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%Body of intermediate AIPSletter for 30 June 2025 version

\documentclass[twoside]{article}
\usepackage{graphics}

\newcommand{\AIPRELEASE}{June 30, 2025}
\newcommand{\AIPVOLUME}{Volume XLV}
\newcommand{\AIPNUMBER}{Number 1}
\newcommand{\RELEASENAME}{{\tt 31DEC25}}
\newcommand{\NEWNAME}{{\tt 31DEC25}}
\newcommand{\OLDNAME}{{\tt 31DEC24}}
\newcommand{\THISYEAR}{2025}
\newcommand{\NEWYEAR}{2026}
\newcommand{\OLDYEAR}{2024}

%macros and title page format for the \AIPS\ letter.
\input LET98.MAC
%\input psfig

\newcommand{\MYSpace}{-11pt}

\normalstyle

\section{Happy 46$^{\rm th}$ birthday \AIPS\ and FITS}

The FITS format was devised in a meeting at the VLA site on March 27
and 28, 1979.  Don Wells (then of NOAO) and Eric Greisen (still of
the NRAO) were the primary authors while Barry Clark and other NRAO
staff members provided valuable suggestions.  The FITS format, enhanced
by later extensions, is still in wide spread use in astronomy and is the
envy of other scientific fields.  The FITS format then colored the
design of the \AIPS\ internal formats.  The \AIPS\ project was begun
officially on July 1, 1979 and has stood the test of time remarkably
well.

Your editor does find times when he would like interesting things to do.
If you find any problems with \AIPS\ or have any suggestions for new or
improved functions, please do not hesitate to e-mail {\tt
  daip@nrao.edu}.  Do note that the \AIPS\ web site has become a secure
({\tt https:}) web site.


\subsection{\Aipsletter\ publication}

We have discontinued paper copies of the \Aipsletter\ entirely.  The
\Aipsletter\ will be available in PostScript and pdf forms as always
from the web site listed above.  New issues will be announced in the
NRAO eNews mailing and on the bananas and MNJ list server.  Readers are
encouraged to subscribe to one of these low volume mail lists at
{\tt htps://listmgr.nrao.edu/mailman/listinfo}.

\subsection{Current and future releases}

We have formal \AIPS\ releases on an annual basis.  While all
architectures can do a full installation from the source files, Linux
(64-bit only), and MacIntosh OS/X (Intel and ARM) systems may install
binary versions of recent releases.  The last ``slushy'' release is
called \OLDNAME\@.  It gets occasional bug fixes until changes in
operating system versions force it to be frozen.  \RELEASENAME\ remains
under active development.  You may fetch and install a copy of these
versions at any time using {\it anonymous} {\tt ftp} for source-only
copies and {\tt rsync} for binary copies.  This \Aipsletter\ is intended
to advise you of improvements to date in \RELEASENAME\@. Having fetched
\RELEASENAME, you may update your installation whenever you want by
running the so-called ``Midnight Job'' (MNJ) which copies and compiles
the code selectively based on the changes and compilations we have done.
The MNJ will also update sites that have done a binary installation.
There is a guide to the install script and an \AIPS\ Manager FAQ page on
the \AIPS\ web site.

The MNJ for binary versions of \AIPS\ now uses solely the tool {\tt
  rsync} as does the initial installation.  For locally compiled
(``source'') installations, the Unix tool {\tt cvs} running with
anonymous ftp was used for the MNJ\@.  That has been replaced with
{\tt rsync} to download any changed text files.  The only installations
to still use {\tt cvs} are the four machines inside the Socorro Array
Operations Center.  Do not modify \AIPS\ text files (\eg\ Fortran tasks)
in the standard locations since {\tt rsync} will over-write them.  For
local versions, use a copy of the task and its help file in a private
disk area instead.

{\tt 31DEC20} contains a change to the TV display program {\tt XAS} that
makes it incompatible with previous releases when characters are
displayed.  {\tt 31DEC14} contains a change to the ``standard'' random
parameters in $uv$ data and adds columns to the {\tt SN} table.  Note,
however, that the random parameters written to FITS files have not been
changed.  Older releases of \AIPS\ cannot handle the new {\it internal}
$uv$ format and might be confused by the {\tt SN} table as well.  You
are encouraged to use a relatively recent version of \AIPS, whilst those
with recent VLA data to reduce should get release \OLDNAME\ or,
preferably, the latest development release.

\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, in each copy of \AIPS\
releases, and on the web at {\tt http://www.aips.nrao.edu/COPYING}.

The Linux binary version of \AIPS\ is maintained by a computer running
RedHat 8 with 64-bit load modules.  The 32-bit Linux binary release
was frozen in June 2024 and there is no \RELEASENAME\ 32-bit binary
release.  The {\tt MACINT} binary version is maintained by an old
Intel Mac mini and will be maintained until that machine dies.  It
cannot be replaced.  The {\tt MACARM} binary version is supported by an
M1 Mac mini that will have its operating system updated later this year.
At that time the \OLDNAME\ release will be frozen with no more bug fixes
so that that version will not be affected by the OS upgrade.

\section{Improvements of interest in \RELEASENAME}

We expect to continue publishing the \Aipsletter\ approximately every
six months, but the publication is now primarily electronic.  There are
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 new script
{\tt ADVCHK} to make sure that all verbs, task, and procedures are
listed in the adverb help files used by them, and {\tt ADVCNT} to
check line lengths in all help files.

\subsection{Display}

The \AIPS\ ``TV'' display ({\tt XAS}) has a rather complex internal
structure which was initially suggested by the old IIS Model 70 that we
used in the early days.  With the advent of modern computers, we have
increased the dimensions of {\tt XAS} considerably.  There are 16 memory
planes, loaded with images scaled from 0 to 8191.  Each enabled memory
is passed through a lookup table, called the LUT, in each of the three
colors.  The LUT translates the inputs to the range 0 to 2045.  At that
point all outputs of the LUT are summed and put into another three color
look up table called the OFM (output function memory).  This translates
the 0 to potentially 32735 sum into 0 to 255.  For simplicity,
\AIPS\ normally uses LUTs that are the same in all three colors to do
black-and-white enhancement \eg\ with the verb {\tt TVTRANSF}\@.  Also
for simplicity, \AIPS\ normally uses the OFM to add pseudo coloring in
the range 0 to 2045 with the same coloring applied to all memory planes.
The output from the OFM is in the range 0 to 255 which is all that the
actual terminal screen can handle.  A gamma correction is applied via
the OFM since the response of the terminal is non linear.  The verb {\tt
  TVHUEINT} is the exception to this simplicity.  It uses the LUT in
three colors to take the log of the input images and the OFM to take the
exponential of the sums, effectively multiplying the images through
color filters.

\AIPS\ supports the concept of OFM text files which list the values of
potential OFM pseudo colorings.  There are a number of verbs starting
with {\tt OFM} which allow the user to fetch, modify, and save the
OFM\@.  Verbs {\tt OFMGET} and {\tt OFMSAVE} were changed to
pseudo-verbs, allowing the immediate argument (the name) to be typed
without enclosing quite marks,  Verbs {\tt OFMADJUS} and {\tt OFMTWEAK}
were corrected to work sensibly in the range 0 to 2045. In {\tt
  31DEC25}, we have added a large number of OFM tables derived from
publicly available data using the new service program {\tt COLOR}\@.
To illustrate these tables, plus all previously available tables and any
created by the user, a new task called {\tt OFMPL} was developed.  It
has three display screens, one that shows up to 4 step wedges, one that
plots the red, green, and blue functions, and one that shows an image
with a selected pseudo coloring.  The menu in all three screens lists
every available OFM table in multiple columns.  A new verb was created
called {\tt OFMCOLOR} which allows the user to try out numerous of these
new tables; each of buttons A, B, and C can select 10 different OFMs and
the verb will list the names of each OFM selected.  It is hoped that one
or more of these will let the user bring out the desired information in
the image.  A new verb {\tt OFMSTRCH} lets the user stretch the OFM
function to the left and right.  That operation is also in {\tt
  OFMCOLOR}\@.

The option {\tt OFMCOLOR} has been added to numerous interactive tasks
along with {\tt TVPHLAME} when not already present.  This includes {\tt
  XGAUS}, {\tt AGAUS}, {\tt RMFIT}. {\tt ZEMAN}. {\tt ZAMAN}, {\tt
  TVFLG}, {\tt SPFLG}, {\tt FTFLG}, {\tt UFLAG}, {\tt TVSPC}, and {\tt
  TVIEW}\@.  Numerous \AIPS\ Memos were revised to illustrate their new
menus.  {\tt TVIEW} was revised to display either a reference image or
spectra with a menu option to switch between them.  Windows applied to
one of the displays now apply to all appropriately.

\AIPS\ reserves the value zero in all lookup tables for magic blank
pixels in the image.  {\tt TVLOAD} offers the option of interpolating
the input image with {\tt TXINC} and/or {\tt TYINC} less than zero.
That interpolation was corrected to honor the zeros strictly rather than
allowing zero to be interpolated with non-blanked pixel values.

\begin{description}
  \myitem{XPLOT} was changed to do plotting in the normal way as well as
        n  the previous plot methods.
  \myitem{SYPRT} was corrected to handle looping over IFs,
          polarizations, and data types.
  \myitem{POSSM} did not separate IFs correctly when they were not in a
          complete and regular sequence.
\end{description}

\subsection{UV data}

{\tt SPFLG}, {\tt FTFLG}, and {\tt TVFLG} have received considerable
attention also.  They were fixed to record output flags correctly when
doing clip operations in a sub window.  The displays were correct but the
output flags were not.  Pseudo coloring {\tt TVPHLAME} and {\tt OFMCOLOR}
were added.  The waterfall plots were given the option to zoom via
interpolation in both axes when the TV display is large enough to allow
it.  {\tt TVFLG} also has that option but only in the time ($y$) axis
since interpolating between baselines is meaningless.  These {\tt ALLOW
  X Y ZOOM~?} options complicated the clearing of flagged data, but the
problems with it were solved.  Clip operations now only apply to the
voxel being clipped.  Options to flag additional IFs, channels,
baselines, {\it et al.}~are ignored.  {\tt TVFIDDLE} was replaced by
{\tt TVZOOM} since {\tt TVTRANSF} is better for black-and-white
enhancement.  A long overdue \AIPS\ Memo 127 was written to describe
these tasks in detail.

{\tt SYHIS} is a new task that attempts to auto edit the SysPower ({\tt
  SY}) table while providing a large amount of diagnostic information.
It first measures and plots {\tt SY} histograms.  It then clips the {\tt
  SY} data and runs a median window filter through the values.  It
compares the data to the MW filtered values and generates new histograms
which it can plot and evaluate statistically.  It can then clip based on
the MW difference.  Finally it can run a general smooth operation
through the {\tt SY} values and replace the clipped points or all points
with the smoothed values.  This is {\tt TYSMO} but with smarts and the
ability to use different values for each IF, polarization, and antenna.
It should be regarded as experimental.

The adverb {\tt DOBAND} was added to numerous procedures in {\tt
  VLBAUTIL}\@.  Then {\tt DOBAND} and new adverb {\tt BPSOLINT} were
added to {\tt VLBARUN} to allow time-dependent bandpass solutions.
{\tt VLBARUN} was also changed to plot bandpass solutions separately for
each time in the {\tt BP} table.  {\tt VLBARUN} was also given the {\tt
  IN2NAME} {\it et al.}~adverbs and {\tt NMAPS} to allow a source model
to be used in bandpass solutions.

\vfill\eject
\begin{description}
  \myitem{LISTR} did not check solution weights in the {\tt GAIN} mode
          to make sure the data are valid.
  \myitem{NOIFS} had an error in frequency computation causing the
          output to have one too many channels with the reference channel
          being one too high.
  \myitem{TECOR} was provided with a new model of the Earth's magnetic
          field.  IGRF14 is an updated version of IGRF13 released
          because we have aged another 5 years.
  \myitem{VLAMP} and {\tt DOVLAMP} were changed to handle wide-band EVLA
          data by selecting those IFs that are needed with the VLBA
          data.
\end{description}

\subsection{Analysis}

Spectral index computations received attention with {\tt TVSPX} getting
several new options.  These included {\tt CLEAR LIST} and {\tt CHAR
  MULT} in the main menu, {\tt IMSTAT} in the image menu, and {\tt CHAN
  RANGE}, {\tt RESET CHANS}, and {\tt QUIT} in the redo menu.  A new
task {\tt LISPX} is similar to {\tt TVSPX} but takes its input from a
one-dimensional text file which can contain a third data column to give
the uncertainty.  It writes an output text file that can be used as an
input text file to the task.  New task {\tt SPXMD} was written to add
models containing spectral index to new or existing image cubes.  These
tasks are described in the new \AIPS\ Memo 126.  {\tt PLOTR} was given
the option to read a third data column and plot it as error bars.

One dimensional text files containing spectra (or other data types) can
now be read into \AIPS\ as one dimensional images using new task {\tt
  TX2IM}\@.  The new task {\tt IM2TX} reverses this process, making text
files that can be read by {\tt PLOTR}, {\tt LISPX}, and other \AIPS\ or
non-\AIPS\ programs.

The spectral model fitting tasks {\tt XGAUS}, {\tt AGAUS}, {\tt ZEMAN},
{\tt ZAMAN}, and {\tt RMFIT} have been modified significantly.  In the
edit stage, they were given the {\tt OFMCOLOR} option and an option to
add a blotch region to the pixel list for later flagging or re-fitting.
The {\tt REDO ALL} and {\tt REDO LIST} operations only do pixels that
are bright enough.  {\tt AGAUS} now resets the optical depth spectrum
array for each pixel to guarantee the correct spectrum when setting an
initial guess.  Commands are now given only with TV menus; the awkward
option to type on the terminal for basic fitting was dropped.  When
fitting spectra in the edit stage, \ie\ when doing {\tt REDO ALL} or
{\tt REDO LIST}, an additional option to flag channels is offered both
before and after a fit is attempted (except for {\tt RMFIT})\@.  That
option has its own menu and allows the user to flag and unflag ranges of
channels interactively.  The flagged and unflagged data are plotted in
different colors.  During the initial fitting, one can choose to turn
off the TV to let the task try fitting pixels more quickly.  When it
gets in trouble, it will turn TV interaction back on, often dropping
directly into setting a new guess.  {\tt XGAUS}, {\tt AGAUS}, and {\tt
  RMFIT} were changed so that the plot is in a different color when
setting a new guess, thereby making it obvious that this mode has been
entered.  \AIPS\ Memos 118 and 122 have been revised for all of these
changes.

\subsection{Imaging}

{\tt SETFC} can recommend image sizes and cell spacings.  It also can
make a list of overlapping facets on an hexagonal pattern.  An option to
generate that pattern in a rotated fashion was added.  This may produce
a better pattern of facets than the default.  Use {\tt CHKFC} and {\tt
  FLATN} to evaluate.  The TV display of images in {\tt IMAGR}, {\tt
  SCIMG} and {\tt SCMAP} was enhanced with a labeled step wedge on the
right hand side.  It is displayed whenever the image is labeled
(abs({\tt LTYPE})$ \ge\ 3$).

{\tt DFTIM} and {\tt DFTPL} were given the adverbs {\tt ANTENNAS} and
{\tt BASELINE} to limit the data included.  Adverb {\tt OPTYPE} was
added to allow the tasks to image data types other than the DFT (which
is the real part of the visibility after the shift).  {\tt DFTIM} only
was given additional {\tt OPTYPE}s to measure the difference between the
current data value and an average of the surrounding points.

\vfill\eject
\subsection{General}

The documentation provided with \AIPS\ has been systematically
maintained as well.  The new service program {\tt ADVCNT} was written to
check for long lines in all help files.  A new service script {\tt
  ADVCHK} was written, using new service programs {\tt ADVHLP} and {\tt
  ADVCHK}, to examine all help files to insure that all adverb help
files report all verbs, tasks, and procedures that use them.  A great
many help files were edited as a result.  Pre-existing service programs
were used to update the {\tt ABOUT} files and TAB-completion file.  The
\Cookbook\ was updated systematically in February and May.

\AIPS\ plot ({\tt PL}) and slice ({\tt SL}) files have complex formats
that do not lend themselves to FITS tables.  Nonetheless, in order to
allow \AIPS\ users to back up these files and recover them at a later
time, {\tt FITTP} and {\tt FITAB} were changed to write them as FITS
tables.  Each 1024-byte record is written as a row in this pseudo table
format which is then read back by {\tt FITLD}, {\tt IMLOD}, and {\tt
  UVLOD}\@.  These ``tables'' are expected to be meaningless to other
software systems, but do allow users to retain these potentially
valuable extension files.

The verb {\tt PLGET} allows a user to recover the adverbs used to make a
plot file and the format of plot files was changed in 2023 to allow this
verb to work mostly even if the adverbs to a plot task have changed.
The verb {\tt EXTLIST} tries to display information about extension
files, especially plot files.  Both verbs were updated for changes in
plot tasks again this year.

\section{Recent Memoranda}

All \AIPS\ Memoranda are available from the \AIPS\ home page.  Memo 126
is a new memo describing spectral index fitting in \AIPS\@.  Memo 127 is
a new memo describing the first interactive flagging tasks in
\AIPS\ including the latest modifications.  Memos 120, 121, and 124 have
been updated to describe added display options in interactive tasks.
Memos 118 and 122 have been revised to describe the changes in Gaussian,
Zeeman and rotation measure fitting tasks.  Memo 117 was updated to
describe the  slice files now written to FITS\@.

\begin{tabular}{lp{5.8in}}
{\bf 126} & {\bf Spectral index fitting in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  April 24, 2025\\
   &  \AIPS\ has had the task {\tt SPIXR} to fit the spectral index of
image cubes since 2005.  Beginning in the {\tt 31DEC24} release, a new
interactive task called {\tt TVSPX} became available.  It does the same
fitting as {\tt SPIXR} but then allows the user to examine the results
and to try to improve upon them.  This Memo will describe the usage of
this new task.
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 127} & {\bf Interactive flagging in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  June 12, 2025\\
   &  The first truly interactive task in \AIPS\ was {\tt TVFLG},
introduced in the late 1980s.  It enabled interactive editing primarily
of continuum data.  A similar task suited to spectral line data sets
appeared in January 1990.  This task, {\tt SPFLG}, has recently
undergone some useful changes suggesting that this family of editing
tasks should be described in a memo.
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 117} & {\bf \AIPS\ FITS File Format}\\
   &  Eric W. Greisen, NRAO\\
   &  June 24, 2025 revision, adding slice files in FITS
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 118} & {\bf Modeling Spectral Cubes in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  July 2025 revision, describing {\tt XGAUS}, {\tt ZEMAN}, and
      {\tt RMFIT}
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 120} & {\bf Exploring Image Cubes in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  April 20, 2025 revision, describing {\tt TVSPC}
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 121} & {\bf Editing on a $uv$ grid in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  April 30, 2025 revision, describing {\tt UFLAG}
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 122} & {\bf Modeling Absorption-line Cubes in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  July 1, 2025 revision, describing {\tt AGAUS} and {\tt ZAMAN}
\end{tabular}

\begin{tabular}{lp{5.8in}}
{\bf 124} & {\bf Further Exploration of Image Cubes in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  April 22, 2025 revision, describing {\tt TVIEW}
\end{tabular}


\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 locally-compiled installations.  It will also do a proper
update for binary installations.  Therefore there is no reason to
continue the old procedure.  Major bug corrections will be 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
has had a number of these ``patches'':

\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}
\end{enumerate}

\vfill\eject
\section{\AIPS\ Distribution}

We log apparent MNJ accesses and downloads of the tar balls and binary
installations.  We count these by unique IP address.  Since some systems
assign the same computer different IP addresses at different times,
this will be a bit of an over-estimate of actual sites/computers.
However, a single IP address is often used to provide \AIPS\ to a
number of computers, so these numbers are probably an under-estimate
of the number of computers running current versions of \AIPS\@.
So far in \THISYEAR\ more than 217 IP addresses have downloaded the
now slushy form of \OLDNAME, while more than 223 IP addresses have
downloaded \RELEASENAME\@.  A total of 297 different IP addresses have
appeared in one of our transaction log files.  These numbers are rather
less than those of last year at this time although the numbers for {\tt
  TST} are fairly close.

\vspace{1em}
\centerline{\resizebox{!}{4.9in}{\includegraphics{FIG/Plot2425a.eps}}}

%\vfill\eject
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  \centerline{{\huge \tt \AIPRELEASE}}
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\phantom{...}
\centerline{\resizebox{!}{!}{\includegraphics{FIG/AIPSLETS.PS}}}

\end{document}
