sdapy.snerun.snobject._ax3¶

snobject._ax3(xpred=None, index=0, show_title=False, show_legend=False, ylabel_2right=True, show_data=True, show_fits=False, show_gp=False, show_fit_error=True, show_texp=True, color=None, marker=None, markersize=None, label=None, ls=None, fillstyle=None, fontsize=None, **kwargs)¶

Colour curve plot.

Parameters

jd_x0float: x axis zeropoint for mag/flux LCs
ax3_xstylestr: x axis for mag (_ax2) LCs: [rp] rest frame since peak [jd] Junlian date since jd_x0
ax3_xlimlist: x limit
ax3_ylimlist: y limit
show_titlebool: if show title
show_legendbool: if show legend
ylabel_2rightbool: if put y label to right
show_databool: if show data points
show_fit_errorbool: if False, only show best fit, otherwise, show errors or random samplings
show_fitsbool: if show model fittings
show_gpbool: if show GP modellings
show_texpbool: if show explosion epochs
alphabestfloat between 0 and 1: matplotlib alpha for best fit fitting
alphasamplefloat between 0 and 1: matplotlib alpha for random samplings or errors
plot_mcmctfloat between 0 and 1: a threshold that select good mc samples for plotting, rangiing from 0 to 1, e.g. 0.5 means selecting samplings from the top 50 percent of all samplings relying on the likelihoods
plot_nsamplesint: how many random MC samples to be plotted
verbosebool: Enable progress report
If snobject.colors not available, will run snobject.calc_colors to calculate color first, with parameters below
xpredlist: colour phases, if None will use observing epochs of the color_bands
color_bandslist: two bands of the colour
color_interpstr: estimate flux with data epoch less than than tdbin, or interpolation from GP/fits
tdbinfloat: threshold for binning
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