sdfitold – ASAP SD task [DEPRECATED]: Fit a spectral line – single dish task

Description

### DEPRECATION WARNING ################################################# This task will be removed in CASA 5.1. The functionality of this task with MeasurementSet format is replicated with sdfit. #########################################################################

Task sdfitold is a basic line-fitter for single-dish spectra. It assumes that the spectra have been calibrated in sdcal or sdreduce.

Parameters

Title
Parameter	Default	Description
infile	`''`
antenna	`int(0)`
fluxunit	`''`	units of the flux ['K' or 'Jy'] (''=current)
telescopeparam	`''`
field	`''`
spw	`''`
restfreq	`''`
frame	`''`	frequency reference frame ['LSRK', 'TOPO', 'LSRD', 'BARY', 'GALACTO', 'LGROUP', or 'CMB'] (''=current)
doppler	`''`	doppler convention ['RADIO', 'OPTICAL', 'Z', 'BETA', or 'GAMMA'] (''=current).
scan	`''`
pol	`''`
timeaverage	`False`	average spectra over time [True, False] (see examples in help)
tweight	`'tintsys'`	weighting for time averaging ['tintsys', 'tsys', 'tint', 'var', or 'median']
scanaverage	`False`	average spectra within a scan number [True, False] (see examples in help)
polaverage	`False`	average spectra over polarizations [True, False]
pweight	`'tsys'`	weighting for polarization averaging ['tsys' or 'var']
fitfunc	`'gauss'`	function for fitting ['gauss', 'lorentz']
fitmode	`'auto'`	mode for fitting ['auto', 'list', or 'interact']
nfit	`numpy.array( [ ] )`
thresh	`float(5.0)`
min_nchan	`int(3)`
avg_limit	`int(4)`
box_size	`float(0.2)`
edge	`numpy.array( [ int(0) ] )`
outfile	`''`
overwrite	`False`	overwrite the output file if already exists [True, False]
plotlevel	`int(0)`
xstat	`[ ]`

Parameter Explanations

infile

''

name of input SD dataset

antenna

int(0)

select an antenna name or ID, e.g. 'PM03' (only effective for MS input)

fluxunit

''

units of the flux (''=current)

telescopeparam

''

parameters of telescope for flux conversion (see examples in help)

field

''

select data by field IDs and names, e.g. '3C2*' (''=all)

spw

''

select data by IF IDs (spectral windows), e.g. '3,5,7' (''=all)

restfreq

''

the rest frequency, e.g. '1.41GHz' (default unit: Hz) (see examples in help)

frame

''

frequency reference frame (''=current)

doppler

''

doppler convention (''=current). Effective only when spw selection is in velocity unit.

scan

''

select data by scan numbers, e.g. '21~23' (''=all)

pol

''

select data by polarization IDs, e.g. '0,1' (''=all)

timeaverage

False

average spectra over time (see examples in help)

tweight

'tintsys'

weighting for time averaging

scanaverage

False

average spectra within a scan number (see examples in help)

polaverage

False

average spectra over polarizations

pweight

'tsys'

weighting for polarization averaging

fitfunc

'gauss'

function for fitting

fitmode

'auto'

mode for fitting

nfit

numpy.array( [ ] )

list of number of gaussian/lorentzian lines to fit in in maskline region (ignored when fitmode=”auto”)

thresh

float(5.0)

S/N threshold for linefinder

min_nchan

int(3)

minimum number of consecutive channels for linefinder

avg_limit

int(4)

channel averaging for broad lines

box_size

float(0.2)

running mean box size

edge

numpy.array( [ int(0) ] )

channels to drop at beginning and end of spectrum

outfile

''

name of output file (See a WARNING in help)

overwrite

False

overwrite the output file if already exists

plotlevel

int(0)

control for plotting of results (see examples in help)

xstat

[ ]

RETURN ONLY: a Python dictionary of line statistics