; FACES ;--------------------------------------------------------------- ;! makes images of catalog sources for initial calibration ;# Task Imaging Modeling Calibration ;----------------------------------------------------------------------- ;; Copyright (C) 2000-2003, 2005, 2008 ;; 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 ;----------------------------------------------------------------------- FACES LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC FACES: Makes images of catalog sources for initial calibration INNAME UV dataset name (name) INCLASS UV dataset name (class) INSEQ 0.0 9999.0 UV dataset name (seq. #) INDISK 0.0 9.0 Disk drive # SOURCES Source selected OUTNAME Output file name OUTDISK Output disk number CELLSIZE 0.0 (X,Y) size of grid in asec IMSIZE 0.0 16384 field size SHIFT Position shift (RA,Dec) asec for all fields BMAJ Clean beam FWHM in asec FLUX 0.0 Minimum component flux (source * beam) BPARM (1) Inner region radius (deg) (2) Field overlap in pixels (3) Factor to scale NVSS fluxes, 0 -> 1 PBPARM Beam parameters: (1) Cutoff 0 -> 0.023 (2) > 0 -> Use (3)-(7) (3)-(7) Beam shape INLIST NVSS input file name ' ' => AIPS provided. ---------------------------------------------------------------- FACES Type: Task Use: FACES creates (mostly empty) images and CC files containing all NVSS (or WENSS or ??) sources > n milliJy that would fall in the images. The survey flux of each source is multiplied by the single-dish beam pattern out to a specified cutoff. Sources beyond this point are not included. Adverbs: INNAME......The UV dataset name (name). Standard defaults. INCLASS.....The UV dataset name (class). Standard defaults. INSEQ.......The UV dataset name (seq. #). 0 => highest. INDISK......The disk drive #. 0 => any. SOURCES.....The source to be used from a multi-source file; a single source name is required to get the central pointing position from the source table. Ignored for single-source files. OUTNAME.....Name field (12 characters) of output files. ' ' => INNAME. The OUTCLASS is IMOnnn for filed number nnn. The OUTSEQ for field 1 is 0 and that OUTSEQ is used for all other fields. OUTDISK.....Output file disk number. CELLSIZE....Pixel size for the fields in IMAGR in arc seconds. IMSIZE......Size of each field. If CELLSIZE and/or IMSIZE are zero, the data are read to find the maximum baseline and maximum W in order to estimate these parameters. NOTE: FACES may write out only 512 fields but is willing to try as many as 20 times that number. Only those fields which have sources will be written. So IMSIZE may be smaller than one would use with SETFC and IMAGR. SHIFT.......Specifies a position shift in arc seconds at the phase center for all of the fields in the inner portion. The output RA = RA0 + SHIFT(1)/cos(DEC0) and DEC = DEC0 + SHIFT(2) where 0 refers to the input coordinates. BMAJ........Clean beam FWHM in arc seconds. 0 -> 3 * CELLSIZE(1) FLUX........Minumum included component "flux" = source flux times the single-dish beam power. 0 => any in INLIST. Fluxes are read from the table, scaled by BPARM(3), and then compared to FLUX. BPARM.......(1) The radius in degrees to be covered fully by overlapping fields. (2) Field overlap in pixels 0 -> 5. (3) Factor to scale NVSS fluxes (to account for spectral index on average). 0 -> 1 PBPARM......Primary beam parameters: (1) Lowest beam value to believe: 0 -> 0.023 Sources outside this range are ignored. (2) > 0 => Use beam parameters from PBPARM(3)-PBPARM(7) Otherwise use default parameters for the VLA (or ATCA where appropriate) (3-7)..For all wavelengths, the beam is described by the function: 1.0 + X*PBPARM(3)/(10**3) + X*X*PBPARM(4)/(10**7) + X*X*X*PBPARM(5)/(10**10) + X*X*X*X*PBPARM(6)/(10**13) X*X*X*X*X*PBPARM(7)/(10**16) where X is (distance from the pointing position in arc minutes times the frequency in GHz)**2. For the VLA, these parms are, by default, given by Perley's fits: 0.0738 GHz -0.897 2.71 -0.242 0.3275 -0.935 3.23 -0.378 1.465 -1.343 6.579 -1.186 4.885 -1.372 6.940 -1.309 8.435 -1.306 6.253 -1.100 14.965 -1.305 6.155 -1.030 22.485 -1.417 7.332 -1.352 43.315 -1.321 6.185 -0.983 For the ATCA, these are by default: 1.5 GHz -1.049 4.238 -0.8473 0.09073 -5.004E-3 2.35 -0.9942 3.932 -0.7772 0.08239 -4.429E-3 5.5 -1.075 4.651 -1.035 0.12274 -6.125E-3 8.6 -0.9778 3.875 -0.8068 0.09414 -5.841E-3 20.5 -0.9579 3.228 -0.3807 0.0 0.0 See explain for details INLIST......Catalog input file name. For format see Explain ' ' => AIPS-provided file with 237600 objects, either 'AIPSTARS:NV00.0030' for J2000 or 'AIPSTARS:NV50.0030' for B1950. Other AIPSTARS: files available are Epoch 2000: FLUX >= 1.000 NV00.1000 ( 2267 objects) FLUX >= 0.300 NV00.0300 ( 14456 objects) FLUX >= 0.100 NV00.0100 ( 63411 objects) FLUX >= 0.030 NV00.0030 (237600 objects) Epoch 1950: FLUX >= 1.000 NV50.1000 ( 2267 objects) FLUX >= 0.300 NV50.0300 ( 14456 objects) FLUX >= 0.100 NV50.0100 ( 63411 objects) FLUX >= 0.030 NV50.0030 (237600 objects) The WENSS/WISH surveys ar also available $AIPSTARS as FLUX >= 0.100 WE00.0100 ( 99709 object 2000) FLUX >= 0.100 WE50.0100 ( 99709 object 1950) Some sites may choose to download really large source lists to deeper flux levels. These may include from the NVSS survey: FLUX >= 0.003 NV00.0003 (1560007 objects, 2000) FLUX >= 0.003 NV50.0003 (1560007 objects, 1950) and the WENSS/WISH survey: FLUX >~ 0.010 WE00.0000 (319770 objects, 2000) FLUX >~ 0.010 WE50.0000 (319770 objects, 1950) These deep files may be particularly useful for BOXES but may be too deep to be of use here. Note: the WENSS survey covers +90 to +28 degrees declination and the WISH survey covers -25 to -15 with some sources to -9. ---------------------------------------------------------------- FACES: Task to make images from the NVSS (or WENSS or ??) DESCRIPTION The task creates images matching the Fly's eye portion of the fields that would be found by SETFC. The NVSS or other source catalog is then searched for all sources which would fit in these images within the primary or single-dish beam. Those sources that fit in one or more of the images are added to those images. They are also added to the CC file of the field closest to them. These images and the CC files may be used as a model for the area observed. The CC sources will not lie on grid cells. The CC model may be used only with CMETHOD = 'DFT'. In order to do all this, the position (RA,DEC) of the pointing phase center is required. This is obtained from the input UV data set. In the case of a single-source data set, it is read from the header. In the case of a multi-source data set, the source must be specified in the first element of the adverb SOURCES, and the position is read from the SU extension. The selection of sources is by the adverbs BPARM(3), and BPARM(5-10). See their description above. The source catalog may be specified in INLIST or you may use one of the AIPS-provided versions of the NVSS. The format of the file is: All lines beginning with a semi-colon are ignored. They are the copyleft, a descriptive text in the AIPS files, and other comments. Be careful about the epoch of the coordinates. Remaining give the Right ascension in degrees, Declination in degrees, Flux in mJy, and optionally a FWHM in arc seconds using format F9.5,1X,F9.5,I7,F10.4. A sample is given below no width is shown since none are used by FACES. ;----------------------------------------------------------------------- ; Copyright (C) 1999-2000, 2002 ; 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 ;----------------------------------------------------------------------- ; NRAO/VLA Sky Survey (NVSS) from CATALOG39.FIT ; 2267 sources brighter than 1.0 Jy ; Catalog made on 1998-07-10 with 1814748 entries ;RA(2000) Dec(2000) Flux ; deg deg mJy 0.08521 55.65239 1518 0.22108 40.90052 1301 0.84166 -17.45316 2415 1.23802 12.80524 1071 1.37727 69.39949 1105 1.55780 -6.39310 2051 1.59416 -0.07363 3898 2.12217 -5.97935 1323 ;..... 358.54728 32.91998 1183 358.59049 45.88455 1873 358.78961 49.83570 2306 358.97312 15.69069 1104 359.25280 -34.75882 1286 359.32748 14.76875 1020 359.38022 -11.42748 1814 359.64781 44.07789 1940 RICK PERLEY'S REPORT Polynomial Coefficients from LSq Fit to VLA Primary Beam raster scans. Functional form fitted: 1 + G1.X^2 + G2.X^4 + G3.X^6 where X = r.F, and r = radius in arcminutes F = frequency in GHz. Fits were made to 3% cutoff in power for 24 antennas. Poor fits, and discrepant fits were discarded, and the most consistent subset of antennas had their fitted coefficients averaged to produce the following 'best' coefficients. Freq. G1 G2 G3 ---------------------------------------------------------- 0.0738 -0.897E-3 2.71 E-7 -0.242E-10 0.3275 -0.935 3.23 -0.378 1.285 -1.329 6.445 -1.146 * 1.465 -1.343 6.579 -1.186 4.885 -1.372 6.940 -1.309 8.435 -1.306 6.253 -1.100 14.965 -1.305 6.155 -1.030 22.485 (old) -1.350 6.526 -1.090 * 22.485 (new) -1.417 7.332 -1.352 43.315 -1.321 6.185 -0.983 ----------------------------------------------------------- The estimated errors (from the scatter in the fitted coefficients) are generally very small: G1: .003 at all bands except Q (.014) G2: .03 to .07 at all bands except Q (.15) G3: .01 to .02 at all bands except Q (.04) R. Perley 21/Nov/00 * The 1.285 and 22.485 old feed values are not used.