[gnuastro-commits] master 14dae7b1 1/2: Book: corrected a few minor typos

[Mohammad Akhlaghi]

branch: master
commit 14dae7b115341ff53ad5c55e1f014a19b34e09a5
Author: Raul Infante-Sainz <infantesainz@gmail.com>
Commit: Mohammad Akhlaghi <mohammad@akhlaghi.org>

    Book: corrected a few minor typos
    
    Until now, there were a few very minor typos in the book that I noticed
    while reading these sections.
    
    With this commit, I have corrected them.
---
 doc/gnuastro.texi | 12 ++++++------
 1 file changed, 6 insertions(+), 6 deletions(-)

diff --git a/doc/gnuastro.texi b/doc/gnuastro.texi
index d2422ec2..5b710df7 100644
--- a/doc/gnuastro.texi
+++ b/doc/gnuastro.texi
@@ -7821,7 +7821,7 @@ astcrop "$base"_convolved_scaled.fits --zeroisnotblank \
         --mode=img --section=$st_edge:*-$edge,$st_edge:*-$edge
 
 # Add noise to the image.
-$ astarithmetic "$base"_convolved_scaled_cropped.fits \
+astarithmetic "$base"_convolved_scaled_cropped.fits \
                 7 18 mag-to-counts mknoise-sigma-from-mean \
                 --output=out.fits
 
@@ -29656,8 +29656,8 @@ So to see the discussions below in action (on real 
data), see @ref{Measuring the
 
 Here, we will review some of the most commonly used methods to quantify the 
limits in astronomical data analysis and how MakeCatalog makes it easy to 
measure them.
 Depending on the higher-level analysis, there are more tests that must be 
done, but these are relatively low-level and usually necessary in most cases.
-In astronomy, it is common to use the magnitude (a unit-less scale) and 
physical units, see @ref{Brightness flux magnitude}.
-Therefore the measurements discussed here are commonly used in units of 
magnitudes.
+In astronomy, it is common to use the magnitude (a unit-less scale) and the 
flux (physical units), see @ref{Brightness flux magnitude}.
+The measurements discussed here are commonly used in units of magnitudes.
 
 @menu
 * Standard deviation vs Standard error::  Differnece between these important 
measures.
@@ -29814,7 +29814,7 @@ Note that the @mymath{10.0} below was reported as 
``standard deviation'' in the
 
 @dispmath{\sigma_{\bar{x}}\approx\frac{\sigma}{\sqrt{N}} = \frac{10.0}{200} = 
0.05}
 
-Therefore the standard error of the mean is directly related to the number of 
pixels you used to measure the mean
+Therefore the standard error of the mean is directly related to the number of 
pixels you used to measure the mean.
 You can test this by changing the @code{200}s in the commands above to smaller 
or larger values.
 As you make larger and larger images, you will be able to measure the mean 
much more precisely (the standard error of the mean will go to zero).
 But no matter how many pixels you use, the standard deviation will always be 
the same.
@@ -29825,7 +29825,7 @@ Within MakeCatalog, the options related to 
dispersion/error in the measurements
 For example @option{--std} or @option{--sigclip-std}.
 These return the standard deviation of the values within a label.
 If the underlying object (in the noise) is flat, then this will be the 
@option{\sigma} that is mentioned above.
-However, no object in astronomy in flat!
+However, no object in astronomy is flat!
 So this option should be used with extreme care!
 It only makes sense in special contexts like measuring the radial profile 
where we assume that the values at a certain radius have the same flux (see 
@ref{Generate radial profile}).
 
@@ -29840,7 +29840,7 @@ You can use @ref{NoiseChisel} to generate such an image.
 
 If the underlying profile and sky standard deviations is flat, then 
@option{--sum-error} will be the standard deviation that we discussed in this 
section and @option{--mean-error} will be the standard error.
 When the values are different, the combined error is calculated by adding the 
variances (second power of the standard deviation) of each pixel, added with 
its value.
-When the values are smaller than one a correction is applied (that is defined 
in Section 3.3 of Akhlaghi and Ichikawa @url{https://arxiv.org/abs/1505.01664, 
2015}).
+When the values are smaller than one, a correction is applied (that is defined 
in Section 3.3 of Akhlaghi and Ichikawa @url{https://arxiv.org/abs/1505.01664, 
2015}).
 @end table
 
 @node Magnitude measurement error of each detection, Surface brightness error 
of each detection, Standard deviation vs Standard error, Quantifying 
measurement limits