- modify the configuration file drslib/config.py in order to set the
right directory path for raw and reduced files (CONFIG['BASE_RAW']
and CONFIG['BASE_RED_DIR'])
- run "python gofioDRS.py -h" for help
Output:
- intermediate: *_str.fits, 2D images with orders straightened and bad pixel removed
- final output: *_ms1d.fits. The spectra are flat-fielded, extracted, calibrated, and the cosmic rays are removed. The echelle orders are not merged. The FITS table has 50 rows and 4 columns, and it stores each echelle order in a row. The columns are: the number of the echelle order (from 32 - the reddest - to 81 - the bluest), the wavelength in nanometers, the fluxes and the signal-to-noise ratios.
- final output (optional): *_s1d.fits. The spectra are flat-fielded, extracted, calibrated, and the cosmic rays are removed. The echelle orders are merged. The barycentric correction is applied. These are monodimensional spectra with constant step in wavelength.
- intermediate: *_str.fits, 2D images with orders straightened
and bad pixel removed
- final output: *_ms1d.fits. The spectra are flat-fielded, extracted,
calibrated, and the cosmic rays are removed.
The echelle orders are not merged.
The FITS table has 50 rows and 4 columns, and it stores each echelle
order in a row. The columns are: the number of the echelle order
(from 32 - the reddest - to 81 - the bluest), the wavelength in nanometers,
the fluxes and the signal-to-noise ratios.
- final output (optional): *_s1d.fits. The spectra are flat-fielded, extracted,
calibrated, and the cosmic rays are removed. The echelle orders are merged.
The barycentric correction is applied. These are monodimensional spectra with
constant step in wavelength.
The program gofio2ascii.py may be used to convert the outputs from FITS format
to ASCII files. It requires as input a text list with the filepaths of the
#CONFIG['WLCOEFFS'] = {'k1':(' '.join((CONFIG['KEY_DRS'],'CAL K1')),'k1 coefficient of the calibration function'),'k2':(' '.join((CONFIG['KEY_DRS'],'CAL K2')),'k2 coefficient of the calibration function'),'k3':(' '.join((CONFIG['KEY_DRS'],'CAL K3')),'k3 coefficient of the calibration function'),'l0':(' '.join((CONFIG['KEY_DRS'],'CAL L0')),'l0 coefficient of the calibration function'),'xc':(' '.join((CONFIG['KEY_DRS'],'CAL XC')),'xc coefficient of the calibration function'),'rms':(' '.join((CONFIG['KEY_DRS'],'CAL RMSE')),'[m/s] RMS error of the calibration')}
CONFIG['USE_FLAT']={'global':False,'order':True,'nor':False}# global: flat normalized by global mean value - order: flat normalized order by order by mean value - nor: flat normalized row by row by continuum fitting, removing the blaze function - No True value: no flat division
CONFIG['FLAT_EXPT']=100.0
CONFIG['WLCAL_EXPT']=100.0
CONFIG['FP_EXPT']=60.0
CONFIG['DARKLIST']={10:[],30:[],60:[],100:[],200:[],300:[],600:[]}# exptime dei dark
CONFIG['NDARK']=len(CONFIG['DARKLIST'])# quanti tipi di dark (esempio: 10,30,60,100 sec = 4) meglio sovrastimare
CONFIG['WEXT']=5# extraction half-window for wavelength calibration, it will extract 2*wext around the center of the order
CONFIG['WEXT']=10# extraction half-window for wavelength calibration, it will extract 2*wext around the center of the order
#
# CCD info
# Detector info
#
CONFIG['RON']=5.0# electrons
...
...
@@ -266,6 +263,7 @@ CONFIG['XCCD'] = 2048
CONFIG['YCCD']=2048
CONFIG['N_ORD']=50# number of echelle orders
CONFIG['W_ORD']=41# width of straighten order in pixel
CONFIG['SHIFT_Y']=20# expected bottom position of flat signal on the lowest order and the left side of the detector. DO NOT CHANGE.
