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%Body of final AIPSletter for 31 December 2020
\documentclass[twoside]{article}
\usepackage{graphics}

\newcommand{\AIPRELEASE}{December 31, 2020}
\newcommand{\AIPVOLUME}{Volume XL}
\newcommand{\AIPNUMBER}{Number 2}
\newcommand{\RELEASENAME}{{\tt 31DEC20}}
\newcommand{\OLDNAME}{{\tt 31DEC19}}
\newcommand{\NEWNAME}{{\tt 31DEC21}}
\newcommand{\Tsys}{${\rm T}_{\rm sys}$}
\newcommand{\THISYEAR}{2020}
\newcommand{\NEWYEAR}{2021}
\newcommand{\OLDYEAR}{2019}


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

\newcommand{\MYSpace}{-11pt}
\normalstyle

\section{General developments in \AIPS}

\subsection{Help desk, COVID-19}

Users of the NRAO Science help desk, will notice a changed appearance.
We are using new software to manage helpdesk tickets, but we hope to
continue to provide help to our users as we have done.  Use {\tt
  https://help.nrao.edu}, the same as before.

Due to the outbreak of the COVID-19 pandemic, the NRAO went to
``infectious disease operating status'' on March 16, 2020.  Telescope
operations (other than ALMA) continued with a skeleton support staff.
On June 8 we began the first steps to return to the new normal.
Primarily, this means that those employees who could not do their jobs
properly from home have returned to work with numerous safety
precautions.  Telescope operations have continued and we have even
managed VLA re-configurations safely.  Those of us who can work from
home will continue to do so indefinitely.

This status means that 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 me.


%\subsection{Reduction of VLB,  VLA and ALMA data in \AIPS}

%\AIPS\ continues to be the main software system for the reduction of
%VLBI data from the VLBA and other telescopes.  Since 2010, there have
%been numerous improvements to \AIPS\ that enable full calibration of
%data from the Karl G. Jansky VLA and most imaging operations as well.
%The one exception is the wide-band (bandwidth synthesis) deconvolution
%algorithm (``MSMFS'') being developed in \CASA\ by Urvashi Rao
%Venkata, for which there is no comparable function in \AIPS\@.
%Calibrated $uv$ data may be exported from \AIPS\ in ``UVFITS'' format
%for use in that program.  ALMA data may also be reduced in \AIPS,
%although the package is not fully qualified to calibrate data from
%linearly-polarized feeds.  Chapter 4 of the \AIPS\ Cookbook,
%available via the \AIPS\ web site, was revised to describe the new
%calibration operations.

\subsection{\Aipsletter\ publication}

We have discontinued paper copies of the \Aipsletter\ entirely, at least
for this issue.  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.

\subsection{Current and future releases}

We have formal \AIPS\ releases on an annual basis.  We recommend a
full binary installation method for both the frozen and development
versions for MacIntosh OS/X (Intel chips only), and Linux (32- and
64-bit) systems, but all architectures can do a full installation from
the source files.  There are no longer binary versions available for
Solaris and Mac PPC chip architectures.  If you develop \AIPS\ code
locally {\it or have system managers that forbid the use of\/} {\tt
  rsync} or {\tt cvs}, you will need to do a source-level installation.
The current release is called \RELEASENAME\ and is now ``frozen.''  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 frozen 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 cvs}, {\tt rsync}, and/or transaction files 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 175-Mbyte {\tt   \NEWNAME.tar.gz} compressed tar file.
Binary installations use only {\tt rsync}, while locally compiled
versions also use {\tt cvs}.  Linux sites will almost certainly have
{\tt cvs} installed; other sites may have installed it along with
other GNU tools.  Secondary MNJs will still be possible using {\tt
  ssh} or {\tt rcp} or NFS as with previous releases.  We have found
that {\tt cvs} works very well, although it has one quirk. If a site
modifies a file locally, but in an \AIPS-standard directory, {\tt cvs}
will detect the modification and attempt to reconcile the local
version with the NRAO-supplied version.  This usually produces a file
that will not compile or run as intended.  Use a new name for the task
or put a copy of the task and its help file in a private disk area
instead.

\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}\@.


\subsection{Installing a new version}

If compiling locally, new releases must be installed from the tar ball
for that release.  {\tt 31DEC15} 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).

{\tt 31DEC09} contains a change in the format of antenna files.
Previous releases will not understand the antenna coordinates for
arrays that were traditionally left-handed (VLBI primarily).  The
format change occurs automatically when any {\tt 31DEC09} or later
antenna-file specific code reads the file, after which older releases
will have difficulties.  {\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, new tasks appeared including {\tt
FTARS} to do Q/U fitting of {\tt TARS} Faraday rotation data, {\tt
SYPRT} to print the contents of SysPower {\tt SY} tables in detail,
{\tt MASKS} to make a mask image from an \AIPS\ boxfile for input to
CASA, {\tt OFUDG} to process a UV data file applying a user-created
algorithm to the data ({\tt FUDGE} without calibration), {\tt FIXFR} to
reorder the frequencies in the spectral and IF axes to be in one
direction, {\tt BPEPL} to plot bandpass functions with multiple times
over-plotted, {\tt ACIMG} to make a frequency-time image from
auto-correlation $uv$ data, {\tt RIRMS} to find the mean and rms of the
real and imaginary parts of visibility data as a function of time and
baseline, and {\tt CDFIX} to repair catalog file headers that have been
corrupted in the keyword records.  A new verb called {\tt TV2COLOR}
implements a 2-color scheme for the \AIPS\ TV display.  A new {\tt RUN}
file called {\tt CXIMAGR} implements an experimental complex imaging
process.  In the first six months of the year new tasks appeared
including {\tt UVRMS} to compute statistics on a time series of selected
averaged visibility data, {\tt SPRMS} to plot the spectra of mean and
standard deviation of selected visibility data, {\tt MOD3D} to convert a
set of facet Clean Component files into a single ``3-dimensional''
{\tt CC} table,  {\tt PDPLT} to plot polarization D-term spectra from
multiple antennas and/or data sets, {\tt DENAN} to report and remove
NaNs from data sets, {\tt MTARS} to compute rotation measure models for
input to {\tt TARS} (the test task for {\tt FARS}), and {\tt RMTFC} to
plot the convolution of the complex rotation measure transfer function
with various RM thickness models.

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,
this is somewhat of an oversight.  We urge you to run the ``Midnight
Job'' at least once after \RELEASENAME\ is frozen 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 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{VLBI matters}

The VLB data reduction pipeline {\tt VLBARUN} continued to get attention
in the reporting period.  Since significant bad data can make {\tt
  BPASS} find erroneous solutions, the option to run {\tt CLIP} before
the {\tt BPASS} step was added.  {\tt CLIP} is, optionally, run either
just before {\tt BPASS} or just before the long {\tt FRING} step.  The
option to clip bad rates and then smooth the rates was added.  It is
done on the output of {\tt FRING}\@.  An option to self-calibrate all of
the calibration sources before the final {\tt SPLIT} was added.  This
option makes Clean images of each calibration source and then runs {\tt
  FRING} one source at a time with the resulting models.

The procedures for automatically downloading EOP (Earth orientation) and
TEC (Total electron content) data from NASA  have changed.  The
procedures in {\tt RUN} files {\tt VLBAUTIL} and {\tt VLAUTIL} were
revised to use the new method of download (with {\tt curl}) and the
new upper part of the web address.  The previous download methods and
addresses were discontinued by NASA on November 1, 2020.

\begin{description}
\myitem{FITLD} had two significant bugs corrected.  The scaling of
   auto-correlation data from the old VLBA correlator was wrong by a
   factor of order $10^6$ due to the new weight scaling.  The value of
   {\tt DIGICOR} was damaged for non-VLBA data, causing the correction
   to be omitted for any included files after the first.
\myitem{ACIMG} is a new task to grid auto-correlation data making an
   image with frequency and time on the $x$ and $y$ axes, respectively.
   It should be helpful in examining data sets for RFI\@.  See the color
   figure at the end of this section.
\end{description}

\subsection{Imaging and Display}

A scheme for imaging data in a fully complex fashion has been
implemented.  The new {\tt RUN} file {\tt CXIMAGR} implements the full
process.  {\tt UVIMG} was changed to allow uniform weighting with {\tt
  ROBUST} prior to the convolution to the grid.  The option to suppress
the use of the Hermitian property was added as was the option to make
a ``beam'' image with all the same weighting and convolution options.
{\tt FFT} was given new {\tt OPCODE}s to make images from the complex
$uv$ plane images produced by {\tt UVIMG}\@.   {\tt CXCLN} required only
minor changes to honor the input reference pixels and to actually honor
the option to write a residual image rather than the restored Clean
image.  {\tt CCMRG} and {\tt PRTCC} were changed to handle complex Clean
Component ({\tt CX}) files as well as the usual {\tt CC} files.  The
{\tt RUN} file procedure {\tt CXIMAGR} then runs {\tt UVIMG} to make
real, imaginary, and beam uv-plane images.  It {\tt FFT}'s them to make
map-plane images.  It rescales those so that the peak of the beam is
one.  Then it renames them as if they were Q and U images so that {\tt
  CXCLN} can, optionally, Clean them.  This scheme works rather well
but, I suspect, is inferior the the normal imaging done by {\tt
  IMAGR}\@.

\begin{description}
\myitem{UVPLT} was given a new axis type ``baseline'' which plots the
   data at baseline {\it i-j} and also at {\it j-i}.  It can be very
   helpful in finding questionable data.  {\tt IMSIZE} was added to
   allow control of the grid size used.
\myitem{ISPEC} and {\tt RPSEC} were changed to allow numerous circular
   and rectangular windows with {\tt NBOXES} and {\tt CLBOX}, both of
   which may be set interactively with {\tt TVBOX}.
\myitem{MASKS} is a new task to make a mask image from \AIPS' boxes in a
   {\tt BOXFILE}\@.  CASA requires a mask image rather than the list of
   circular and rectangular boxes used by \AIPS.
\myitem{TV2COLOR}\hspace{1em} is a new verb to implement an interactive,
   two-color only TV enhancement.  It should be useful for images having
   interesting negative as well as positive values such as images of Q
   and U polarization, residual images, or images of the deflection of
   the dish surface from ideal.
\myitem{TVLABEL} was corrected to preserve the data needed to plot the
   Clean beam.
\end{description}

\subsection{UV data}

\begin{description}
\myitem{RIRMS} is a new task to compute the mean and rms of the real and
   imaginary parts of the visibilities over short time intervals as a
   function of time and baseline.  It prints a matrix of the mean and
   rms of these for all antennas.  It then can plot the time series or
   the histograms for selected baselines.
\myitem{SYPRT} is a new task to print the contents of the SysPower ({\tt
   SY}) tables in glorious detail.
\myitem{BPEPL} is a new task to plot bandpass values with multiple times
   on the same plot.  This is like the plots in {\tt BPEDT} but can
   make plot files.  It uses a grid in memory to compute the plot
   efficiently.
\myitem{EDITA} and {\tt EDITR}, {\tt BPEDT}, {\tt SNEDT}, and {\tt
   PCEDT} were changed to allow use of an in-core dynamic memory to
   compute each plot before displaying it on the TV.  In complex cases,
   this will speed up the operation significantly.
\myitem{FIXFR} is a new task to re-order spectral windows and spectral
   channels so that the frequency all goes in one direction.  The VLA
   can produce spectral windows in seemingly arbitrary order.
\myitem{VLANT} was enhanced with {\tt DETIME} to limit how long after an
   observation one allows corrections to be made.
\myitem{Calibration} tasks now emit a message to say to what parameters
   calibration is being, and is not being, applied.
\end{description}

\subsection{Analysis}

\begin{description}
\myitem{FTARS} is a new task to fit Q/U values to the input spectrum
   supplied to the rotation-measure synthesis study task {\tt TARS}\@.
   It uses the algorithms of {\tt RMFIT} with the input and output files
   of {\tt TARS} to fit a complex rotation measure and polarization
   model to the data.
\myitem{HOLOG} had the math for reference pointed observations improved
   including a new option for the slope.  The default magnification was
   changed to 13 which is correct for the VLA\@.  The {\tt OFFSET} equal
   to the distance from the prime focus and the bottom of the
   sub-reflector was added as an option with 0.522 meters (VLA value) as
   the default.  The tilt parameters are now in degrees and the
   Cassegrain offsets may be included in the model.
\myitem{UVHOL} was changed to be more tolerant of small offsets from
   pure horizontal and vertical scans.
\myitem{IMFIT} and {\tt JMFIT} now allow a 40000 pixel window.
\end{description}

\subsection{General}

\begin{description}
\myitem{Help} files for adverbs were systematically updated to reference
   all verbs, tasks, and procedures using the adverb.
\myitem{\Cookbook} was updated on October 21 to account for numerous
   changes to help files and to mention new tasks and other changes.
\myitem{EXTLIST} and {\tt PLGET} were updated to account for changes to
   existing plot tasks and for the new ones.
\myitem{AIPSPATH}\hspace{1em} scripts were changed to put \AIPS\
   directories at the end of \$PATH and \$LD\_LIBRARY\_PATH variables.
   Because Mac OS X does not differentiate on case when executing
   procedures, new procedure names {\tt AIPP}, {\tt AIFC}, and {\tt
     AILINK} were created to replace the now-conflicted names for
   pre-processing, compiling, and linking \AIPS\ Fortran.
\myitem{OFUDG} is a ``new'' paraform task to process a $uv$ data set
   through a user-created algorithm without the complication of all the
   calibration adverbs.
\myitem{CDFIX} is a new stand-alone program to repair catalog header
   files which have had the keyword section (records 2 and perhaps up)
   damaged.
\myitem{RedHat 6} is no longer supported.  All Linux binaries are now
   computed on a RedHat 7 system.  Mac OS binaries are now computed on a
   10.15 system but with an option that should allow systems as old as
   10.10 to use the load modules.
\end{description}

\vfill

\centerline{\resizebox{!}{5in}{\includegraphics{FIG/ACIMG.2.eps}}}

Example of output from {\tt ACIMG}\@.  The $x$ axis is FQID (frequency
ID number) because the channel increments over all 4 spectral windows is
not entirely regular.  The time axis is labeled in days.

\eject
\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.
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 434 different IP
addresses downloaded the frozen form of \OLDNAME\ and 796 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 1230.  The table below shows these numbers as a
function of year since we began recording them.  The plot of numbers
versus time shows that 2020 exceeded 2019, perhaps from people
installing \AIPS\ to run from home.

\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 \\
\hline
\end{tabular}
\end{center}

\centerline{\resizebox{!}{3.5in}{\includegraphics{FIG/PLOTIT1920all.eps}}}

\vfill\eject

\section{Patch Distribution for \OLDNAME}

Because of the extensive use of binary installations, we now patch the
master copy of the most recently frozen version.  Older versions are
not corrected even for egregious errors.  Thus, \OLDNAME\ was patched
during \THISYEAR\ and \RELEASENAME\ will be patched as needed during
\NEWYEAR.  Your copy of them may be corrected simply by running a
Midnight Job.  Information about patches and the code may be found using
links from the main \AIPS\ web page or by  {\it anonymous} \ftp\ to the
NRAO server {\tt ftp.aoc.nrao.edu}.  Documentation about patches to a
release is placed on this site at {\tt pub/software/aips/}{\it
  release-name} and the code is placed in suitable sub-directories
below this.  Patches to older releases are kept here as well, but they
will require local compilation.

The \OLDNAME\ release is no longer available for installation and will
no longer receive patches even for egregious errors.  It had a number
of important patches during \THISYEAR.  They are
\begin{enumerate}
  \item\ {\tt BPASS} had a bad call sequence causing aborts. {\it
    2020-01-22}
  \item\ {\tt FACSET} did not include all the flux of standard
    calibration source models. {\it 2020-01-27}
  \item\ {\tt UVFIX} did not compute the aberration correction properly,
    especially when converting from B1950 to J2000.  {\it 2020-02-28}
  \item\ {\tt EVAUV} did not compute the DFT subtraction model
    correctly, aborting due to a call sequence error.  {\it 2020-03-02}
  \item\ {\tt RENUMBER} aborted if the catalog file required expansion.
    {\it 2020-03-03}
  \item\ {\tt CLIP} over counted cross-hand flags when cross-hands are
    flagged because of parallel hands.  {\it 2020-03-25}
  \item\ {\tt CLPLT, CAPLT} died when trying to self-scale plots with
    only one point. {\it 2020-04-07}
  \item\ {\tt VLBAUTIL} had an error when trying to use curl to fetch
    the EOP file.  {\it 2020-04-21}
  \item\ {\tt VLBARUN} had 2 errors when trying {\tt DOPLOT=2}  to
    make a very large number of plots.  {\it 2020-05-07}
  \item\ {\tt RLDLY} had an error when selecting data.  {\it
    2020-06-10}
  \item\ {\tt PRTSY} sorted on the wrong column when {\tt OPCODE} was
    set.  {\it 2020-06-12}
  \item\ {\tt CLCOR}  got confused on {\tt EOPS} when the {\tt CT}
    table had multiple nearly identical entries. {\it 2020-06-19}
  \item\ {\tt OMFIT} had 3 {\tt FORMAT} statements that were improper
    when writing to character string variables. {\it 2020-06-29}
  \item\ {\tt VLBAUTIL} was changed for changes in the location and
    access of the data files needed by {\tt VLBAEOPS} and {\tt
    VLBATECR}. {\it 2020-07-22}
  \item {\tt IMEAN} and {\tt TVLABEL} needed minor fixes. {\it
      2020-07-29}
  \item {\tt FITLD} had a bad scaling for auto-correlations from the old
    VLBA hardware correlator. {\it 2020-09-02}
  \item {\tt FITLD} messed up {\tt DIGICOR} for non-VLBA data for all
    files after the first. {\it 2020-12-21}
\end{enumerate}
\vfill\eject

% Order form and mailer page
%\cleardoublepage
\pagestyle{empty}
%\vfill
%\centerline{\resizebox{!}{23.3cm}{\includegraphics{FIG/AIPSORDER.PS}}}
\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}

