From: Robert A. Knop Jr. (robert.a.knop@vanderbilt.edu)
Date: Thu Feb 27 2003 - 11:47:05 PST
Reading the 1998 "dark side" paper, it's a little difficult to figure
out what the prior they used on E(B-V) was. From reading it, I can
figure out that it's 0 for E(B-V)<0, but it's hard to figure out what
the high end cutoff is.
Does anybody know what what was the real probability distribution they
used as a prior, and how they used it?
My plan is to take their mB and mV values, subtract them to get a color,
and use that to figure out E(B-V). This isn't really consistent with
how I did it for our supernovae, but it's the best approximation I can
get without refitting their lightcurve data. HOWEVER, if their
uncertainties *already* include the color uncertainty, we'll be
double-counting that uncertainty; do that? Also, if their mB values
have already included the bias of this prior, we'll also be
double-biasing. Does anybody know what the case is?
The more I think about this, the more I fear I may be stuck refitting
their lightcurve data :/
-Rob
-- --Prof. Robert Knop Department of Physics & Astronomy, Vanderbilt University robert.a.knop@vanderbilt.edu
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