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%Body of final AIPSletter for 31 December 2018

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

\newcommand{\AIPRELEASE}{December 31, 2018}
\newcommand{\AIPVOLUME}{Volume XXXVIII}
\newcommand{\AIPNUMBER}{Number 2}
\newcommand{\RELEASENAME}{{\tt 31DEC18}}
\newcommand{\OLDNAME}{{\tt 31DEC17}}
\newcommand{\NEWNAME}{{\tt 31DEC19}}
\newcommand{\Tsys}{${\rm T}_{\rm sys}$}

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

\newcommand{\MYSpace}{-11pt}

\normalstyle

\section{Sad news}

We are sorry to report that Leonia Kogan passed away on November 18 in
Mt.~Vernon, Washington.  He retired from NRAO in 2012 after working
for NRAO for nearly 20 years, most of that assisting the \AIPS\
project.  His first {\tt CHANGE.DOC} entry was May 21, 1993.  He was a
mathematician by training and temperament and solved many of our most
difficult, mathematically-based issues.  Most recently he worked on
{\tt FARS}, implementing NRAO's first Faraday Rotation Synthesis
algorithm.  But he is also well known for {\tt UVFIX} which computes
$u,v,w$ from antenna locations and time with much trusted accuracy and
for several correction functions in {\tt CLCOR}, most notably that for
the position of the Earth's pole.  He is widely known for his work on
array configurations, represented in \AIPS\ by tasks {\tt CONFI}
(array optimization) and {\tt UVCON} (array simulation)\@.  VLBI data
calibration received a lot of his attention through tasks such as {\tt
  FRMAP}, {\tt PCCOR}, {\tt PCLOD}, {\tt ACCOR}, {\tt COHER}, {\tt
  DELZN}, and {\tt ATMCA} as well as work on handling orbiting
antenn\ae.  He developed {\tt UVRFI} to excise RFI from EVLA data and
did substantial work on tasks {\tt VPLOT}, {\tt SPLAT}, {\tt FGPLT},
{\tt ELINT}, and {\tt RMSD}\@.  Leonia's name appears on very many
entries in {\tt CHANGE.DOC} encompassing a much wider range of matters
than the list given above would suggest and reflecting his ready
willingness to help wherever he was needed.  Leonia is missed.


\section{General developments in \AIPS}

\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\ other than for
libraries and NRAO staff.  The \Aipsletter\ will be available in
PostScript and pdf forms as always from the web site listed above and
will be shipped with all distributions of \AIPS\@.  It will be
announced on the bananas and MNJ list servers and, usually, in the
NRAO e-News mailing.

\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
\RELEASENAME\ 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 2019 to convert your copy of \RELEASENAME\ into the frozen version.
However, when patches to \RELEASENAME\ are announced in 2019, 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 135-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 2018 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.  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\@.

%\vfill\eject
\section{Improvements of interest to users in \RELEASENAME}

In the latter half of 2018, new tasks appeared including {\tt PDEDT}
to flag the polarization D term table data and visibility data, {\tt
  PEEK} to solve for updates to VLA pointing parameters, {\tt TGREP}
to examine a user's {\tt TGET} files for usage of a specified task,
{\tt TVIEW} to display a spectral-line cube interactively in all 3
transpositions, and {\tt SNBLP} to display calibration tables in
baseline form, \ie\ as they would apply to data.  A new verb {\tt
  SCAT} was added to list all scratch files and a new procedure {\tt
  OKCOLORS} was added to set colors for {\tt LWPLA} that use less
printer ink.  New tasks in the first half of 2018 include {\tt TLCAL}
to convert VLA telcal files into an initial {\tt SN} table, {\tt
  XYDIF} to solve for the X minus Y phase difference for linear
polarization data, {\tt PLOTC} to display the colors used by various
tasks on {\tt DO3COLOR TRUE} with labeling to show which polarization,
spectral window, channel, and/or source goes with which color, and
{\tt SPFIX} to make a spectral cube from the intensity and spectral
index images produced by {\tt SPIXR}\@.

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: Miscellaneous}

\begin{description}
\myitem{FITLD} was changed to offer the {\tt DOWEIGHT} option to set
     data weights to more reasonable values (\ie\ scaled by
     integration time and bandwidth).  The maximum number of sources
     was raised to 10000.
\myitem{CLCOR} was changed to get the {\tt EOPS} option to handle
     correctly concatenated data sets with messy groups of times in
     the {\tt CT} table.
\myitem{DTSIM} was changed to enable Nasmyth mount antennas and to
     handle polarization properly.  In both cases, correct code was
     present in the task but the access to it was flawed.  Added the
     option to correct for parallactic angle or not.
\myitem{VPLOT} was changed to detect good data no matter what its
     weight and the bandpass routines were changed to ignore the
     outermost channels even for VLB data.
\myitem{BSCAN} was corrected for inaccuracy in data times and now gets
     more correct results.
\myitem{VLBAUTIL} procedures for EOPS and TECR were changed to allow
     the user to download the data files in advance.  {\tt VLBARUN}
     was updated to support these options.
\end{description}

\subsection{UV data: Miscellaneous}

\begin{description}
\myitem{FRING} and {\tt RLDLY} were given a new option to allow the
     user to specify which IFs should have the same delay and rate.
     This allows the groups to have different numbers of IFs, an
     option in frequent use on the VLA\@.  {\tt PIPEAIPS} was updated
     to support this option.  {\tt RLDLY} was given the option to
     average over all times when {\tt SOLINT < 0}.
\myitem{PDEDT} is a new interactive task to edit polarization D-term
     tables and, optionally, the corresponding $uv$ data.  Since the
     {\tt PD} table does not contain source or time information, the
     user must specify the sources and time range to be flagged.
\myitem{BPEDT} was changed to allow editing on {\tt BP} table weights,
     to allow more colors (\ie\ times), to reduce the number of
     messages and flags generated, to defend the user from excessive
     {\tt FLAG ABOVE} and {\tt FLAG BELOW} commands, and to improve
     the finding of samples selected by the user.
\myitem{EDITR} was changed to correct an error affecting the last data
     time.  The whole edit class had the improved finding of samples
     algorithm added.
\myitem{Table} sorting can request very large buffers, so the maximum
     size of I/O buffers was increased to 256 Mega words.
\myitem{SETJY} was given more synonyms for the new special sources
     (3C380, Cygnus A, etc.) added to the flux information.
\myitem{Polarization} calibration was corrected to handle failed
     solutions, flagging appropriate data.
\myitem{RLDIF} was changed to include a modest frequency dependence
     for the polarization angle of 3C286 and the values for 3C48 and
     3C147 were corrected (they used those for 3C138!).
\myitem{PEEK} is a new task to read VLA pointing correction files to
     determine updates to the VLA pointing parameters.  It replaces a
     stand-alone program having less certain maintenance.
\myitem{OOSUB} was corrected so that it can work with one source read
     from a  multi-source data set.
\myitem{UVHOL} was changed to improve the labeling of plots, to have
     the option to scale amplitudes by the flux in the source table,
     and to label the output data columns.  {\tt HOLOG} reads that
     label and now can handle real/imaginary as well as
     amplitude/phase.
\myitem{CQ} tables are now provided with \AIPS\ data files read in by
     {\tt BDF2AIPS}\@.  They are used to correct amplitudes for delay
     errors when post-correlation frequency averaging is done.  The
     code was changed to correct VLA data as well as VLBI data.  This
     has led to a number of annoying messages when the {\tt CQ} data
     are not available when one would like them to be.
\myitem{BPWAY} was given an option to control how input weights are
     used (or not).
\myitem{REWAY} was given the option to substitute the average
     cross-hand weight found for all weights.  Parallel-hand
     visibilities can appear noisier than they are due to real source
     structure.
\end{description}

\subsection{Imaging and Display: Miscellaneous}

\begin{description}
\myitem{IMAGR} was corrected to use and output the simple average
     frequency when the spectral-index option is invoked.  A more
     carefully computed frequency is used otherwise.
\myitem{TVIEW} is a new interactive task to display a spectral-line
     cube in all 3 transpositions along with an optional reference
     image.  \AIPS\ Memo 124, describing its use, was written.
\myitem{SNBLP} is a new task to plot {\tt SN} and {\tt CL} table
     solutions on a baseline basis, \ie\ as they would be applied to
     data.  Phases that appear noisy on an antenna basis may not
     appear noisy on all baselines.  This is the basis of the {\tt
       JUMP} option in {\tt SNFLG}.
\myitem{XYRATIO} caused some plot tasks to make plot symbols with
     different sizes in the two axes.  This was corrected.
\myitem{OKCOLORS} \hspace{1em} is a new built-in procedure designed to
     make suitable colors for {\tt LWPLA} but with a white rather than
     black background.
\myitem{LISTR} can now display azimuth.  Previously it could do only
     elevation and parallactic angle.
\myitem{PLOTC} was enhanced to support {\tt BPEDT} and {\tt PCEDT}.
\end{description}

\subsection{General}

\begin{description}
\myitem{\Cookbook} chapters were updated in July and August for
     various minor updates and a new appendix covering holography and
     VLA-specific tasks was written.
\myitem{SCAT} is a new verb that lists any scratch files over all
     disks.
\myitem{TGREP} is a new task which reads {\tt TGET} files for all
     users and reports any usage of the specified task including date
     and time.  This is helpful in finding when you last used tasks.
\myitem{GO} and {\tt TPUT} made an error in communicating parameters
     to the task data file when the adverbs exactly filled an integer
     number of disk records.  {\tt RLDLY} caused this error to be
     found when {\tt BPARM} was added.
\myitem{EXTLIST} and {\tt PLGET} were updated to include support for
     {\tt BPEDT}, {\tt PCEDT}, {\tt PEEK}, and {\tt LOCIT}.
\end{description}

\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 2018, a total of 368 different IP
addresses downloaded the frozen form of \OLDNAME\ and 684 IP
addresses downloaded \RELEASENAME\ in tarball or binary form.  Fully
461 IP addresses accessed the NRAO cvs master.  Each of these has at
least installed some version of \AIPS, but with the change to the MNJ
we are unable even to guess how many sites have run the MNJ\@.  The
total number of unique IP addresses in these three lists was 1099.
The table below shows these numbers as a function of year since we
began recording them.  The plot of numbers versus time shows that 2017
and 2018 were very similar for the first half of the year but then
2018 fell off the 2017 pace.


\begin{center}
\begin{tabular}{|rrrrrrrrr|}
\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 &
 \hspace{1em}{\tt cvs} & unique \\
\hline
2004 & {\tt 31DEC04} & {\tt 31DEC03} &  808 & 196 &      &     &  797
 & 1276 \\
2005 & {\tt 31DEC05} & {\tt 31DEC04} &  832 & 246 &  299 &  48 &  982
 & 1460 \\
2006 & {\tt 31DEC06} & {\tt 31DEC05} &  806 & 191 &  402 &  94 & 1050
 & 1398 \\
2007 & {\tt 31DEC07} & {\tt 31DEC06} &  965 & 277 &  669 & 161 & 1385
 & 1811 \\
2008 & {\tt 31DEC08} & {\tt 31DEC07} & 1058 & 246 &  986 & 303 & 1667
 & 2107 \\
2009 & {\tt 31DEC09} & {\tt 31DEC08} & 1228 & 307 & 1082 & 478 & 1855
 & 2399 \\
2010 & {\tt 31DEC10} & {\tt 31DEC09} & 1228 & 307 & 1203 & 477 & 1914
 & 2416 \\
2011 & {\tt 31DEC11} & {\tt 31DEC10} & 1105 & 270 & 1064 & 424 & 1747
 & 2228 \\
2012 & {\tt 31DEC12} & {\tt 31DEC11} &  940 & 284 & 1028 & 396 & 1309
 & 1698 \\
2013 & {\tt 31DEC13} & {\tt 31DEC12} & 1014 & 307 &  990 & 443 & 1264
 & 1937 \\
2014 & {\tt 31DEC14} & {\tt 31DEC13} & 1045 & 333 &  848 & 431 & 1023
 & 1843 \\
2015 & {\tt 31DEC15} & {\tt 31DEC14} & 1104 & 309 & 1001 & 350 & 1070
 & 1817 \\
2016 & {\tt 31DEC16} & {\tt 31DEC15} &  878 & 222 &  788 & 372 &  761
 & 1330 \\
2017 & {\tt 31DEC17} & {\tt 31DEC16} &  874 & 408 &  768 & 386 &  644
 & 1383 \\
2018 & {\tt 31DEC18} & {\tt 31DEC17} &  684 & 368 &  603 & 343 &  461
 & 1099 \\
\hline
\end{tabular}
\end{center}

\vfill\eject
% \centerline{\resizebox{!}{4.7in}{\includegraphics{FIG/Plot1718.eps}}}

\section{Recent \AIPS\ Memoranda}

All \AIPS\ Memoranda are available from the \AIPS\ home page.  \AIPS\
Memo 124 was written to describe the usage of the new spectral-line
viewer {\tt TVIEW}\@.

\begin{tabular}{lp{5.8in}}
{\bf 124} & {\bf Further Exploration of Image Cubes in \AIPS}\\
   &  Eric W. Greisen, NRAO\\
   &  November 15, 2018\\
   &  \AIPS\ has powerful tasks to fit models to the spectral axis of
  image cubes.  Tasks like {\tt XGAUS} and {\tt RMFIT} are easier to
  run if the user is already familiar with the general structure of
  the data cube.  Task {\tt TVSPC} was written to explore data cubes
  with emphasis on plots of spectra.  Now a new task {\tt TVIEW} has
  been written to explore data cubes with displays of
  position-velocity transpositions of the data cube.  This task
  provides an additional exploration tool within the \AIPS\
  environment, rather than requiring users to export their cubes to
  one or more of the many excellent visualization tools now available.
  {\tt TVIEW} offers the option of rotating the image in the celestial
  axes so that the position-velocity curves may be viewed along axes
  pertinent to the source, \eg\ the major axis.
\end{tabular}

\vspace{0.25in}
\centerline{\resizebox{!}{4.7in}{\includegraphics{FIG/TVIEWb.eps}}}
\vspace{0.25in}
Screen shot from {\tt TVIEW}: HI moment-zero reference image with
image cube in 3 transpositions.  The images are labeled, the reference
image has been sub-imaged, Y and S planes have been changed by a {\tt
  ROAM} in the lower right image.

\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 2018 and \RELEASENAME\ will be patched as needed during 2019.
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 2018.  They are
\begin{enumerate}
  \item\ Linear polarization handling applied the parallactic angle
      twice. {\it 2018-01-09}
  \item\ Batch has not worked for some years. {\it 2018-01-16}
  \item\ {\tt CALIB} would not use {\tt SMODEL} on multi-source data
      sets  {\it 2018-01-16}
  \item\ {\tt UVSUB} did not do {\tt OPCODE 'MODL'} correctly for
      multiple facets.  {\it 2018-01-20}
  \item\ {\tt SETJY} printed erroneous error bars with the latest 2017
      flux scale. {\it 2018-03-01}
  \item\ {\tt UVSUB} did not do {\tt OPCODE 'MODL'} correctly; weights
      came out zero.  {\it 2018-03-14}
  \item\ Large gridded models did not allocate sufficient memory. {\it
      2018-04-04}
  \item\ Antenna file reformatting in place failed on files with large
      numbers of IFs. {\it 2018-04-04}
  \item\ {\tt FITLD} did not correct duplicate FQ IDs properly. {\it
      2018-04-04}
  \item\ {\tt DBAPP} had an old version of the data pointers and
      failed to copy modern data properly.  {\it 2018-04-09}
  \item\ {\tt FQUBE} wrote many {\tt CG} tables when none were input.
      {\it 2018-04-23}
  \item\ {\tt FITLD} did not handle antenna files properly when
      concatenating. {\it 2018-04-24}
  \item\ {\tt DOBAND 3} interpolation flagged too much data with
      failed bandpass solutions. {\it 2018-04-27, 2018-06-26}
  \item\ Model computation made errors in DFT mode when 4
      polarizations were being computed. {\it 2018-06-20}
  \item\ {\tt UVSUB} did not do {\tt MODL} correctly with compressed
      data. {\it 2018-06-20}
  \item {\tt DOBAND 3} interpolation flagged still too much data when
      there were failed bandpass solutions and the {\tt LNX64} version
      confused the compiler. {\it 2018-06-26}
  \item {\tt DOPOL} true did not handle magic blanks in the
      polarization solutions. {\it 2018-07-16}
  \item {\tt OOSUB} did not handle multi-source files correctly.  {\it
      2018-08-10}
  \item {\tt AIPS} did not do {\tt TPUT} correctly when there was an
     exact alignment of the number of adverb values with record
     boundaries.  {\it 2018-08-17}
  \item {\tt RM} could not handle more than 5 or 10 spectral channels
     due to a very small buffer.  {\it 2018-10-03}
  \item {\tt RLDIF} used the wrong position angles for 3C48 and 3C147.
     {\it 2018-12-18}
\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}

