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

#### Convert Flux ⇒ Luminosity

 Flux = erg/cm2/s keV/cm2/s W/m2 input is log(F)? At distance = pc kpc Mpc z using DL =Mpc OUTPUT L = keV/s erg/s W L☉ M•@fEdd=1 M•@fEdd=0.001 log10L =

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

 Flux density = 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 input is log[Fν/Fλ]? At wavelength = Å nm μm mm m } Fill in one of these OR at frequency = 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 Lν or Lλ = erg/s/keV erg/s/Hz W/Hz W/Å erg/s/Å Abs Mag log10 = Output bandwidth = fractional eV keV GHz MHz μm nm Å OUTPUT ΔνLν or ΔλLλ = erg/s W L☉ 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.