13.32 SPECTRAL
Almost all parts of AIPS are general enough to handle mutiple
dimensions of data including multiple frequency channels in the
uv domain and 3 or more dimensional "cubes" in the image domain.
\zxhlp{ACFIT} Determine antenna gains from autocorrelations
\zxhlp{AGAUS} Fits 1-dimensional Gaussians to absorption-line spectra
\zxhlp{ALTDEF} Sets frequency vs velocity relationship into image header
\zxhlp{ALTSWTCH} Switches between frequency and velocity in image header
\zxhlp{AVSPC} Averages uv-data in the frequency domain
\zxhlp{BASRM} Task to remove a spectral baseline from total power spectra
\zxhlp{BCHAN} sets the beginning channel number
\zxhlp{BDAPL} Applies a BD table to another data set
\zxhlp{BLOAT} converts line data to greater number channels
\zxhlp{BLPLT} Plots \zxhlp{BLCAL} tables in 2 dimensions as function of baseline and IF
\zxhlp{BLSUM} sums images over irregular sub-images, displays spectra
\zxhlp{BPASS} computes spectral bandpass correction table
\zxhlp{BPASSPRM} Control adverb array for bandpass calibration
\zxhlp{BPEPL} Plots bandpass tables overlaying multiple times like \zxhlp{BPEDT}
\zxhlp{BPERR} Print and plot \zxhlp{BPASS} closure outputs
\zxhlp{BPLOT} Plots bandpass tables in 2 dimensions as function of time
\zxhlp{BPSMO} Smooths or interpolates bandpass tables to regular times
\zxhlp{BPVER} specifies the version of the bandpass table to be applied
\zxhlp{CHANNEL} sets the spectral channel number
\zxhlp{CHANSEL} Array of start, stop, increment channel numbers to average
\zxhlp{CHINC} the increment between selected channels
\zxhlp{CPASS} computes polynomial spectral bandpass correction table
\zxhlp{CUBIT} Model a galaxy’s density and velocity distribution from full cube
\zxhlp{CVEL} shifts spectral-line UV data to a given velocity
\zxhlp{DCHANSEL} Array of start, stop, increment channel #S + IF to avoid
\zxhlp{DOAPPLY} Flag to indicate whether an operation is applied to the data
\zxhlp{ECHAN} define an end for a range of channel numbers
\zxhlp{FIXAL} least squares fit aliasing function and remove
\zxhlp{FLGIT} flags data based on the rms of the spectrum
\zxhlp{FQUBE} collects n-dimensional images into n+1-dimensional \zxhlp{FREQID} image
\zxhlp{FRMAP} Task to build a map using fringe rate spectra
\zxhlp{FRPLT} Task to plot fringe rate spectra
\zxhlp{FTARS} Fits 1-dimensional polarization spectrum to Q/U text file
\zxhlp{FTFLG} interactive flagging of UV data in channel-time using the TV
\zxhlp{FXALIAS} least squares fit aliasing function and remove
HLPFTFLG Interactive time-channel visibility Editor - run-time help
HLPPCFLG Interactive time-channel PC table Editor \zxhlp{PCFLG} - run-time help
HLPSPFLG Interactive time-channel visibility Editor \zxhlp{SPFLG} - run-time help
HLPTVHUI Interactive intensity-hue-saturation display - run-time help
HLPTVRGB Interactive red-green-blue display - run-time help
HLPZAMAN Fits 1-dimensional Zeeman model to absorption data - run-time help
HLPZEMAN Fits 1-dimensional Zeeman model to data - run-time help
\zxhlp{ICHANSEL} Array of start, stop, increment channel #S + IF to average
\zxhlp{IMLIN} Fits and removes continuum emission from cube
\zxhlp{IRING} integrates intensity / flux in rings / ellipses
\zxhlp{ISPEC} Plots and prints spectrum of region of a cube
\zxhlp{MCUBE} collects n-dimensional images into n+1-dimensional image
\zxhlp{MODAB} Makes simple absorption/emission spectral-line image in I/V
\zxhlp{MORIF} Combines IFs or breaks spectral windows into multiple windows (IFs)
\zxhlp{NCHAV} Number of channels averaged in an operation
\zxhlp{ORDER} Adverb used usually to specify the order of polynomial fit
\zxhlp{PCASS} Finds amplitude bandpass shape from pulse-cal table data
\zxhlp{PCFIT} Finds delays and phases using a pulse-cal (PC) table
\zxhlp{PCPLT} Plots pulse-cal tables in 2 dimensions as function of time
\zxhlp{PCVEL} shifts spectral-line UV data to a given velocity: planet version
\zxhlp{PDVER} specifies the version of the spetral polarization table to use
\zxhlp{PLCUB} Task to plot intensity vs x panels on grid of y,z pixels
\zxhlp{PLRFI} Plots spectral statistics from output of \zxhlp{VBRFI} & \zxhlp{VLBRF}
\zxhlp{POLANGLE} Intrinsic polarization angles for up to 30 sources
\zxhlp{POSSM} Task to plot total and cross-power spectra.
\zxhlp{PRRFI} Prints excess spectral statistics from output of \zxhlp{VBRFI} & \zxhlp{VLBRF}
\zxhlp{QUFIX} determines Right minus Left phase difference, corrects cal files
\zxhlp{REFREQ} Specifies the frequency to be uased as the reference
\zxhlp{REIFS} Breaks spectral windows into multiple spectral windows (IFs)
\zxhlp{RM2PL} Plots spectrum of a pixel with \zxhlp{RMFIT} fit
\zxhlp{RMFIT} Fits 1-dimensional polarization spectrum to Q/U cube
\zxhlp{RSPEC} Plots and prints spectrum of rms of a cube
\zxhlp{SDLSF} least squares fit to channels and subtracts from SD uv data
\zxhlp{SDVEL} shifts spectral-line single-dish data to a given velocity
\zxhlp{SERCH} Finds line signals in transposed data cube
\zxhlp{SMOTH} Task to smooth a subimage from upto a 7-dim. image
\zxhlp{SPECFLUX} Specifies the flux at the reference frequency
\zxhlp{SPECINDX} Spectral index used to correct calibrations
\zxhlp{SPECPARM} Spectral index per polarization per source
\zxhlp{SPECR} Spectral regridding task for UV data
\zxhlp{SPECTRAL} Flag to indicate whether an operation is spectral or continuum
\zxhlp{SPECURVE} Spectral index survature used to correct calibrations
\zxhlp{SPFLG} interactive flagging of UV data in channel-TB using the TV
\zxhlp{SPMOD} Modify UV database by adding a model with spectral lines
\zxhlp{SPRMS} Plots spectral statistics of a selected subset of a uv data set
\zxhlp{SQASH} Task to collapse several planes in a cube into one plane or row
\zxhlp{SYSVEL} Systemic velocity
\zxhlp{UJOIN} modifies UV data converting IFs to spectral channels
\zxhlp{UV2TB} Converts UV autocorrelation spectra to tables
\zxhlp{UVBAS} averages several channels and subtracts from uv data.
\zxhlp{UVDEC} Decrements the number of spectral channels, keeping every nth
\zxhlp{UVFRE} Makes one data set have the spectral structure of another
\zxhlp{UVGLU} Glues UV data frequency blocks back together
\zxhlp{UVLIN} Fits and removes continuum visibility spectrum, also can flag
\zxhlp{UVLSD} least squares fit to channels and divides the uv data.
\zxhlp{UVLSF} least squares fit to channels and subtracts from uv data.
\zxhlp{UVMLN} edits data based on the rms of the spectrum
\zxhlp{UVMOD} Modify UV database by adding a model incl spectral index
\zxhlp{VBGLU} Glues together data from multiple passes thru the VLBA corr.
\zxhlp{VBRFI} Plots spectral statistics of VLBA autocorrelation data for \zxhlp{RFI}
\zxhlp{VLBABPSS} computes spectral bandpass correction table
\zxhlp{VLBRF} Plots spectral statistics of VLBA autocorrelation data for \zxhlp{RFI}
\zxhlp{VTEST} Measures velocity discrepancy across fields
\zxhlp{WTSUM} Task to do a a sum of images weighted by other images
\zxhlp{XBASL} Fits and subtracts nth-order baselines from cube (x axis)
\zxhlp{XG2PL} Plots spectrum of a pixel with \zxhlp{XGAUS}/\zxhlp{AGAUS} and \zxhlp{ZEMAN}/\zxhlp{ZAMAN} fits
\zxhlp{XGAUS} Fits 1-dimensional Gaussians to images: restartable
\zxhlp{XPLOT} Plots image rows one at a time on the graphics or TV screen
\zxhlp{ZAMAN} Fits 1-dimensional Zeeman model to absorption-line data
\zxhlp{ZEMAN} Fits 1-dimensional Zeeman model to data