# "A Modern Mean Stellar Color and Effective Temperature Sequence for O9V-Y0V Dwarf Stars" # http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt # Eric Mamajek (University of Rochester) # Version 2014.09.29 # # Much of the content (but not all) 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. 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 # the LTY dwarfs. # # The author's notes on standard stars and the mean properties 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, 2MASS JHKs, and WISE W1 photometry. # #SpT Teff logT BCv Mv logL B-V Bt-Vt U-B V-Rc V-Ic V-Ks J-H H-K Ks-W1 Msun logAge b-y #SpT M_J M_K Mbol O9V 34000 4.531 -3.20 -4.00 4.77 -0.318 ... -1.114 ... -0.369 -1.000 -0.164 -0.071 ... 19.6 6.6* -0.128 O9V -3.44 -3.20 -7.20 O9.5V 32000 4.505 -3.06 -3.90 4.67 -0.312 ... -1.087 ... -0.361 -0.977 -0.161 -0.069 ... 18 6.7* -0.125 O9.5V -3.25 -3.02 -6.96 B0V 31500 4.498 -3.03 -3.80 4.65 -0.307 ... -1.067 ... -0.355 -0.958 -0.159 -0.067 ... 17.7 6.8* -0.121 B0V -3.17 -2.94 -6.83 B0.5V 29000 4.462 -2.87 -3.60 4.47 -0.295 ... -1.026 ... -0.338 -0.913 -0.153 -0.063 ... 13.8 6.9* -0.120 B0.5V -3.01 -2.79 -6.47 B1V 26000 4.415 -2.61 -3.00 4.13 -0.278 ... -0.995 -0.115 -0.325 -0.874 -0.148 -0.059 ... 11.0 7.0* -0.114 B1V -2.14 -1.93 -5.41 B1.5V 24800 4.394 -2.43 -2.60 3.89 -0.252 -0.274 -0.910 -0.114 -0.281 -0.752 -0.132 -0.047 0.035 9.6 7.1* -0.105 B1.5V -2.03 -1.85 -5.03 B2V 20600 4.314 -2.06 -1.70 3.38 -0.210 -0.219 -0.790 -0.094 -0.230 -0.602 -0.113 -0.032 0.036 7.4 7.2* -0.096 B2V -1.25 -1.10 -3.75 B2.5V 18500 4.267 -1.79 -1.40 3.10 -0.198 -0.206 -0.732 -0.087 -0.210 -0.544 -0.105 -0.026 0.036 6.1 7.3* -0.090 B2.5V -0.88 -0.75 -3.19 B3V 17000 4.230 -1.58 -1.10 2.96 -0.178 -0.184 -0.673 -0.080 -0.192 -0.492 -0.098 -0.021 0.036 5.4 7.4* -0.085 B3V -0.73 -0.61 -2.78 B4V 16700 4.223 -1.53 -0.80 2.81 -0.165 -0.170 -0.619 -0.074 -0.176 -0.447 -0.092 -0.016 0.036 5.0 7.5* -0.081 B4V -0.46 -0.35 -2.33 B5V 15700 4.196 -1.37 -0.70 2.71 -0.156 -0.160 -0.581 -0.070 -0.165 -0.417 -0.089 -0.013 0.036 4.6 7.7* -0.075 B5V -0.38 -0.28 -2.07 B6V 14500 4.161 -1.16 -0.50 2.54 -0.140 -0.142 -0.504 -0.062 -0.145 -0.358 -0.081 -0.007 0.035 4.0 7.8* -0.068 B6V -0.23 -0.14 -1.66 B7V 14000 4.146 -1.07 -0.40 2.47 -0.128 -0.129 -0.459 -0.058 -0.133 -0.325 -0.077 -0.004 0.035 3.9 7.9* -0.061 B7V -0.15 -0.07 -1.47 B8V 12500 4.097 -0.79 -0.20 2.24 -0.109 -0.107 -0.364 -0.048 -0.108 -0.254 -0.067 0.003 0.034 3.4 8.1* -0.049 B8V 0.10 0.16 -0.99 B9V 10700 4.029 -0.44 0.50 1.86 -0.070 -0.063 -0.200 -0.028 -0.061 -0.121 -0.050 0.016 0.032 2.8 8.3* -0.035 B9V 0.59 0.62 0.06 B9.5V 10400 4.017 -0.38 0.80 1.71 -0.050 -0.040 -0.130 -0.017 -0.035 -0.048 -0.044 0.021 0.031 2.5 8.4* -0.026 B9.5V 0.83 0.85 0.42 A0V 9700 3.987 -0.24 1.11 1.54 0.000 0.013 -0.005 0.001 0.004 0.041 -0.032 0.028 0.030 2.3 8.5 0.000 A0V 1.07 1.07 0.87 A1V 9200 3.965 -0.15 1.34 1.41 0.043 0.056 0.033 0.019 0.044 0.101 -0.024 0.031 0.030 2.2 8.6 0.017 A1V 1.25 1.24 1.19 A2V 8840 3.946 -0.10 1.48 1.33 0.074 0.091 0.063 0.042 0.091 0.188 -0.010 0.034 0.029 2.1 8.7 0.038 A2V 1.32 1.29 1.38 A3V 8550 3.932 -0.06 1.55 1.29 0.090 0.109 0.077 0.050 0.108 0.228 -0.002 0.034 0.029 2.00 8.7 0.055 A3V 1.35 1.32 1.49 A4V 8270 3.917 -0.04 1.76 1.20 0.140 0.166 0.097 0.078 0.164 0.353 0.022 0.037 0.029 1.91 8.8 0.071 A4V 1.47 1.41 1.72 A5V 8080 3.907 -0.03 1.84 1.16 0.160 0.185 0.100 0.089 0.186 0.403 0.031 0.038 0.029 1.90 8.8 0.090 A5V 1.51 1.44 1.81 A6V 8000 3.903 -0.02 1.89 1.14 0.170 0.194 0.098 0.094 0.197 0.428 0.036 0.038 0.029 1.83 8.9 0.099 A6V 1.54 1.46 1.87 A7V 7800 3.892 0.00 2.07 1.06 0.210 0.233 0.091 0.117 0.242 0.528 0.055 0.040 0.029 1.76 8.9 0.107 A7V 1.64 1.54 2.07 A8V 7500 3.874 0.00 2.29 0.97 0.250 0.274 0.082 0.140 0.288 0.626 0.075 0.042 0.028 1.67 9.0 0.132 A8V 1.78 1.66 2.29 A9V 7440 3.872 0.00 2.30 0.97 0.255 0.279 0.080 0.143 0.294 0.638 0.078 0.043 0.028 1.66 9.0 0.145 A9V 1.78 1.66 2.30 F0V 7200 3.857 -0.01 2.51 0.89 0.294 0.317 0.053 0.166 0.339 0.732 0.098 0.045 0.028 1.58 9.1 0.158 F0V 1.90 1.76 2.50 F1V 7030 3.847 -0.01 2.79 0.77 0.334 0.350 0.021 0.190 0.385 0.828 0.119 0.047 0.028 1.50 9.1 0.204 F1V 2.13 1.96 2.78 F2V 6810 3.833 -0.02 2.99 0.70 0.374 0.390 -0.008 0.213 0.432 0.925 0.140 0.050 0.028 1.44 9.2 0.250 F2V 2.26 2.07 3.97 F3V 6720 3.827 -0.03 3.08 0.67 0.389 0.405 -0.016 0.222 0.449 0.961 0.147 0.051 0.028 1.43 9.2 0.263 F3V 2.32 2.12 3.05 F4V 6640 3.822 -0.04 3.23 0.61 0.412 0.428 -0.026 0.236 0.476 1.017 0.159 0.052 0.028 1.37 9.2 0.277 F4V 2.42 2.21 3.19 F5V 6510 3.814 -0.04 3.40 0.54 0.438 0.455 -0.029 0.252 0.506 1.079 0.173 0.054 0.028 1.32 9.3 0.290 F5V 2.55 2.32 3.36 F6V 6340 3.802 -0.05 3.70 0.43 0.484 0.504 -0.021 0.276 0.553 1.185 0.199 0.057 0.028 1.25 9.4 0.317 F6V 2.78 2.52 3.65 F7V 6240 3.795 -0.06 3.87 0.36 0.510 0.534 -0.012 0.290 0.579 1.244 0.213 0.060 0.027 1.21 9.5 0.332 F7V 2.90 2.63 3.81 F8V 6150 3.789 -0.07 4.01 0.31 0.530 0.558 0.001 0.300 0.599 1.290 0.225 0.061 0.027 1.18 9.6 0.350 F8V 3.01 2.72 3.94 F9V 6040 3.781 -0.08 4.15 0.26 0.552 0.587 0.014 0.312 0.620 1.340 0.237 0.063 0.027 1.14 9.7 0.378 F9V 3.11 2.81 4.07 G0V 5920 3.772 -0.09 4.39 0.17 0.588 0.638 0.049 0.331 0.656 1.421 0.258 0.066 0.027 1.09 9.7 ... G0V 3.29 2.97 4.30 G1V 5880 3.769 -0.10 4.50 0.13 0.604 0.661 0.067 0.340 0.672 1.458 0.267 0.068 0.027 1.07 9.8 ... G1V 3.38 3.04 4.40 G2V 5770 3.761 -0.11 4.79 0.01 0.650 0.724 0.133 0.363 0.713 1.564 0.293 0.073 0.028 1.00 9.8 ... G2V 3.57 3.20 4.68 G3V 5720 3.757 -0.12 4.86 -0.01 0.661 0.739 0.152 0.368 0.722 1.590 0.299 0.074 0.028 1.00 ... ... G3V 3.64 3.27 4.74 G4V 5680 3.754 -0.13 4.94 -0.04 0.674 0.757 0.175 0.374 0.733 1.621 0.307 0.075 0.028 0.99 ... ... G4V 3.70 3.32 4.80 G5V 5660 3.753 -0.13 4.98 -0.05 0.680 0.764 0.185 0.377 0.738 1.635 0.310 0.076 0.028 0.98 ... ... G5V 3.74 3.35 4.84 G6V 5590 3.747 -0.15 5.13 -0.11 0.704 0.796 0.227 0.388 0.758 1.691 0.324 0.079 0.028 0.97 ... ... G6V 3.84 3.44 4.98 G7V 5530 3.743 -0.16 5.18 -0.12 0.713 0.809 0.243 0.393 0.766 1.712 0.329 0.080 0.028 0.96 ... ... G7V 3.88 3.47 5.02 G8V 5490 3.734 -0.17 5.32 -0.17 0.737 0.842 0.284 0.404 0.786 1.768 0.342 0.082 0.028 0.94 ... ... G8V 3.97 3.55 5.15 G9V 5340 3.728 -0.21 5.55 -0.25 0.777 0.894 0.358 0.423 0.820 1.861 0.365 0.087 0.029 0.91 ... ... G9V 4.14 3.69 5.34 K0V 5280 3.723 -0.22 5.76 -0.33 0.816 0.944 0.436 0.443 0.853 1.953 0.387 0.091 0.030 0.89 ... ... K0V 4.29 3.81 5.54 K1V 5170 3.713 -0.26 5.91 -0.37 0.847 0.982 0.502 0.460 0.883 2.034 0.405 0.094 0.030 0.86 ... ... K1V 4.47 3.97 5.65 K2V 5040 3.706 -0.29 6.19 -0.47 0.893 1.047 0.600 0.487 0.929 2.155 0.432 0.099 0.031 0.85 ... ... K2V 4.57 4.04 5.88 K3V 4840 3.685 -0.41 6.57 -0.58 0.990 1.166 0.801 0.544 1.025 2.410 0.490 0.110 0.034 0.81 ... ... K3V 4.76 4.16 6.16 K4V 4620 3.665 -0.55 7.04 -0.71 1.100 1.306 1.004 0.640 1.190 2.733 0.544 0.125 0.039 0.78 ... ... K4V 4.98 4.31 6.48 K5V 4450 3.648 -0.67 7.25 -0.75 1.134 1.352 1.056 0.671 1.246 2.835 0.560 0.130 0.041 0.75 ... ... K5V 5.11 4.42 6.58 K6V 4200 3.623 -0.86 7.88 -0.92 1.257 1.454 1.199 0.771 1.448 3.190 0.605 0.151 0.051 0.70 ... ... K6V 5.45 4.69 7.07 K7V 4050 3.607 -1.00 8.30 -1.04 1.336 1.538 1.222 0.824 1.574 3.407 0.623 0.168 0.061 0.64 ... ... K7V 5.68 4.89 7.30 K8V 3970 3.599 -1.11 8.60 -1.12 1.382 1.592 1.213 0.859 1.671 3.554 0.630 0.181 0.069 0.62 ... ... K8V 5.86 5.05 7.52 K9V 3880 3.589 -1.25 8.96 -1.22 1.418 1.634 1.198 0.900 1.802 3.728 0.624 0.197 0.081 0.60 ... ... K9V 6.05 5.23 7.77 M0V 3850 3.585 -1.30 9.16 -1.26 1.431 1.650 1.190 0.913 1.848 3.790 0.622 0.203 0.086 0.58 ... ... M0V 6.14 5.37 7.90 M1V 3680 3.566 -1.53 9.80 -1.42 1.484 ... 1.171 0.974 2.074 4.100 0.608 0.227 0.104 0.52 ... ... M1V 6.54 5.70 8.27 M2V 3550 3.550 -1.65 10.30 -1.57 1.500 ... 1.170 1.001 2.173 4.240 0.600 0.234 0.110 0.5 ... ... M2V 6.89 6.06 8.65 M3V 3400 3.531 -1.97 11.14 -1.78 1.544 ... 1.181 1.079 2.420 4.600 0.579 0.252 0.122 0.4 ... ... M3V 7.40 6.54 9.17 M4V 3200 3.505 -2.59 12.80 -2.20 1.661 ... 1.215 1.241 2.831 5.250 0.557 0.282 0.139 0.24 ... ... M4V 8.39 7.55 10.21 M5V 3050 3.484 -3.28 14.30 -2.52 1.874 ... 1.433 1.446 3.277 5.942 0.580 0.311 ... 0.15 ... ... M5V 9.25 8.36 11.02 M6V 2800 3.447 -4.36 16.62 -3.02 2.000 ... ... 1.950 4.100 7.300 0.605 0.352 ... 0.10 ... ... M6V 10.28 9.32 12.26 M7V 2650 3.423 -5.06 17.81 -3.21 2.060 ... ... 2.180 4.520 8.050 0.613 0.386 ... 0.098 ... ... M7V 10.76 9.76 12.75 M8V 2570 3.410 -5.66 18.75 -3.35 2.130 ... ... 2.150 4.600 8.700 0.675 0.446 ... 0.082 ... ... M8V 11.16 10.04 13.09 M9V 2450 3.389 -5.73 19.26 -3.53 ... ... ... 1.890 4.370 8.850 0.749 0.481 ... 0.065 ... ... M9V 11.64 10.41 13.53 L0V 2250 3.352 ... 19.8 ... ... ... ... ... 4.6 9.3 0.79 0.50 ... ... ... ... L0V 11.67 10.38 ... L1V 2200 3.342 ... 20.3 ... ... ... ... ... 4.8 9.6 0.80 0.54 ... ... ... ... L1V 12.37 11.03 ... L2V 2190 3.340 ... 20.8 ... ... ... ... ... 4.9 9.9 0.87 0.57 ... ... ... ... L2V 12.61 11.17 ... L3V 1920 3.283 ... 21.3 ... ... ... ... ... 5.0 10.2 1.00 0.63 ... ... ... ... L3V 12.82 11.22 ... L4V 1810 3.258 ... 22.2 ... ... ... ... ... 5.5 10.8 1.14 0.63 ... ... ... ... L4V 13.14 11.47 ... L5V 1750 3.243 ... 23.1 ... ... ... ... ... 6.0 11.4 1.13 0.65 ... ... ... ... L5V 13.55 11.82 ... L6V 1670 3.223 ... ... ... ... ... ... ... ... ... 1.08 0.64 ... ... ... ... L6V 13.95 12.27 ... L7V 1590 3.201 ... ... ... ... ... ... ... ... ... 1.10 0.62 ... ... ... ... L7V 14.26 12.62 ... L8V 1430 3.155 ... ... ... ... ... ... ... ... ... 1.14 0.63 ... ... ... ... L8V 14.43 12.70 ... L9V 1400 3.146 ... ... ... ... ... ... ... ... ... 1.10 0.63 ... ... ... ... L9V 14.44 12.74 ... T0V 1370 3.137 ... ... ... ... ... ... ... ... ... 1.02 0.54 ... ... ... ... T0V 14.34 12.90 ... T1V 1325 3.122 ... ... ... ... ... ... ... ... ... 1.02 0.45 ... ... ... ... T1V 14.21 12.87 ... T2V 1280 3.107 ... ... ... ... ... ... ... ... ... 0.86 0.27 ... ... ... ... T2V 14.12 13.19 ... T3V 1240 3.093 ... ... ... ... ... ... ... ... ... 0.68 0.08 ... ... ... ... T3V 14.14 13.69 ... T4V 1205 3.081 ... ... ... ... ... ... ... ... ... 0.35 -0.19 ... ... ... ... T4V 14.32 14.51 ... T4.5V 1185 3.073 ... ... ... ... ... ... ... ... ... 0.2 -0.06 ... ... ... ... T4.5V 14.48 14.66 ... T5V 1160 3.064 ... ... ... ... ... ... ... ... ... 0.2 -0.08 ... ... ... ... T5V 14.68 14.90 ... T5.5V 1055 3.023 ... ... ... ... ... ... ... ... ... 0.2 -0.10 ... ... ... ... T5.5V 14.92 15.18 ... T6V 970 2.987 ... ... ... ... ... ... ... ... ... 0.1 -0.03 ... ... ... ... T6V 15.20 15.54 ... T7V 950 2.978 ... ... ... ... ... ... ... ... ... 0.0 0.00 ... ... ... ... T7V 15.91 16.36 ... T7.5V 815 2.911 ... ... ... ... ... ... ... ... ... 0.2 -0.05 ... ... ... ... T7.5V 16.36 16.85 ... T8V 730 2.863 ... ... ... ... ... ... ... ... ... 0.2 -0.05 ... ... ... ... T8V 16.89 17.43 ... T8.5V 630 2.799 ... ... ... ... ... ... ... ... ... 0.2 ... ... ... ... ... T8.5V 17.55 ... ... T9V 555 2.744 ... ... ... ... ... ... ... ... ... 0.1 -0.20 ... ... ... ... T9V 18.40 18.48 ... T9.5V 500 2.699 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... T9.5V 19.52 19.32 ... #Y0V 400 2.602 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... Y0V 24 ... ... #SpT Teff logT BCv Mv logL B-V Bt-Vt U-B V-Rc V-Ic V-Ks J-H H-K Ks-W1 Msun lgAge b-y #SpT M_J M_Ks Mbol # #The adopted mean masses and log(age/yr)s 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 Ca #meron Bell! # ## Publications which have used this table (last updated 6/1/2013) ## Please email me if you use the table in your research and/or have ## any questions. - EEM # #http://adsabs.harvard.edu/abs/2012ApJ...746..154P (Pecaut et al., 2012, ApJ, 746 #, 154) #http://adsabs.harvard.edu/abs/2012ApJ...756..133C (Chen et al., 2012, ApJ, 756, #133) #http://adsabs.harvard.edu/abs/2012ApJ...761..162H (Hynes et al., 2012, ApJ, 761, # 162) #http://adsabs.harvard.edu/abs/2012MNRAS.427.3358G (Goulding et al., 2012, MNRAS, # 427, 3358) #http://adsabs.harvard.edu/abs/2013ApJ...766....6B (Barenfeld et al., 2013, ApJ, #766, 6) #http://adsabs.harvard.edu/abs/2013MNRAS.428.3543R (Ratti et al., 2013, MNRAS, 42 #8, 3543) #http://adsabs.harvard.edu/abs/2013MNRAS.428.2118D (de Marco et al., 2013, MNRAS, # 428, 2118) #http://adsabs.harvard.edu/abs/2013MNRAS.431L..10R (Ratti et al., 2013, MNRAS, 43 #1, L10) #(Konishi et al., 2014, PASJ, in press) #