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We'll parameterize this with an exponent alpha and define the Shape Measurement Merit as
SMMFWLMF_r=sqrt(t/15)*(T/1)*(sqrt(1/sky))*(1/FWHM)^(1+alpha).
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For F filters there is a time penalty associated with changing filters. This can be represented by a symmetrical F x F matrix, but it's probably fine to just use a scalar t_filter.
Scientific Weighting Factors
Not all science goals are equal. We should assign pre-factors to the photometric and weak lensing merit functions, and any others that might be useful, such that the sum of all weights is 1.
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Oct 18 2013, C. Stubbs
Observations obtained at angles z from zenith suffer from two effects:
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- determine the rank-ordered priority of all fields on the meridian, in each passband, for different potential values of seeing.
- reject the fields that never appear in the top 1000. These have such low priority we'd never get to them.
- For each parametric value of seeing, compute the sequence of observations that maximizes the merit function, including the slew overhead contribution.
A merit function function we'd seek to maximize therefore might look something like this:
MF=(sequence efficiency) * sum_fields {temporal merit} {(Point source weight)*PSPMF+(1-Point source weight)*WLMF}{Field and filter priority}
subject to these constraints:
- sum of time used = total time available
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Some references
LSST science book
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