Spitzer Documentation & Tools
IRS Instrument Handbook

## 9.5  Computation of IRS Synthetic Photometry

Photometry calculations are carried out in using the following definitions:

ν = c / λ

Tν = value in the response (transmission curve) table, interpolated for ν

Rν = Tν         for MIPS 24

= Tν / ν   for all others

fν = interpolated flux at ν

σν = interpolated uncertainty of flux at ν

CC = color correction factor, 0.9679 for MIPS 24, and 1.0000 for all others.

Computation of the MIPS 24 value is explained below.

BB(ν)  = blackbody flux density at ν for a temperature of 10,000 Kelvin

Photometric flux is calculated as follows:

FLUX  = CC * ∫  fν Rν dν   /     ∫  Rν

The flux uncertainty is calculated by first integrating the input uncertainties:

UNCinitial  =  ∫  σν Rν dν   /      ∫  Rν

UNCfinal  =  sqrt ( UNCinitial2 + (FLUX * uncadjust)2 )

For all bands except MIPS 24, the standard reference spectrum is fν =1/ν so that the color correction factor is CC=1. For MIPS 24, a 10,000 Kelvin blackbody is used as a reference, necessitating a modest color correction factor at 24 microns.  Calculation of the color correction factor CC for MIPS 24 starts with computing the effective wavelength:

λ eff   =  ∫ Rλ  dλ   /    ∫ λ-1  Rλ  dλ     =    23.6749 micron

νeff    =  c  / λ eff   =    1.2663e+13  Hz

BB(νeff)  =  BB(1.2663e+13)  =  4.7694e-7

Then the uncalibrated flux from the blackbody spectrum is computed:

uncalibrated_flux_bb =  ∫ BB(ν) ν Rν dν   /    ∫ ν Rν dν  = 4.9275e-7

Finally,  we get the color correction factor by dividing into blackbody flux density at the effective wavelength:

CC  =  BB(νeff)  / uncalibrated_flux_bb  =  0. 9679

The uncertainty adjustment factors are discussed in more detail in Section 9.3.2.