sdapy.snerun.snobject.lyman_bol

snobject.lyman_bol(xpred=None, index=0, returnv=False, **kwargs)

Calculate bolometric LC from colours, with Lyman bolometric correction.

Parameters

make_bollist

how to make bolometric lcs: [lyman] with BC defined by Lyman approach, [bb] blackbody fits, or [spec] absolute calibrated spectra

lyman_bandslist

two bands of the colour

lyman_interpstr

estimate flux with data epoch less than than tdbin, or interpolation from GP/fits

lyman_bc_phasestr

which Lyman BC to be used: [normal] phase, [cool] phase

verbosebool

show process

returnvbool

if return the luminosities, or store them in the class

xpredlist

colour phases, if None will use observing epochs of the color_bands

bin_rangelist

for bin method, predict range

gp_rangelist

for GP method, predict range

fit_rangelist

for fit method, predict range

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

See also

snobject.calc_colors

Notes

• This function will use colours from snobject.calc_colors if it had been done, otherwise, will call snobject.calc_colors first.

Therefore, parts of kwargs above were for snobject.calc_colors.

• sntype should be defined properly, so that can be used to find a BC function,

at https://github.com/saberyoung/HAFFET/blob/master/sdapy/data/bc_table.txt. Here, we include Ib/Ic/IIb/Ic-BL for SESNe. If you assume for instance SLSN had similar BC as SESNe, you could add it in the BC_Lyman, at https://github.com/saberyoung/HAFFET/blob/master/sdapy/functions.py.