SMOOTH Type: Adverb (REAL(3)) Use: SMOOTH specifies the type of spectral smoothing to be applied to a uv database or other spectra. The default is not to apply any smoothing. The elements of SMOOTH are as follows: SMOOTH(1) = type of smoothing to apply: 0 => no smoothing 1 => Hanning applied before bandpass calibration 2 => Gaussian applied before bandpass calibration 3 => Boxcar applied before bandpass calibration 4 => Sinc (i.e. sin(x)/x) applied before bandpass cal. 5 => Hanning applied after bandpass calibration 6 => Gaussian applied after bandpass calibration 7 => Boxcar applied after bandpass calibration 8 => Sinc (i.e. sin(x)/x) applied after bandpass cal. SMOOTH(2) = the "diameter" of the function, i.e. width between first nulls of Hanning triangle and sinc function, FWHM of Gaussian, width of Boxcar. Defaults (if < 0.1) are 4, 2, 2 and 3 channels for SMOOTH(1) = 1 - 4. SMOOTH(3) = the diameter over which the convolving function has value - in channels. Defaults: 1, 3, 1, 4 times SMOOTH(2) used when input SMOOTH(3) < net SMOOTH(2). When applied to uv data, it is important to decide whether the smoothing should be applied before or after application of the bandpass calibration. If SMOOTH was used in BPASS (or CPASS), then the same SMOOTH must be used with all the data (and SMOOTH(1) must be 1 through 4). If SMOOTH was not used in BPASS, then SMOOTH(1) must be 5 - 8 for correct results. Null Value: 0 A null value of SMOOTH(1) means no smoothing is desired; the useage of null values for other parameters depend on the application. The usual defaults are listed above. Symmetry: Hanning, Gaussian, and Sinc functions are always symmetric. Boxcar allows only integer widths and has value 1.0 in all included channels. If the integer is odd, the function is symmetric. If it is even, the function is asymmetric having one more channel included to the "right". Thus width 2 averages channels 1 and 2 in output channel 1. Width 4 averages channels 1 through 4 in output channel 2. The frequency reference pixel is suitably adjusted in such cases. This is a change from symmetric boxcars made in March 2021. Discussion: Frequency smoothing of UV data interacts with data flagging in ways that are not entirely intuitive. In fact, it is strongly recommended that any data smoothing to be applied before the bandpass be done, once and for all (with e.g. SPLAT), before any channel-dependent flagging is done. Data with RFI frequently requires a Hanning smooth up front to reduce ringing. Do this with SPLAT once and for all eraly in your data reduction. Post bandpass smoothing also interacts with flags and the computatin of Stokes parameters. A SMOOTH of, e.g. 6,0,0 functions as follows: 1. Smooth each polarization separately ignoring flagged channels and maintaining the flagging. 2. Combine polarizations to make the Stokes parameters. This can be particularly odd with Stokes I - which is taken to be (RR+LL)/2 unless one of RR and LL is flagged, in which case the other is taken. Thus smooth values of RR and LL are averaged but isolated channels of only RR or LL also appear. These isolated channels will have smoothed values appropriate to RR or to LL but not to the average unless RR and LL are nearly identical. Thus single channels will stick out from the otherwise smooth spectrum. Even with Stokes F (formal I), Q, U, and V, odd results may arise. Flagging of one of the two observed polarizations for these parameters leads to flagging of the result at the particular flagged channel. But, if one of e.g. RL and LR is not flagged, then those unflagged values will affect the adjacent channels in the smoothing that preceeds the Stokes computation. Thus, at a good channel, the results will be different from the results if all polarizations rather than just 1 are flagged at the flagged channels. POSSM has a special option where the spectra are averaged with no smoothing and then smoothed just before displaying them. In this way, most of the complications described above are avoided. Procedures: LINIMAGE......Build image cube from multi-IF data set. Tasks: ACFIT.........Determine antenna gains from autocorrelations. ACIMG.........Makes image of autocorrelation data showing time vs frequency ACLIP.........Edits suto-corr data for amplitudes, phases, and weights out of range. ACSCL.........Corrects cross amplitudes using auto correlation measurements. ALVAR.........Plots the Allan Variance statistic of a UV data set. ALVPR.........Prints statistics on the Allan Variance of a UV data set. ANBPL.........Plots and prints uv data converted to antenna based values. AVSPC.........Averages uv-data in the frequency domain. BLCAL.........Compute closure offset corrections. BLCHN.........Compute closure offset corrections on a channel-by-channel basis. BLING.........Find residual rate and delay on individual baselines. BPASS.........Computes spectral bandpass correction table. BPWAY.........Determines channel-dependent relative weights. BPWGT.........Calibrates data and scales weights by bandpass correction. BSCAN.........Seeks best scan to use for phase cal, fringe search, .. CALIB.........Determines antenna calibration: complex gain. CAPLT.........Plots closure amplitude and model from CC file. CLIP..........Edits data based on amplitudes, phases, and weights out of range. CLPLT.........Plots closure phase and model from CC file. CORER.........Calculates correlator statistics and flags bad ones. CPASS.........Computes polynomial spectral bandpass correction table. DECOR.........Measures the decorrelation between channels and IF of uv data. DEFLG.........Edits data based on decorrelation over channels and time. DFTIM.........Makes image of DFT at arbitrary point showing time vs frequency. DFTPL.........Plots DFT of a UV data set at arbitrary point versus time. DIFRL.........Divides the RR data by LL data. EDITR.........Interactive baseline-oriented visibility editor using the TV. EVAUV.........Subtracts & divides a model into UV data, does statistics on results. FGCNT.........Counts samples comparing two flag tables. FGSPW.........Flags bad spectral windows. FINDR.........Find normal values for a uv data set. FLAGR.........Edit data based on internal RMS, amplitudes, weights. FLGIT.........Flags data based on the rms of the spectrum. FLOPM.........Reverses the spectral order of UV data, can fix VLA error. FRING.........Fringe fit data to determine antenna calibration, delay, rate. FRMAP.........Task to build a map using fringe rate spectra. FRPLT.........Task to plot fringe rate spectra. FTFLG.........Interactive flagging of UV data in channel-time using the TV. FUDGE.........Modifies UV data with user's algorithm: paraform task. IBLED.........Interactive BaseLine based visibility EDitor. IMAGR.........Wide-field and/or wide-frequency Cleaning / imaging task. ISPEC.........Plots and prints spectrum of region of a cube. KRING.........Fringe fit data to determine antenna calibration, delay, rate. LISTR.........Prints contents of UV data sets and assoc. calibration tables. LPCAL.........Determines instrumental polarization for UV data. MAPBM.........Map VLA beam polarization. NOIFS.........Makes all IFs into single spectrum. OMFIT.........Fits sources and, optionally, a self-cal model to uv data. PCAL..........Determines instrumental polarization for UV data. PHSRF.........Perform phase-referencing within a spectral line database. PLRFI.........Plots spectral statistics from output of VBRFI POSSM.........Task to plot total and cross-power spectra. REWAY.........Computes weights based in rms in spectra. RFI...........Look for RFI in uv data. RFLAG.........Flags data set based on time and freq rms in fringe visibilities. RIRMS.........Computes rms of real/imag of a selected subset of a uv data set RLCAL.........Determines instrumental right-left phase versus time (a self-cal). RLDIF.........Determines Right minus Left phase difference, corrects cal files. RLDLY.........Fringe fit data to determine antenna R-L delay difference. RSPEC.........Plots and prints spectrum of rms of a cube. SCIMG.........Full-featured imaging plus self-calibration loop with editing. SCMAP.........Imaging plus self-calibration loop with editing. SHOUV.........Displays uv data in various ways. SPCAL.........Determines instrumental polzn. for spec. line UV data. SPFLG.........Interactive flagging of UV data in channel-TB using the TV. SPLAT.........Applies calibration and splits or assemble selected sources. SPLIT.........Converts multi-source to single-source UV files w calibration. SPMOD.........Modify UV database by adding a model with spectral lines. SPRMS.........Plots spectral statistics of a selected subset of a uv data set. SUFIX.........Modifies source numbers on uv data. TI2HA.........Modifies times in UV data to hour angles. TIORD.........Checks data for time baseline ordering, displays failures. TRUEP.........Determines true antenna polarization from special data sets. TVFLG.........Interactive flagging of UV data using the TV. UFLAG.........Plots and edits data using a uv-plane grid and the TV. UV2MS.........Append single-source file to multi-source file. UV2TB.........Converts UV autocorrelation spectra to tables. UVAVG.........Average or merge a sorted (BT, TB) uv database. UVBAS.........Averages several channels and subtracts from uv data. UVFIT.........Fits source models to uv data. UVFND.........Prints selected data from UV data set to search for problems. UVFRE.........Makes one data set have the spectral structure of another. UVGIT.........Fits source models to uv data. UVHGM.........Plots statistics of uv data files as histogram. UVHIM.........Makes image of the histogram on two user-chosen axes. UVHOL.........Prints holography data from a UV data base with calibration. UVIMG.........Grid UV data into an "image". UVLIN.........Fits and removes continuum visibility spectrum, also can flag. UVLSD.........Least squares fit to channels and divides the uv data. UVLSF.........Least squares fit to channels and subtracts from uv data. UVMLN.........Edits data based on the rms of the spectrum. UVMOD.........Modify UV database by adding a model incl spectral index. UVMTH......... Averages one data set and applied it to another. UVPLT.........Plots data from a UV data base in multiple ways. UVPRM.........Measures parameters from a UV data base. UVPRT.........Prints data from a UV data base with calibration. UVRFI.........Mitigate RFI by Fourier transform or fitting the circle. UVRMS.........Computes statistics of a selected subset of a uv data set. VPLOT.........Plots uv data and model from CC file. WETHR.........Plots selected contents of WX tables, flags data based on WX. WIPER.........Plots and edits data from a UV data base using the TV. XYDIF.........Find/apply X minus Y linear polarization phase difference. XYMOD.........Compute linear polarization point source model, applies to data.