sdapy.snerun.snobject._ax5¶

snobject._ax5(phase, index=0, interpolation=None, show_title=False, show_legend=False, show_data=True, show_fits=True, show_fit_error=True, **kwargs)¶

show constructed SED of specific epochs

Parameters

ax5_ystylestr: y axis for sed (_ax5) LCs: [linear] or [log] scale
ax5_xlimlist: x limit
ax5_ylimlist: y limit
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
do_kcorrbool: K corrected the photometry or spectra
ab2vegabool: set it True if input UV/IR data in AB, if they’re vega, set to False
sed_typelist: which data to fit the SED: [bb] photometric points from varies of interpolations, or [spec] the spectrum
sed_color_interplist: for SED fitting with multiband photometry, how to estimate the missing bands, 1: epochs with all filters within color_thre hours. 2: epochs with one filter, and the others from analytic fits. 3. epochs with one filter, and the other from Gaussian process
sed_bandslist: filters to make blackbody, give a list. e.g.[‘g’,’r’,’i’], or None will use all possible bands
sed_abscal_bandslist: which photometry bands to be used to absolute calibrate the selected spectra
sed_abscal_methodlist: how to use photometry to calibrate the spectra: [cal]ibrate or [mangle] the spetra
sed_mangle_funclist: mangling function
spec_snrfloat: if no error from spectra, add noise level of snr