 
 
 
 
 
 
 
 
 
 
The zero magnitude of a given ISOPHOT filter is defined as the signal of the `ideal' (i.e. model) Vega which would have been measured in that filter with an infinitely large aperture.
 
The ideal spectrum of Vega was derived from a Kurucz model with
   = 9400 K , log(
 = 9400 K , log( ) = 3.900, metal poor,
) = 3.900, metal poor,  0.0 kms
  0.0 kms and no infrared excess due to circumstellar
  dust, extended to 300
 and no infrared excess due to circumstellar
  dust, extended to 300  m and absolutely calibrated as described by
  Cohen et al. 1992, [6],
  and Walker & Cohen 1992, [55].
m and absolutely calibrated as described by
  Cohen et al. 1992, [6],
  and Walker & Cohen 1992, [55].
 
The magnitude  can be obtained from the PHT
  auto analysis data product by applying the relation:
 can be obtained from the PHT
  auto analysis data product by applying the relation:
 
|  | (D.1) | 
 
  where 
 is the AAR flux density.
  The values for
 is the AAR flux density.
  The values for  with filter identifier and
  reference wavelength
 with filter identifier and
  reference wavelength 
 are listed in
  Table D.1.
 are listed in
  Table D.1.
 
For completeness, we have included in Table D.1
  the corresponding powers on the detector 
 ,
  the ideal Vega flux density at the reference wavelength
,
  the ideal Vega flux density at the reference wavelength
  
 , and the colour correction
, and the colour correction  .
.
  
 can be applied to the SPD products, thereby
  taking into account the point spread function correction, see
  Equations 5.8 and 5.9. The
  values of
 can be applied to the SPD products, thereby
  taking into account the point spread function correction, see
  Equations 5.8 and 5.9. The
  values of  are very close to the ones which have been derived for a
  10000 K blackbody, see Table C.2.
 are very close to the ones which have been derived for a
  10000 K blackbody, see Table C.2.
  
| filter |  |  |  |  |  | 
| ID | [  m] | [W] | [Jy] | [Jy] | [ ] | 
| P_3.29 | 3.3 | 4.60E  13 | 312.0 | 318.2 | 0.981 | 
| P_3.6 | 3.6 | 2.15E  12 | 284.7 | 270.9 | 1.051 | 
| P_4.85 | 4.8 | 1.24E  12 | 163.2 | 152.1 | 1.072 | 
| P_7.3 | 7.3 | 1.01E  12 | 79.96 | 71.09 | 1.125 | 
| P_7.7 | 7.7 | 1.61E  13 | 65.14 | 64.23 | 1.014 | 
| P_10 | 10 | 1.77E  13 | 39.40 | 38.60 | 1.021 | 
| P_11.3 | 11.3 | 3.94E  14 | 29.96 | 30.40 | 0.985 | 
| P_12.8 | 12.8 | 5.71E  13 | 35.47 | 26.97 | 1.315 | 
| P_16 | 15 | 1.26E  13 | 24.21 | 23.79 | 1.018 | 
| P_11.5 | 12 | 5.46E  14 | 17.25 | 17.40 | 0.991 | 
| P_20 | 20 | 5.17E  14 | 9.940 | 9.840 | 1.010 | 
| P_25 | 25 | 3.47E  14 | 8.109 | 6.307 | 1.286 | 
| P_60 | 60 | 7.29E  16 | 1.233 | 1.087 | 1.135 | 
| P_100 | 100 | 3.55E  16 | 0.4068 | 0.3866 | 1.052 | 
| C_50 | 65 | 5.76E  16 | 1.197 | 0.9245 | 1.295 | 
| C_60 | 60 | 7.60E  16 | 1.153 | 1.087 | 1.061 | 
| C_70 | 80 | 5.22E  16 | 0.7489 | 0.6075 | 1.233 | 
| C_90 | 90 | 8.45E  16 | 0.5597 | 0.4787 | 1.169 | 
| C_100 | 100 | 4.03E  16 | 0.4261 | 0.3866 | 1.102 | 
| C_105 | 105 | 2.25E  16 | 0.3683 | 0.3503 | 1.052 | 
| C_120 | 120 | 1.15E  16 | 0.3253 | 0.2672 | 1.217 | 
| C_135 | 150 | 1.32E  16 | 0.1862 | 0.1698 | 1.096 | 
| C_160 | 170 | 1.60E  16 | 0.1587 | 0.1316 | 1.205 | 
| C_180 | 180 | 6.92E  17 | 0.1288 | 0.1172 | 1.099 | 
| C_200 | 200 | 2.27E  17 | 0.0972 | 0.0945 | 1.028 | 
 
 
 
 
 
 
 
 
