============================================================================
OBSERVED SPECTRUM OF ALPHA1 CENTAURI
Assembled 12-5-95.

Alp1 Cen photometry file: photometry actually used to construct the spectrum

 Name      FWHM    Mag.+/-Unc.   Eff Wvl   Eff Wvl    F-lam    Source
			         (Vega)    (star)    W/cm2/um
                                  (um)      (um)
 SAAO-L   0.5648  -1.559 0.015   3.475     3.450     3.00E-14  Carter 1994
 ESO-L    0.6509  -1.552 0.021   3.768     3.768     2.18E-14  Engels+ 1981
 ESO-M    0.5418  -1.437 0.028   4.748     4.759     7.95E-15  Engels+ 1981
 ESO-N1   0.8954  -1.557 0.023   8.394     8.394     9.68E-16  Bouchet+ 1989
 ESO-N2   1.2949  -1.553 0.026   9.886     9.853     5.06E-16  Bouchet+ 1989


 Spectral fragments and portions of these actually used in observed spectrum
 ("used" may include combination with other data where overlaps occur)

 Fragment   Reference    Total range    Start and stop    Average resolving
                            (um)       wavelengths (um)        power

 KAO-NIR        1         3.04- 5.53       3.04- 5.53           160
 KAO-5--9       2         5.07- 9.28       5.07- 9.28           190
 KAO-8--13      3         8.80-13.07          .....             250
 LRS            4         7.67-22.74       7.67-11.55            30
 KAO-Si:Bi      5        15.00-18.51          .....              80
 KAO-Si:P       6        19.48-27.20          .....             180
 LONG           7         1.25-35.00      12.20-35.00            --

 References:
 1,5,6. HIFOGS data of April 10 & 12, 1993 KAO flights [alp1 Cen/alp CMa].
 2,3. HIFOGS data of April 7, 1993 KAO flight [alp1 Cen/alp CMa].  Spectral
   ratios in both these wavelength ranges are additionally confirmed
   by HIFOGS data of July 22, 1994 KAO flight from Australia.
 4. LRS raw data extracted from "LRSVAX" Groningen archive at NASA-Ames.
 7. Engelke Fn. used for T=5770K and ang. diam. of 8.66 mas [see Lydon et
   al. (1993) and Demarque et al. (1986)]; we rescaled this to 8.59 mas.  This
   Engelke Function was locked to the photometrically scaled LRS spectrum by
   splicing and used to replace the observations from 12.20 um.  An error of
   2.0% in EFn. due to effective temperature uncertainty was input for this
   fragment.


 INFORMATION ON SPLICES AND BIASES INCURRED

 Process                   Factor determined      +/-Bias (%)

 NIR cf. photometry            0.796                 1.31
 LRS blue/red bias               --                  0.09
 LRS cf. photometry            0.778                 2.07
 5--9 joint splice to            --
 NIR and LRS                   0.995                 0.16
 Engelke Fn. splice to LRS     0.989                 0.38

============================================================================
 Notes:
 1. Composite spectra are NOT tabulated at equal intervals of the wavelength,
    but rather at the wavelengths of the original model.
 2. In most cases "total uncertainty" is the error term most appropriate to
    use. It is the standard deviation of the spectral irradiance and includes
    the local and global biases.  Local and global biases are given as a
    percent of the irradiance.  The global bias does not contribute error to
    flux ratios or color measurements, and may, in those cases, be removed (in
    the RSS sense) from the total error.
============================================================================