Changeset 9713 for trunk/doc/modules/ModulesSDRS.tex

Timestamp:

Oct 20, 2006, 6:27:38 PM (20 years ago)

Author:

Paul Price

Message:

Fixing so it compiles. Removed photometric systems stuff.

File:

• trunk/doc/modules/ModulesSDRS.tex (modified) (4 diffs)

trunk/doc/modules/ModulesSDRS.tex

@@ -1 @@
-%%% $Id: ModulesSDRS.tex,v 1.78 2006-10-21 00:58:33 price Exp $
+%%% $Id: ModulesSDRS.tex,v 1.79 2006-10-21 04:27:38 price Exp $
 \documentclass[panstarrs,spec]{panstarrs}
 
@@ -87 +87 @@
 
 
-\subsubsection{Configuration information}
+\subsection{Configuration information}
 
 This structure stores the configuration information: the site, camera
@@ -134 +134 @@
 \end{prototype}
 pmConfigRead loads the site configuration (the file name is specified
-by "-site SITE_FILE" on the command-line, the PS_SITE environment
-variable, or it is \code{$HOME/.ipprc}).  The configuration search %$
-path is set. The camera configuration is loaded if it is specified on
-the command line ("-camera CAMERA_FILE"). Recipes specified on the
-command line ("-recipe RECIPE_NAME RECIPE_SOURCE") are also loaded.
-These command-line arguments are removed from from the command-line,
-to simplify parsing.  The psLib log, trace and time setups are also
+by "-site SITE\_FILE" on the command-line, the PS\_SITE environment variable, or
+it is \code{$HOME/.ipprc}).  The configuration search %$ path is
+set. The camera configuration is loaded if it is specified on the
+command line ("-camera CAMERA\_FILE"). Recipes specified on the command
+line ("-recipe RECIPE\_NAME RECIPE\_SOURCE") are also loaded.  These
+command-line arguments are removed from from the command-line, to
+simplify parsing.  The psLib log, trace and time setups are also
 performed if specified in the site configuration.
 
@@ -617 +617 @@
 %\input{CameraGeometry.tex}
 
-\section{Photometry}
-
-\tbd{This section is to be deferred, and for now consists only of
-place holders, with no functional items.}
-
-Photometric observations are performed in an instrumental photometric
-system, and must be related to other photometric systems.  We
-require a data structure which defines a photometric system, as well
-as a structure to define the transformation between photometric
-systems.
-
-The photometric system is defined by the psPhotSystem structure.  
-A photometric system is identified by a human-readable \code{name}
-(ie, SDSS.g, Landolt92.B, GPC1.OTA32.r).  Each photometric system is
-given a unique identifier \code{ID}.  Observations taken with a
-specific camera, detector, and filter represent their own photometric
-system, and it may be necessary to perform transformations between
-these systems.  Photometric systems associated with observations from
-a specific camera/detector/filter combination can be associated with
-those components.
-\begin{datatype}
-typedef struct {
-    const int ID;                       ///< ID number for this photometric system
-    const char *name;                   ///< Name of photometric system
-    const char *camera;                 ///< Camera for photometric system
-    const char *filter;                 ///< Filter used for photometric system
-    const char *detector;               ///< Detector used for photometric system
-} psPhotSystem;
-\end{datatype}
-
-The following structure defines the transformation between two
-photometric systems.
-\begin{datatype}
-typedef struct {
-    psPhotSystem src;                   ///< Source photometric system
-    psPhotSystem dst;                   ///< Destination photometric system
-    psPhotSystem pP, pM;                ///< Primary color reference
-    psPhotSystem sP, sM;                ///< Secondary color reference
-    float pA, sA;                       ///< Color offset for references
-    psPolynomial3D transform;           ///< Transformation from source to destination
-} psPhotTransform;
-\end{datatype}
-
-The transformation between two photometric systems may depend on the
-airmass of the observation and on the colors of the object of
-interest.  For a specific observation, such a transformations can be
-defined as a polynomial function of the color of the star and the
-airmass of the observations.  If sufficient data exists, the
-transformation between the photometric systems may include more than
-one color, constraining the curvature of the stellar spectral energy
-distributions.  This latter term may be significant for stars which
-are highly reddened, for example.  Derived photometric quantities may
-have been corrected for airmass variations, in which case only color
-terms may be measurable.  The structure defines the transformation
-between a source photometric system (\code{src}) and a target
-photometric system (\code{dst}).  The photometric system of a primary
-color is defined by \code{pP, pM} such that the color is constructed
-as $pP - pM$.  A secondary color is defined by \code{sP, sM}.  For
-both, a reference color is specified (\code{pA, sA}): the polynomial
-transformation terms refer to colors in the form $pP - pM - pA$.  The
-transformation is specified as a 3D polynomial.  For a star of
-magnitude $M_{\rm src}$ in the source photometric system, with
-additional magnitude information in the other systems $M_{\rm pP}$,
-$M_{\rm pM}$, $M_{\rm sP}$, $M_{\rm sM}$, observed at an airmass of
-$z$, the magnitude of the star in the target system $M_{\rm dst}$ is
-given by: $M_{\rm dst} = M_{\rm src} + transform(z, M_{\rm pP} -
-M_{\rm pM} - pA, M_{\rm sP} - M_{\rm sM} - sA)$.
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
 
 \section{Image Detrending}