Explanatory text going with the ESO NIR data, both broad band and narrow band data.
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Effective wavelengths, FWHM, zero magnitude fluxes:

     filter  lambda eff      FWHM    Flam,0
	     micron          micron  W m-2 nm-1
     
     J       1.210           0.190   3.44 e-12
     H       1.635           0.269   1.21 e-12
     K       2.197           0.360   4.12 e-13
     L'      3.740           0.580   5.58 e-14
     M       4.759           0.381   2.21 e-14
     
     H0      1.577           0.031   1.36 e-12
     Br      2.161           0.037   4.27 e-13
     K0      2.220           0.038   3.97 e-13
     CO      2.290           0.039   3.54 e-13
     L0      3.706           0.050   5.78 e-14

This calibration is based on the work by Menessier (1995, A&A296, 771).
Because this calibration is an approximation of the zero magnitude flux
using a black body, we have corrected the zero magnitude fluxes of the H0 
and Br filter for the presence of HI absorption lines in the spectra of 
A type stars.


The zero points of the magnitude scale are defined by assuming that

       J(HR3314) - J(Vega) = 3.913
       H(HR3314) - H(Vega) = 3.914
       K(HR3314) - K(Vega) = 3.919

Furthermore we assumed that the (K - L) and (K - M) of HR3314 are 0.

This results in the following magnitudes for HR3314:

       J  = 3.93
       H  = 3.93
       K  = 3.94
       L  = 3.94
       M  = 3.94
       H0 = 3.93
       Br = 3.94
       K0 = 3.94
       CO = 3.94
       L0 = 3.94

A detailed description of this work can be found in van der
Bliek, Manfroid & Bouchet (1996, A&AS 119, 547).


About the filter transmission curves:

Filter transmission curves are available in these web pages. The
transmission curves also include the detector response. 

Nicole van der Bliek
22 Feb 1996