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Hiragino Kaku Gothic Std W8.otf 0 14 ) we have again identified three groups of candidates (Figure \[fig:mips\]) which are all relatively well-matched with our model, and which we here term the first three tiers of candidates. ![Magnitude versus the predicted $Y$ band absolute magnitude for white dwarf candidates from the MPFC15 White Dwarf Catalog with no reliable constraint on parallax (but observed to be within $2\farcs4$ of a star to form a close pair). []{data-label=”fig:mips”}](f8_color.pdf){width=”50.00000%”} Conclusion ========== We have presented the first up-to-date (April 2018) white dwarf catalog from the MPC. We also presented the first model of the absolute magnitudes of white dwarfs as a function of temperature, and explain why the model is so close to the empirical Johnson-Kron-Cousins system. Our model allows us to calculate the distance that each white dwarf will have based on its absolute $I$ magnitude, and we put it online at [ We have also explained how to use this model to quickly and easily identify the right WDs for spectroscopy at high proper motion. Bailer-Jones, C. A. L., 2018,, 155, 46 Bochanski, J. J., West, A. A., Hawley, S. L., & Covey, K. R., 2010,, 139, 200 Buchanan, R. et al., 2006,, 131, 2306 Dahn, C. C., Bergeron, P., Liebert, J., Harris, H. C., Leggett, S. K., & Knapp, G. R., 2002,, 575, 431 Dahn, C. C., & Guinan, E. F., 1998, IAU, 192, 1 Dahn, C. C., Harris, H. C., Leggett, S. K., Guetter, H., & VandenBerg, D. A., 2002,, 124, 1170 Dahn, C. C., et al., 2014,, 787 37a470d65a
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