1.1.1 (2010.04.21; Revision 182)
  o Corrected a problem that has affected all optimally extracted soectra of
    all revisions and releases so far. The problem has been that it has been
    necessary to apply a 0.5pixel offset to the profile spectrum positions
    before the spectrum extraction. Previously this offset was applied in an
    improper way which has not solved the problem. From now on all profile
    positions are offset by 0.5 pixel before the data is saved to the *_cdlp*
    file. In order to achieve a better accuracy in you extracted spectra it is
    necessary to either recalculate the profiles or apply the 0.5 pixel offset
    by hand, before extracting the spectra anew. If you want to know more about
    how important it is with accurate profile center positions for the accuracy
    of your extracted spectra please have a look in Sections 4.1 and 4.4 in
    the p3d paper.
    Note! Most instruments are affected by flexure, which has the potential to
    cause an additional offset between the profiles calculated using a
    continuum or sky flat exposure and the object exposure. p3d does not -yet-
    correct for such offsets (although support might be added soon).
  o The image viewer p3d_imv now also looks for raw data in the directory of
    the main input file (FILENAME) and in the parent directory of FILENAME.
    This makes it easier to inspect the data if the reductions are carried out
    on one machine, and are thereafter transferred to another computer (where
    the path is different).

1.1 (2010.04.16; Revision 162) - Upperkuchen
  o Much improved support for use with the PMAS 4kx4k CCD.
  o Implemented a much more strict checking of the available parameters in the
    instrument keywords file(s).
  o Included support for flipping the raw data on the dispersion axis. The
    flipping is performed when the DFLIP parameter is set (either in the
    instrument parameter file or in the user parameter ditto).
  o File suffixes, and the string that is used with combined images, can now be
    set in the user parameter file.
  o All parameters in the master user parameter file
    (data/master_userparfile.dat) are now fully described.
  o Added transparent support for gzip-compressed input data files.
    Z-compressed files (which were compressed using the UN*X-command compress)
    and bzip2-compressed files are also supported on UN*X platforms - see the
    READFITS routine of astro-lib for more information. Output data files are
    compressed using gzip (all platforms!) if the user parameter compress is
    set to yes (default==no).
  o All references to PASP have been changed to A&A, which is where the paper
    on p3d is published (yes, we changed our mind).
  o Updated PPAK tracing parameters to work more generally.
  o Document headers have been adjusted to work better with the IDL->html
    translation tools of O. Streicher.
  o Fixed numerous smaller bugs.

  o GUI
    - Added several different filters in the file dialogs, supporting
      compressed files as well as non-compressed ones.
    - Only the first-block files of multi-block instruments are now shown by
      default in the file dialogs.
    - The default width of file dialogs is now set to 500px when using the VM
      (see the Xdefaults file in vm/).

  o Image combination
    - All image-combination-related operations have been moved to a separate
      routine (routines/p3d_misc_imcombine_wrapper.pro) to comply with the
      "Don't Repeat Yourself" coding principle.
    - Added a slow combination method since the fast MIN() function of IDL
      gives strange results (with PMAS at least). This slow method is now also
      the default.

  o Spectrum extraction
    - The optimal extraction routines MOX and MPD have been moved to their own
      routines.
    - The default extraction method for MPD is now 'banddiagonal' and not 'svd'
      as previously ('svd' is painfully slow).
    - Information about what is going on is now also printed on the console
      when verbose==1.

  o Master Bias
    - It is now possible to pick only one file and then let p3d smooth it
      before it is used as a master bias. This now also works with the
      PMAS 4kx4k CCD.

  o Wavelength calibration / Dispersion Mask creation
    - Now works properly with two input files for all supported instruments.
      Two files (ideally of different exposure time) can be used if arc lines
      on one side of the detector are much fainter/brighter than on the other
      side.
    - After entries in the line list were matched with the data a more precise
      Gaussian fitting (or weighting) was previously performed in the
      "Create dispersion mask" step. In order to allow a checking of the more
      precise fitting this fitting has now been given its own function in the
      GUI ("Fit centroids"). This function (button) must now be used after the
      "Match centroids" step, and before the "Create dispersion mask" step.
    - The default behavior for p3d is now to not rebin the data on the
      dispersion axis before starting the GUI. This allows big data sets to be
      used on very small screens (DBIN=1). If the user still wants to have the
      data rebinned then she/he can select another mode in the Options menu,
      or simply set the DBIN parameter in the user parameter file.

  o Object extraction
    - Now accepts a cosmic ray mask (although this method does not work well at
      all).
    - p3d can now also save output spectra in the E3D-format (finally; as we
      have promised in the paper on p3d).


1.0 (2010.02.02; Revision 30) - Destiny
  o Initial version.
