sdapy.snerun.snobject._color_at¶

snobject._color_at(filt1, filt2, phase, interpolation=None, index=0, **kwargs)¶

Estimate colour at a given phase.

Parameters

filt1str: filter1
filt2str: filter2
phasefloat: rest frame phase (days) relative to t0
tdbinfloat: threshold for binning
interpolationstr: estimate flux with data epoch less than than tdbin, or interpolation from GP/fits
corr_mkwbool: if correct milky way extinction
corr_hostbool: if host galaxy extinction
indexint: if multiple models available, which of them to be used
quantilelist: use 50 percentile as mean, and 1 sigma (68%% -> 16%% - 84%%) as errors
clobberbool: Redo analysis
zpfloat: zeropoint to convert magnitude to flux. zp = 23.9 for micro Jansky to AB mag zp = 48.6 for ergs/s/cm2/Hz to AB mag e.g. mab = -2.5 * log10(fv[Jy]/3631) = -2.5 * log10(fv[mJy]) + 2.5*log10(3631*1e6)
snrtfloat: SNR threshold to distinguish detection/limit

Returns