1 ASPROTOFITS
        ASPROTOFITS

    This program converts UVT files in OI‐FITS FITS files for Optical Inter‐
    ferometry.

    2 UVT$
         The input u,v (Aspro format .uvt) file
2 OIFITS$
         The output OITS file name
2 SIMULATENOISE$
        If yes, interferometric observables in the output OI‐FITS file  will
    be distrubted randomly according to the noise. Otherwise, the value will
    be exact.
2 ARRNAME$
        Array Name (for bookeeping)
2 CENTERXYZ$
        Array Center Coordinates
2 ARRAYDESCR$
        Array Description File. A file in the ASPRO distribution  that  con‐
    tains the positions of telescopes of the array.
2 TELDIAM$
        Telescope Diameter (m)
2 INSNAME$
        Instrument  Name  (for  bookeeping). The "NONE" instrument name will
    prevent computing noises and errors.
2 TOTALOBSTIME$
        Total Acquisition time (calibrated, on‐sky) per observed u,v  point,
    in seconds.
2 LAMBDA$
        Observation wavelength, in microns
2 SPECTRALRES$
        Spectral Resolution
2 TRANSMISSION$
        Transmission  of  interferometer+instrument  at observed wavelength,
    real between 0 and 1.
2  DIT$
        Detector Integration Time (seconds)
2 RON$
        Detector Readout Noise (electrons)
2 DETSAT$
        Saturation of the detector (or value for start of non‐linearity), in
    electrons
2 INSVIS$
        Instrumental Visibility [0.0‐1.0].
2 VBIAS$
        The  Visibility  Bias  (percent of V) that is present in the instru‐
    ment´s V2. No error will be below VBIAS*v2, even if the S/N of the  data
    would  compute  otherwise. Used to give conservative values to simulated
    visibilities for a particular instrument.
2 PBIAS$
        The Phase Bias (in degrees) that will be unavoidable in the  instru‐
    ment´s  closures. No phase error will be below PBIAS, even if the S/N of
    the data would compute otherwise. Used to give  conservative  values  to
    simulated closures for a particular instrument.
2 NBPIXINTERF$
        The number of pixels of the camera on which the fringes at one spec‐
    tral resolution element are coded. 4 pixels is the minimum for 1 fringe.
    AMBER  has  32  pixels for 3 fringes. Normally taken a spatial sampling,
    but can be used for temporal coding, in which case it is the  number  of
    pixels  used  times  the  number of temporal samples used to get all the
    fringes.
2 NBPIXPHOTO$
        nb of pixels to code EACH photometry. use 0 if the  instrument  does
    not use simultaneous photometry.
2 FRACFLUXI$
        Fraction of flux in interferometry (fringes) measurements.
2 FTPRESENT$
        Tells  whether a Fringe Tracker is Present. In this case, the FT in‐
    formation will be used to compute the best S/N available given the limi‐
    tations of the FT (integration time, limiting magnitude...)
2 FTINSVIS$
        Fringe Tracker´s (multiplicative) Instrumental Visibility
2 FTLIMIT$
        Fringe  Tracker  cannot be used if the object´s magnitude in FT band
    is gt. this value
2 FTTIMLIMIT$
        Fringe Tracker Max Integration Time (s)
2 OBJECTMAG$
        Object Magnitude in Observing Band
2 AOMAG$
        Object Magnitude in AO´s Band (for AO performances)
2 FTMAG$
        Object Magnitude in Fringe Tracker´s Band of FT ref star
2 SEEING$
        Seeing (arc sec). The program will compute the strehl given  the  AO
    parameters and the seeing, and scale the object´s flux accordingly.
2 NBOFACTUATORS$
        Number of Actuators of AO. A tip‐tilt is 2 actuators.

1 END









































