[gnuastro-commits] master d8ffb610: Book: some mandatory changes in building the extended PSF section

[Mohammad Akhlaghi]

branch: master
commit d8ffb6109c93d13743423036c617ef5d50f0817d
Author: Sepideh Eskandarlou <sepideh.eskandarlou@gmail.com>
Commit: Mohammad Akhlaghi <mohammad@akhlaghi.org>

    Book: some mandatory changes in building the extended PSF section
    
    Until now, there were some mistakes in the tuotrial of the making the
    extended PSF, for instance name of 'astcrop' input was incorrect, the
    kernel directory did not determinesd, the word how was repetead twice in
    the text.
    
    With this commit, the input name of 'astcrop' has been corrected, the
    directory of the kernel has been determined and finally the extra word are
    deleted.
---
 doc/gnuastro.texi | 11 ++++++-----
 1 file changed, 6 insertions(+), 5 deletions(-)

diff --git a/doc/gnuastro.texi b/doc/gnuastro.texi
index 463f688f..9f3e1728 100644
--- a/doc/gnuastro.texi
+++ b/doc/gnuastro.texi
@@ -5447,7 +5447,7 @@ To have the center identified as a single clump, we 
should mask these saturated
 To find the saturation level, let's make a smaller crop of @mymath{50\times50} 
pixels around the star with the command below, then have a look at the 
distribution of pixels with a value larger than 100 (above the noise level):
 
 @example
-$ astcrop image-crop.fits --mode=wcs --widthinpix --width=50 \
+$ astcrop saturated.fits --mode=wcs --widthinpix --width=50 \
           --center=203.3916736,46.7968652 --output=saturated-center.fits
 $ aststatistics saturated-center.fits --greaterequal=100
 Histogram:
@@ -5489,6 +5489,9 @@ Histogram:
  |********************* *** *  ***   * *****  *** *   * *** * * ********
  |----------------------------------------------------------------------
 
+@noindent
+We still see an increase in the histogram around 3000.
+Therefore, We can set the saturation level in this image@footnote{In raw 
exposures, this value is usually around 65000 (close to @mymath{2^{16}}, since 
most CCDs have 16-bit pixels). But that is not the case here, because this is a 
processed/stacked image that has been calibrated.} to 2500.
 
 $ aststatistics saturated-center.fits --greaterequal=100 --lessthan=2500
 -------
@@ -5508,8 +5511,6 @@ Histogram:
 @end example
 
 @noindent
-We still see an increase in the histogram around 3000.
-Therefore, We can set the saturation level in this image@footnote{In raw 
exposures, this value is usually around 65000 (close to @mymath{2^{16}}, since 
most CCDs have 16-bit pixels). But that is not the case here, because this is a 
processed/stacked image that has been calibrated.} to 2500.
 Let's mask all such pixels with the command below:
 
 @example
@@ -5589,7 +5590,7 @@ $ astmkprof --kernel=gaussian,2,5 --oversample=1 \
 $ astarithmetic flat/67510.fits set-i i i 2500 gt \
                 2 dilate 2 dilate 2 dilate 2 dilate nan where \
                 --output=flat/67510-no-sat.fits
-$ astconvolve flat/67510-no-sat.fits --kernel=kernel.fits \
+$ astconvolve flat/67510-no-sat.fits --kernel=label/kernel.fits \
               --domain=spatial --output=label/sat-masked-conv.fits
 $ astarithmetic label/sat-masked-conv.fits 2 interpolate-maxofregion \
                 --output=label/image-conv.fits
@@ -5618,7 +5619,7 @@ In @ref{Preparing input for extended PSF}, we described 
how to create a Segment
 So we are now ready to start building the outer parts of the PSF.
 
 First we will build the outer parts of the PSF, so we want the brightest stars.
-You will see we have several bright stars in this very large field of view, 
but we don't yet have a feeling how how many they are, and at what magnitudes.
+You will see we have several bright stars in this very large field of view, 
but we don't yet have a feeling how many they are, and at what magnitudes.
 So let's use Gnuastro's Query program to find the magnitudes of the brightest 
stars (those brighter than magnitude 12).
 For more on Query, see @ref{Query}.