; NOISE
;---------------------------------------------------------------
;! estimates the noise in images, noise level cutoff
;# ADVERB IMAGING EDITING
;-----------------------------------------------------------------------
;;  Copyright (C) 1995, 2011, 2020
;;  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
;-----------------------------------------------------------------------
NOISE     LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC
----------------------------------------------------------------
NOISE
Type:  Adverb  (array(64))
Use:   Gives the noise estimate for up to 64 fields in the *TESS
       imaging tasks.  In UV flagging, used as a noise level cutoff as
       a function of up to 64 IFs.  Used elsewhere when a large array
       is needed.
Null value:
       None
Tasks:
   FIXBX.......Converts a BOXFILE to another for input to IMAGR.  NOISE
               is misused to convey the old RASHIFT values.
   FLATN.......Re-grid multiple fields into one image incl sensitivity.
               NOISE gives the relative error for each pointing.
   LTESS.......Makes mosaic images by linear combination.
   OMFIT.......Fits sources and, optionally, a self-cal model to uv
               data.  NOISE gives the a priori noise and 2 cutoffs.
   RFLAG.......Flags data set based on time and freq rms in fringe
               visibilities.  NOISE is an IF-dependent cutoff for time
               rms values.
   SOUSP.......Fits source spectral index from SU table or adverbs.
               NOISE gives the expected noise for up to 64 frequencies.
   STESS.......Finds sensitivity in mosaicing.
   UTESS.......Deconvolves polarization images by maximizing emptiness.
   VTESS.......Deconvolves sets of images by the Maximum Entropy Method.
   WTMOD.......Modifies weights in a UV data set.  NOISE provides the
               weight scale for each antenna.
----------------------------------------------------------------