sfr_ha

edge_pydb.conversion.sfr_ha(flux_ha, flux_hb=None, e_flux_ha=None, e_flux_hb=None, name='sigsfr', column=True, imf='kroupa')

Convert Halpha intensity to SFR surface density, optionally with extinction estimates and corrections (if flux_hb is provided). Note that both e_flux_ha and e_flux_hb must not be None in order to propagate the error. Otherwise the SFR is computed without dust correction (if flux_hb=None) or without error estimation.

Parameters:

flux_haastropy.table.Column

The H-alpha flux values

flux_hbastropy.table.Column

The H-beta flux values. If not provided, no dust correction is made.

e_flux_haastropy.table.Column

Errors in H-alpha flux values. If not provided, error propagation skipped.

e_flux_hbastropy.table.Column

Errors in H-beta flux values.

namestring

Name of the output Column; error column will be prepended with ‘e_’

columnboolean

True to return astropy Column objects, otherwise return arrays

imfstring

‘salpeter’ to scale result by 1.51 (default uses Kroupa IMF)

Returns:

several columns depending on input (see code)