================================================================================
Title: A high resolution, multi-epoch spectral atlas of peculiar stars 
       including RAVE, GAIA and HERMES wavelength ranges  
Authors: Tomasella L., Munari U., Zwitter T.
================================================================================
Description of contents: This tar package contains 4 directories, named 
  PECULIARS, FLAT, STANDARD, TELLURIC.  The 425 scientific spectra (listed in 
  Table 2) of 108 well-known objects representative of the most common types of
  peculiar and variable stars presented in the atlas, are collected as FITS 
  files into PECULIARS directory. Each individual spectrum cover the spectral 
  range 4600-9400 Ang. (25 Echelle orders).  The majority of the program stars 
  were observed at more than one observing epoch.  In addition to stellar 
  spectra, we provide also other products. Flat field tracings are collected in
  FLAT directory. The flats are named using the same root name as the 
  corresponding stellar spectrum (for ex.  AFDra_1.fits is the stellar 
  spectrum, and flat_AFDra_1.fits is the corresponding flat).  The 
  spectro-photometric standards (listed in Table 3) and telluric dividers 
  (listed in Table 4) are collected in STANDARD and in TELLURIC directory, 
  respectively. 

System requirements: The FITS files can be visualized using IRAF or others 
  reduction packages.

Additional comments: Each final spectrum presented in this atlas was built 
  starting from several (at least three) individual exposures obtained 
  consecutively at the telescope.  Each individual exposure was extracted, 
  reduced and calibrated separately, before summing them into the final 
  spectrum. Before merging, the resulting individual spectra were carefully 
  compared order by order to spot and remove the presence of cosmic rays or 
  other   defects.  We restrained from doing this automatically during data 
  reduction, principally to avoid potential problems with very sharp emission 
  lines and to keep a strict control over the whole data reduction process.
  Cool objects could have their reddest Echelle orders saturated while the
  blue part of the spectrum would remain under-exposed. In such cases we
  obtained consecutive observations with varying exposure times. The final   
  spectrum was obtained by combining the best exposures of individual
  Echelle orders and scaling their counts to a uniform exposure time.
  Multiple exposures with varying exposure time were also used for objects 
  with bright emission lines that saturated the deep exposures. Shorter
  exposures were used to recover the unsaturated emission line profiles,   
  usually those of the H{alpha} line.

================================================================================