Sample selection:

Dwarf galaxies - \(8<logM_{\star}9\), \(z<0.02\), no AGN

Massive galaxies - \(10<logM_{\star}<11\), \(z<0.07\), no AGN

Comparison sample - Same except out to \(z<2\times z_{max,sample}\). Incomplete, but we only use these objects to derive fiber corrections.

Dust correction - derive E(B-V) from Balmer decrement

Fiber corrections (requires involved discussion):

-Define ”overlap sample” between science sample and corresponding comparison sample: -”Sceince overlap sample” - objects in the science sample that do not fit into fiber at sample redshifts, but would at comparison redshifts

-”Comparison overlap sample” - objects in the science sample that do fit into fiber at comparison redshifts, but would not at sample redshifts

-At fixed size, how do we scale the science overlap sample so as to bring it into agreement with the comparison overlap sample?

-Assume correction factor goes as \(\Psi^{-\alpha}\), where \(\Psi\) is the fraction of the galaxy’s area contained within the fiber

-Fit for alpha such that the median parameters (e.g. \(H\alpha\) EW) of the overlap sample are equal

Balmer decrement, from which we derive reddening corrections.