FLOYDS Data Products

Here we describe the data products available to the end user that are available in a tar file. floydsauto is the executable used to perform the automatic reductions at LCOGT headquarters. floydsauto runs every day with a cron job on the last 5 days of observations. For each night, it divides the observations using the PROPID1, reduces the data, and groups them in tar files.

Each tar file will have in the name the Proposal ID, the telescope, the date of observations, and the MJD2 when the reduction was performed. If a standard star was observed the same night, a tar file of automatic reductions for the standard frames will also be produced. The tar file for standard prereduced frames will all start with “STD”, e.g.:


Each tar file will contain the following files:

ESO323G077_offset_fts_20130727_red_2.0_56505_1.fits             (Trimmed raw red part of the science frame)
ESO323G077_offset_fts_20130727_blue_2.0_56505_1.fits            (Trimmed raw blue part of the science frame)
arc_ESO323G077_fts_20130727_red_2.0_56505_1.fits                (Trimmed raw red part of the arc frame)
arc_ESO323G077_fts_20130727_blue_2.0_56505_1.fits               (Trimmed raw blue part of the arc frame)
flatESO323G077_offset_fts_20130727_red_2.0_56505_1.fits         (Trimmed raw red part of the flat frame)
flatESO323G077_offset_fts_20130727_blue_2.0_56505_1.fits        (Trimmed raw blue part of the flat frame)

ttESO323G077_offset_fts_20130727_red_2.0_56505_1.fits           (rectified red part of the science frame)
ttESO323G077_offset_fts_20130727_blue_2.0_56505_1.fits          (rectified blue part of the science frame)
ttarc_ESO323G077_fts_20130727_red_2.0_56505_1.fits              (rectified red part of the arc frame)
ttarc_ESO323G077_fts_20130727_blue_2.0_56505_1.fits             (rectified blue part of the arc frame)
ttflatESO323G077_offset_fts_20130727_blue_2.0_56505_1.fits      (rectified blue part of the flat frame)
ttflatESO323G077_offset_fts_20130727_red_2.0_56505_1.fits       (rectified red part of the flat frame)

nttESO323G077_offset_fts_20130727_red_2.0_56505_1.fits          (flat-field corrected red part of the science frame)

ttESO323G077_offset_fts_20130727_blue_2.0_56505_1_2df.fits      (2D flux calibrated blue frame)
ttESO323G077_offset_fts_20130727_red_2.0_56505_1_2df.fits       (2D flux calibrated red frame)
nttESO323G077_offset_fts_20130727_red_2.0_56505_1_2df.fits      (2D flat-field corrected, flux calibrated red frame)

nttESO323G077_offset_fts_20130727_merge_2.0_56505_1_2df_ex.fits (fast reduction 1D spectrum)

In summary, the extension “2df” indicates a flux calibrated spectrum, the prefix “tt” indicates that the frame has been geometrically transformed along x- and y-axes, “n” indicates that the frame has been flat field corrected. The typical science name is composed (in order) of object name, telescope, observation date, “blue” or “red” (indicating second or first order), slit width, and MJD date when the reduction was performed.

Note that the user may reextract the spectrum from the blue and red 2D wavelength and flux calibrated, rectified images using the IRAF task apall.

The tar file also includes extra files to help the user understand if the observations were performed correctly. It includes a pdf file with the acquisition image and first guiding images, together with some useful plots with information on the guiding and the flux of the guiding star during the full exposure. An example of the summary pdf file is shown in Fig. \ref{fig:summer}.

Filenames are of the form:


  1. PROPID is a unique number that identifies different proposals

  2. The number reported is actually not the MJD, but MJD \(\pm\) 1 day. This number will update at midnight local time in order to remain the same as far as the reducer compute the reduction during day-time and during the same day.