param_description.txt

#detailed explanation of all parameters in param file

target: name of target source; string

obsDate: observation date to distinguish between different epochs of the same source; string

refFrequency: frequency band of observations; string

intervalSizeX: time bin size, H is hours (integer), M is minutes (integer), S is seconds (integer or float)

interval_set: instead of specifying an HMS for teh timebin, you can select 'int' (integration time),'scan' (scan timescale), or 'full' (full observation); string

visibility: path to CASA MS; string

imageSize: image size in pixels; integer

numberIters: max number iterations in clean; integer, default is 5000

cellSize: cell size in arcseconds; string, 'XXarcsec'

taylorTerms: number of taylor terms to use; integer, default is 1

decon: deconvolver for tclean to use; string, hogbom if nterms=1, mtmfs if nterms>1

myStokes: stokes parameter; string, default is 'I'

thre: cleaning threshold; string, default is '1mJy'

spw_choice: spectral window selection, string

robust: Briggs robust parameter; integer, set when weighting='briggs', range from -2[uniform] to 2[natural], default is 0.0

weighting: Image weighting, string; options are 'natural', 'uniform', or 'briggs'

mask_option: specify choice of clean mask; string, options are 'box' (just targetBox around source), 'file' (provide own
mask file specified in mask_file parameter), or 'aegean' (box around all detected sources from Aegean script if run)

mask_file: path to mask file if mask_option='file'; string

var_anal: toggle to do variability analysis; string, options are 'T' or 'F'

power_spec: toggle to make power spectra; string, options are 'T' or 'F'

seed: seed threashold (i.e., peak pixels) for aegean in sigmas; integer, default is 5

flood: flood threashold (i.e., surrounding pixels) for aegean in sigmas; integer, default is 4

tele: telescope for latutude determination by aegean; string, default is 'VLA'

lat: only set if not on list (VLA, SMA, NOEMA) in scope2lat func of aegean.py; string

runObj: toggle to run object detection; string, options are 'T' or 'F'; **hard coded to 'F'

targetBox: target box in pixels, only set if not doing object detection or mask_option='box'; string ('X1,Y1,X2,Y2')

outlierFile: provide path to outlier file for clean if needed; string
(see example_outlier_file.txt for example).

runClean: toggle to run clean, if off can refit a data set provided images were saved (if saved images a cutout 
then fit_cutout must be 'T'); string, options are 'T' or 'F' or 'U' (only uv plane); **hard coded to 'T'

fix_pos: toggle to fix position in individual images to that of whole data set fit; string, options are 'T' or 'F'

do_monte: toggle to monte carlo sample position of full data set if fix_pos='T'; string, options are 'T' or 'F'

integ_fit: toggle to write both integrated and peak flux to data file; string, options are 'B' (both), 'T' (integrated only),
'F' (peak only), default is 'B';

uv_fit: toggle to do uv plane fitting; string, options are 'T' or 'F'

uv_fix: toggle to fix position in uv fitting from position of whole data set; string, options are 'T' or 'F'

uv_initp: if doing uv fitting, provide the path to the intial guess file for uv fitting; string
Format of this file is a row for each point source, with ra offset from phase center (arcsec),
dec offset from phase center (arcsec), and flux (Jy) on each row. Target MUST be first source in file
(see uv_init_example.txt for example).

def_times: toggle to manually define start and end times (next 6 params), default is start and end of observation; string,
options are 'T' or 'F'

startTimeX: manual start time in format integer hour, minute, second; string, only set if def_times='T'

endTimeX: manual end time in format integer hour, minute, second; string, only set if def_times='T'

startX: manual start date in format integer day, month, year; string, only set if def_times='T'

endX: manual end date in format integer day, month, year; string, only set if def_times='T'

lc_scale_unit: unit for lightcurve flux density; string, options are '' (Jy), 'm' (mJy), 'u' (microJy), default is 'm'

lc_scale_time: unit for lightcurve time; string, options are 'H' (hours), 'M' (minutes), 'S' (seconds), default is 'M'

image_view: Do you want to interactively scan through the time bin images at end of script; string, options are 'T' of 'F'

im_shift_time: if imag_view set to 'T', this is the time interval in seconds between images in the viewer; integer