[gnuastro-commits] master 3a7a50c: Minor corrections in the book indexs

[Mohammad Akhlaghi]

branch: master
commit 3a7a50c10ca5c33b0676d327e07d5cc531c9473e
Author: Mohammad Akhlaghi <address@hidden>
Commit: Mohammad Akhlaghi <address@hidden>

    Minor corrections in the book indexs
    
    Some duplications in the index were corrected in the book.
---
 doc/gnuastro.texi | 28 +++++++++++++---------------
 1 file changed, 13 insertions(+), 15 deletions(-)

diff --git a/doc/gnuastro.texi b/doc/gnuastro.texi
index c9987d8..cfcb4f6 100644
--- a/doc/gnuastro.texi
+++ b/doc/gnuastro.texi
@@ -1085,7 +1085,7 @@ their recipients to know that what they have is not what 
we distributed,
 so that any problems introduced by others will not reflect on our
 reputation.
 
address@hidden GNU General Public License
address@hidden GNU General Public License (GPL)
 @cindex GNU Free Documentation License
 The full text of the licenses for the Gnuastro book and software can be
 respectively found in @ref{GNU General Public address@hidden
@@ -2231,10 +2231,9 @@ night's measurements on the ecliptic.
 @node General program usage tutorial, Detecting large extended targets, Sufi 
simulates a detection, Tutorials
 @section General program usage tutorial
 
address@hidden HST
 @cindex XDF survey
address@hidden Hubble Space Telescope
address@hidden Extreme Deep Field survey
address@hidden Hubble Space Telescope (HST)
address@hidden eXtreme Deep Field (XDF) survey
 Measuring colors of astronomical objects in broad-band or narrow-band
 images is one of the most basic and common steps in astronomical
 analysis. Here, we will use Gnuastro's programs to detect objects in a
@@ -4519,8 +4518,7 @@ KISS principle ("keep it simple, stupid") as the general 
guideline, and
 focuses on elegance, code correctness, minimalism and simplicity, and
 expects the user to be willing to make some effort to understand the
 system's operation''. Arch Linux uses ``Package manager'' (Pacman) to
-manage its packages. Please run the following command to install Gnuastro's
-mandatory and optional dependencies:
+manage its packages.
 @example
 $ sudo pacman -S ghostscript libtool libjpeg libtiff libgit2 \
                                                              \
@@ -8117,7 +8115,7 @@ statistics).
 @cindex Bias current
 @cindex Subaru Telescope
 @cindex Hyper Suprime-Cam
address@hidden Hubble Space Telescope
address@hidden Hubble Space Telescope (HST)
 For raw image processing, a single tessellation/grid is not sufficient. Raw
 images are the unprocessed outputs of the camera detectors. Modern
 detectors usually have multiple readout channels each with its own
@@ -9912,7 +9910,7 @@ to significantly reduce the run time.
 @cindex Image mosaic
 @cindex COSMOS survey
 @cindex Imaging surveys
address@hidden Hubble Space Telescope
address@hidden Hubble Space Telescope (HST)
 Astronomical surveys are usually extremely large. So large in fact, that
 the whole survey will not fit into a reasonably sized file. Because of
 this, surveys usually cut the final image into separate tiles and store
@@ -12863,8 +12861,8 @@ those distortions prior to the analysis.
 @cindex WFC3
 @cindex Wide Field Camera 3
 @cindex Charge-coupled device
address@hidden Hubble Space Telescope
 @cindex Advanced camera for surveys
address@hidden Hubble Space Telescope (HST)
 @item
 @strong{Detector not on focal plane:} In some cases (like the Hubble
 Space Telescope ACS and WFC3 cameras), the CCD might be tilted
@@ -12943,8 +12941,8 @@ combinations of these transformations can be displayed 
with one
 @dispmath{\left[\matrix{a&b\cr c&d}\right]}
 
 @cindex Wide Field Camera 3
address@hidden Hubble Space Telescope
 @cindex Advanced Camera for Surveys
address@hidden Hubble Space Telescope (HST)
 The transformations above can cover a lot of the needs of most
 coordinate transformations. However they are limited to mapping the
 point @mymath{[\matrix{0&0}]} to @mymath{[\matrix{0&0}]}. Therefore
@@ -15551,7 +15549,7 @@ many illustrative figures) is Section 3.2 of
 @url{https://arxiv.org/abs/1505.01664, Akhlaghi and Ichikawa [2015]}.
 
 @cindex river
address@hidden Watershed
address@hidden Watershed algorithm
 As a summary, Segment first finds true @emph{clump}s over the
 detections. Clumps are associated with local maxima/address@hidden
 default the maximum is used as the first clump pixel, to define clumps
@@ -16469,8 +16467,9 @@ multiple of @mymath{\sigma_m} as (see @ref{Flux 
Brightness and magnitude}):
 
 @dispmath{SB_{\rm Pixel}=-2.5\times\log_{10}{(n\sigma_m)}+z}
 
address@hidden XDF
address@hidden CANDELS
address@hidden XDF survey
address@hidden CANDELS survey
address@hidden eXtreme Deep Field (XDF) survey
 As an example, the XDF survey covers part of the sky that the Hubble space
 telescope has observed the most (for 85 orbits) and is consequently very
 small (@mymath{\sim4} address@hidden). On the other hand, the CANDELS
@@ -29353,8 +29352,7 @@ $ ./pgdemoXX
 @appendix GNU Gen. Pub. License v3
 
 @cindex GPL
address@hidden GNU GPL
address@hidden GNU General public license
address@hidden GNU General Public License (GPL)
 @include gpl-3.0.texi