... 0.985 G4V G5V 5660 3.753 -0.105 -0.05 4.88 0.977 4.98 0.680 0.764 -0.179 0.850 0.473 4.801 ... 0.185 0.377 0.738 1.635 0.310 0.076 3.73 3.345 0.062 -0.052 -0.041 -0.014 0.500 ... ... 0.98 G5V G6V 5600 3.748 -0.115 -0.10 4.99 0.949 5.10 0.700 0.796 -0.186 0.869 0.483 4.914 ... 0.227 0.388 0.758 1.691 0.324 0.079 3.81 3.409 0.063 -0.053 -0.040 -0.012 0.520 ... ... 0.97 G6V G7V 5550 3.744 -0.125 -0.13 5.08 0.927 5.20 0.710 0.809 -0.194 0.880 0.489 5.006 ... 0.243 0.393 0.766 1.705 0.327 0.080 3.90 3.495 0.064 -0.054 -0.040 -0.013 0.540 ... ... 0.95 G7V G8V 5480 3.739 -0.14 -0.17 5.16 0.914 5.30 0.730 0.842 -0.202 0.900 0.499 5.098 ... 0.284 0.404 0.786 1.768 0.342 0.082 3.96 3.532 0.065 -0.057 -0.039 -0.018 0.570 ... ... 0.94 G8V G9V 5380 3.731 -0.16 -0.26 5.39 0.853 5.55 0.775 0.894 -0.210 0.950 0.524 5.34 ... 0.358 0.423 0.820 1.857 0.364 0.087 4.14 3.693 0.067 -0.060 -0.038 -0.018 0.600 ... ... 0.90 G9V K0V 5270 3.723 -0.195 -0.34 5.59 0.813 5.78 0.816 0.944 -0.227 0.983 0.56 5.553 ... 0.436 0.443 0.853 1.953 0.387 0.091 4.31 3.827 0.070 -0.063 -0.037 -0.015 0.620 ... ... 0.88 K0V K1V 5170 3.713 -0.23 -0.39 5.72 0.797 5.95 0.857 0.976 -0.25 1.01 0.56 5.65 ... 0.491 0.457 0.879 2.06 0.404 0.094 4.39 3.889 0.071 -0.064 -0.038 -0.013 0.690 ... ... 0.86 K1V K2V 5100 3.708 -0.26 -0.43 5.81 0.783 6.07 0.884 1.035 -0.27 1.10 0.62 5.83 ... 0.581 0.482 0.920 2.13 0.427 0.098 4.46 3.938 0.073 -0.068 -0.037 -0.009 0.740 ... ... 0.82 K2V K3V 4830 3.684 -0.375 -0.55 6.13 0.755 6.50 0.990 1.150 -0.32 1.21 0.66 6.20 ... 0.776 0.537 1.013 2.40 0.487 0.109 4.70 4.100 0.079 -0.071 -0.031 -0.008 0.850 ... ... 0.78 K3V K4V 4600 3.663 -0.52 -0.69 6.46 0.713 6.98 1.090 1.292 -0.42 1.34 0.70 6.53 ... 0.986 0.635 1.182 2.70 0.539 0.123 4.91 4.247 0.087 -0.072 -0.030 0.009 0.990 ... ... 0.73 K4V K5V 4440 3.647 -0.63 -0.76 6.65 0.701 7.28 1.150 1.373 -0.44 1.43 0.74 6.83 ... 1.081 0.685 1.272 2.88 0.568 0.132 5.10 4.397 0.092 -0.073 -0.029 0.019 1.040 ... ... 0.70 K5V K6V 4300 3.633 -0.75 -0.86 6.89 0.669 7.64 1.240 1.439 -0.51 1.53 0.79 7.02 ... 1.184 0.759 1.420 3.08 0.601 0.148 5.31 4.56 0.101 ... ... ... 1.140 ... ... 0.69 K6V K7V 4100 3.613 -0.93 -1.00 7.23 0.630 8.16 1.340 1.506 -0.58 1.70 0.86 7.57 ... 1.222 0.802 1.519 3.35 0.619 0.164 5.59 4.81 0.110 ... ... ... 1.260 ... ... 0.64 K7V K8V 3990 3.601 -1.03 -1.06 7.40 0.615 8.43 1.363 1.562 -0.625 1.73 0.88 7.74 ... 1.216 0.843 1.632 3.48 0.626 0.171 5.75 4.95 0.115 ... ... ... 1.290 ... ... 0.62 K8V K9V 3930 3.594 -1.07 -1.10 7.49 0.608 8.56 1.400 1.593 -0.66 1.79 0.90 8.03 ... 1.210 0.866 1.699 3.55 0.631 0.180 5.82 5.01 0.117 ... ... ... 1.320 ... ... 0.59 K9V M0V 3850 3.585 -1.15 -1.16 7.65 0.588 8.80 1.420 1.623 -0.70 1.84 0.92 8.16 ... 1.204 0.889 1.766 3.65 0.627 0.190 5.97 5.15 0.120 ... ... ... ... 0.33 ... 0.57 M0V M0.5V 3770 3.576 -1.29 -1.27 7.91 0.544 9.20 1.445 ... -0.76 1.97 0.97 8.44 ... 1.184 0.924 1.886 3.84 0.620 0.208 6.19 5.36 0.125 ... ... ... ... 0.37 ... 0.54 M0.5V M1V 3660 3.563 -1.42 -1.39 8.22 0.501 9.64 1.485 ... -0.82 2.09 1.00 8.82 ... 1.172 0.956 2.005 4.00 0.614 0.222 6.48 5.64 0.130 ... ... ... ... 0.41 ... 0.50 M1V M1.5V 3620 3.559 -1.50 -1.44 8.35 0.482 9.85 1.495 ... -0.87 2.13 1.02 8.98 ... 1.170 0.978 2.089 4.10 0.608 0.227 6.59 5.75 0.135 ... ... ... ... 0.47 ... 0.47 M1.5V M2V 3560 3.551 -1.62 -1.54 8.59 0.446 10.21 1.505 ... -0.925 2.23 1.06 9.29 ... 1.170 1.001 2.173 4.23 0.600 0.234 6.81 5.98 0.140 ... ... ... ... 0.53 ... 0.44 M2V M2.5V 3470 3.540 -1.78 -1.64 8.82 0.421 10.61 1.522 ... -1.02 2.39 1.10 9.67 ... 1.175 1.041 2.306 4.43 0.589 0.244 7.01 6.18 0.145 ... ... ... ... 0.57 ... 0.40 M2.5V M3V 3430 3.535 -1.93 -1.79 9.21 0.361 11.15 1.53 ... -1.10 2.50 1.13 10.05 ... 1.181 1.079 2.420 4.60 0.579 0.252 7.38 6.55 0.150 ... ... ... ... 0.61 ... 0.37 M3V M3.5V 3270 3.515 -2.28 -2.03 9.82 0.300 12.10 1.60 ... -1.28 2.78 1.19 10.87 ... 1.200 1.178 2.680 5.00 0.558 0.269 7.93 7.10 0.170 ... ... ... ... 0.66 ... 0.27 M3.5V M4V 3210 3.507 -2.51 -2.14 10.10 0.274 12.61 1.65 ... -1.40 2.94 1.24 11.21 ... 1.222 1.241 2.831 5.25 0.557 0.280 8.20 7.36 0.180 ... ... ... ... 0.71 ... 0.23 M4V M4.5V 3110 3.493 -2.84 -2.40 10.74 0.217 13.58 1.69 ... -1.54 3.16 1.28 12.04 ... 1.23 1.345 3.073 5.65 0.564 0.301 8.80 7.93 0.200 ... ... ... ... 0.81 ... 0.184 M4.5V M5V 3060 3.486 -3.11 -2.52 11.04 0.196 14.15 1.83 ... -1.70 3.35 1.33 12.45 ... 1.24 1.446 3.278 5.95 0.580 0.312 9.09 8.20 0.210 0.17 ... ... ... 0.91 0.47 0.162 M5V M5.5V 2930 3.467 -3.58 -2.79 11.72 0.156 15.30 1.94 ... -1.95 3.71 1.38 13.35 ... 1.3 1.656 3.664 6.50 0.588 0.329 9.72 8.80 0.220 0.19 ... ... ... 1.13 0.52 0.123 M5.5V M6V 2810 3.449 -4.13 -2.98 12.19 0.137 16.32 2.01 ... -2.37 4.16 1.43 14.26 ... 1.3 1.950 4.10 7.10 0.605 0.352 10.18 9.22 0.225 0.21 ... ... ... 1.45 0.60 0.102 M6V M6.5V 2740 3.438 -4.62 -3.10 12.48 0.126 17.10 2.07 ... -2.70 4.50 1.48 14.40 ... ... 1.988 4.26 7.60 0.609 0.360 10.47 9.50 0.235 0.22 ... ... ... 1.58 0.64 0.093 M6.5V M7V 2680 3.428 -4.99 -3.19 12.71 0.120 17.70 2.12 ... -2.98 4.65 1.52 14.72 ... ... 2.180 4.50 8.00 0.613 0.390 10.70 9.70 0.240 0.24 ... ... ... 1.77 0.70 0.090 M7V M7.5V 2630 3.420 -5.32 -3.24 12.84 0.116 18.16 2.14 ... -3.15 4.72 1.55 15.20 ... ... 2.160 4.56 8.35 0.650 0.422 10.88 9.81 0.260 0.25 ... ... ... 1.85 0.74 0.088 M7.5V M8V 2570 3.410 -5.65 -3.28 12.95 0.114 18.60 2.15 ... -3.11 4.86 1.57 15.20 ... ... 2.150 4.62 8.70 0.677 0.450 11.05 9.92 0.285 0.26 ... ... ... 1.93 0.77 0.085 M8V M8.5V 2420 3.384 -5.78 -3.47 13.42 0.104 19.20 2.16 ... -3.09 5.10 1.59 15.90 ... ... 1.967 4.63 8.90 0.69 0.465 11.46 10.30 0.310 0.265 ... ... ... 1.96 0.80 0.080 M8.5V M9V 2380 3.377 -5.86 -3.52 13.54 0.102 19.40 2.17 ... -3.00 4.78 1.60 16.20 ... ... 1.890 4.66 9.00 0.72 0.47 11.59 10.40 0.330 0.27 ... ... ... 1.99 0.82 0.079 M9V M9.5V 2350 3.371 -6.13 -3.57 13.67 0.101 19.75 ... ... -3.10 4.86 1.61 16.40 ... ... 2.510 4.73 9.30 0.745 0.50 11.75 10.50 0.350 0.27 ... ... ... 2.00 0.84 0.078 M9.5V L0V 2270 3.356 -6.25 -3.60 13.75 0.102 20.0 ... ... -3.45 ... 1.68 16.60 ... ... ... 4.85 9.40 0.76 0.51 11.76 10.55 0.36 0.27 ... ... ... 2.01 0.86 0.077 L0V L1V 2160 3.334 -6.48 -3.71 14.02 0.0995 20.5 ... ... ... ... 1.66 16.90 ... ... ... 4.91 9.65 0.82 0.54 12.12 10.77 0.37 0.28 ... ... ... 2.02 0.88 0.076 L1V L2V 2060 3.314 -6.62 -3.82 14.28 0.0970 20.9 ... ... ... ... 1.69 17.30 ... ... ... 5.05 9.90 0.89 0.58 12.47 11.00 0.47 0.28 ... ... ... 2.04 0.90 0.075 L2V L3V 1920 3.283 -7.05 -3.96 14.65 0.0942 21.7 ... ... ... ... 1.70 18.10 ... ... ... 5.29 10.1 0.97 0.61 12.78 11.40 0.50 0.29 ... ... ... 2.10 0.92 ... L3V L4V 1870 3.272 -7.53 -4.01 14.77 0.0940 22.3 ... ... ... ... 1.74 18.35 ... ... ... 5.57 10.5 1.00 0.63 13.09 11.50 0.60 0.30 ... ... ... 2.20 0.94 ... L4V L5V 1710 3.233 -7.87 -4.20 15.23 0.0909 ... ... ... ... ... 1.71 18.50 ... ... ... 6.28 11.1 1.02 0.648 13.46 11.87 0.68 0.32 ... ... ... 2.33 0.97 ... L5V L6V 1550 3.190 ... -4.38 15.70 0.0891 ... ... ... ... ... 1.74 19.25: ... ... ... ... ... 1.06 0.654 13.89 12.20 0.76 0.36 ... ... ... 2.51 1.00 ... L6V L7V 1530 3.185 ... -4.41 15.77 0.0886 ... ... ... ... ... 2.11 19.30: ... ... ... ... ... 1.13 0.645 14.31 12.55 0.84 0.41 ... ... ... 2.71 1.04 ... L7V L8V 1420 3.152 ... -4.55 16.12 0.0875 ... ... ... ... ... 1.87 20.00: ... ... ... ... ... 1.16 0.625 14.65 12.74 0.845 0.48 ... ... ... 2.93 1.09 ... L8V L9V 1370 3.137 ... -4.61 16.27 0.0877 ... ... ... ... ... ... ... ... ... ... ... ... 1.18 0.59 14.82 12.93 0.82 0.57 ... ... ... 3.15 1.16 ... L9V T0V 1255 3.099 ... -4.66 16.39 0.098 ... ... ... ... ... ... ... ... ... ... ... ... 1.02 0.54 14.81 13.12 0.70 0.68 ... ... ... 3.36 1.23 ... T0V T1V 1240 3.093 ... -4.69 16.47 0.100 ... ... ... ... ... ... ... ... ... ... ... ... 1.02 0.45 14.63 13.29 0.58 0.82 ... ... ... 3.55 1.33 ... T1V T2V 1220 3.086 ... -4.73 16.57 0.100 ... ... ... ... ... ... ... ... ... ... ... ... 0.86 0.27 14.52 13.45 0.53 0.99 ... ... ... 3.70 1.43 ... T2V T3V 1200 3.079 ... -4.77 16.67 0.102 ... ... ... ... ... ... ... ... ... ... ... ... 0.68 0.08 14.45 13.52 ... 1.19 ... ... ... 3.82 1.55 ... T3V T4V 1180 3.072 ... -4.84 16.84 0.101 ... ... ... ... ... ... ... ... ... ... ... ... 0.35 -0.19 14.55 14.20 ... 1.43 ... ... ... 3.90 1.68 ... T4V T4.5V 1170 3.068 ... -4.90 16.99 0.099 ... ... ... ... ... ... ... ... ... ... ... ... 0.2 -0.06 14.69 14.55 ... 1.57 ... ... ... 3.93 1.75 ... T4.5V T5V 1160 3.064 ... -4.95 17.12 0.101 ... ... ... ... ... ... ... ... ... ... ... ... 0.2 -0.08 14.88 14.9 ... 1.70 ... ... ... 3.95 1.81 ... T5V T5.5V 1040 3.017 ... -5.04 17.34 0.099 ... ... ... ... ... ... ... ... ... ... ... ... 0.2 -0.10 15.13 15.1 ... 1.86 ... ... ... 3.97 1.89 ... T5.5V T6V 950 2.978 ... -5.12 17.54 0.100 ... ... ... ... ... ... ... ... ... ... ... ... 0.1 -0.03 15.34 15.3 ... 2.0 ... ... ... 3.98 1.96 ... T6V T7V 825 2.916 ... -5.37 18.17 0.098 ... ... ... ... ... ... ... ... ... ... ... ... 0.0 0.00 15.83 15.8 ... 2.4 ... ... ... 4.01 2.11 ... T7V T7.5V 750 2.875 ... -5.54 18.59 0.095 ... ... ... ... ... ... ... ... ... ... ... ... 0.2 -0.05 16.61 16.5 ... 2.6 ... ... ... 4.05 2.19 ... T7.5V T8V 680 2.833 ... -5.71 19.02 0.095 ... ... ... ... ... ... ... ... ... ... ... ... 0.2 -0.05 17.30 16.9 ... 2.8 ... ... ... 4.08 2.26 ... T8V T8.5V 600 2.778 ... -5.93 19.57 0.097 ... ... ... ... ... ... ... ... ... ... ... ... 0.2 ... 18.05 18.3 ... 3.0 ... ... ... ... ... ... T8.5V T9V 560 2.748 ... -6.15 20.12 0.100 ... ... ... ... ... ... ... ... ... ... ... ... 0.1 -0.20 18.51 18.6 ... 3.2 ... ... ... ... ... ... T9V T9.5V 510 2.708 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... 19.75 20.5 ... 3.4 ... ... ... ... ... ... T9.5V Y0V 450 2.653 ... -6.52 21.04 0.104 ... ... ... ... ... ... ... ... ... ... ... ... ... -0.5 20.15 21.0 ... 3.6 ... ... ... ... ... ... Y0V Y0.5V 400 2.602 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... -0.6 22.0 21.6 ... 3.9 ... ... ... ... ... ... Y0.5V Y1V 360 2.556 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... 22.7 22.2 ... 4.1 ... ... ... ... ... ... Y1V Y1.5V 325 2.512 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... -0.8 23.2 22.9 ... 4.4 ... ... ... ... ... ... Y1.5V Y2V 320 2.505 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... 23.6 23.5 ... 4.7 ... ... ... ... ... ... Y2V Y4V 250 2.398 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... .... ... ... 28.2 ... ... 6.1 ... ... ... ... ... ... Y4V #SpT Teff logT BCv logL Mbol R_Rsun Mv B-V Bt-Vt G-V Bp-Rp G-Rp M_G b-y U-B V-Rc V-Ic V-Ks J-H H-K M_J M_Ks Ks-W1 W1-W2 W1-W3 W1-W4 g-r i-z z-Y Msun #SpT The adopted mean masses a for a given dwarf subtype are tentative. With only a few minor exceptions (mainly for b-y colors; see notes below), this is *not* a compilation of values adopted from similar tables published by other authors. The author's motivation was to construct a "modern" table of mean stellar parameters based on an *independent* survey of the literature and catalog values. In the process, I've made judgements on which stars and stellar classifications reflect the "modern" MK system. You can get a sense of the messiness and care that went into this process by perusing the spectral type note files in the previously mentioned directory. This is an independently constructed compendium, and the author will make small adjustments, corrections, and add content periodically. Values in the table marked by a asterisk (*) are very preliminary, and probably shouldn't be used for any serious calculations yet. -EEM Further notes by spectral class, followed by summaries of updates. OB stars: A major redux of the Q-method of dereddening in Oct 2011 results in some shifts to the color scale among the late-O/early-B stars. There are no O-B2 stars within the Local Bubble (at least out to 75 pc; this is a long standing problem with empirical color calibrations, e.g. Johnson & Morgan 1953), so one must attempt some bootstrap some dereddening in order to empirically derive the intrinsic color sequence. To augment the samples of negligibly reddened stars within 75 pc, I have taken a sample of stars which have measured neutral hydrogen (H I) column densities, as measured through modeling of Lyman alpha absorption in UV spectra (e.g. Bohlin et al. 1983), then estimated E(B-V) from adoption of the E(B-V)/N_HI relation from Savage & Mathis (1979; N(HI)/E(B-V) = 4.8e21 atoms/cm^2/mag). While there may be intrinsic scatter in the N(HI)/E(B-V) relation through the ISM, we consider this a useful statistical dereddening technique for getting at the intrinsic color sequence of hot dwarf stars. While the E(B-V)/N_HI relation is calibrated using E(B-V)s for hot stars that rely on an intrinsic SpT vs. color sequence (and hence one could object that there is some circularity in our calibration scheme), the *slope* of the relation mostly rely on the HI column densities for hot stars with relatively large reddenings - hence any zero-point issues in the color sequence at the 8 parallaxes that place the stars within 75 pc, and have "A0V" classifications, and which have both B-V and U-B photometry in Mermilliod(1991). These will define the curve in the B-V vs. U-B sequence near zero colors. (2) Stars with B class and V luminosity class in the Hipparcos catalog with S/N > 8 parallaxes that place the stars within 75 pc, and which have both B-V and U-B photometry in Mermilliod(1991). These mostly define the approximately linear color sequence between ~B3V and ~B9V. (3) A subsample of O/early-B spectral standard dwarf and/or subgiant stars (V or IV luminosity classifications, preferentially within a few hundred pc) with UBV photometry in the Mermilliod Johnson photometry compendium, *and* an estimate of the neutral hydrogen column density. All of the notes on the dereddening of these hot stars and adopted input parameters are listed in the files (sorted by MK subtype) in the directory at: http://www.pas.rochester.edu/~emamajek/spt/. If one adopts the Q parameter formula: Q = (U-B) - 0.72*(B-V) We have confirmed the Johnson reddening slope - we independently estimate an average reddening slopes of E(U-B)/E(B-V) = 0.732+-0.010 for the ensemble of all Hipparcos O8-B9 dwarfs with UBV photometry in the Mermilliod compendium of Johnson photometry. We retain a slope of 0.72 for continuity with published estimates of the "Q" parameter. The final fits for OB stars (i.e. (U-B)o < 0) are: (B-V)o = -4.776008156728d-03 + 5.522012574154d-01*Q + 1.151583004497d+00*Q^2 + 1.829921229667d+00*Q^3 + 8.933113140506d-01*Q^4 [-0.32 < (B-V)o < 0.02] (U-B)o = 6.230566666312d-03 + 1.533217755592d+00*Q + 1.385407188924d+00*Q^2 + 2.167355580182d+00*Q^3 + 1.075207514655d+00*Q^4 [-1.13 < (U-B)o < 0.02] (U-B)o = -1.368272076317e-02 + 1.590637348534e+00*(B-V) - 1.477363936224e+01*(B-V)^2 + 5.039982446611e+01*(B-V)^3 + 5.472117191781e+02*(B-V)^4 + 9.445941583982e+02*(B-V)^5 [rms = 0.042 mag; -0.32 < (B-V)o < 0.02] (B-V)o = 8.440163260524e-03 + 5.780296047218e-01*(U-B) + 1.322981897905e+00*(U-B)^2 + 2.141912996160e+00*(U-B)^3 + 1.531076773342e+00*(U-B)^4 + 4.212960258861e-01*(U-B)^5 [rms = 0.016 mag; -1.13 < (U-B)o < 0.02] The extinction at V-band was then calculates using the relation listed in Olson (1975): A_V(Johnson) = 3.25*E(B-V) + 0.25*(B-V)o*E(B-V) + 0.05*E(B-V)^2) Our revised Q-method relations were used to deredden the OB stars. The calculated E(B-V) values were then used to deredden the VIJHK photometry so that we could determine the intrinsic color sequence for the hot stars. From the reddening parameters in the Asiago photometric database, we adopted the following reddening relations for our OB stars: A_I(Cousins) = E(B-V)*(1.805 + 0.024*E(B-V)) A_J(2MASS) = E(B-V)*(0.832 + 0.013*E(B-V)) A_H(2MASS) = E(B-V)*(0.527 + 0.009*E(B-V)) A_Ks(2MASS) = E(B-V)*(0.356 + 0.006*E(B-V)) For typical late-O/early-B type stars with (B-V) ~ -0.3, and small extinctions (like the stars used for our calibrations), these relations translate to familiar ratios of total-to-selective extinction of: A_I/A_V ~ 0.57 A_J/A_V ~ 0.26 A_H/A_V ~ 0.17 A_Ks/A_V ~ 0.11 We then deredden the combined UBVIJHKs photometry using these relations (and the updated Q-method calibration to calculate E(B-V)), and fit color sequences to the OB stars for those stars that had reddenings of E(B-V) < 0.3. This was only done for stars that had a Hipparcos multiplicity flag of Ncomp=1, 2MASS photometry quality flags of "AAA" for the JHKs photometry (i.e. the highest reliability level for all 3 near-IR bands), and V-I colors in Hipparcos (which are a mix of published Cousins V-I colors and values carefully interpolated using other published color information, see the ESA 1997 Hipparcos & Tycho volume). There are very few stars with (V-Ks) < -0.8 that satisfied all of our criteria, so their intrinsic colors are an extrapolation of these color relations (and the few points available seem to support the extrapolation, within the photometric uncertainties). M Dwarfs: I *highly* recommend that you use the colors in this table, and spectral standards recommended in the files in the directory: http://www.pas.rochester.edu/~emamajek/spt/. The M standards have changes significantly since the 1950s-1970s, and the 1990s era standards used by Kirkpatrick, Henry, and collaborators have been heavily used over the past two decades. So older compilations of colors/Teffs from the 1980s and early 1990s are likely to be out of date primarily due to shifts in the use of accepted standard stars. Indeed the "dancing" of choice of the standard stars among the M subtypes was one of the motivations for putting together this table. L/T/Y Dwarfs: The Teffs for L/T dwarfs are drawn from the author's compiled list of published Teffs for such objects (each type listed had at least 5 published Teff estimates for representative members of that temperature subclass). I do not yet have note files by each spectral subtype yet for the L/T/Y dwarfs. # UPDATES (I'm obviously calling the version #s by year.month.day) 2011.5.11: updated B9.5V-A2V colors very slightly - fixed a minor, previously unaccounted for discontinuity in V-K vs. B-V sequence, which had minor <0.01 magnitude effects on other colors. 2011.6.21: fixed typo V-I(F4V) = 0.412 => 0.476 (thanks Rahul Patel, Stony Brook). Slightly adjusted colors for G2V stars based on updated discussion on solar color in: http://www.pas.rochester.edu/~emamajek/sun.txt . 2011.6.26: I've added what I consider to be good consensus values for V-band bolometric correction (BCv), absolute V magnitude (Mv) and bolometric luminosities (logL, normalized to Sun) for spectral types A0V through M7V. The values are discussed in the individual spectral type files at: http://www.pas.rochester.edu/~emamajek/spt/ . 2011.6.28: updated Mv, logL for K/M stars by incorporating the sequence of V-Ks vs. Mv by fitting Neill Reid's photometry for CNS3 (nearby) stars. The fit is (for 2.0 < V-K < 9.1): Mv = 1.018502543505d+01 - 9.263270647616d+00*(V-Ks) + 6.602690052816d+00*(V-Ks)^2 - 2.147548532548d+00*(V-Ks)^3 + 3.874832372602d-01*(V-Ks)^4 - 3.536870767807d-02*(V-Ks)^5 + 1.260298536591d-03*(V-Ks)^6, with the rms = 0.46 mag in Mv. This compares fairly well to the V-Ks vs. Mv sequence of Johnson & Apps (2009). Most of the new Mv values for a given spectral type are averages of the Mv vs. V-Ks sequence (for an adopted V-Ks) based on the Johnson & Apps (2009) and custom fit to Reid's photometry compendium for CNS3 stars. Also made minor shifts to the colors for M7V (adopting V-Ks=7.30 instead of 7.23). 2011.8.17: I've added a preliminary 2MASS Ks minus WISE W1 color (Ks - W1) sequence based on the colors of thousands of nearby unreddened BAFGKM stars. I found an intrinsic color sequence for (Ks-W1) between -0.05 < (H-Ks) < 0.30 of (Ks-W1) = 3.401881177741d-02 - 1.331277406699e-01*(H-Ks) - 9.041089929636e-01*(H-Ks)^2 + 2.500587445557e+01*(H-Ks)^3 - 5.485829130472e+01*(H-Ks)^4. One can safely adopt an intrinsic color (Ks-W1) = 0.03 across the AFG dwarf spectral classes. 2011.8.22: added log10(Teff) and uncertainties (assuming one integer subtype; i.e. uncertainty in Teff for B5V is simply approximated as [Teff(B4V)-Teff(B6V)]/2). Added line for O9V and O9.5V. Recheck of BCv scale of OB stars taking into account Lanz & Hubeny (2003, 2007) resulted in minute changes to BCv and logL scale. [I have since removed Teff uncertainties for now] 2011.8.23: added preliminary Teffs for T9V, T9.5V, and Y0V based on Cushing et al. 2011 (http://arxiv.org/abs/1108.4678). 2011.8.24: added (b-y) colors for A stars from Crawford 1979. (b-y) for A0V-A2V from Gray & Garrison 1987, values adopted for 100 < vsini < 200 km/s bin. (b-y) colors for O9V-B9.5V stars are from Warren (1976; MNRAS, 174, 111). (b-y) colors for F2V, F5V-F9V from Crawford 1975 (AJ, 80, 955), with F1V, F3V, F4V colors interpolated. 2011.9.17: minor changes to Teff for F0V and F1V, and minor shift in colors for F1V. 2011.10.4: Bolometric corrections have been edited slightly. The current values were calculated using the median value calculated for the adopted Teff from multiple published calibrations, including Lanz & Hubeny (2003), Code et al. (1976), Balona et al. (1994), Bessell et al. (1998), Bertone et al. (2004), Flower et al. (1996), Masana et al. (2006), and Casagrande et al. (2008). While this median value may not represent the latest, greatest estimate, it does benefit from representing a concensus of literature calibrations (some of which are dependent on the same model atmospheres, e.g. Kurucz), and is relatively insensitive to outlier calibrations. I have added the column "uBCv" which is a naive estimate of the *systematic* uncertainty in the BCv(Teff) scale, calculated using the standard deviation of the BCv values calculated using the various BCv calibrations as a function of Teff. The meaning of uBCv should not be taken too literally (more detailed models in the future could concievably shift the BCv scale at the high and low Teff ends?), but it is a reasonable estimate of the scatter in the BCv scale given the published literature. For the M stars, I explicitly omitted Flower (1996) in the calculations as its BCv(Teff) values were seriously at odds with the Casagrande et al. (2008) BCv scale. The Flower (1996) calibration relies heavily on giants, and the Casagrande et al. calibration draws from modern stellar atmosphere models for cool stars and a large body of optical/near-IR photometry for dwarf stars. For example, for Teff = 3300 K, Flower (1996) predicts BCv = -3.12 mag, while Casagrande et al. (2008) predicts BCv = -1.86 mag. For cooler stars, the Flower (1996) curve should probably be avoided. Use of erroneous bolometric corrections for M dwarfs could systematically, and drastically, affect the inferred luminosities (and hence ages and masses) of pre-MS M stars. 2011.10.8: updated intrinsic (B-V) and (U-B) colors for O9V and O9.5V stars using updated Q-method calculations in the spectral type files. I largely recover a color sequence close to the original Johnson publications. 2011.10.9: updated and screened (B-V), (U-B), Mv, logL, BCv values for O9V-B3V stars. These take into account the updated Q-method calibration and some new estimates of Mv among the standard stars, and the observed main sequence for the Orion Nebula Cluster (ONC) and Upper Sco (US). Added lines for B1.5V and B2.5V subtypes (b-y colors are simply interpolated halfway between the integer subtypes). 2011.10.28: used the revised Q-method to deredden Hipparcos OB stars, and then with the derived Av values, dereddened UBVIJHK magnitudes and calculated recalculated colors for O9V-B9.5V stars. 2011.11.1: Rewrote discussion on deriving the intrinsic color sequence of hot OB stars using the Q-method and dereddening of lightly reddened stars. I've added a column of predicted masses and ages ("lgAge" = log10(age/yr)) for the mean HR diagram positions using adopted "protosolar" evolutionary tracks of Bertelli et al. (2009) [Z=0.017, Y=0.26]. 2011.11.21: Reordered columns in table. 2011.12.2: Removed systematic uncertainty in BCv ("uBCv") and estimated uncertainty in logTeff (for one subtype uncertainty). J-H and H-Ks colors for L dwarfs come from mean estimates calculated using 2MASS photometry with <0.1 mag photometric errors for L and T dwarfs within 0.5 subtype of a given subtype in the DwarfArchives.org database. 2011.12.3: Using data from DwarfArchives.org, I fit polynomials to absolute J magnitude vs. subtype for L and T dwarfs. I find (x = subtype; 0 = 'L0', 10 = 'T0'): M_J = 1.166986798277e+01 + 1.175748107692e+00*x - 6.522381898768e-01*x^2 + 1.992648437227e-01*x^3 - 2.904023621364e-02*x^4 + 2.134433926696e-03*x^5 - 7.715657229082e-05*x^6 + 1.099122975611e-06*x^7. I calculated absolute K magnitude using this M_J relation and the adopted J-H and H-K colors for each subtype. Note that the scatter in the absolute J magnitude vs. subtype is +-0.4 mag, and only 27 L dwarfs and 34 T dwarfs define the relation. 2011.12.13: Slight revision to adopted masses for FGK stars and added masses for M0-M6 dwarfs. 2011.12.21: Minor changes to bolometric correction BCv values of A/F/G stars at the +-0.01 mag level, from inclusion of Masana+2006 and Bertone+2004 BC values into the consensus estimates of BCv(Teff). 2012.8.17: Minor shifts to mass scale for K5V-M5V stars taking into account M_Ks vs. mass calibration from Delfosse+2000. Added mass estimates for late M dwarfs. 2012.11.25: Updated preamble text. Added list of publications citing this online table. 2012.11.26: Updated Teff and BCv scale for O9V-B3V based on new assessments of median Teffs (calculated and from literature) for standard stars. See corresponding updates to notes in individual spectral type note files in directory at: http://www.pas.rochester.edu/~emamajek/spt/ (e.g. O9V.txt, B0V.txt, etc.). 2012.11.30: Updated/reviewed Teff, BCv, logL for B7V, B8V, A0V based on reassessment of median Teffs for standards. 2012.12.01: Updated/reviewed Teff, BCv, logL for B8V, B9V, B9.5V based on reassessment of median Teffs for standards. 2012.12.10: Slight revision to Y0V Teff based on results from Leggett et al. 2013 (and check on Teffs for T9 and T9.5): http://arxiv.org/abs/1212.1210. And added line for T8.5V based on Teffs from Burgasser et al. 2011, Warren et al. 2007, and Burningham et al. 2011. 2012.12.27: The M dwarf files in /spt/ are undergoing a major check up regarding assessing the rank/quality of standards, median colors, bolometric corrections, Teffs, etc. I've made a preliminary update to the Teff scale. Changes to colors have been minor, however the effects on bolometric corrections has been sizeable due to incorporation of results from Casagrande08, Leggett01, and Golimowski04. The overhaul should be done within a few weeks. 2012.12.29: Updated G2V colors and Teff. Updated notes at: http://www.pas.rochester.edu/~emamajek/spt/G2V.txt 2013.02.16: Minor updates to logL and Mbol values. Checked logTeff values. 2013.04.23: Teff, logT, BCv, logL, and Mbol checked, with some minor updates, for all K subtypes. Minor update to Teff scale for M dwarfs. Added approximate V-K colors and Mv estimates for L0 through L3 dwarfs based on Dahn02 photometry. 2013.06.01: Made subtle edits to color tables (usually at 0.001 mag level) and for thorough update before publication of much of the O9-M9 part of the table in Pecaut & Mamajek (submitted to ApJ). Teff estimates were re-checked, and minor shifts made for some GKM stars (usually at <+-50 K level). Added V-Rc colors based on V-Ic to V-R trend from Caldwell et al. (1993, SAAO Circulars, 15, 1) for B through mid-M dwarfs, and based on average V-Ic and R-Ic colors for late Ms from Liebert & Gizis (2006, PASP, 118, 659). Made minors shifts to mass scale for late O and B stars based on including some results from eclipsing binary masses. 2013.06.18: Updated parameters for B0.5V stars due to reexamination of data for Beta Sco Aa (standard star) and B3V (absolute magnitudes). 2013.06.23: Slight shift in absolute magnitude and luminosity for M4V due to inclusion of individual abs mag estimates for M4V standards. 2013.07.02: Minor shifts to adopted optical colors for M6/M7/M8/M9 dwarfs. The mean V-Ic and V-Rc colors for these late M dwarfs are uncertain at the ~0.05-0.1 mag level. 2013.07.05: Based on discussion in Pecaut & Mamajek (2013), we adopt Vmag = -26.71+-0.02 mag and BCv(Sun,G2V) = -0.11. This results in a systematic shift of the bolometric correction scale at the 0.04 mag level, where BCv(Sun) = -0.07 (old) => -0.11 (new). I have shifted all of the BCv and Mbol values to reflect this shift. The new solar BCv value is commensurate with the revised solar constant from Kopp & Lean (2011), and revised inferred solar luminosity (Mamajek 2012), and is calculated as the synthetic V magnitude needed to fit the revised solar irradiance constant (Kopp & Lean 2011) using Teff=5772K BT-Settl model using solar composition. Note that the fitting of BT-Settl models to the empirically derived solar colors from Ramirez12 leads to a solar effective temperature (5776+-22K) which is spot on with the measured value (5772K). A slight shift in adopted V magnitude (~0.03 mag level, from V=-26.74 => -26.71) is needed to force the solar diameter measurements to that predicted from the SED-fitting. The new adopted Vmag is similar to that recently derived by Engelke08 using several different solar spectrum calibrations (their solar V mags are consistent with V = -26.71+-0.01). I still need to make the minor shift to the luminosity scale. 2014.01.23: Updated introduction information to mention Pecaut & Mamajek (2013). 2014.02.23: Included Tycho Bt-Vt colors based on a new analysis of B-V vs. Bt-Vt colors of nearby dwarfs stars plus a small number of lightly reddened O-early-B-type dwarfs. 2014.03.26: Updated J-H (2MASS system) colors for L3-Y0 dwarfs based on examination of Figure 5 of Kirkpatrick et al. (2011, ApJS, 197, 19). Updated Mv estimates for L0-L5 dwarfs based on Dieterich+2014 Mvs as function of V-Ks. 2014.11.14: Fixed equation for Av as function of E(B-V) and (B-V)o. Thanks to Cameron Bell! 2015.06.18: Updated main sequence masses incorporating luminosity-mass calibrations of Eker+2015. 2015.07.03: Added Teffs, BCv, LogL, Mbol, Mv for O3-O8.5V stars. B-V and U-B should be considered preliminary, and are based mainly on previous compilations (e.g. Johnson, Schmidt-Kaler). Minor adjustments to Mbol, logL, Mv for B dwarfs. 2015.09.22: Updated L0-T9 Teffs, logL, and M_J values to those from Fillipazzo+2015. 2016.02.19: Minor updates to temperatures and colors of early M dwarfs; added M1.5V and M2.5V. 2016.04.24: added Sloan/SDSS i-z, Sloan/SDSS-UKIDSS z-Y, and WISE W1-W2 color for M5-T8 dwarfs from Skrzypek+ (2015; A&A 574, A78). The Y, W1, W2 photometry is already on the Vega system. The Sloan/SDSS iz photometry is originally on the AB magnitude system, but Skrzypek+2015 converts it to Vega system using the offsets from Hewett+2006. 2016.05.13: added estimates for M4.5V and M5.5V subtypes. Slight revisions to B-V, U-B colors for mid Ms. 2016.06.09: minor updates to K7/K8/K9V colors, bolometric magnitudes and corrections, etc. 2016.08.01: minor shift in Teff for F8V. 2016.08.21: minor shifts in adopted masses for K8V-M9V incorporating the new empirical mass-luminosity relation of Benedict+2016. 2017.01.27: added line for M3.5V and made minor shift to Teff for M3V. 2017.02.03: added fiducial Teffs and approximate absolute magnitudes for Y0-Y2 based on data from Leggett+2015 and Schneider+2015. 2017.03.03: added line for M6.5V, minor shifts to surrounding Teff scale based on updates to Teffs for M standards. 2017.03.14: added W1-W2, W1-W3, W1-W4 colors based on dwarf locus as function of Tycho Bt-Vt color from Patel+2014 for B5V-K5V. 2017.09.01: minor edits to parameters for K5V, K6V & K7V after further screening of standards of non-standard field stars with multiple classifications of that subtype, and updating of Teffs and related quantities. i-z colors for M0V-M4V added from West+(2011; 2011AJ....141...97W). Added lines for M8.5V, M9.5V. 2017.09.12: updated V-Ic colors for M6V-L5V following Dahn+2017 (https://arxiv.org/abs/1709.02729). 2017.09.25: Add dwarf sequence radius estimates based on Teff, logL - rounded to 3 significant figures. updated M0V parameters and Teff for K7V, and added M0.5V. K8V and K9V parameters are not well defined compared to K7V and M0V, and so in favor of continuity, I've favored simple linear interpolation of parameters for K8V and K9V. 2017.10.07: Check and minor edits to luminosities and masses of O8-B0V stars. 2017.10.10: Added V-G (Johnson-GaiaDR1) color based on a sample of stars within 75pc (negligible reddening), using V magnitudes from Mermilliod (1991) compendium of homogenized Johnson photometry and G magnitudes from Gaia DR1. Scatter in B-V vs. V-G color for stars between roughly A0V and K0V is ~0.025 mag. Stars near the main sequence with -0.04 < B-V < 0.90 are well fit by this low-order polynomial fit: V-G = -8.3585362075385319d-02 + 6.8599239804051382d-01*(B-V) - 6.2235530089560731d-01*(B-V)^2 + 4.1223236421001502d-01*(B-V)^3. 2017.10.17: Minor shift to most values for K1V. 2018.01.02: Updated (b-y) colors for OB dwarfs to values from Kaltcheva et al. (2017). (b-y) colors for B0.5V-B9.5V stars adopted from Table 2 (low-reddened sample), and (b-y) colors for O4.5V-B0V taken from Table 1 of that paper (with some smoothing of the values for the subtypes whose mean values were calculated for only a few stars). 2018.03.07: Updated K7V parameters taking into account well-characterized non-standard K7V stars along with the K7V standards. 2018.03.22: Minor shift to most values for K3V, accounting for properties of more standards and stars with multiple K3V classifications. 2018.05.19: Estimated parameters for K0.5V, K1.5V, K2.5V, K3.5V, K4.5V, K5.5V, K6.5V subtypes based on properties of nearby dwarf stars classified by Gray et al. (2006) on Keenan system of standards, and made some minor edits to parameters for some K dwarfs. 2018.05.24: Changed "H-K" => "H-Ks" in Table column headers to reflect explicitly that the 'K' is explicitly 2MASS Ks (both H and Ks are 2MASS system). 2018.08.02: Accounted for latest dynamical mass vs. absolute Ks magnitude trend for dwarfs of type K1-L2 from Mann et al. (2018). 2018.08.03: added line for F9.5V. Best standard is bet Com. 2018.12.10: preliminary G-V colors added based on median colors of spectral standards from K0V to L0V (with the M7-L0 sequence smoothed), and from the fits for (G-V) as functions of (B-V), (V-Rc), and (V-Ic) from Evans+2018 (where I've plugged in current best estimates for those colors as functions of spectral type into the Evans+2018 polynomials and taken the average G-V). I need to look at this trend a bit more closely for AFG stars. 2019.03.01: added Bp-Rp colors for late K and M dwarfs based on GaiaDR2 colors for standard and stars within 10 pc with vetted spectral types. Absolute G magnitudes (M_G) and G-Rp colors on Gaia DR2 system for L dwarfs come from Smart+2019 (https://arxiv.org/abs/1902.07571). 2019.03.22: added Gaia DR2 Bp-Rp, G-Rp colors for B9 through late K dwarfs, and included absolute G magnitude (M_G) for types where V-G colors were determinable. Based on d<60pc dwarf stars between B9V and late K in SIMBAD - the majority of which now have either Gaia DR2 parallaxes now, or revised Hipparcos parallaxes (for the bright ones). 2019.09.24: Reviewed and updated Teffs for OBAFGKM stars. Updated BCv values for FGK dwarfs to put them on system where BCv=-0.085 for Teff=5772K(Sun) - adopting this value based on estimates from Casagrande+2018 once their values are placed on IAU2015 bolometric magnitude system (they adopt a slightly different Mbol(Sun) and Lsun than IAU values). Reviewed Teff, Mv, Mbol, logL, Rad values and made some minor updates. Removed 0.5-subtype K dwarf entries (will review these and reassess whether these are worth including again). 2019.10.18: For OB dwarfs, updated Teff, BCv, logL, Mbol, Rad. 2019.11.03: For M dwarfs, updated Teff, logL, Mv, Rad, Mass. 2020.02.07: For O3-B1 dwarfs, made minor shifts to U-B, B-V color sequences, Mv, HRD parameters (Mbol, logL, Teff, BCv, Rad). 2020.04.02: Vetted and updated some masses for O through early L. A good fit of log(Mass/Msun) for main sequence (V) stars as function of Mv between O7V and L2V for absolute magnitudes 20.9 < Mv < -4.8 is: a0 = 5.3132790322903922e-001 a1 = -1.5853156020421624e-001 a2 = 8.7346091280499586e-003 a3 = 8.3698240396409276e-004 a4 = -6.6566352189549794e-005 a5 = -1.5435681229533762e-005 a6 = 1.7714870318666100e-006 a7 = -6.3188987403139114e-008 a8 = 7.3812559571593096e-010 log(M/Msun) = a0 + a1*Mv + a2*Mv^2 + a3*Mv^3 + a4*Mv^4 + a5*Mv^5 + a6*Mv^6 + a7*Mv^7 + a8*Mv^8 2020.07.05: Minor shifts to HRD positions for B3V and B4V. Minor changes to B-V, Rad for M dwarfs. 2020.08.06: Have done a full vetting of the Teff, Mv, V-Ks, J-H, and H-K values from O3 through L9 from the most recent estimates from the spectral type data files in directory http://www.pas.rochester.edu/~emamajek/spt/, and incorporated them into this table. g-r colors were added based on a mix of values from 1) Covey+2007, 2) g-r values calculated from B-V colors using Bilir+2005 transformation, and 3) g-r values calculated from R-I colors using Jordi+2006 transformation. 2020.11.18: Have done a complete scrubbing of the adopted Gaia colors (Bp-Rp) and (G-Rp) for M dwarfs via comparison to colors for nearby dwarf standards and exemplars. (Bp-Rp) colors show a peak around M8.5V. 2020.12.05: W1-W2 colors for T6V-Y4V adopted from polynomial trend of Kirkpatrick19. WISE J1828+2650 was assigned Y2V and WISE J0855-0714 assigned Y4V following Kirkpatrick20. Properties of late Ts and Ys draws heavily from Kirkpatrick19 and Kirkpatrick20. 2021.03.02: Minor shifts to Mv, M_G, logL, Rad in K5V-M0V range. 2022.04.08: Updated G-V colors for B1.5V-B9.5V stars based on fitting low reddening (E(B-V)<0.03) B dwarfs from Hipparcos catalog with plx > 3 mas from Kervella+2019 catalog. For 627 B dwarfs with -0.79 < (V-Ks) < 0.10, I fit: (G-V) = 1.5662975867923815e-2 - 4.5474915703530211e-2*(V-Ks) - 2.0632426850689073e-1*(V-Ks)^2 - 1.0690949761461190e-1*(V-Ks)^3 (rms = 0.0148 mag). 2022.04.16: Updated O dwarf masses. # Please email me if you use the table in your research and/or have # any questions. - EEM