Changeset 770

Timestamp:

12/05/05 11:30:12 (19 years ago)

Author:

mar637

Message:

merge from Release12

Location:

trunk

Files:

• bin/install.sh (modified) (3 diffs)
• doc/README (modified) (1 diff)
• doc/cookbook.tex (modified) (26 diffs)
• web/index.html (modified) (3 diffs)

trunk/bin/install.sh

@@ -1 +1 @@
 #!/bin/sh
 
-pypath=/usr/local/lib/python2.3
+prefix=/usr/local
+pypath=${prefix}/lib/python2.3
+base=`pwd`
 
 if [ ! -d ${pypath} ]; then
@@ -18 +20 @@
    cp bin/asap /usr/local/bin
 fi
+
+if [ ! -d ${prefix}/share/asap ]; then
+    echo "creating asap data directory"
+    mkdir ${prefix}/share/asap
+fi
+
+cp share/ipythonrc-asap /usr/local/share/asap/
+
 if [ -d /usr/local/share/asap/data ]; then
     echo "removing old data directory"
@@ -23 +33 @@
 fi
 
-echo "installing asap data directory"
-cp -rf data /usr/local/share/asap
+echo "extracting and installing asap data directory"
+cd /usr/local/share/asap
+tar jxf ${base}/share/data.tar.bz2 
+echo "The asap python module has been installed in"
+echo " ${pypath}/site-packages"
+echo "asap data is in ${prefix}/share/asap"

trunk/doc/README

@@ -15 +15 @@
 =======
 
-To install simply run 
-  ./install.sh
+To install simply run (as root or 'sudo')
+  ./bin/install.sh
 which will install asap into /usr/local
 

trunk/doc/cookbook.tex

@@ -1 +1 @@
 \documentclass[11pt]{article}
 \usepackage{a4}
+\usepackage{calc}
 \usepackage[dvips]{graphicx}
 
@@ -11 +12 @@
 \setlength{\parskip}{1ex}
 
-
-\title{ATNF Spectral Analysis Package\\Cookbook }
+\title{ATNF Spectral Analysis Package\\User Guide }
 \author{Chris Phillips}
 
-
 \newcommand{\cmd}[1]{{\tt #1}}
+
+\newcommand{\asaprc}[3]{
+  \begin{minipage}[t]{45mm}#1\end{minipage}
+  \begin{minipage}[t]{30mm}\raggedright #2\end{minipage}\hspace{3mm}
+  \begin{minipage}[t]{\textwidth-75mm}#3\end{minipage}
+}
 
 \begin{document}
@@ -26 +31 @@
 ASAP is a single dish spectral line processing package currently being
 developed by the ATNF. It is intended to process data from all ATNF
-antennas, and can probably be used for other antnnas if they can
+antennas, and can probably be used for other antennas if they can
 produce ``Single Dish FITS'' format. It is based on the AIPS++
 package.
@@ -45 +50 @@
 \end{itemize}
 
-To start asap log onto one of these Linux hosts and  enter
+To start asap log onto one of these Linux hosts and enter
 
 \begin{verbatim}
@@ -87 +92 @@
 There can be many objects of the same type. Each object is referred to
 by a variable name made by the user. The name of this variable is not
-important and can be set to whatever the user prefers (ie ``s'' and
+important and can be set to whatever the user prefers (i.e. ``s'' and
 ``ParkesHOH-20052002'' are equivalent).  However, having a simple and
 consistent naming convention will help you a lot.
@@ -113 +118 @@
   ASAP> av = scans(msk,weight='tsys')
   ASAP> av = scans(mask=msk,weight='tsys')
-  ASAP> av = scans(msk,True)
+  ASAP> av = scans(msk,tsys)
   ASAP> scans.polybaseline(mask=msk, order=0, insitu=True)
   ASAP> scans.polybaseline(msk,0,True)
@@ -128 +133 @@
 \subsection{Interactive environment}
 
-ipython has a number of useful interactive features and a few things to be aware
-of for the new user.
+ipython has a number of useful interactive features and a few things
+to be aware of for the new user.
 
 \subsubsection{String completion}
@@ -157 +162 @@
 fail with an syntax error.
 
+\subsubsection{Variable Names}
+
+During normal data processing, the user will have to create named
+variables to hold spectra etc. These must conform to the normal python
+syntax, specifically they cannot contain ``special'' characters such
+as \@ \$ etc and cannot start with a number (but can contain numbers).
+Variable (and function) names are case sensitive.
+
 \subsubsection{Unix Interaction}
 
@@ -221 +234 @@
   scantable.save             : 'ASAP'
 
-
   # default frequency frame to set when function
   # scantable.set_freqframe is called
@@ -229 +241 @@
   scantable.autoaverage      : True
 \end{verbatim}
+
+For a complete list of \cmd{.asaprc} values, see the appendix.
 
 \section{Scantables}
@@ -340 +354 @@
 
 Examples are the selection of beam, IF and polarisation,  spectral unit
-(e.g. km/s) frequency reference frame (e.g. BARY) and velocity Doppler
+(e.g. km/s), frequency reference frame (e.g. BARY) and velocity Doppler
 type (e.g. RADIO).
 
@@ -405 +419 @@
 
 \begin{verbatim}
-  # Select for specified source/IF
-  ASAP> scans.set_restfreqs(freqs=1.667359e9, source='NGC253', theif=0)
-
-  # Select for all sources and IFs
-  ASAP> scans.set_restfreqs(freqs=1.667359e9)
-\end{verbatim}
-
+  # Set rest frequency for all IFs
+  ASAP> scans.set_restfreqs(freqs=[1.6654018e9,1.667359e9,])
+
+\end{verbatim}
 
 In both of the above modes, you can also specify the rest frequencies via
@@ -422 +433 @@
   ASAP> scans.set_restfreqs(lines=['OH1665','OH1667'])
 \end{verbatim}
-
 
 
@@ -581 +591 @@
 %How and when?
 \subsection{Auto quotient}
-Quotients can becomputed ``automatically''. This requires the data to have matching source/reference pairs or one refrence for multiple sources.
+Quotients can be computed ``automatically''. This requires the data to
+have matching source/reference pairs or one reference for multiple
+sources. Auto quotient assumes reference scans have a trailing ``\_R''
+in the source name for data from Parkes and Mopra, and a trailing
+``e'' or ``w'' for data fro, Tidbinbilla.
 
 \begin{verbatim}
@@ -645 +659 @@
 
 The default is to use integration time weighting. The alternative is
-to use none, variance , Tsys weighting or Tsys \& integration time.
+to use none, variance, Tsys weighting or Tsys \& integration time.
 
 \begin{verbatim}
@@ -675 +689 @@
 
 The function \cmd{auto\_poly\_baseline} can be used to automatically
-baseline your data with out having to specify channel ranges for
-the line free data. It automatically figures out the line-free
-emission and fits a polynomial baseline to that data. The user can use
-masks to fix the range of channels or velocity range for the fit as
-well as mark the band edge as invalid.
+baseline your data without having to specify channel ranges for the
+line free data. It automatically figures out the line-free emission
+and fits a polynomial baseline to that data. The user can use masks to
+fix the range of channels or velocity range for the fit as well as
+mark the band edge as invalid.
 
 Simple example
@@ -727 +741 @@
 \subsubsection{Brightness Units}
 
-RPFITS files to not contain any information as to whether the telescope
+RPFITS files do not contain any information as to whether the telescope
 calibration was in units of Kelvin or Janskys.  On reading the data a
 default value is set depending on the telescope and frequency of
@@ -772 +786 @@
 As higher frequencies (particularly $>$20~GHz) it is important to make
 corrections for atmospheric opacity and gain-elevation effects.
+
+{\em Note that currently the elevation is not written correctly into
+Tidbinbilla rpfits files. This means that gain-elevation and opacity
+corrections will not work until a work around is implemented.}
 
 Gain-elevation curves for some telescopes and frequencies are known to
@@ -819 +837 @@
 \cmd{perif} argument. By default it will align each source and freqid
 separately. This is needed for scan tables containing multiple
-sources. However if scan-based Doppler tracking has been made at the observatory,
-each row will have a different freqid. In these cases run with
-\cmd{perif=True} and all rows of a source will be aligned to the same
-frame. In general \cmd{perif=True} will be needed for most
+sources. However if scan-based Doppler tracking has been made at the
+observatory, each row will have a different freqid. In these cases run
+with \cmd{perif=True} and all rows of a source will be aligned to the
+same frame. In general \cmd{perif=True} will be needed for most
 observations as Doppler tracking of some form is made at Parkes, Tid
 and Mopra.
@@ -927 +945 @@
 \section{Plotter}
 
-Scantable spectra can be plotter at any time. An asapplotter object is
+Scantable spectra can be plotted at any time. An asapplotter object is
 used for plotting, meaning multiple plot windows can be active at the
 same time. On start up a default asapplotter object is created called
@@ -1155 +1173 @@
 \subsection{Simple Calibration}
 
-{\em Currently the receiver position angle is not stored in the RPFITS
-file. This severely hampers correct handling of polarimetry. In the future
-we aim to define a general framework and populate the RPFITS files
-with the data required for transparent polarimetric calibration.}
+{\em Currently the receiver position angle is not read from the RPFITS
+file and a position angle of zero is assumed. This severely hampers
+correct handling of polarimetry. In the future we aim to define a
+general framework and populate the RPFITS files with the data required
+for transparent polarimetric calibration.}
 
 It is possible that there is a phase offset between polarisation which
@@ -1199 +1218 @@
 
 \begin{verbatim}
-  ASAP> plotter.set_cursor(pol=[``I'',''Q'']
-  ASAP> plotter.set_cursor(pol=[``RR'',''LL'']
-  ASAP> plotter.set_cursor(pol=[``XX'',''YY'']
-  ASAP> plotter.set_cursor(pol=[``I'',''Plinear'']
+  ASAP> plotter.set_cursor(pol=``I Q'')
+  ASAP> plotter.set_cursor(pol=``RR LL'')
+  ASAP> plotter.set_cursor(pol=``XX YY'')
+  ASAP> plotter.set_cursor(pol=``I Plinear'')
 \end{verbatim}
 
@@ -1220 +1239 @@
 \end{verbatim}
 
-\section{Function Summary}
+
+\section{Scantable Mathematics}
+
+It is possible to to simple mathematics directly on scantables from
+the command line using the \cmd{+, -, *, /} operators as well as their
+cousins \cmd{+=, -= *=, /=}. This works between two scantables or a
+scantable and a float. (Note that it does not work for integers).
+
+\begin{verbatim}
+  ASAP> sum = scan1+scan2
+  ASAP> scan2 = scan1+2.0
+  ASAP> scan *= 1.05
+\end{verbatim}
+
+\section{Scripting}
+
+Because asap is based on python, it easy for the user write their own
+scripts and functions to process data. This is highly recommended as
+most processing of user data could then be done in a couple of steps
+using a few simple user defined functions. A Python primer is beyond
+the scope of this userguide. See the asap home pages for a scripting
+tutorial or the main python website for comprehensive documentation.
+
+\hspace{1cm} http://www.atnf.csiro.au/computing/software/asap/tutorials
+\hspace{1cm} http://www.python.org/doc/Introduction.html
+
+\subsection{Running scripts}
+
+The asap global function \cmd{execfile} reads the named text file and
+executes the contained python code. This file can either contain
+function definitions which will be used in subsequent processing or
+just a set of commands to process a specific dataset.
+
+\subsection{asapuserfuncs.py}
+
+The file $\sim$/.asap/asapuserfuncs.py is automatically read in when
+asap is started. The user can use this to define a set of user
+functions which are automatically available each time asap is
+used. The \cmd{execfile} function can be called from within this file.
+
+\section{Worked examples}
+
+In the following section a few examples of end-to-end processing of
+some data in asap are given. 
+
+\subsection{Mopra}
+
+\subsection{Parkes Polarimetry}
+
+The following example is processing of some Parkes polarmetric
+observations of OH masers at 1.6~GHz. Because digital filters where
+used in the backend, the baselines are stable enough not to require a
+quotient spectra. The 4~MHz bandwidth is wide enough to observe both
+the 1665 and 1667~MHz OH maser transitions. Each source was observed
+once for about 10 minutes. Tsys information was not written to the
+rpfits file (a nominal 25K values was used), so the amplitudes need
+to be adjusted based on a separate log file. A simple user function is
+used to simplify this, contained in a file called mypol.py:
+
+\begin{verbatim}
+def xyscale(data,xtsys=1.0,ytsys=1.0,nomtsys=25.0) :
+
+ data.set_cursor(pol=0)
+ data.scale(xtsys/nomtsys,allaxes=False)
+
+ data.set_cursor(pol=1)
+ data.scale(ytsys/nomtsys,allaxes=False)
+
+ data.set_cursor(pol=2)
+ data.scale((xtsys+ytsys)/(2*nomtsys),allaxes=False)
+
+ data.set_cursor(pol=3)
+ data.scale((xtsys+ytsys)/(2*nomtsys),allaxes=False)
+\end{verbatim}
+
+The typical asap session would be
+
+\begin{verbatim}
+  
+# Remind ourself the name of the rpfits files
+ls 
+
+# Load data from an rpfits file
+d1665 = scantable('2005-10-27_0154-P484.rpf')
+
+# Check what we have just loaded
+d1665.summary
+
+# View the data in velocity
+d1665.set_unit('km/s')
+d1665.set_freqframe('LSRK')
+
+# Correct for the known phase offset in the crosspol data
+d1665.rotate_xyphase(-4)
+
+# Create a copy of the data and set the rest frequency to the 1667 MHz 
+# transition
+d1667 = d1665.copy()
+d1667.set_restfreqs(lines=['OH1667'])
+d1667.summary
+
+# Copy out the scan we wish to process
+g351_5 = d1665.get_scan('351p160')
+g351_7 = d1667.get_scan('351p160')
+
+# Plot the data
+plotter.plot(g351_5,g351_7) # Only shows one panel
+
+# Tell the plotter to stack polarisation and panel scans
+plotter.set_mode('p','s')
+
+# Correct for the Tsys using our predefined function
+execfile('mypol.py') # Read in the function
+xyscale(g351_5,23.2,22.7) # Execute it on the data
+xyscale(g351_7,23.2,22.7)
+
+# Only plot the velocity range of interest
+plotter.set_range(-30,10)
+
+# Baseline the data
+msk = g351_5.create_mask([-20,-15],[0,5])
+g351_5.poly_baseline(msk,1)
+msk = g351_7.create_mask([-20,-15],[0,5])
+g351_7.poly_baseline(msk,1)
+
+# Update the plot with the baselined data
+plotter.plot()
+
+# Look at the various polarisation products
+plotter.set_cursor(pol='RR LL')
+plotter.set_cursor(pol='I Plinear')
+plotter.set_cursor(pol='I Q U V')
+
+# Save the plot as postscript
+plotter.save('g361_stokes.ps')
+
+# Save the process spectra
+g351_5.save('junk5.asap')
+g351_7.save('junk7.asap')
+
+\end{verbatim}
+
+\subsection{Tidbinbilla}
+
+The following example is processing of some Tidbinbilla observations
+of NH$_3$ at 12~mm. Tidbinbilla has (at the time of observations) a
+single polarisation, but can process two IFs simultaneously. In the
+example, the first half of the observation was observing the (1,1) and
+(2,2) transitions simultaneously). The second half observed only the
+(4,4) transition due to bandwidth limitations. The data is position
+switched, observing first an reference to the west, then the source
+twice and finally reference to the east.
+
+\begin{verbatim}
+
+# Load the rpfits file and inspect
+d = scantable('2003-03-16_082048_t0002.rpf')
+print d
+
+# Make the quotient spectra
+q = d.auto_quotient()
+print q
+
+# Plot/select in velocity
+q.set_freqframe('LSRK')
+q.set_unit('km/s')
+
+# Seperate data from the (1,1)&(2,2) and (4,4) transitions
+g1 = q.get_scan(range(6))     # Rows 0..5
+g2 = q.get_scan(range(6,12))  # Rows 6..11
+
+# Align data in velocity 
+g1.freq_align(perif=True)
+g2.freq_align(perif=True)
+
+# Average individual scans
+a1 = g1.average_time()
+a2 = g2.average_time()
+
+# Rpfits file only contrains a single rest frequency. Set both
+a1.set_restfreqs(freqs= [23694.4700e6,23722.6336e6])
+
+plotter.plot(a1,a2)
+plotter.set_mode('i','s')
+x = raw_input()
+
+a1.auto_poly_baseline()
+a2.auto_poly_baseline()
+
+plotter.plot()
+
+a1.smooth('gauss',5)
+a2.smooth('gauss',5)
+plotter.plot()
+
+\end{verbatim}
+
+\newpage
+
+\section{Appendix}
+
+\subsection{Function Summary}
 
 \begin{verbatim}
@@ -1341 +1561 @@
         execfile            - execute an asap script, e.g. execfile('myscript')
         list_rcparameters   - print out a list of possible values to be
-                              put into $HOME/.asaprc
+                              put into \$HOME/.asaprc
         mask_and,mask_or,
         mask_not            - boolean operations on masks created with
@@ -1359 +1579 @@
 \end{verbatim}
 
-\section{Scantable Mathematics}
-
-It is possible to to simple mathematics directly on scantables from
-the command line using the \cmd{+, -, *, /} operators as well as their
-cousins \cmd{+=, -= *=, /=}. This works between two scantables or a
-scantable and a float. (Note that it does not work for integers).
-
-\begin{verbatim}
-  ASAP> sum = scan1+scan2
-  ASAP> scan2 = scan1+2.0
-  ASAP> scan *= 1.05
-\end{verbatim}
-
-%\section{Scripting}
-
-%Malte to add something
-
-\section{Appendix}
-
 \subsection{Installation}
 
@@ -1399 +1600 @@
 \subsection{.asaprc settings}
 
+\asaprc{verbose}{{\bf True}/False}{Print verbose output}
+
+\asaprc{insitu}{{\bf True}/False}{Apply operations on the input
+scantable or return new one}
+
+% plotting
+
+\asaprc{useplotter}{{\bf True}/False}{Preload a default plotter}
+
+\asaprc{plotter.gui}{{\bf True}/False}{Do we want a GUI or plot to a
+file}
+
+\asaprc{plotter.stacking}{{\bf Pol} Beam IF Scan Time}{Default mode for
+colour stacking}
+
+\asaprc{plotter.panelling}{Pol Beam IF {\bf Scan} Time}{Default mode
+for panelling}
+
+\asaprc{plotter.ganged}{{\bf True}/False}{Push panels together, to
+share axislabels}
+
+\asaprc{plotter.decimate}{True/{\bf False}}{Decimate the number of
+points plotted by a factor of nchan/1024}
+
+% default colours/linestyles
+%\asaprc{plotter.colours}{.}{.}
+%\asaprc{plotter.linestyles{.}{.}
+
+% scantable
+\asaprc{scantable.save}{{\bf ASAP} SDFITS FITS ASCII MS2}{Default output
+format when saving} 
+
+\asaprc{scantable.autoaverage}{{\bf True}/False}{Auto averaging on
+read}
+
+\asaprc{scantable.freqframe}{{\bf LSRK} TOPO BARY etc}{default
+frequency frame to set when function scantable.set\_freqframe is
+called}
+
+\asaprc{scantable.allaxes}{{\bf True}/False}{Apply action to all axes
+not just the cursor location}
+
+\asaprc{scantable.plotter}{{\bf True}/False}{Use internal plotter}
+
+\asaprc{scantable.verbosesummary}{True/{\bf False}}{Control the level
+of information printed by summary}
+
 \end{document}
+

trunk/web/index.html

@@ -44 +44 @@
 line observations</em>. At this stage it is tuned towards data from
 ATNF instruments and reads/writes <em>rpfits, sdfits and ms</em> data.
-A release 1.2 of ASAP is available on linux systems at ATNF
 <a href="intro.html">more...<a>
+
+<h2>Current Release</h2>
+ASAP latest stable version 1.2 was released on November, 30<sup>th</sup> 2005. It can be obtained in the <a href="#download">Download</a> section.
 
 <h2>Screenshots</h2>
@@ -66 +68 @@
 
 <h2>Documentation</h2>
-ASAP has a cookbook for general use, and a reference manual for people
-who want to write scripts to reduce and analyse their data.
+ASAP has a user guide for general use and telescope specific examples,
+and a reference manual for people who want to write scripts to reduce
+and analyse their data.
 <ul>
   <li> List of commands <a href="commands.html">(html)</a> </li>
-  <li> Cookbook  <a href="cookbook/">(html)</a> or Cookbook <a href="cookbook.pdf">(pdf)</a></li>
+  <li> User Guide<a href="userguide/">(html)</a> or User Guide <a href="userguide.pdf">(pdf)</a></li>
   <li> Reference manual <a href="refman/">(html)</a> <a href="refman.pdf">(pdf)</a></li>
   <li><a href="tutorials/">Tutorials</a></li>
@@ -78 +81 @@
 <p>
 
-<h2>Download</h2>
-
+<a name="download"><h2>Download</h2></a>
+ASAP source code and binaries are available in the <a href="http://www.atnf.csiro.au/pub/software/asap/">ATNF ftp area</a>
 <ul>
-  <li> The current release source code snapshot <a
+  <li>Current stable release source code snapshot <a
       href="ftp://ftp.atnf.csiro.au/pub/software/asap/asap_src.tar.bz2">asap source</a> </li>
-  <li> A binary tar archive <a
+  <li> A binary tar archive of the latest stable release<a
       href=ftp://ftp.atnf.csiro.au/pub/software/asap/asap_linux.tar.bz2>linux binary</a>.
       You will need to have the following libraries:<br>
       gcc-3.3, blas, lapack, g2c, boost_python and of course
       python2.3.<br>
-      The matplotlib python module has to be installed too.      
+      The matplotlib python module has to be installed too.
   </li>
   <li>For Mac OSX 10.4 follow <a href="./osx.html">these instructions.</a>