;SOUSP ;----------------------------------------------------------------------- ;! fits source spectral index from SU table or adverbs ;# TASK UV CALIBRATION ;----------------------------------------------------------------------- ;; Copyright (C) 2010-2012 ;; Associated Universities, Inc. Washington DC, USA. ;; ;; This program is free software; you can redistribute it and/or ;; modify it under the terms of the GNU General Public License as ;; published by the Free Software Foundation; either version 2 of ;; the License, or (at your option) any later version. ;; ;; This program is distributed in the hope that it will be useful, ;; but WITHOUT ANY WARRANTY; without even the implied warranty of ;; MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the ;; GNU General Public License for more details. ;; ;; You should have received a copy of the GNU General Public ;; License along with this program; if not, write to the Free ;; Software Foundation, Inc., 675 Massachusetts Ave, Cambridge, ;; MA 02139, USA. ;; ;; Correspondence concerning AIPS should be addressed as follows: ;; Internet email: aipsmail@nrao.edu. ;; Postal address: AIPS Project Office ;; National Radio Astronomy Observatory ;; 520 Edgemont Road ;; Charlottesville, VA 22903-2475 USA ;----------------------------------------------------------------------- SOUSP LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC SOUSP Fits, plots, returns spectral index parameters INNAME Input UV file name (name) INCLASS Input UV file name (class) INSEQ 0.0 9999.0 Input UV file name (seq. #) INDISK 0.0 9.0 Input UV file disk unit # SOURCES Source name (SOURCES(1) only) CALCODE Calibrator code QUAL -1.0 Source qualifier -1 => any ORDER Order of fit NOISE Noise in Jy for each freq 0 => all same FLDSIZE (Flux, freq) in (Jy, GHz) 0 => use source table DOCONFRM -1.0 1.0 > 0 => replace SU table values with fit SYMBOL 0.0 24.0 Symbol to use on plot FACTOR 0.0 10.0 Scale plot symbols PIXRANGE Control the Y plot range DOTV > 0 => plot on TV, 0 no plots < 0 => make 2 plot files GRCHAN 0.0 7.0 TV graphics channel to use SPECINDX @ Spectral index SPECURVE @ Spectral index curvature ---------------------------------------------------------------- SOUSP Task: This task fits fluxes for a source to determine the spectral index and spectral index curvature: log10 (flux) = A + SPECINDX * log10(f) + SPECURVE(1) * [log10(f)]^2 + ... where A is log10 of the flux at 1 GHz and f is the frequency in GHz. It can then plot the fit on the TV or plot files in both log ang linear space. It will return the adverbs SPECINDX and SPECURVE for use in other tasks such as BPASS. Adverbs: INNAME.....Input UV file name (name). Standard defaults. INCLASS....Input UV file name (class). Standard defaults. INSEQ......Input UV file name (seq. #). 0 => highest. INDISK.....Disk drive # of input UV file. 0 => any. SOURCES....Name of source - only SOURCES(1) is used. ' ' not allowed CALCODE....SOURCES(1) may occur more than once in the source table with different calibator codes. CALCODE may then be used to select which one you want. ' ' => any calibrator code selected '* ' => any non blank code (cal. only) '-CAL' => blank codes only (no calibrators) anything else = calibrator code to select. NB: The CALCODE test is applied in addition to the other tests, i.e. SOURCES(1) and QUAL, in the selection of the source for which to determine the solution. QUAL.......Source qualifier: -1 => any, 0 is a real value. ORDER......<= 1 => fit spectral index only, 2 also fit SPECURVE(1), 3 also fit SPECURVE(2), 4 also fit SPECURVE(3). You will normally not wish to use more than 2. NOISE......Noise value for frequencies 1 up to 64. If FLDSIZE is not used, then these apply to the fluxes in the SU table for the named source. Otherwise, they apply to the fluxes and frequencies listed in FLDSIZE. FLDSIZE....FLDSIZE(1,i) is the flux for the i'th frequency to be fit in Jy and FLDSIZE(2,i) is the frequency in GHz. The number of frequencies to be fit is determined by the number of FLDSIZE pairs that are both > 0. If all are 0, then the SU table is used to provide the fluxes for the various IF frequencies. DOCONFRM...> 0 => ask after plotting if the SU table values should be replaced by the fit values - a YES or yes answer must be given to make this happen. This is only done if all of FLDSIZE is 0. <= 0 => do not change the fluxes in the SU table and do not ask about it. SYMBOL.....1: Plus sign (default) 12: Five pointed star 2: Cross (X) 13: Star of David 3: Circle 14: Seven-pointed star 4: Box 15: Eight-pointed star 5: Triangle 16: Nine-pointed star 6: Diamond 17: Ten-pointed star 7: Pentagon 18: 11-pointed star 8: Hexagon 19: 12-pointed star 9: Septagon 20: 13-pointed star 10: Octagon 21: 14-pointed star 11: Nine-gon 22: Plus with gap 23: vertical line 24: Cross with gap FACTOR.....Scale plot symbols by FACTOR 0 -> 1. If FACTOR < 0, draw lines between the points and use abs(FACTOR) to scale the points plotted. PIXRANGE...If PIXRANGE(2) > PIXRANGE(1), the plot will only cover that range in flux. Otherwise it will cover the full trange of the data (only). DOTV.......> 0 => plot directly on the TV device, otherwise make a plot file for later display on one or more devices (including the TV if desired). GRCHAN.....Graphics channel (1 - 7) to use for line drawing. A value of 0 causes more than one graphics channel to be used. SPECINDX...Spectral index defined above. SPECURVE...Spectral index curvature parameters based on a reference frequency of 1 GHz and base-10 logarithms. ----------------------------------------------------------------