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<h3><a name="tcubeExamples">B.27.2 Examples</a></h3>
<p>
<dl>
<dt><strong><pre>
stilts tcube in=2QZ_6QZ_pubcat.fits out=ccm.fits \
cols='Bj_R U_Bj Bj' binsizes='0.05 0.05 0.5' bounds='-2:1 -3:2 :'
</pre></strong></dt>
<dd>Calculates a 3-dimensional colour-colour-magnitude grid from
three existing columns in a table. The bin (pixel) sizes are specified.
The data bounds are specified explicitly for the (first two)
colour dimensions, but for the (third) magnitude dimension it is
determined from the minimum and maximum values the data in
that column of the table.
The output is a three-dimensional FITS cube.
</dd>
<dt><strong><pre>
stilts tcube in=iras_psc.vot out=iras_psc_map.fits \
icmd='addskycoords fk5 galactic ra dec glat glon' \
cols='glat glon' nbins='400 200'
</pre></strong></dt>
<dd>Calculates a map of object densities in galactic coordinates from
a catalogue of IRAS point sources. The output is a two-dimensional
FITS image representing the sky in galactic coordinates.
Bounds are determined automatically from the data, and the number of
pixels in each dimension (400 in latitude and 200 in longitude) are
specified, which means that the pixel sizes don't have to be.
Since the input table contains sky positions in equatorial
coordinates rather than galactic ones, the <code>addskycoords</code>
filter is used to preprocess the data before the cube generation
step (see <a href="filterSteps.html">Section 6.1</a>).
</dd>
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<hr><i>STILTS - Starlink Tables Infrastructure Library Tool Set<br>Starlink User Note256<br>STILTS web page:
<a href="http://www.starlink.ac.uk/stilts/">http://www.starlink.ac.uk/stilts/</a><br>Author email:
<a href="mailto:m.b.taylor@bristol.ac.uk">m.b.taylor@bristol.ac.uk</a><br>Mailing list:
<a href="mailto:topcat-user@jiscmail.ac.uk">topcat-user@jiscmail.ac.uk</a><br></i></body>
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