CU6
Development Cycle 2

Here is a short explanation on how the data available below have been obtained. A more detailed explanation is included in the note: GAIA-C6-TN-OPM-PS-002.pdf.

The data are produced using the CU2 GaiaSimulator. The originals are spectra of dwarf stars computed using the Kurucz model. The source original spectra are included in each tar file in a directory named "original". Each spectrum is simulated with 3 to 5 different magnitudes. The absorption is set to 0 for all (Av=0). The spectra are for a single CCD (no transit spectra-combination is done).

The instrument effects included are:
- The response curve computed using the GaiaParamDataBase values for the mirrors and the CCD-QE (red variant of CCD91-72 from e2v technologies) the RVS curve is not in database and is implemented as a simple rectangular function.
- The dispersion is assumed to be constant (independent on wave and on focal plane position).
- The PSF is modelled as a gaussian (FWHM = 860.5/11500 nm)
- The background, poisson noise, dark and total detection noise are included.
- The sampling scheme is: samples = 3x10 pix for V>11 (total of 368 samples), sample=1x10 pixels for V<11 (total 1104 samples).
In addition, a template spectrum without any noise added is also computed for each spectral type and each magnitude.

The format of the files is ASCII. The files have 2 columns: the first column contains the wavelength corresponding to the middle of the sample, the second column contains the total number of photons per sample.
There is one file per spectrum and the filename contains the informations on the source spectral type and magnitude: (eg: for RVS_K0V_magV1350_250.txt, the spectral type is K0V, the magnitude V=13.50 and the spectrum number is 250).

Any feedback about the data is welcome.