Hi,
Not sure this is the good place for this issue as this is more a physical question, but I'll give it a shot. Related to #44
The spectra computed with PyatomDB are in the object rest frame. If the object lies at redshift z, how to compute its spectra in the observer frame ?
As I understand :
- If the band of interest is
X1 to X2 keV in the observer frame, then one should compute the raw spectrum in the rest frame in the band X1*(1+z) - X2*(1+z) keV
- Then because the units are
photons and bins^-1, there is no need to divide the spectrum by (1+z) (?) (usually one would do that for the K-correction). So the X1*(1+z) - X2*(1+z) keV spectrum is directly the X1 to X2 keV spectrum.
- So the only transformation needed is
f * ne * np * Volume / (4*pi*DL(z)^2) * Aeff
- (If needed, rmf & arf have to be applied in last)
Is there anything wrong with this ?
Hi,
Not sure this is the good place for this issue as this is more a physical question, but I'll give it a shot. Related to #44
The spectra computed with PyatomDB are in the object rest frame. If the object lies at redshift z, how to compute its spectra in the observer frame ?
As I understand :
X1 to X2 keVin the observer frame, then one should compute the raw spectrum in the rest frame in the bandX1*(1+z) - X2*(1+z) keVphotonsandbins^-1, there is no need to divide the spectrum by(1+z)(?) (usually one would do that for the K-correction). So theX1*(1+z) - X2*(1+z) keVspectrum is directly theX1 to X2 keVspectrum.f * ne * np * Volume / (4*pi*DL(z)^2) * AeffIs there anything wrong with this ?