; UVGLU ;--------------------------------------------------------------- ;! Glues UV data frequency blocks back together ;# Task UV SPECTRAL ;----------------------------------------------------------------------- ;; Copyright (C) 1995 ;; 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 ;----------------------------------------------------------------------- ;--------------------------------------------------------------- UVGLU LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC UVGLU Task which glues uv frequency blocks back together 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 # IN2NAME Second UV file name (name) IN2CLASS Second UV file name (class) IN2SEQ 0.0 9999.0 Second UV file name (seq. #) IN2DISK 0.0 9.0 Second UV file disk unit # OUTNAME Output UV file name (name) OUTCLASS Output UV file name (class) OUTSEQ -1.0 9999.0 Output UV file name (seq. #) OUTDISK 0.0 9.0 Output UV file disk unit #. ---------------------------------------------------------------- UVGLU Task: This task will try to glue the spectral line data from the second file onto the spectral line data of the first file, creating a file with the sum of the number of channels. It will only work if the databases are perfect- ly matched. Headers should only differ in frequency and the highest frequency + 1 of the first file should be the first frequency in the second. 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. IN2NAME....Second file name. IN2CLASS...Second file class IN2SEQ.....Second file sequence number. IN2DISK....Second file sequence number. OUTNAME....Output UV file name (name). Standard defaults. OUTCLASS...Output UV file name (class). Standard defaults. OUTSEQ.....Output UV file name (seq. #). 0 => highest unique OUTDISK....Disk drive # of output UV file. 0 => highest with space for the file. ---------------------------------------------------------------- UVGLU Glues UV data frequency blocks back together DOCUMENTOR: H.J. van Langevelde (Sterrewacht Leiden) PURPOSE UVGLU will check the headers of the two input files. If it decides that these match perfectly (not considering any spectral line information), it will than check that the second file contains the next block in frequency. When this is OK it will create the output file in which the number of channels will be the sum of the number of channels in the input files and copy the visibilities in the proper place. While doing this it checks whether the visibilities indeed come from the same baseline. Values for the random parameters in the output file are copied from the first input file. The header of the first input file is used to create the output header, keeping the right reference frequency for the u,v,w values. UVGLU does not require that the number of visibility points in each file agree exactly. If the files do differ in size it is assumed that the data in each file are sorted in time-baseline order. UVGLU is useful in big spectral line experiments where you may want do deal with chunks of spectral line at the time. Use UVCOP to split your data up and UVGLU to put them back together.