MIDAS
Procedures and Scripts
for the FIASCO Spectrograph in alphabetical order -
Version 1.1
by C. Guirao
|
| PROCEDURES |
DESCRIPTION
& USAGE
|
| aligning.prg |
Aligns the spectrum of a 2dim image in rows by rotating it. It generates
a set of rotated frames.
| Usage: |
@@
aligning frame.fit |
| |
@@
aligning frame.bdf |
|
| alignment.prg |
Calculates the central row of the spectrum on a 2dim image at three (begin,
middle ane end) positions in the x-axis. Usuful information to calculate
the correct alignment of the spectrum along the rows.
| Usage: |
@@
alignment frame.fit |
| |
@@
alignment frame.bdf |
|
| allblackbodies.prg |
Plots the blackbody spectra at different temperatures (3,4,5,6,7,8,9
at 10K) between 400nm-700nm and all normalized at same value. Labels for
each curve are printed with left mouse button and fixed with the right
mouse button.
|
| averaging.prg |
Calculates a median averaged BDF image out of a set of images FITS or
BDF images. Median average removes cosmic rays.
| Usage: |
@@ averaging dark*.fit
master_dark |
| |
@@
averaging dark*.bdf master_dark |
|
| blackbody.prg |
Plots the blackbody curve at the input temperature in the given wavelength,
and creates a table blackbody_.tbl with FLUX vs. WAVELENGTH
| Usage: |
@@ blackbody T
[wavelength-range] |
|
| compute_fits.prg |
Converts FITS into BDF. At the same time it may fix some CCD problems
like: -Wrong range values, e.g. Hale CCDs -Negative values above a limit,
e.g. Wendelstein -Negative values above a limit, e.g. Wendelstein -Flip
left with right to get Blue_to_Red, e.g. Ponchado -Rotate 90 to get spectrum
in horizontal. Weldenstein -Hot column corrections, e.g. Hale CCD -Bad
columns, e.g. Hale CCD. -Rotating images to align spectra in rows. Default:
only convert FITS into BDF.
| Usage: |
@@ compute_fits
file.fit newfile |
| |
@@ compute_fits
file.fit |
|
| dark_subtraction.prg |
Subtracts dark_current to a BDF or FITS frame.
If input is a FITS frame, bias is also subtracted. The procedure uses a
table called master_dark.tbl that contains a list of master_dark
files at different exposures. It calculates the best master_dark frame based
in median average and scalates it to the same value of the input frame.
The scaled dark frame is subtracted to input framet. The master_dark.tbl
is created with the procedure master_dark.prg.
| Usage: |
@@ dark_subtraction
file.fit output.bdf |
| |
@@ dark_subtraction
file.bdf output.bdf |
|
| displaying.prg |
Opens a display window with the same size of
the input frame. Sets LUT to heat.lut.
| Usage: |
@@
displaying file.bdf |
| |
@@
displaying file.fit |
|
| extracting.prg |
Extracts the spectrum from a 2dim BDF or FITS
frame. If input frame is in FITS format, bias and dark current are also
subtracted. It calculates the central row for the spectrum and with FWHM
above and below that row, extracts the spectrum and generates a 1dimensions
output BDF frame.
| Usage: |
@@
extracting file.fit output.bdf |
| |
@@
extracting file.bdf output.bdf |
|
| identifying.prg |
My attempt to develop an automatic tool to identify
absorption lines in Sun solar spectra by comparing them with table solar.tbl,
a table of the strongest lines and the identified ions. |
| file_ext.prg |
Cannot be used interactively. Used only from
other procedures to separate basename from ex,. e.g. filename
dark.fit is separated in basename=dark and ext=.fit.
| Usage: |
@@
file_ext filename.ext |
|
| flux_calib.prg |
Generates a BDF function master_flux.bdf
as the result of dividing the computed spectra of a spectrophotometric star
with an observed one. Catalogs of spectrophotometric stars are obtained
from Jeremy Walsh's web page at http://www.eso.org/observing/standards/spectra.
The fitting between computed and observed spectrum is done manually.
| Usage: |
@@
flux_calib star.fit star.tbl |
| |
@@
flux_calib star.bdf star.tbl |
|
| ills.dat |
A very long long ASCII table with absorption
lines and their identified ions in the 4500-7000 range. |
| ills.fmt |
Format file to create ills.dat into MIDAS ills.tbl with:
CREATE/TABL ills 2 100
ills.dat ills.fmt
|
| master_dark.prg |
Creates a catalog of master dark
images at different exposures. It also creates a table with the mean average
value for each master dark. The output from this procedure (master_dark.cat
and master_dark.tbl) are used late by dark_subtraction.prg
to calculate the best master dark current appropriate to each spectrum.
| Usage: |
@@
master_dark master_dark*.bdf |
|
| master_flat.prg |
Creates a master flat image master_flat.bdf
by averaging a set of flat images FITS or BDF and normalizing the result
to 1.
| Usage: |
@@
master_flat flats*.fit |
| |
@@
master_flat flats*.bdf |
|
| master_trans.prg |
It creates a function representing the low frequency
modulation of the system. It uses dome flat images, average them, remove
pixel to pixel variations and extract the central row. NOT BEING USED IN
PIPELINE
| Usage: |
@@
master_trans dome_flats*.fit |
|
| pre_pipeline |
This script checks all the calibration data
and files that should be ready for running a successful pipeline. The script
also informs the operator about the procedures required to create the missing
data. |
| pipeline |
Script to run the pipeline in an automatic way.
The script waits in the current directory for new FITS files generated by
the data acquisition system (normally the software of the CCD camera). For
each FITS file, the script launches the MIDAS pipeline. The only requirement
to run the pipeline is to have all the calibration data ready, which is
checked by executing the pre_pipeline script. |
| pipeline.prg |
It extracts and calibrates the spectrum
of a target from a raw 2dim image. The script requires to have ready all
master calibration images: master_bias.bdf for bias subtraction,
master_dark*.bdf for dark current subtraction, master_flat.bdf
for flat field division, session.tbl for wavelength calibration,
master_flux.bdf for relative flux calibration (please, use the shell
script prep_pipeline to check that all the master calibration files
are ready). It generates a FITS file and a postscript file with the fully
calibrated spectrum.
| Usage: |
@@
pipeline frame.fit |
| |
@@
pipeline frame.bdf |
|
| search.prg |
Searches the row central of the
spectrum in a 2dim image FITS or BDF.
| Usage: |
@@
search frame.fit |
| |
@@
search frame.bdf |
|
| solar.dat |
My own table with the strongest absorption lines
and their ions in the Solar spectrum from 4500-7000. Used by procedure identifying.prg
requires to be converted into the MIDAS table solar.tbl with the
command solar.prg. |
| solar.fmt |
Format file used by solar.prg to convert
solar.dat into MIDAS table solar.tbl. |
| solar.prg |
Procedure to convert solar.dat into solar.tbl. |
| solar_corona_plot.prg |
Just a set of plot commands to document a spectrum
like the solar corona obtained at the eclipse 11 August 1999. |
| synthesizing.sh |
Creates a synthetic solar spectrum using the
SPECTRUM and SMOOTH programs from Richard O. Gray. This script is used by
the MIDAS procedure synthesizing.prg.
| Usage: |
$cmd
input output begin_wavelength \ end_wavelength output_resolution step
|
|
| synthesizing.prg |
Plots the synthetic spectrum created
with synthesizing.sh using MIDAS. It uses the script synthesizing.sh
to execute the command spectrum and smooth (these two command
obtained from the installation of the SPECTRUM package).
| Usage: |
@@
synthesizing sun.dat sun.bdf 5500,6500 1.5 0.8 |
|
| wave_calib.prg |
Probably the most useful procedure
ever written for FIASCO. Automatically identifies the emission lines of
a calibration line and generates the wavelength calibration function. You
may need to play a little bit with the input parameters, in particular is
very important you give the wavelength range. By looking to the results
and repeating the procedure you will end with an acceptable calibration
function. It accepts frames in FITS or BDF formats.
| Usage: |
@@
wave_calib hear.fit hear.tbl 5500,6500 8 |
|
| threeblackbodies.prg |
Plots the blackbody spectra of blackbodies at
4700K (Arcturus), 5780 (Sun) and 7000K (Procyon) in the wavelength range
from 300nm to 900nm
| Usage: |
@@
threeblackbodies |
|