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TomDwelly.com
Astro-software engineer for hire
Luminosity to Flux

#### Convert Luminosity ⇒ Flux

 Luminosity = erg/s keV/s W L☉ M•@fEdd=1 M•@fEdd=0.001 input is log(L)? At distance = cm m au pc kpc Mpc z using DL =Mpc OUTPUT Flux = keV/cm2/s erg/cm2/s W/m2 JyHz log10F =

#### Convert Luminosity Density ⇒ Flux Density and Flux

 Luminosity density = erg/s/keV erg/s/Hz W/Hz L☉/Hz Abs Mag W/freq erg/s/freq Lsol/freq W/m W/Å erg/s/Å L☉/Å W/wavelength erg/s/wavelength Lsol/wavelength input is log(L)? At wavelength = Å nm μm mm m } Fill in one of these OR at frequency = Hz MHz GHz THz OR at Energy = eV Ry keV MeV Assuming a distance = z cm m km miles au pc kpc Mpc Gpc using DL =Mpc OUTPUT Fν or Fλ = Jy mJy μJy nJy erg/cm2/s/Hz keV/cm2/s/Hz erg/cm2/s/keV keV/cm2/s/keV mW/m2/Hz W/m2/Hz AB mag erg/cm2/s/Å W/m2/Å W/m2/μm W/m2/m log10 = Output bandwidth = fractional eV keV GHz MHz μm nm Å OUTPUT ΔλFλ or ΔνFν = keV/cm2/s erg/cm2/s JyHz W/m2 log10 =

Note, for redshift-to-distance calculations, this converter uses the analytical Luminosity Distance
approximation of T. Wickramasinghe & T.N. Ukwatta (2010), astroph-1003.0483
Which is valid for flat space cosmologies (i.e. ⇒ ΩΛM = 1) only.
Will be using the following (adjustable) cosmological parameters:
H0 = km s-1 Mpc-1, ΩΛ=, ΩM = ⇒ ΩΛM=

This page uses a modified version of Jan Moesen's Javascript implemenation of the sprintf() function.