Commit 016ff94a authored by Danny Boxhoorn's avatar Danny Boxhoorn
Browse files

Version from 2007/01/31

parent b4e05a81
Fri Apr 1 2005 Claus Goessl <cag@usm.uni-muenchen.de>
Mon Jan 15 2007 Johannes Koppenhoefer <koppenh@mpe.mpg.de>
* cvs checkin as module and autoconf extension
......
......@@ -261,8 +261,8 @@ base functions are read from the files "cc???.fits". </dd>
<center><i>
This task was implemented by A. Riffeser<br>
Dokumentation maintained by J. Koppenhfer<br>
This file was last time updated on 21 Mar 2005
Documentation maintained by J. Koppenhfer<br>
This file was last time updated on 15 Jan 2007
</i></center>
<hr>
......
<html><head><title>errortoweight</title></head>
<body bgcolor="#ffffff">
<hr>
<font size="7"><b>errortoweight</b></font>
<hr>
<!-- NAME -->
<h2>NAME</h2>
<p> errortoweight -- convert an MDia error image into a Sextractor weight map </p><br>
<!-- USAGE -->
<h2>USAGE</h2>
<p>
<tt>errortoweight [flags] </tt><br><br>
<table width="10%" cellpadding="0" cellspacing="0" border="0">
<tbody>
<tr><td align="left"> input </td><td align="center"> i </td><td align="right">
"" </td></tr>
<tr><td align="left"> output </td><td align="center"> o </td><td align="right">
"" </td></tr>
</tbody>
</table>
</p><br>
<!-- PARAMETERS -->
<h2>PARAMETERS</h2>
<dl>
<dt> input = "" </dt>
<dd> The input MDia error image filename. </dd>
</dl>
<dl>
<dt> output = "" </dt>
<dd> The output Sextractor weight map filename.</dd>
</dl><br>
<!-- DESCRIPTION -->
<h2>DESCRIPTION</h2>
<p>
The task errortoweight reads a MDia error image (specified by the <tt>i</tt>-flag) which contains the 1 sigma
error values for each pixel. This image is transformed into a sigma<sup>-2</sup> image
(which can be used e.g. as a Sextractor weight map) and written to a file (specified by the <tt>o</tt>-flag).</pre>
</p><br>
<!-- INPUT -->
<h2>INPUT</h2>
<p> A MDia error image. </p><br>
<!-- OUTPUT -->
<h2>OUTPUT</h2>
<p> A weight map. </p><br>
<!-- EXAMPLES -->
<h2>EXAMPLE</h2>
<p> errortoweight -i my_error_image.fits -o my_weight_map.fits <p>
<hr>
<center><a href="overview.html">Task index</a></center>
<center><i>
This task was implemented by J. Koppenhfer<br>
Documentation maintained by J. Koppenhfer<br>
This file was last time updated on 15 Jan 2007
</i></center>
<hr>
</body></html>
\ No newline at end of file
<html><head><title>make_mask</title></head>
<body bgcolor="#ffffff">
<hr>
<font size="7"><b>make_mask</b></font>
<hr>
<!-- NAME -->
<h2>NAME</h2>
<p> make_mask -- create a fits file to be used for masking of variable stars </p><br>
<!-- USAGE -->
<h2>USAGE</h2>
<p>
<tt>make_mask [flags] </tt><br><br>
<table width="13%" cellpadding="0" cellspacing="0" border="0">
<tbody>
<tr><td align="left"> varlist </td><td align="center"> v </td><td align="right">
"" </td></tr>
<tr><td align="left"> output </td><td align="center"> o </td><td align="right">
"" </td></tr>
<tr><td align="left"> image </td><td align="center"> i </td><td align="right">
"" </td></tr>
<tr><td align="left"> radius </td><td align="center"> r </td><td align="right">
5,10 </td></tr>
<tr><td align="left"> x_column </td><td align="center"> x </td><td align="right">
2 </td></tr>
<tr><td align="left"> flux_column </td><td align="center"> f </td><td align="right">
5 </td></tr>
</tbody>
</table>
</p><br>
<!-- PARAMETERS -->
<h2>PARAMETERS</h2>
<dl>
<dt> varlist = "" </dt>
<dd> Input list of variable objects. </dd>
</dl>
<dl>
<dt> output = "" </dt>
<dd> Output mask filename. </dd>
</dl>
<dl>
<dt> image = "" </dt>
<dd> Reference frame filename. The <tt>NAXIS</tt> header keywords are beeing read from
this file and used as dimensions of the mask. </dd>
</dl>
<dl>
<dt> radius = 5,10 </dt>
<dd> Minimum and maximum masking radius. A mask radius is assigned to each
variable object according to its flux value specified in the input list of
variable stars. The brightest star will get the maximum radius whereas the
faintest variable in the input list will be masked with the minimum
radius. Inbetween the radii are linearily distributed. </dd>
</dl>
<dl>
<dt> x_column = 2 </dt>
<dd> This number specifies the column which contains the x positions of the
objects to be masked. The column of the y positions is assumed to be
<tt>x_column</tt> + 1. </dd>
</dl>
<dl>
<dt> flux_column = 5 </dt>
<dd> This number specifies the column which contains the fluxs of the
objects to be masked. </dd>
</dl><br>
<!-- DESCRIPTION -->
<h2>DESCRIPTION</h2>
<p>
The task make_mask creates a mask containing 0 and 1 values which can be used (e.g. during the difference
imaging process) to mask out variable objects. The dimensions of the mask will
be identical to the reference image specified by the <tt>image</tt>-flag.
In the beginning the x-, y- and flux-values are read from the input list of
variable objects specified by the <tt>varlist</tt>-flag. The list format must be
ASCII. The x-values must be in column <tt>x_column</tt>, the y-values in the
following column and the flux values in the column specified by the
<tt>flux_column</tt>-flag. Around each variable object position a circular
region is masked with a radius according to the object flux. The brightest star
will get the maximum radius (second value specified by <tt>radius</tt>-flag) whereas the
faintest variable in the input list will be masked with the minimum
radius (first value specified by <tt>radius</tt>-flag). Inbetween the radii are
linearily distributed. </pre>
</p><br>
<!-- INPUT -->
<h2>INPUT</h2>
<p> Reference frame, list of variable objects. </p><br>
<!-- OUTPUT -->
<h2>OUTPUT</h2>
<p> Mask (fits file). </p><br>
<!-- EXAMPLES -->
<h2>EXAMPLE</h2>
<p> make_mask -o mask.fits -v variables.tbl -x 2 -f 6 -i reference.fits -r 15,40 <p>
<hr>
<center><a href="overview.html">Task index</a></center>
<center><i>
This task was implemented by J. Koppenhöfer<br>
Documentation maintained by J. Koppenhöfer<br>
This file was last time updated on 17 Jan 2007
</i></center>
<hr>
</body></html>
\ No newline at end of file
<html><head><title>mupipe - Task Index</title></head>
<html><head><title>MDia - Task Index</title></head>
<body bgcolor="#ffffff">
<center><font size="7"><b>
mupipe - Task Index
MDia - Task Index
</b></font></center>
<hr>
......@@ -14,28 +14,46 @@ mupipe - Task Index
<li><a href="diffima.html">
<b>diffima</b></a> -- compute difference images
</li>
<li><a href="errortoweight.html">
<b>errortoweight</b></a> -- convert an MDia error image into a Sextractor weight map
</li>
<li><a href="getsky.html">
<b>getsky</b></a> -- skysubtract image
</li>
<li><a href="prepare.html">
<b>prepare</b></a> -- create initial error images according to photon noise
</li>
<li><a href="make_mask.html">
<b>make_mask</b></a> -- create a fits file to be used for masking of variable stars
</li>
<li><a href="select_stars.html">
<b>select_stars</b></a> -- select isolated reference stars from an input table
</li>
<li><a href="skycalc.html">
<b>skycalc</b></a> -- photometrically align images
</li>
<li><a href="starphot.html">
<b>starphot</b></a> -- photometry tool
<b>starphot</b></a> -- measure PSF
</li>
<li><a href="subby.html">
<b>subby</b></a> -- replace masked regions and optionally do weighted stacking of images
<b>subby</b></a> -- replace masked regions and do weighted stacking of images
</li>
<li><a href="usmphot.html">
<b>usmphot</b></a> -- do iterative PSF-photometry
</li>
<li><a href="wcscut.html">
<b>wcscut</b></a> -- cut/expand images to common region
</li>
<li><a href="weight.html">
<b>weight</b></a> -- compute optimal stacking weights from background and seeing
<b>weight</b></a> -- compute optimal stacking weights from background rms and seeing
</li>
</ul>
<hr>
<center><i>
Dokumentation maintained by J. Koppenhfer<br>
This file was last time updated on 28 Nov 2006
Documentation maintained by J. Koppenhfer<br>
This file was last time updated on 17 Jan 2007
</i></center>
</body></html>
\ No newline at end of file
<html><head><title>weight</title></head>
<body bgcolor="#ffffff">
<hr>
<font size="7"><b>weight</b></font>
<hr>
<!-- NAME -->
<h2>NAME</h2>
<p> weight -- compute optimal stacking weights from background and seeing </p><br>
<!-- USAGE -->
<h2>USAGE</h2>
<p>
<tt>weight [flags] images</tt><br><br>
<table width="20%" cellpadding="0" cellspacing="0" border="0">
<tbody>
<tr><td align="left"> factor </td><td align="center"> f </td><td align="right"> 10000.0 </td></tr>
<tr><td align="left"> reg </td><td align="center"> r </td><td align="right"> 380:490,310:460 </td></tr>
</tbody>
</table>
</p><br>
<!-- PARAMETERS -->
<h2>PARAMETERS</h2>
<dl>
<dt> factor = 10000.0 </dt>
<dd> the weight are scaled up with this factor in order to make them "human readable". </dd>
</dl>
<dl>
<dt> reg = 380:490,310:460 </dt>
<dd> Region in which the sky background errors are measured in the input errorframes.</dd>
</dl><br>
<!-- DESCRIPTION -->
<h2>DESCRIPTION</h2>
<p>
The task weight gets the seeing condidions s(i) of all the input images by reading the header keyword <tt>PSF-FWHM</tt> and measures the sky
background b(i) in the input errorframes using a region specified by the <tt>reg</tt>-flag. Each input image gets a factor a(i) which is written to
the header of the input images with the keyword <tt>ALPHA</tt>. The weights are calculated as:<br>
<pre> (i) = ( s(i) * b(i) )<sup>-2</sup></pre>
</p><br>
<!-- OUTPUT -->
<h2>OUTPUT</h2>
<p> No output! Only the keyword <tt>ALPHA</tt> is added to the headers of all input images. </p><br>
<!-- EXAMPLES -->
<h2>EXAMPLE</h2>
<p> weight -r 324:343,373:391 stars_*.fits <p>
<hr>
<center><a href="overview.html">Task index</a></center>
<center><i>
This task was implemented by A. Riffeser<br>
Dokumentation maintained by J. Koppenhöfer<br>
This file was last time updated on 24 Feb 2005
</i></center>
<hr>
</body></html>
\ No newline at end of file
<html><head><title>weight</title></head>
<body bgcolor="#ffffff">
<hr>
<font size="7"><b>weight</b></font>
<hr>
<!-- NAME -->
<h2>NAME</h2>
<p> weight -- compute optimal stacking weights from background and seeing </p><br>
<!-- USAGE -->
<h2>USAGE</h2>
<p>
<tt>weight [flags] images</tt><br><br>
<table width="20%" cellpadding="0" cellspacing="0" border="0">
<tbody>
<tr><td align="left"> factor </td><td align="center"> f </td><td align="right"> 10000.0 </td></tr>
<tr><td align="left"> reg </td><td align="center"> r </td><td align="right"> 380:490,310:460 </td></tr>
</tbody>
</table>
</p><br>
<!-- PARAMETERS -->
<h2>PARAMETERS</h2>
<dl>
<dt> factor = 10000.0 </dt>
<dd> the weight are scaled up with this factor in order to make them "human readable". </dd>
</dl>
<dl>
<dt> reg = 380:490,310:460 </dt>
<dd> Region in which the sky background errors are measured in the input errorframes.</dd>
</dl><br>
<!-- DESCRIPTION -->
<h2>DESCRIPTION</h2>
<p>
The task weight gets the seeing condidions s(i) of all the input images by reading the header keyword <tt>PSF-FWHM</tt> and measures the sky
background b(i) in the input errorframes using a region specified by the <tt>reg</tt>-flag. Each input image gets a factor a(i) which is written to
the header of the input images with the keyword <tt>ALPHA</tt>. The weights are calculated as:<br>
<pre> (i) = ( s(i) * b(i) )<sup>-2</sup></pre>
</p><br>
<!-- OUTPUT -->
<h2>OUTPUT</h2>
<p> No output! Only the keyword <tt>ALPHA</tt> is added to the headers of all input images. </p><br>
<!-- EXAMPLES -->
<h2>EXAMPLE</h2>
<p> weight -r 324:343,373:391 stars_*.fits <p>
<hr>
<center><a href="overview.html">Task index</a></center>
<center><i>
This task was implemented by A. Riffeser<br>
Dokumentation maintained by J. Koppenhöfer<br>
This file was last time updated on 24 Feb 2005
</i></center>
<hr>
</body></html>
\ No newline at end of file
......@@ -218,8 +218,8 @@ magnitude-column is added to the output table. </p><br>
<center><i>
This task was implemented by A. Riffeser<br>
Dokumentation maintained by J. Koppenhöfer<br>
This file was last time updated on 1 Apr 2005
Documentation maintained by J. Koppenhöfer<br>
This file was last time updated on 15 Jan 2007
</i></center>
<hr>
......
<html><head><title>weight</title></head>
<body bgcolor="#ffffff">
<hr>
<font size="7"><b>weight</b></font>
<hr>
<!-- NAME -->
<h2>NAME</h2>
<p> weight -- compute optimal stacking weights from background and seeing </p><br>
<!-- USAGE -->
<h2>USAGE</h2>
<p>
<tt>weight [flags] images</tt><br><br>
<table width="20%" cellpadding="0" cellspacing="0" border="0">
<tbody>
<tr><td align="left"> factor </td><td align="center"> f </td><td align="right"> 10000.0 </td></tr>
<tr><td align="left"> reg </td><td align="center"> r </td><td align="right"> 380:490,310:460 </td></tr>
</tbody>
</table>
</p><br>
<!-- PARAMETERS -->
<h2>PARAMETERS</h2>
<dl>
<dt> factor = 10000.0 </dt>
<dd> the weight are scaled up with this factor in order to make them "human readable". </dd>
</dl>
<dl>
<dt> reg = 380:490,310:460 </dt>
<dd> Region in which the sky background errors are measured in the input errorframes.</dd>
</dl><br>
<!-- DESCRIPTION -->
<h2>DESCRIPTION</h2>
<p>
The task weight gets the seeing condidions s(i) of all the input images by reading the header keyword <tt>PSF-FWHM</tt> and measures the sky
background b(i) in the input errorframes using a region specified by the <tt>reg</tt>-flag. Each input image gets a factor a(i) which is written to
the header of the input images with the keyword <tt>ALPHA</tt>. The weights are calculated as:<br>
<pre> (i) = ( s(i) * b(i) )<sup>-2</sup></pre>
</p><br>
<!-- OUTPUT -->
<h2>OUTPUT</h2>
<p> No output! Only the keyword <tt>ALPHA</tt> is added to the headers of all input images. </p><br>
<!-- EXAMPLES -->
<h2>EXAMPLE</h2>
<p> weight -r 324:343,373:391 stars_*.fits <p>
<hr>
<center><a href="overview.html">Task index</a></center>
<center><i>
This task was implemented by A. Riffeser<br>
Dokumentation maintained by J. Koppenhöfer<br>
This file was last time updated on 24 Feb 2005
</i></center>
<hr>
</body></html>
\ No newline at end of file
<html><head><title>wcscut</title></head>
<body bgcolor="#ffffff">
<hr>
<font size="7"><b>wcscut</b></font>
<hr>
<!-- NAME -->
<h2>NAME</h2>
<p> wcscut -- cut/expand images to common region </p><br>
<!-- USAGE -->
<h2>USAGE</h2>
<p>
<tt>wcscut [flags] images </tt><br><br>
<table width="15%" cellpadding="0" cellspacing="0" border="0">
<tbody>
<tr><td align="left"> prefix </td><td align="center"> p </td><td align="right">
"cut_" </td></tr>
<tr><td align="left"> border </td><td align="center"> b </td><td align="right">
0 </td></tr>
<tr><td align="left"> expand </td><td align="center"> e </td><td align="right">
false </td></tr>
<tr><td align="left"> error </td><td align="center"> </td><td align="right">
false </td></tr>
</tbody>
</table>
</p><br>
<!-- PARAMETERS -->
<h2>PARAMETERS</h2>
<dl>
<dt> prefix = "cut_" </dt>
<dd> Output filename prefix. </dd>
</dl>
<dl>
<dt> border = 0 </dt>
<dd> Size in pixels of an additional border region in output images.</dd>
</dl>
<dl>
<dt> error = false </dt>
<dd> Apply cutting or expansion also to corresponding error images. The input error
images must have conventional filename, i.e. "e." + image filename. The output
error images are named "e." + prefix + image filename.</dd>
</dl>
<dl>
<dt> expand = false </dt>
<dd> If this flag is set, all images are expanded to the sum of the regions
covered by all input images. If not, all input images are cutted to the part that is
common to all of them.</dd>
</dl><br>
<!-- DESCRIPTION -->
<h2>DESCRIPTION</h2>
<p>
The task wcscut is used to either cut all input images to the part that is
common to all of them (<tt>expand</tt>-flag = false) or to expand them to the
sum of the regions covered by at least one of all input images (<tt>expand</tt>-flag =
true). This is done using the CRVAL and CRPIX header information. All images
must have been resamled to the same pixel grid (i.e. must have identical CD-matices).
The filenames of each cutted/expanded output image is prefix + input image filename.
If the <tt>error</tt>-flag is set true, the cutting/expansion is applied also
to the corresponding error images. These must have conventional the filename,
i.e. "e." + image filename. The filenames of each output error image is "e." +
prefix + input image filename. An additional border with zero values can be
added using the <tt>border</tt>-flag.
</p><br>
<!-- INPUT -->
<h2>INPUT</h2>