Table 1: The polynomial fit used in the model.
  a0 a1 a2 a3 a4 a5 a6 rms error
MR 1.063e+01 -1.265e+01 6.343e+00 -1.333e+00 1.438e-01 -7.656e-03 1.591e-04 0.433
MI 8.075e+00 -9.450e+00 4.890e+00 -1.031e+00 1.102e-01 -5.768e-03 1.175e-04 0.315
MJ 1.064e+00 -5.835e-01 8.581e-01 -1.886e-01 2.033e-02 -1.063e-03 2.160e-05 0.076
MH 1.202e-01 8.509e-01 7.639e-02 -1.412e-02 1.294e-03 -5.493e-05 8.356e-07 0.039
The fits take the form $M_X = \sum_i a_i M_K^i$. As in the SIPSII survey the R/I bands are photographic $R_{\rm 59F}$/ $I_{\rm IVN}$ and the J, H, and $K_{\rm s}$ bands are on the 2MASS system. Objects in the fit in different photometric systems had their magnitudes converted using Bessell (1986) for the optical data and Carpenter (2001) for the infrared.

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