Fig. 2 from Characterization of M, L, and T Dwarfs in the Sloan Digital Sky Survey

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Characterization of M, L, and T Dwarfs in the Sloan Digital Sky Survey

Authors: Suzanne L. Hawley, Kevin R. Covey, Gillian R. Knapp, David A. Golimowski, Xiaohui Fan, Scott F. Anderson, James E. Gunn, Hugh C. Harris, Željko Ivezić, Gary M. Long, Robert H. Lupton, Peregrine M. McGehee, Vijay Narayanan, Eric Peng, David Schlegel, Donald P. Schneider, Emily Y. Spahn, Michael A. Strauss, Paula Szkody, Zlatan Tsvetanov, Lucianne M. Walkowicz, J. Brinkmann, Michael Harvanek, Gregory S. Hennessy, S. J. Kleinman, Jurek Krzesinski, Dan Long, Eric H. Neilsen, Peter R. Newman, Atsuko Nitta, Stephanie A. Snedden, and Donald G. York

Hawley et al. 2002 The Astronomical Journal 123 3409.

Provider: AAS Journals

Caption: Fig. 2.

Difference between the 2MASS J magnitude and the MKO J magnitude plotted for 21 late‐type dwarfs measured with both systems. Numerical spectral types are assigned as M0 = 0, M5 = 5, L0 = 10, L5 = 15, T0 = 20, and T5 = 25 here and in all subsequent figures where numerical spectral types are used for fits. The linear least‐squares fit shown is given in the text. MKO J magnitudes given in Table 4 (and in Leggett et al. 2002 for other previously published objects in the sample) were transformed to the 2MASS system by using this relation.

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