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Commit 1740564b authored by Emmanuel Bertin's avatar Emmanuel Bertin
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Doc: Added description of WIN positions and two figures.

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doc/src/Config.rst 0 → 100644
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.. File Config.rst
The configuration file
======================
Each time it is run, |SExtractor| looks for a configuration file. If no
configuration file is specified in the command-line, it is assumed to be
called :file:`default.sex` and to reside in the current directory. If no
configuration file is found, |SExtractor| will use its own internal
default configuration.
Creating a configuration file
-----------------------------
SExtractor can generate an ASCII dump of its internal default
configuration, using the ``-d`` option. By redirecting the standard output
of SExtractor to a file, one creates a configuration file that can
easily be modified afterwards:
.. code-block:: console
$ sex -d > default.sex
A more extensive dump with less commonly used parameters can be
generated by using the ``-dd`` option.
Format of the configuration file
--------------------------------
The format is ASCII. There must be only one parameter set per line,
following the form::
Config-parameter      Value(s)
Extra spaces or linefeeds are ignored. Comments must begin with a ``#``
and end with a linefeed. Values can be of different types: strings (can
be enclosed between double quotes), floats, integers, keywords or
Boolean (`Y`/`y` or `N`/`n`). Some parameters accept zero or several values,
which must then be separated by commas. Integers can be given as
decimals, in octal form (preceded by digit O), or in hexadecimal
(preceded by `0x`). The hexadecimal format is particularly convenient for
writing multiplexed bit values such as binary masks. Environment
variables, written as ``$HOME`` or ``${HOME}`` are expanded.
.. _param_list:
Configuration parameter list
----------------------------
Here is a complete list of all the configuration parameters known to
|SExtractor|. Please refer to the next sections for a detailed description
of their meaning.
.. include:: keys.rst
doc/src/Installing.rst
View file @ 1740564b
.. File Installing.rst
***********************
Installing the software
=======================
***********************
Hardware requirements
---------------------
=====================
|SExtractor| runs in (ANSI) text-mode from a shell. A graphical environment
is not necessary to operate the software.
......@@ -24,7 +25,7 @@ install the standard binary package the comes with your Linux distribution.
Run, e.g., ``apt-get sextractor`` (on Debian) or ``dnf sextractor`` (Fedora) as
root and |SExtractor|, as well as all its dependencies, will automatically be
installed. If you decided to install the package this way you may skip the
following and move straight to the :ref:`next section <using_sextractor>`.
following and move straight to the :ref:`next section <Using Sextractor>`.
However if |SExtractor| is not available in your distribution, or to obtain the
most recent version, the |SExtractor| source package can be downloaded from
......
doc/src/Introduction.rst
View file @ 1740564b
......@@ -3,7 +3,7 @@
Introduction
============
|SExtractor|_ (Source-Extractor) is a program that builds a catalogue
|SExtractor|_ (Source-Extractor) is a program that builds a catalog
of objects from an astronomical image. It is particularly oriented
towards the reduction of large scale galaxy-survey data, but it also performs
well on moderately crowded star fields. Its main features are:
......@@ -14,14 +14,14 @@ well on moderately crowded star fields. Its main features are:
thanks to buffered image access
* Real-time filtering of images to improve detectability
* Robust deblending of overlapping extended objects
* Flexible catalogue output of desired parameters only
* Flexible catalog output of desired parameters only
* Pixel-to-pixel photometry in dual-image mode
* Fast and accurate Point-Spread-Function and galaxy model fitting.
* Handling of weight maps and flag maps.
* Optimum handling of images with variable SNR.
* Built-in catalogue cross-identification.
* Built-in catalog cross-identification.
* Special mode for photographic scans.
* |XML|_ |VOTable|_-compliant catalogue output.
* |XML|_ |VOTable|_-compliant catalog output.
* |XSLT|_ filter sheet provided for convenient access to metadata from a
regular web browser.
......
doc/src/Measurements.rst 0 → 100644
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Measurements
============
Once sources have been detected and deblended, they enter the
measurement phase. |SExtractor| performs two categories of measurements.
Measurements from the first category are made on the isophotal object
profiles. Only pixels above the detection threshold are considered. Many
of these isophotal measurements (like ``X_IMAGE``, ``Y_IMAGE``, etc.) are
necessary for the internal operations of |SExtractor| and are therefore
executed even if they are not requested. Measurements from the second
category have access to all pixels of the image. These measurements are
generally more sophisticated and are done at a later stage of the
processing (after CLEANing and MASKing).
.. toctree::
:numbered:
:maxdepth: 2
Position
PositionWin
.. include:: keys.rst
doc/src/Param.rst 0 → 100644
View file @ 1740564b
.. File Param.rst
The catalog parameter file
============================
In addition to the configuration file detailed above, |SExtractor| requires a
file containing the list of parameters that will be listed in the output
catalog for every detection. This allows the software to compute only
catalog parameters that are needed. The name of this
catalog-parameter file is traditionally suffixed with ``.param``, and must
be specified using the ``PARAMETERS_NAME`` config parameter. The full set
of parameters can be queried with the command
.. code-block:: console
$ sex -dp
Format
------
The format of the catalog parameter list is ASCII, and there must be
*a single keyword per line*. Presently two kinds of keywords are
recognized by |SExtractor|: scalars and vectors. Scalars, like ``X_IMAGE``,
produce single numbers in the output catalog. Vectors, like ``MAG_APER(4)``
or ``VIGNET(15,15)``, produce arrays of numbers. The ordering of measurements
in the output catalog is identical to that of the keywords in the parameter
list. Comments are allowed, they must begin with a ``#``.
Variants
--------
For many catalog parameters, especially those related to flux,
position, or shape, several variants of the same measurement are
available:
Fluxes
~~~~~~
may be expressed in linear (ADU) units or as Pogson
:cite:`1856MNRAS..17...12P` magnitudes. Flux measurements in ADUs
are prefixed with ``FLUX_``, for example: ``FLUX_AUTO``, ``FLUX_ISO``, etc.
Magnitudes are prefixed with ``MAG_`` e.g., ``MAG_AUTO``, ``MAG_ISO``, ... In
|SExtractor| the magnitude :math:`m` of a source is derived from the flux
:math:`f`:
.. math::
m = \left\{\begin{array}{ll}
m_{ZP} -2.5 \log_{10} f\ &\mbox{if } f > 0\\
99.0 &\mbox{otherwise},
\end{array}\right.
where :math:`m_{ZP}` is the magnitude zero-point set with the
``MAG_ZEROPOINT`` configuration parameter.
Flux uncertainties
~~~~~~~~~~~~~~~~~~
They follow a scheme similar to that of fluxes. Flux uncertainties are
prefixed with ``FLUXERR_``, as in ``FLUXERR_AUTO`` or ``FLUXERR_ISO``. Magnitude
uncertainties start with ``MAGERR_``, for instance: ``MAGERR_AUTO``,
``MAGERR_ISO``,... Magnitude uncertainties :math:`\sigma_m` are derived
from the estimated 1-\ :math:`\sigma` flux error :math:`\sigma_f`:
.. math::
\sigma_m = \left\{\begin{array}{ll}
(2.5/\ln 10) (\sigma_f/f)\ &\mbox{if } f > 0\\
99.0 &\mbox{otherwise}.
\end{array}\right.
Positions
~~~~~~~~~
Positions and distances can be expressed in image pixels, world coordinates,
or in celestial coordinates. Measurements in units of image pixels are
indicated by the suffix ``_IMAGE``, for example: ``Y_IMAGE``,
``ERRAWIN_IMAGE``, ... Following the FITS convention, in SExtractor the
center of the first image pixel has coordinates (1.0,1.0). Positions and
small distances may also be expressed in so-called “world coordinates”,
if World Coordinate System (WCS) metadata :cite:`2002A&A...395.1061G` are
present in the FITS image header.
.. include:: keys.rst
doc/src/Position.rst
View file @ 1740564b
Positional parameters derived from the isophotal profile
========================================================
.. File Position.rst
Position and shape parameters derived from the isophotal profile
================================================================
The following parameters are derived from the spatial distribution
:math:`\cal S` of pixels detected above the extraction threshold. *The
pixel values* :math:`I_i` *are taken from the (filtered) detection image*.
**Note that, unless otherwise noted, all parameter names given below are
only prefixes. They must be followed by “\_IMAGE” if the results shall
be expressed in pixel units (see §..), or “\_WORLD” for World Coordinate
only prefixes. They must be followed by “_IMAGE” if the results shall
be expressed in pixel units (see §..), or “_WORLD” for World Coordinate
System (WCS) units (see §[astrom])**. For example: THETA
:math:`\rightarrow` THETA\_IMAGE. In all cases, parameters are first
computed in the image coordinate system, and then converted to WCS if
......@@ -60,7 +62,7 @@ with likelihood maps, or when searching for artifacts. For better
robustness, PEAK coordinates are computed on *filtered* profiles if
available. On symmetrical profiles, PEAK positions and barycenters
coincide within a fraction of pixel (XPEAK and YPEAK coordinates are
quantized by steps of 1 pixel, thus XPEAK\_IMAGE and YPEAK\_IMAGE are
quantized by steps of 1 pixel, thus XPEAK_IMAGE and YPEAK_IMAGE are
integers). This is no longer true for skewed profiles, therefore a
simple comparison between PEAK and barycenter coordinates can be used to
identify asymmetrical objects on well-sampled images.
......@@ -69,7 +71,7 @@ identify asymmetrical objects on well-sampled images.
-----------------------------
(Centered) second-order moments are convenient for measuring the spatial
spread of a source profile. In SExtractor they are computed with:
spread of a source profile. In |SExtractor| they are computed with:
.. math::
......@@ -163,17 +165,17 @@ following equations derived from ([eq:varproj]) after some algebra:
- \sqrt{\left(\frac{\overline{x^2}-\overline{y^2}}{2}\right)^2 + \overline{xy}^2}.\end{aligned}
Note that A and B are exactly halves the :math:`a` and :math:`b`
parameters computed by the COSMOS image analyser (Stobie 1980,1986).
Actually, :math:`a` and :math:`b` are defined by Stobie as the
semi-major and semi-minor axes of an elliptical shape with constant
parameters computed by the COSMOS image analyser :cite:`1980SPIE..264..208S`.
Actually, :math:`a` and :math:`b` are defined in :cite:`1980SPIE..264..208S`
as the semi-major and semi-minor axes of an elliptical shape with constant
surface brightness, which would have the same 2nd-order moments as the
analysed object.
analyzed object.
Ellipse parameters: CXX, CYY, CXY
---------------------------------
A, B and THETA are not very convenient to use when, for instance, one
wants to know if a particular SExtractor detection extends over some
wants to know if a particular |SExtractor| detection extends over some
position. For this kind of application, three other ellipse parameters
are provided; CXX, CYY and CXY. They do nothing more than describing the
same ellipse, but in a different way: the elliptical shape associated to
......@@ -186,7 +188,7 @@ a detection is now parameterized as
where :math:`R` is a parameter which scales the ellipse, in units of A
(or B). Generally, the isophotal limit of a detected object is well
represented by :math:`R\approx 3` (Fig. [fig:ellipse]). Ellipse
represented by :math:`R\approx 3` (:numref:`fig_ellipse`). Ellipse
parameters can be derived from the 2nd order moments:
.. math::
......@@ -202,6 +204,14 @@ parameters can be derived from the 2nd order moments:
THETA} \left( \frac{1}{{\tt A}^2} - \frac{1}{{\tt B}^2}\right) = -2\,
\frac{\overline{xy}}{\overline{x^2} \overline{y^2} - \overline{xy}^2}\end{aligned}
.. _fig_ellipse:
.. figure:: figures/ellipse.*
:figwidth: 100%
:align: center
Meaning of shape parameters.
By-products of shape parameters: ELONGATION and ELLIPTICITY [1]_
----------------------------------------------------------------
......@@ -213,15 +223,15 @@ These parameters are directly derived from A and B:
{\tt ELONGATION} & = & \frac{\tt A}{\tt B}\ \ \ \ \ \mbox{and}\\
{\tt ELLIPTICITY} & = & 1 - \frac{\tt B}{\tt A}.\end{aligned}
Position errors: ERRX2, ERRY2, ERRXY, ERRA, ERRB, ERRTHETA, ERRCXX, ERRCYY, ERRCXY
----------------------------------------------------------------------------------
Position uncertainties: ERRX2, ERRY2, ERRXY, ERRA, ERRB, ERRTHETA, ERRCXX, ERRCYY, ERRCXY
-----------------------------------------------------------------------------------------
Uncertainties on the position of the barycenter can be estimated using
photon statistics. Of course, this kind of estimate has to be considered
as a lower-value of the real error since it does not include, for
instance, the contribution of detection biases or the contamination by
neighbours. As SExtractor does not currently take into account possible
correlations between pixels, the variances simply write:
photon statistics. In practice, such estimates are a lower-value of the full
uncertainties because they do not include, for instance, the contribution of
detection biases or contamination by neighbors. Furthermore, |SExtractor| does
not currently take into account possible correlations of the noise between adjacent
pixels. Hence variances simply write:
.. math::
......@@ -288,7 +298,7 @@ Handling of “infinitely thin” detections
----------------------------------------
Apart from the mathematical singularities that can be found in some of
the above equations describing shape parameters (and which SExtractor
the above equations describing shape parameters (and which |SExtractor|
handles, of course), some detections with very specific shapes may yield
quite unphysical parameters, namely null values for B, ERRB, or even A
and ERRA. Such detections include single-pixel objects and horizontal,
......@@ -306,14 +316,14 @@ sufficiently thin line of pixels, which we translate mathematically by
\overline{x^2}\,\overline{y^2} - \overline{xy}^2 < \rho^2,
then :math:`\overline{x^2}` and :math:`\overline{y^2}` are incremented
by :math:`\rho`. SExtractor sets :math:`\rho=1/12`, which is the
by :math:`\rho`. |SExtractor| sets :math:`\rho=1/12`, which is the
variance of a 1-dimensional top-hat distribution with unit width.
Therefore :math:`1/\sqrt{12}` represents the typical minor-axis values
assigned (in pixels units) to undersampled sources in SExtractor.
assigned (in pixels units) to undersampled sources in |SExtractor|.
Positional errors are more difficult to handle, as objects with very
high signal-to-noise can yield extremely small position uncertainties,
just like singular profiles do. Therefore SExtractor first checks that
just like singular profiles do. Therefore |SExtractor| first checks that
([eq:singutest]) is true. If this is the case, a new test is conducted:
.. math::
......@@ -329,4 +339,7 @@ where :math:`\rho_e` is arbitrarily set to :math:`\left( \sum_{i \in {\cal S}}
.. [1]
Such parameters are dimensionless and therefore do not accept any
\_IMAGE or \_WORLD suffix
_IMAGE or _WORLD suffix
.. include:: keys.rst
doc/src/PositionWin.rst 0 → 100644
View file @ 1740564b
.. File PositionWin.rst
Windowed positional parameters
==============================
Parameters measured within an object’s isophotal limit are sensitive to
two main factors: 1) changes in the detection threshold, which create a
variable bias and 2) irregularities in the object’s isophotal
boundaries, which act as additional “noise” in the measurements.
Measurements performed through a *window* function (an *envelope*) do
not have such drawbacks. |SExtractor| implements “windowed” versions for most
of the measurements described in [chap:isoparam]:
+----------------------------------------+-------------------------------------------------+
| Isophotal parameters | Equivalent windowed parameters |
+========================================+=================================================+
| X_IMAGE, Y_IMAGE | XWIN_IMAGE, YWIN_IMAGE |
+----------------------------------------+-------------------------------------------------+
| ERRA_IMAGE, ERRB_IMAGE, ERRTHETA_IMAGE | ERRAWIN_IMAGE, ERRBWIN_IMAGE, ERRTHETAWIN_IMAGE |
+----------------------------------------+-------------------------------------------------+
| A_IMAGE, B_IMAGE, THETA_IMAGE | AWIN_IMAGE, BWIN_IMAGE, THETAWIN_IMAGE |
+----------------------------------------+-------------------------------------------------+
| X2_IMAGE, Y2_IMAGE, XY_IMAGE | X2WIN_IMAGE, Y2WIN_IMAGE, XYWIN_IMAGE |
+----------------------------------------+-------------------------------------------------+
| CXX_IMAGE, CYY_IMAGE, CXY_IMAGE | CXXWIN_IMAGE, CYYWIN_IMAGE, CXYWIN_IMAGE |
+----------------------------------------+-------------------------------------------------+
The computations involved are roughly the same except that the pixel
values are integrated within a circular Gaussian window as opposed to
the object’s isophotal footprint. The Gaussian window is scaled to each
object; its FWHM is the diameter of the disk that contains half of the
object flux (:math:`d_{50}`). Note that in double-image mode
(§[chap:using]) the window is scaled based on the *measurement* image.
Windowed centroid: XWIN, YWIN
-----------------------------
This is an iterative process. The computation starts by initializing the
windowed centroid coordinates :math:`\overline{x_{\tt WIN}}^{(0)}` and
:math:`\overline{y_{\tt WIN}}^{(0)}` to their basic :math:`\overline{x}`
and :math:`\overline{y}` isophotal equivalents, respectively. Then at
each iteration :math:`t`, :math:`\overline{x_{\tt WIN}}` and
:math:`\overline{y_{\tt WIN}}` are refined using:
.. math::
\begin{aligned}
\label{eq:xwin}
{\tt XWIN}^{(t+1)} & = & \overline{x_{\tt WIN}}^{(t+1)}
= \overline{x_{\tt WIN}}^{(t)} + 2\,\frac{\sum_{r_i^{(t)} < r_{\rm max}}
w_i^{(t)} I_i \ (x_i - \overline{x_{\tt WIN}}^{(t)})}
{\sum_{r_i^{(t)} < r_{\rm max}} w_i^{(t)} I_i},\\
\label{eq:ywin}
{\tt YWIN}^{(t+1)} & = & \overline{y_{\tt WIN}}^{(t+1)}
= \overline{y_{\tt WIN}}^{(t)} + 2\,\frac{\sum_{r_i^{(t)} < r_{\rm max}}
w_i^{(t)} I_i\ (y_i - \overline{y_{\tt WIN}}^{(t)})}
{\sum_{r_i^{(t)} < r_{\rm max}} w_i^{(t)} I_i},\end{aligned}
where
.. math:: w_i^{(t)} = \exp \left(-\frac{r_i^{(t)^2}}{2s_{\tt WIN}^2} \right),
with
.. math::
r_i^{(t)} = \sqrt{\left(x_i - \overline{x_{\tt WIN}}^{(t)}\right)^2 + \left(y_i
- \overline{y_{\tt WIN}}^{(t)}\right)^2}
and :math:`s_{\tt WIN} = d_{50} / \sqrt{8 \ln 2}`. The process stops
when the change in position between two iterations is less than
:math:`2\times10^{-4}` pixel, a condition which is generally achieved in
about 3 to 5 iterations.
Although the iterative nature of the processing slows down the
processing , it is recommended to use whenever possible windowed
parameters instead of their isophotal equivalents, since the
measurements they provide are much more precise (:numref:`fig_xwinprec`).
The precision in centroiding offered by XWIN_IMAGE and YWIN_IMAGE is
actually very close to that of PSF-fitting on focused and properly
sampled star images, and can also be applied to galaxies. It has been
verified that for isolated, Gaussian-like PSFs, its accuracy is close to
the theoretical limit set by image noise [1]_.
.. _fig_xwinprec:
.. figure:: figures/xwinprec.*
:figwidth: 100%
:align: center
Comparison between isophotal and windowed centroid measurement residuals on
simulated, background noise-limited images.
*Left*: histogram of the difference between X_IMAGE and the true centroid
in x.
*Right*: histogram of the difference between XWIN_IMAGE and the true centroid
in x.
Windowed 2nd order moments: X2, Y2, XY
--------------------------------------
Windowed second-order moments are computed on the image data once the
centering process from §[chap:wincent] has converged:
.. math::
\begin{aligned}
{\tt X2WIN} & = \overline{x_{\tt WIN}^2}
= & \frac{\sum_{r_i < r_{\rm max}} w_i I_i (x_i - \overline{x_{\tt WIN}})^2}
{\sum_{r_i < r_{\rm max}} w_i I_i},\\
{\tt Y2WIN} & = \overline{y_{\tt WIN}^2}
= & \frac{\sum_{r_i < r_{\rm max}} w_i I_i (y_i - \overline{y_{\tt WIN}})^2}
{\sum_{r_i < r_{\rm max}} w_i I_i},\\
{\tt XYWIN} & = \overline{xy_{\tt WIN}}
= & \frac{\sum_{r_i < r_{\rm max}} w_i I_i (x_i - \overline{x_{\tt WIN}})
(y_i - \overline{y_{\tt WIN}})}
{\sum_{r_i < r_{\rm max}} w_i I_i}.\end{aligned}
Windowed second-order moments are typically twice smaller than their
isophotal equivalent.
Windowed ellipse parameters: CXXWIN, CYYWIN, CXYWIN
---------------------------------------------------
They are computed from the windowed 2nd order moments exactly the same
way as in §[chap:cxx].
Windowed position uncertainties: ERRX2WIN, ERRY2WIN, ERRXYWIN, ERRAWIN, ERRBWIN, ERRTHETAWIN, ERRCXXWIN, ERRCYYWIN, ERRCXYWIN
-----------------------------------------------------------------------------------------------------------------------------
Windowed position uncertainties are computed on the image data once the
centering process from §[chap:wincent] has converged. Assuming that
noise is uncorrelated among pixels, standard error propagation applied
to ([eq:xwin]) and ([eq:xwin]) gives us:
.. math::
\begin{aligned}
{\tt ERRX2WIN} & = {\rm var}(\overline{x_{\tt WIN}})
= & 4\,\frac{\sum_{r_i < r_{\rm max}} w_i^2 \sigma^2_i (x_i-\overline{x})^2}
{\left(\sum_{r_i < r_{\rm max}} w_i I_i\right)^2},\\
{\tt ERRY2WIN} & = {\rm var}(\overline{y_{\tt WIN}})
= & 4\,\frac{\sum_{r_i < r_{\rm max}} w_i^2 \sigma^2_i (y_i-\overline{y})^2}
{\left(\sum_{r_i < r_{\rm max}} w_i I_i\right)^2},\\
{\tt ERRXYWIN} & = {\rm cov}(\overline{x_{\tt WIN}},\overline{y_{\tt WIN}})
= & 4\,\frac{\sum_{r_i < r_{\rm max}}
w_i^2 \sigma^2_i (x_i-\overline{x_{\tt WIN}})(y_i-\overline{y_{\tt WIN}})}
{\left(\sum_{r_i < r_{\rm max}} w_i I_i\right)^2}.\end{aligned}
The semi-major axis ERRAWIN, semi-minor axis ERRBWIN, and position angle
ERRTHETAWIN of the :math:`1\sigma` position error ellipse are computed
from the covariance matrix elements
:math:`{\rm var}(\overline{x_{\tt WIN}})`,
:math:`{\rm var}(\overline{y_{\tt WIN}})`,
:math:`{\rm cov}(\overline{x_{\tt WIN}},\overline{y_{\tt WIN}})`,
exactly as in §[chap:poserr]: see eqs. ([eq:erra]), ([eq:errb]),
([eq:errtheta]), ([eq:errcxx]), ([eq:errcyy]) and ([eq:errcxy]).
.. [1]
see http://www.astromatic.net/forum/showthread.php?tid=581
.. include:: keys.rst
doc/src/Using.rst
View file @ 1740564b
.. File Using.rst
Using SExtractor
================
......@@ -35,57 +37,5 @@ about the source extraction process:
remote web server), alternative |XSLT| translation URLs may be specified
using the ``XSL_URL`` configuration parameter.
The configuration file
----------------------
Each time it is run, |SExtractor| looks for a configuration file. If no
configuration file is specified in the command-line, it is assumed to be
called :file:`default.sex` and to reside in the current directory. If no
configuration file is found, |SExtractor| will use its own internal
default configuration.
Creating a configuration file
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
SExtractor can generate an ASCII dump of its internal default
configuration, using the ``-d`` option. By redirecting the standard output
of SExtractor to a file, one creates a configuration file that can
easily be modified afterwards:
.. code-block:: console
$ sex -d > default.sex
A more extensive dump with less commonly used parameters can be
generated by using the ``-dd`` option.
Format of the configuration file
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
The format is ASCII. There must be only one parameter set per line,
following the form::
Config-parameter      Value(s)
Extra spaces or linefeeds are ignored. Comments must begin with a ``#``
and end with a linefeed. Values can be of different types: strings (can
be enclosed between double quotes), floats, integers, keywords or
Boolean (`Y`/`y` or `N`/`n`). Some parameters accept zero or several values,
which must then be separated by commas. Integers can be given as
decimals, in octal form (preceded by digit O), or in hexadecimal
(preceded by `0x`). The hexadecimal format is particularly convenient for
writing multiplexed bit values such as binary masks. Environment
variables, written as ``$HOME`` or ``${HOME}`` are expanded.
.. _param_list:
Configuration parameter list
~~~~~~~~~~~~~~~~~~~~~~~~~~~~
Here is a complete list of all the configuration parameters known to
|SExtractor|. Please refer to the next sections for a detailed description
of their meaning.
.. include:: keys.rst
doc/src/figures/xwinprec.svg 0 → 100644
View file @ 1740564b
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doc/src/index.rst
View file @ 1740564b
......@@ -18,7 +18,9 @@ Contents
License
Installing
Using
Position
Config
Param
Measurements
references
Indices and tables
......
doc/src/references.bib
View file @ 1740564b
@ARTICLE{1996A&AS..117..393B,
author = {{Bertin}, E. and {Arnouts}, S.},
title = "{SExtractor: Software for source extraction.}",
journal = {\aaps},
journal = {A\&AS},
keywords = {METHODS: DATA ANALYSIS, TECHNIQUES: IMAGE PROCESSING, GALAXIES: PHOTOMETRY},
year = 1996,
month = jun,
......@@ -12,10 +12,25 @@
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{2002A&A...395.1077C,
author = {{Calabretta}, M.~R. and {Greisen}, E.~W.},
title = "{Representations of celestial coordinates in FITS}",
journal = {A\&A},
eprint = {astro-ph/0207413},
keywords = {methods: data analysis, techniques: image processing, astronomical data bases: miscellaneous, astrometry},
year = 2002,
month = dec,
volume = 395,
pages = {1077-1122},
doi = {10.1051/0004-6361:20021327},
adsurl = {http://adsabs.harvard.edu/abs/2002A&A...395.1077C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{2002A&A...395.1061G,
author = {{Greisen}, E.~W. and {Calabretta}, M.~R.},
title = "{Representations of world coordinates in FITS}",
journal = {\aap},
journal = {A\&A},
eprint = {astro-ph/0207407},
keywords = {methods: data analysis, techniques: image processing, astronomical data bases: miscellaneous},
year = 2002,
......@@ -27,18 +42,16 @@
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{2002A&A...395.1077C,
author = {{Calabretta}, M.~R. and {Greisen}, E.~W.},
title = "{Representations of celestial coordinates in FITS}",
journal = {\aap},
eprint = {astro-ph/0207413},
keywords = {methods: data analysis, techniques: image processing, astronomical data bases: miscellaneous, astrometry},
year = 2002,
month = dec,
volume = 395,
pages = {1077-1122},
doi = {10.1051/0004-6361:20021327},
adsurl = {http://adsabs.harvard.edu/abs/2002A&A...395.1077C},
@ARTICLE{1856MNRAS..17...12P,
author = {{Pogson}, N.},
title = "{Magnitudes of Thirty-six of the Minor Planets for the first day of each month
of the year 1857}",
journal = {MNRAS},
year = 1856,
month = nov,
volume = 17,
pages = {12-15},
adsurl = {http://adsabs.harvard.edu/abs/1856MNRAS..17...12P},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
......@@ -87,3 +100,19 @@ booktitle = {Astronomical Data Analysis Software and Systems (ADASS) XIII},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@INPROCEEDINGS{1980SPIE..264..208S,
author = {{Stobie}, R.~S.},
title = "{Application of moments to the analysis of panoramic astronomical photographs}",
keywords = {Astronomical Photography, Classifications, Image Processing, Imaging Techniques, Moments, Accuracy, Computer Techniques, Photographs},
booktitle = {Conference on Applications of Digital Image Processing to Astronomy},
year = 1980,
series = {Proc. SPIE},
volume = 264,
editor = {{Elliott}, D.~A.},
pages = {208-212},
doi = {10.1117/12.959806},
adsurl = {http://adsabs.harvard.edu/abs/1980SPIE..264..208S},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
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