autoreduce

pydis.autoreduce(speclist, flatlist='', biaslist='', HeNeAr_file='', stdstar='', trace_recenter=False, trace_interac=True, trace1=False, ntracesteps=15, airmass_file='apoextinct.dat', flat_mode='spline', flat_order=9, flat_response=True, apwidth=8, skysep=3, skywidth=7, skydeg=0, HeNeAr_prev=False, HeNeAr_interac=True, HeNeAr_tol=20, HeNeAr_order=3, display_HeNeAr=False, std_mode='spline', std_order=12, display_std=False, trim=True, write_reduced=True, display=True, display_final=True, HeNeAr_second_pass=True, silent=True)

A wrapper routine to carry out the full steps of the spectral reduction and calibration. Steps include: 1) combines bias and flat images 2) maps wavelength in the HeNeAr image 3) perform simple image reduction: Data = (Raw - Bias)/Flat 4) trace spectral aperture 5) extract spectrum 6) measure sky along extracted spectrum 7) apply flux calibration 8) write output files

Parameters

specliststr

Path to file containing list of science images.

flatliststr

Path to file containing list of flat images.

biasliststr

Path to file containing list of bias images.

HeNeAr_filestr

Path to the HeNeAr calibration image

stdstarstr

Name of the standard star to use for flux calibration. If nothing is entered for “stdstar”, no flux calibration will be computed. (Default is ‘’). NOTE1: must include the subdir for the star, e.g. ‘spec50cal/feige34’. NOTE2: Assumes the first star in “speclist” is the standard star.

trace1bool, optional

use trace1=True if only perform aperture trace on first object in speclist. Useful if e.g. science targets are faint, and first object is a bright standard star. Note: assumes star placed at same position in spatial direction. (Default is False)

trace_recenterbool, optional

If trace1=True, set this to True to allow for small linear adjustments to the trace (default is False)

trace_interacbool, optional

Set to True if user should interactively select aperture center for each object spectrum. (Default is True)

ntracestepsint, optional

Number of bins in X direction to chop image into. Use fewer bins if ap_trace is having difficulty, such as with faint targets (default here is 25, minimum is 4)

apwidthint, optional

The width along the Y axis of the trace to extract. Note: a fixed width is used along the whole trace. (default here is 3 pixels)

skysepint, optional

The separation in pixels from the aperture to the sky window. (Default is 25)

skywidthint, optional

The width in pixels of the sky windows on either side of the aperture. (Default is 75)

HeNeAr_interacbool, optional

Should the HeNeAr identification be done interactively (manually)? (Default here is False)

HeNeAr_tolint, optional

When in automatic mode, the tolerance in pixel units between linelist entries and estimated wavelengths for the first few lines matched… use carefully. (Default here is 20)

HeNeAr_orderint, optional

The polynomial order to use to interpolate between identified peaks in the HeNeAr (Default is 2)

display_HeNeArbool, optional

std_modestr, optional

Fit mode to use with the flux standard star. Options are ‘spline’ and ‘poly’ (Default is ‘spline’)

std_orderint, optional

The order of polynomial to fit, if std_mode=’poly’. (Default is 12)

display_stdbool, optional

If set, display plots of the flux standard being fit (Default is False)

trimbool, optional

Trim the image using the DATASEC keyword in the header, assuming has format of [0:1024,0:512] (Default is True)

write_reducedbool, optional

Set to True to write output files, including the .spec file with columns (wavelength, flux); the .trace file with columns (X pixel number, Y pixel of trace); .log file with record of settings used in this routine for reduction. (Default is True)

displaybool, optional

Set to True to display intermediate steps along the way. (Default is True)

display_finalbool, optional

Set to False to suppress plotting the final reduced spectrum to the screen. Useful for running in quiet batch mode. (Default is True)