% -*- latex -*-
%-----------------------------------------------------------------------
%;  Copyright (C) 2025
%;  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
%-----------------------------------------------------------------------
%Body of final AIPSletter for 31 December 2025
\documentclass[twoside]{article}
\usepackage{graphics}

\newcommand{\AIPRELEASE}{December 31, 2025}
\newcommand{\AIPVOLUME}{Volume XLV}
\newcommand{\AIPNUMBER}{Number 2}
\newcommand{\RELEASENAME}{{\tt 31DEC25}}
\newcommand{\OLDNAME}{{\tt 31DEC24}}
\newcommand{\NEWNAME}{{\tt 31DEC26}}
\newcommand{\Tsys}{${\rm T}_{\rm sys}$}
\newcommand{\THISYEAR}{2025}
\newcommand{\NEWYEAR}{2026}
\newcommand{\OLDYEAR}{2024}


%macros and title page format for the \AIPS\ letter.
\input LET98.MAC
\newcommand{\keyw}[1]{\hbox{{\tt #1}}}
\newcommand{\MYSpace}{-11pt}
\normalstyle

\section{General developments in \AIPS}

\subsection{\Aipsletter\ publication}

We have discontinued most paper copies of the \Aipsletter\ entirely.
The \Aipsletter\ will be available in PostScript and pdf formats as
always from the web site listed above.  New issues will be announced on
the {\tt bananas} and {\tt mnj} list servers and sometimes in the NRAO
eNews.

\subsection{Current and future releases}

\AIPS\ is now copyright \copyright\ 1995 through \THISYEAR\ by
Associated Universities, Inc., NRAO's parent corporation, but may be
made freely available under the terms of the Free Software Foundation's
General Public License (GPL)\@.  This means that User Agreements are no
longer required, that \AIPS\ may be obtained via anonymous ftp without
contacting NRAO, and that the software may be redistributed (and/or
modified), under certain conditions.  The full text of the GPL can be
found in the \texttt{15JUL95} \Aipsletter\ and is included with every
distribution in file {\tt \$AIPS\_ROOT/{\it release-name}/COPYING}\@.

We have formal \AIPS\ releases on an annual basis.  We recommend a
full binary installation method for both the ``slushy'' and
``development'' versions for MacIntosh OS/X (Intel {\it and} ARM chips),
and Linux (64-bit) systems, but all architectures can do a full
installation from the source files.  There are no longer binary versions
available for 32-bit Linux, Solaris, and Mac PPC chip architectures.  If
you develop \AIPS\ code locally {\it or have system managers that forbid
  the use of\/} {\tt rsync}, you will need to do a source-level
installation.  The current release is called \RELEASENAME\ and is now
``slushy.''  If you took a development copy of this version at some
earlier date, you should use the ``Midnight Job'' (MNJ) to bring it up
to date.  You need to run a MNJ only once in \NEWYEAR\ to convert your
copy of \RELEASENAME\ into the slushy version.  However, when patches to
\RELEASENAME\ are announced in \NEWYEAR, you may apply them with the
MNJ\@.  This \Aipsletter\ is intended to advise you of corrections and
improvements in this release.

We have begun a new version, called \NEWNAME, which is now under
development by the \AIPS\ Group.  You may fetch and install a complete
copy of this version at any time.  Having fetched \NEWNAME, you may
update your installation whenever you want by running the MNJ\@.  This
uses {\tt rsync} to copy all changed text files and then to copy the
binary files or to compile the code selectively based on the code
changes and compilations we have done.  We expect users to take their
source-only or binary version of \NEWNAME\ \AIPS\ over the Internet (via
\emph{anonymous} ftp).  Both versions require you to copy the
installation procedure {\tt install.pl} via {\tt ftp}; the source-only
version also requires you to ftp the 201-Mbyte {\tt \NEWNAME.tar.gz}
compressed tar file.

\vfill\eject

If compiling locally, new releases must be installed from the tar ball
for that release.  {\tt 31DEC22} and later versions contain improvements
to the code which should make local compilation more reliable.  If using
the binary installation, a full new installation must also be done with
{\tt rsync}.  When installing a new \AIPS\ release in a system that
already has a previous release, we recommend that {\tt install.pl} be
used and that the previous release be left in place, at least until the
new installation has been verified.  If you do this, then you will not
have to re-edit the disk, printer, and tape lists and can simply skip
all those pages in the {\tt install.pl} menus.  The old {\tt
  \$HOME/.AIPSRC} file may be left in place, but it will need to be
edited.  The lines giving the {\tt DOWNLOADED} and {\tt UNPACKED}
parameters should be cleared and the {\tt CCOMOPT} line should be
changed to point to the current release rather than the previous one.
If you have made a special version of {\tt do\_daily.{\it host}}, you
should preserve it under a new name and restore it after the install. If
you have an odd set of \AIPS\ versions, the {\tt
  \$AIPS\_ROOT/AIPSPATH.*SH} files may need to be edited after the
install to set the desired versions.  The file {\tt
  \$SYSLOCAL/UPDCONFIG} also needs to be edited to correct your e-mail
address(es).  A new installation will not change your current \AIPS\
data files.

{\tt 31DEC15} contains a change in the headers of $uv$ data sets which
will not be understood by previous versions.  {\tt 31DEC20} contains a
change to the {\tt XAS} TV server which will cause problems with older
versions.  Note that the only version which we will patch for major
errors is \RELEASENAME; even \OLDNAME\ will no longer be changed.

%\section{Preview of coming attractions}

%The \NEWNAME\ release already contains a few changes that we decided
%were a bit risky or not needed in \RELEASENAME\@.

\section{Improvements of interest to users in \RELEASENAME}

In the latter half of \THISYEAR, four new tasks, four new verbs, and 2
new procedures appeared.  The tasks are {\tt DFTQU} to make an image
in Q and U polarizations of a point as a function of time, {\tt XG2XG}
to copy an {\tt XG} or {\tt ZE} table to a new one with a different
number of possible components, {\tt RESOU} to renumber sources in a
data set, and {\tt PRPLT} to plot image ``profiles'' which are the
average of the image over 2 axes as a function of the third.  The new
verbs are {\tt CAT2LOG} through {\tt CAT5LOG} to do the {\tt CATALOG}
operation with the second through fifth sets of file name adverbs.  The
new procedures are {\tt TV3LOD} to load and display on the TV an RGB
image cube and a large {\tt RUN} file called {\tt VLBAPIPE} to reduce
VLBI data with tasks in a different order than that used in {\tt
  VLBARUN}\@.

In the first six months, there were six new user tasks, 2 new verbs, and
four new service programs in \RELEASENAME\@.  The new tasks are {\tt
  SYHIS} to analyze the contents of SysPower ({\tt SY}) tables, {\tt
  IM2TX} to write one-dimensional text files from image data, {\tt
  TX2IM} to create one-dimensional image files from text files, {\tt
  LISPX} to compute spectral indexes from one-dimensional text files,
{\tt SPXMD} to add spectral index models to image cubes, and {\tt OFMPL}
to display on the TV all available OFM tables.  The new verbs are {\tt
  OFMCOLOR} to choose from 30 pseudo color tables for the current TV
image and {\tt OFMSTRCH} to modify the TV pseudo color table.  The new
service programs, used mainly by your editor, are {\tt COLOR} to
translate publicly available color tables into OFM files, {\tt ADVHLP}
and {\tt ADVCHK} to be used by the new script also named {\tt ADVCHK} to
make sure that all verbs, tasks, and procedures are listed in the adverb
help files used by them, and {\tt ADVCNT} to check line lengths in all
help files.

Normally, bugs which appear in an \AIPS\ {\tt TST} version and then
are fixed in that same version before its release get little or no
discussion in the \Aipsletter\@.    Since a rather large number
of sites now install the {\tt TST} version of \AIPS\ during its
development, not describing temporary bugs in {\tt TST} is somewhat of
an oversight.  We urge you to run the ``Midnight Job'' at least once
after \RELEASENAME\ is turned slushy to bring it up to date and to fix
all bugs of this sort.  We urge active sites to use the MNJ and, when
something odd occurs, to examine {\tt CHANGE.DOC} using the cgi tool
available from the \AIPS\ documentation web page ({\tt
  http://www.aips.nrao.edu/aipsdoc.html}).  Please do not hesitate to
contact us via the NRAO science user help desk ({\tt
  https://help.nrao.edu}) or via e-mail {\tt daip@nrao.edu} with any
questions or suspicions that there are problems.

\subsection{System matters}

Due to the ``end of life'' for RedHat 7, we chose to freeze {\tt
  31DEC23} completely in June 2024.  In this way, the binary version
for {\tt LNX64} could remain as produced by RedHat 7.  {\tt 31DEC24} for
64-bit Linux was then re-compiled with RedHat 8, producing a binary
version incompatible with the older operating system.  At the same time,
we discontinued any development of the 32-bit Linux binary version.
That version is available in binary form but only up to June 20, 2024.
{\tt 31DEC25} does not contain a binary version for 32-bit Linux.  Old
Linux systems left behind by these actions should note that it is
relatively easy to compile all of \AIPS\ on whatever machine you may
have.  Versions of {\tt gfortran} at least 4.8, but better 6 or more,
are required.  The latest {\tt gfortran} versions should also work.

The {\tt MACARM} binary version of {\tt 31DEC25} is computed on a
machine that was upgraded to ``Sequoia'' (OS version 15.6.1) with a
gfortran upgraded to version 12.2.  The load modules should work on
any system at OS 13.0 or greater.  The {\tt 31DEC23} version was frozen
at the previous operating system level.  The {\tt MACINT} binary version
continues to be developed, but if the computer used to produce it dies,
our support for that binary version will halt.  Again, you should note
that compiling \AIPS\ locally should go right on working.

{\tt LNX64} now requires two ``containers'' to support the new task {\tt
  ALBUS}\@.  They should be copied by rsync either by {\tt install.pl}
or in the MNJ even for text (locally-compiled) installations.  These
files are large, one is 373 Mbytes, the more recent one is almost 410
Mbytes.  These containers are not available for Macs.

\subsection{UV data}

Work on the {\tt ALBUS} task revealed that \AIPS\ has used a simple
geometric computation to compute antenna longitude and latitude from the
antenna (X,Y,Z) location parameters.  All of \AIPS\ was changed to use
the ``geodetic latitude'' instead using a new subroutine.  The geometric
latitude of the VLA differs from the geodetic latitude by about 11 arc
minutes or about 20 km to the South.

The \AIPS\ task called {\tt ALBUS} was given further attention.  The
desired GPS stations may now be specified with a new adverb, sensibly
named {\tt STATIONS}\@.  The stations actually used in the solution are
listed in the message file and written to the history file.  Each
station is listed only once unless a new antenna is specified (as in
VLBI)\@.  The file {\tt \$AIPSIONS/ALBUS.stations} provides an enormous
list of GPS stations which might be used by the program.  That list was
upgraded to drop duplicates, correct West longitudes (previously
specified without a minus sign!), and to contain a description of the
station location.  The reading of negative latitudes from this file was
corrected to handle the pernicious -00 degrees issue.  Note that the
{\tt 31DEC24} version of {\tt ALBUS} did not receive these changes other
than the upgraded stations file.  The default {\tt TECRTYPE} was changed
to the model called {\tt G01} which seems best for VLA data.

A new VLBI {\tt RUN} file ``pipeline'' called {\tt VLBAPIPE} was
written.  It borrows heavily from {\tt VLBARUN} but does some of the
steps in a different order.  The most important of these is to do
the full (every scan) run of {\tt FRING} before doing the {\tt BPASS}
step.  When the user has more than one scan on the bandpass calibrator
this can make quite a difference.  Extensive discussion on these
pipelines can be found from the VLBA section of the web site listed at
the start of this \Aipsletter.  Both pipelines were changed to use
{\tt LISUN} rather than {\tt LISTR} to generate the summary of the
data set written to the output message file.  The {\tt RUN} files for
{\tt VLBAUTIL} and both pipelines were changed to allow the procedures
to be run from multiple \AIPS\ numbers for a single user number and
output data area.

The interactive data display and editing task {\tt EDITR} was given a
new {\tt CLIP EVERYTHING} menu option that uses the {\tt FLAG ABOVE}
interaction to set a clip level which is then applied to {\it every}
baseline in the IFs, polarizations, and times currently displayed in the
edit window.  It displays what it is doing while running and
automatically updates the display when it finishes.  {\tt EDITR} was also
changed to display and edit upon a ``coherence'' parameter defined as
the scalar averaged amplitude divided by the vector averaged amplitude
minus 1.0.  Note that this parameter requires data to be time averaged
on the fly.  {\tt EDITR} was also corrected to handle the optional
second data set properly.  The ``expert'' mode was not changed and
probably should be deleted.

The new task {\tt DFTQU} is similar to {\tt DFTPL} and {\tt DFTIM} but
writes out an image cube with Stokes Q and U and RGB color as the axes.
The image contains the image of the Q and U Stokes of the data at a user
selected celestial coordinate.  Time is then used to set the color.
This task should allow analysis of time-variable polarized sources of
small diameter.

\begin{description}
\myitem{VPLOT} was corrected to compute amplitude rms properly and
        plotting of phase rms was added.  An option to extend the rms
        computation over spectral channels as well as time was added.
        An optional text file output was also added.
\vfill\eject
\myitem{LISTR} was given a phase rms option in the {\tt 'MATX'} and {\tt
        'LIST'} operations.  The rms options in {\tt 'LIST'} were
        corrected to do a proper computation since the ``count''
        parameter in the code was actually a sum of weights.  The
        handling of antenna selection was changed to honor the
        \AIPS-standard specification allowing the list to be inclusive
        or exclusive.
\myitem{LISUN} was enhanced with a listing of the antennas in the array.
        Antenna number, station name, (X,Y,Z) coordinates, and longitude
        and latitude are given.
\myitem{UVFLG} was given an option to flag scans too close to the
        Sun. Changed the code to allow elevation, shadowing, pulse cal,
        and Sun distance to be done all at once, although in separate
        passes through the data.
\myitem{RESOU} is a new task to allow the changing of up to 30 source
        numbers while copying a data set.  It is very similar to {\tt
          DSORC} and parts of {\tt MATCH} without some of their
        complications.
\myitem{CLPLT} was changed to do all of the optional {\tt OUTTEXT}
        output before any plotting.  This guarantees that all print out
        is obtained even when {\tt DOTV=1} displays are terminated
        early.  A bug was fixed that caused the last tine sample to be
        lost.  The bad computation and plotting of error bars was
        corrected.
\myitem{CAPLT} was changed to have an {\tt OUTTEXT} option and its
        computation and plotting of error bars was corrected.
\myitem{UVDIF} was changed to include or exclude auto-correlation and
        cross-correlation data.
\myitem{DIFUV} was given a new option to to compute the difference of
        the two data sets divided by the second.  Output displays of
        mean, rms, max, and min were added along with a control of the
        writing of an output data set.
\myitem{UVHGM} and {\tt UVHIM} were given a channel averaging option.
\myitem{TVFLG,} {\tt SPFLG} and {\tt FTFLG} were corrected to handle I/O
        with short rows.  {\tt TVFLG} was corrected to record the upper
        time properly in the {\tt ANTENNA-DT} operation.
\myitem{ELINT} was corrected to copy the one IF solution to all IFs.
\myitem{CLCOR} was changed when doing the {\tt EOPS} correction to
        assume the usual values when the (old) {\tt CT} tables have all
        times equal to zero.
\end{description}

\subsection{Imaging, Analysis, and Display}

{\tt XGAUS}, {\tt ZEMAN}, {\tt AGAUS} and {\tt ZAMAN} are used to fit
spectra with Gaussians and measure Zeeman splitting.  They received a
number of changes reported in the previous \Aipsletter\ and several more
in the last six months.  {\tt XGAUS} was changed from always allowing
only eight components to allowing up to 32 with the number to be allowed
set when the {\tt XG} table is created.  This forced changes to the menu
operations when the number of allowed components becomes large.  The
task now also computes an image of the rms of the residual after fitting
which can be used in the editing stage and written to a cataloged file.
{\tt AGAUS} which fits absorption spectra was changed similarly.  The
Zeeman tasks now respond to the number of Gaussians in the {\tt XG}
table used when {\tt OPTYPE = 'GAUS'}\@.  Because a user may expend
considerable effort on an {\tt XG} or {\tt ZE} file, a new task {\tt
  XG2XG} was written to copy one of these tables to another with a
change to the maximum number of components allowed.  The task {\tt
  XG2PL} was changed to accommodate the changes in these tables.

The concept of an image ``profile'' was added to the {\tt GREYS} task.
The profile in {\tt GREYS} is the average in each column of the image
which is then plotted along the top and/or the average in each row which
is then plotted to the right.  An example is shown in the accompanying
figure.  This image was produced by {\tt DFTIM} for a study by Emmanuel
Momjian of the new VLA online RFI excision.  A new task called {\tt
  PRPLT} has also been written to plot any or all three profiles from an
image cube.  An example plot of an HI galaxy cube is illustrated.  The
plot from the image $x$ axis being the average over all $(y,z)$, the
plot from the image $y$ axis being the average over all $(x,z)$, and the
plot along the $z$ axis being the average over all $(x,y)$.

\centerline{\resizebox{5.7in}{4.9in}{\includegraphics{FIG/Greys.3.eps}}}

\centerline{\resizebox{!}{4.4in}{\includegraphics{FIG/PRPLT.3.eps}}}

\vfill\eject
\begin{description}
\myitem{IMAGR} was changed to put the version numbers of the tables
        actually used for calibration and flagging into the history
        file.  The imaging TV display was changed to prevent excess
        initialization of the look-up tables when the timeout option is
        used.
\myitem{IMEAN} was corrected to count ``overflow'' pixels properly and
        to display the Gaussian fit parameters when that option is
        selected.
\myitem{TV3LOD} is a new procedure automatically available to load
        an RGB image to 3 TV planes and turn them on in proper colors.
\myitem{BLANK} was given a simple {\tt 'BOX'} option to select or
        deselect up to 10 circular or rectangular areas.
\myitem{LEVS} contour levels are displayed whenever contours are drawn.
        The routine to generate the display string did unfortunate
        things to {\tt LEVS} greater than 1000.
\myitem{}
\end{description}

\subsection{Verbs, general, and documentation}

The old verb {\tt CATALOG} was changed to ignore {\tt INTYPE} when
displaying all catalog entries matching the other name parameters.
New verbs {\tt CAT2LOG}, {\tt CAT3LOG}, {\tt CAT4LOG} and {\tt CAT5LOG}
were created to perform the same function with the other sets of name
parameters.

Verb {\tt PLGET}, which fills in the adverbs used to create a plot file,
was revised as needed to match changes in plot tasks.  Another
little-known verb {\tt EXTLIST}, which provides information on the
  contents of extension files, was revised as needed.

The \Cookbook\ was systematically updated in February, May, July,
October, and November.  Display problems with the {\tt ABOUT} lists of
Chapter 13 in the web-capable pdf and html versions were corrected.
The TAB completion, {\tt APROPOS}, and {\tt ABOUT} text files were
updated at the same time.  The help files for adverbs contain lists of
the verbs, procedures, and tasks which use them.  These were also
updated regularly and were revised so that the same format is used in
all such files.

\section{Recent Memoranda}

All \AIPS\ Memoranda are available from the \AIPS\ home page.  Memo 117
which details the FITS format used by \AIPS\ was updated for changes in
the {\tt XG} and {\tt ZE} tables.  Memo 118 and 122 which describe the
interactive spectral-fitting tasks in \AIPS\ were updated substantially
to account for the numerous changes in these tasks.

\begin{tabular}{lp{5.8in}}
{\bf 118} & {\bf Modeling Spectral Cubes in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  October 6, 2025 revision\\
   &   \AIPS\ has done Gaussian fitting along the $x$-axis of image cubes
  with task \keyw{XGAUS} since the 1980s.  That task was overhauled
    in 2013 to be much easier to use and much more capable.  In like
  fashion, tasks \keyw{ZEMAN} and \keyw{RMFIT} were developed.  The
  former fits the standard leakage and scaling terms for Stokes V cubes,
  including a new option to do this for each of the Gaussians found by
  \keyw{XGAUS}\@.  The latter fits polarization models to Stokes Q and U
  cubes, using the output of Faraday Rotation Measure Synthesis
  (\AIPS\ task \keyw{FARS}) to assist with initial guesses.  The models
  can contain multiple components each with a polarization flux, angle,
  rotation measure, and rotation measure ``thickness.''  The present
  memo will describe the functions of these tasks in some detail with
  numerous graphical examples.  A revision of this memo discusses
  changes made for the {\tt 31DEC15} release and two new tasks to plot
  spectra with model fits and a number of tasks which make visibility
  and image model files.  The November 2017 revision includes new
  display options in {\tt RMFIT}\@.  The April and July 2025
    revisions add display and edit options and correct display and
    pixrange setting.  The September 2025 revision contains changes
    made to allow more than 8 components in {\tt XGAUS} and {\tt
      ZEMAN}\@.
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 122} & {\bf Modeling Absorption-line Cubes in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  October 6, 2025 revision\\
   &  \AIPS\ does Gaussian fitting of spectral lines with overhauled task
  \keyw{XGAUS} and can fit V polarization image cubes for Zeeman
  splitting with the task \keyw{ZEMAN}\@.  Both of these tasks are
  designed for emission spectra in which the noise is not a function of
  spectral channel.  In absorption, however, the noise in optical depth
  becomes high when the optical depth is high.  Therefore, new tasks
  \keyw{AGAUS} and \keyw{ZAMAN} have been written to provide similar
  functions but with mathematics suitable for absorption lines.  This
  memo describes the new tasks in some detail and includes a description
  of a new, simplified modeling task \keyw{MODAB} which may also be
  useful.  That task has shown that the results of these four tasks are
  biased by the presence of the Zeeman splitting and need modest
  correction if they are meant to describe the actual pre-splitting line
  widths and magnetic field.
\end{tabular}

\section{\AIPS\ Distribution}

From the NRAO system logs, we count apparent MNJ accesses, downloads
of the tar balls, and {\tt rsync} accesses by unique IP address.  In
November 2025 one of our counting cron jobs stopped working; recovery
of the counts may not be totally accurate.  Mysteriously, the number
counted for binary is slightly larger than the count intended to
represent all.  Since DSL and some university and other connections may
be assigned different IP addresses at different times, this will be a
bit of an over-estimate of actual sites.  However, a single IP address
is often used to provide \AIPS\ to a number of computers, so these
numbers are at the same time an under-estimate of the number of
computers running current versions of \AIPS\@.  In \THISYEAR, a total of
187 different IP addresses downloaded the slushy form of \OLDNAME\ and
512 IP addresses downloaded \RELEASENAME\ in tarball or binary form.
With the change to the MNJ (rsync only) we are unable even to guess how
many sites have run the MNJ\@.  The total number of unique IP addresses
in these five lists was 613, about 90 \%\ of last year.  The plot of
numbers versus time and the table shows that 2025 was a bit ahead of
2024 in the {\tt TST} version, but rather behind in the {\tt NEW}
version numbers.  A new scheme to count {\tt rsync} uses of {\tt
  \$ARCH/LOAD} was developed in the hope of learning which architectures
are used for \AIPS\@,  The results were confusing, but clearly show {\tt
  LNX64} as very popular with {\tt TST MACARM} following rather far
behind.

\centerline{\resizebox{!}{4.0in}{\includegraphics{FIG/PLOTIT2425all.eps}}}

\vfill\eject

\section{Patch Distribution for \OLDNAME}

Normally, this section lists the patches that have been released for
\OLDNAME\@.  This was based on the assumption that users would want to
download individual files to compile them locally.  However, the
``Midnight Job'' ({\tt \$HOME/do\_daily.}{\it hostname}) will do this
for you on both locally-compiled and binary installations.  Therefore
there is no reason to continue the old procedure.  Major bug corrections
were moved to \OLDNAME\ as they occur and users should use the MNJ on
occasion on both the {\tt NEW} and {\tt TST} versions of \AIPS\@.

The \OLDNAME\ release is still available for installation, but is not
recommended and will no longer receive patches even for egregious
errors.  It had a number of important patches during \THISYEAR\@.
The patches are

\begin{enumerate}
  \item\ {\tt TVSPX} was given new options and corrected for handling
    zoom and large images. {\it 2025-01-23}
  \item\ {\tt QBEAM} was corrected for number of adverbs and its
    handling of {\tt CUTOFF}. {\it 2025-01-28}
  \item\ {\tt AU8A} ({\tt EXTLIST} verb) was corrected for its handling
    of 30-value adverbs in {\tt PLOTR}. {\it 2025-01-28}
  \item\ {\tt TECOR} was changed to issue a warning about leaving the
    reliable model behind (date $> 2025.0$) only once. {\it 2025-01-19}
  \item\ {\tt TEPLT} was changed to use finer plot range limits on {\tt
    DIFF}\@. {\it 2025-01-19}
  \item\ {\tt ZACTV9.C} had a C error preventing compilation on the
    latest compilers. {\it 2025-01-19}
  \item\ {\tt FITTP} and {\tt FITAB} were changed to write Slice ({\tt
    SL}) files as pseudo-FITS tables.  {\tt FITLD}, {\tt UVLOD}, and
    {\tt IMLOD} were changed to read them back in. {\it 2025-03-06}
  \item\ {\tt SYPRT} was corrected to handle page size limitations and
    to loop over IFs, polarizations, and data types properly. {\it
      2025-13-11}
  \item\ {\tt POSSM} had issues with frequency labeling when the IFs
    were not all contiguous. {\it 2025-03-12}
  \item\ {\tt PLRFI}, {\tt VBRFI}, {\tt VLBRF} did not make plot files
    properly with more than one subplot per page. {\it 2025-03-18}
  \item\ {\tt PRTSY} did not sort the {\tt SY} table correctly. {\it
    2025-03-19}
  \item\ {\tt SGDESTR} left a file open, blocking many functions in {\tt
    AIPS}\@. {\it 2025-03-19}
  \item\ {\tt FITAB} and {\tt FITTP} attempted to write the history file
    as a table making an error message. {\it 2025-03-26}
  \item\ New OFMs have been added for use in {\tt OFMGET}. {\it
    2025-04-03}
  \item\ {\tt SPFLG}, {\tt FTFLG} wrote incorrect flags to the flag
    table when doing clip in sub-images.  {\it 2025-04-23}
  \item\ {\tt NOIFS} output one too many channels and set the reference
    channel one too high. {\it 2025-05-05}
  \item\ {\tt LISTR} did not handle arrays with more than 50 antennas
    well.  Fixed both {\tt LIST} and {\tt MATX} listings. {\it
      2025-05-07}
  \item\ {\tt BPEDT} did not check times when deleting {\tt BP} table
    records. {\it 2025-06-23}
  \item\ {\tt IMEAN} counted overflow pixels in the highest plotable box
    rather than one higher.{\it 2025-07-16}
  \item\ {\tt ELINT} in {\tt DOPLOT=3} mode did not copy the solution to
    all IFs. {\it 2025-07-18}
  \item\ {\tt CLCOR} died when the {\tt CT} table times are all zero as
    in old VLBA data sets. {\it 2025-07-31}
  \item\ {\tt BPLOT} confused linear polarization V with Stokes V.
    Labels improved also. {\it 2025-08-06}
  \item\ {\tt FITLD} passed the wrong array to find the {\tt MC} table
    parameters.  {\tt HANNING} tapered data were affected.  Added code
    to detect 256-level antennas and skip the {\tt DIGICOR} for
    them. {\it 2025-09-11}
  \item\ {\tt VPLOT} did not compute amplitude rms correctly.  Added
    phase rms to the possible plot items. {\it 2025-10-14}
\end{enumerate}
\vfill\eject

\section{\AIPS\ systems shipping}

Rather than produce a blank page, we include the chart of systems
shipped.


\begin{center}
\begin{tabular}{|rrrrrrrr|}
\hline
 & & & & & {\tt TST} & {\tt NEW} & Total \\
\noalign{\vspace{-1mm}}
year & {\tt TST} name & {\tt NEW} name & \hspace{1em}{\tt TST} &
 \hspace{1em}{\tt NEW} & binary & binary & unique \\
\hline
2004 & {\tt 31DEC04} & {\tt 31DEC03} &  808 & 196 &      &     & 1276 \\
2005 & {\tt 31DEC05} & {\tt 31DEC04} &  832 & 246 &  299 &  48 & 1460 \\
2006 & {\tt 31DEC06} & {\tt 31DEC05} &  806 & 191 &  402 &  94 & 1398 \\
2007 & {\tt 31DEC07} & {\tt 31DEC06} &  965 & 277 &  669 & 161 & 1811 \\
2008 & {\tt 31DEC08} & {\tt 31DEC07} & 1058 & 246 &  986 & 303 & 2107 \\
2009 & {\tt 31DEC09} & {\tt 31DEC08} & 1228 & 307 & 1082 & 478 & 2399 \\
2010 & {\tt 31DEC10} & {\tt 31DEC09} & 1228 & 307 & 1203 & 477 & 2416 \\
2011 & {\tt 31DEC11} & {\tt 31DEC10} & 1105 & 270 & 1064 & 424 & 2228 \\
2012 & {\tt 31DEC12} & {\tt 31DEC11} &  940 & 284 & 1028 & 396 & 1698 \\
2013 & {\tt 31DEC13} & {\tt 31DEC12} & 1014 & 307 &  990 & 443 & 1937 \\
2014 & {\tt 31DEC14} & {\tt 31DEC13} & 1045 & 333 &  848 & 431 & 1843 \\
2015 & {\tt 31DEC15} & {\tt 31DEC14} & 1104 & 309 & 1001 & 350 & 1817 \\
2016 & {\tt 31DEC16} & {\tt 31DEC15} &  878 & 222 &  788 & 372 & 1330 \\
2017 & {\tt 31DEC17} & {\tt 31DEC16} &  874 & 408 &  768 & 386 & 1383 \\
2018 & {\tt 31DEC18} & {\tt 31DEC17} &  684 & 368 &  603 & 343 & 1099 \\
2019 & {\tt 31DEC19} & {\tt 31DEC18} &  754 & 406 &  686 & 388 & 1155 \\
2020 & {\tt 31DEC20} & {\tt 31DEC19} &  796 & 434 &  750 & 470 & 1230 \\
2021 & {\tt 31DEC21} & {\tt 31DEC20} &  659 & 399 &  604 & 376 & 1215 \\
2022 & {\tt 31DEC22} & {\tt 31DEC21} &  590 & 226 &  572 & 221 &  965 \\
2023 & {\tt 31DEC23} & {\tt 31DEC22} &  597 & 239 &  596 & 243 &  896 \\
2024 & {\tt 31DEC24} & {\tt 31DEC23} &  470 & 284 &  480 & 272 &  678 \\
2025 & {\tt 31DEC25} & {\tt 31DEC24} &  500 & 180 &  512 & 187 &  613 \\
\hline
\end{tabular}
\end{center}

%\vspace*{4in}
%\centerline{This page deliberately left blank.}
\vfill\eject

% Order form and mailer page
%\cleardoublepage
\pagestyle{empty}
%\hphantom{...}
%\vfill\eject
\vbox to 4.4in{
\vspace{12pt}
%\centerline{\rotatebox{-90}{\resizebox{!}{3.5in}{%
%\includegraphics{FIG/Mandrill.color.plt}}}}
\centerline{\resizebox{!}{3.5in}{\includegraphics{FIG/Mandrill.eps}}}
\vspace{12pt}
\centerline{{\huge \tt \AIPRELEASE}}
\vspace{12pt}
\vfill}
\phantom{...}
\centerline{\resizebox{!}{!}{\includegraphics{FIG/AIPSLETS.PS}}}

\end{document}

\begin{figure}
\centering
%\resizebox{!}{3.4in}{\gname{uvpltuv}\hspace{0.1cm}\gname{uvpltbf}}
\resizebox{!}{3.4in}{\gbb{516,541}{uvpltuv}\hspace{0.1cm}\gbb{524,550}{uvpltbf}}
\caption[{\tt UVPLT} displays]{{\tt \tndx{UVPLT}} displays of where
the data were observed in the \uv\ plane (left) and of the visibility
amplitudes as a function of baseline length (right).  The data on
3C336 were provided by Alan Bridle from observations made with the VLA
on 6 December 1987.\Iodx{plot file}}
\label{fig:uvplt}
\end{figure}

\vfill
\end
