Index: /trunk/doc/pslib/psLibSDRS.tex
===================================================================
--- /trunk/doc/pslib/psLibSDRS.tex	(revision 1526)
+++ /trunk/doc/pslib/psLibSDRS.tex	(revision 1527)
@@ -1,3 +1,3 @@
-%%% $Id: psLibSDRS.tex,v 1.66 2004-08-12 04:19:18 price Exp $
+%%% $Id: psLibSDRS.tex,v 1.67 2004-08-13 20:50:59 price Exp $
 \documentclass[panstarrs,spec]{panstarrs}
 
@@ -3407,21 +3407,21 @@
 Three major classes of coordinate transformations are necessary.
 First, linear coordinates from one frame must be converted to linear
-coordinates in a different frame of references.  Simple transformations
-of this type are independent of other quantities of the positions --
-they are simply mapping between two linear spaces.  In practice, these
-transformations may often be a function of the magnitude or color of
-the imaged object.  The second type of conversion is the
-transformation of linear coordinates to angular coordinates and
-vice-versa.  This conversion depends on the desired projection, and
-may represent the real mapping performed by the telescope or may
-simply represent a convenient mechanism to display 3D coordinates in
-useful forms.  The third conversion of interest is the transformation
-of one set of spherical coordinates to another set.  Frequently in
-astronomy, these conversions consist only of rotations between the two
-spherical coordinates systems, where the coordinates of the pole and
-equatorial rotation between the two systems define the
+coordinates in a different frame of references.  Simple
+transformations of this type are independent of other quantities of
+the positions -- they are simply mapping between two linear spaces.
+In practice, these transformations may often be a function of the
+color or even magnitude of the imaged object.  The second type of
+conversion is the transformation of linear coordinates to angular
+coordinates and vice-versa.  This conversion depends on the desired
+projection, and may represent the real mapping performed by the
+telescope or may simply represent a convenient mechanism to display 3D
+coordinates in useful forms.  The third conversion of interest is the
+transformation of one set of spherical coordinates to another set.
+Frequently in astronomy, these conversions consist only of rotations
+between the two spherical coordinates systems, where the coordinates
+of the pole and equatorial rotation between the two systems define the
 transformation.  Conversions between standard coordinate systems such
 as Galactic, Ecliptic, and various epochs of the Celestial coordinates
-are represented by these spherical transformations.  
+are represented by these spherical transformations.
 
 \subsubsection{Linear Coordinate Transformations}
@@ -3432,6 +3432,6 @@
 coordinates and no other quantities of objects at those coordinates.
 The second consists of two 4D polynomials in which the output
-coordinates are also specified to be a function of the magnitude and
-color of the object with the given coordinates.  This type of
+coordinates are also specified to be a function of the color and
+magnitude of the object with the given coordinates.  This type of
 coordinate transformation is necessary to represent the
 (color-dependent) optical distortions caused by the atmosphere and
@@ -3466,5 +3466,5 @@
 The \code{psPlaneDistort} represents an optical distortion.  The
 lowest two terms are the $x$ and $y$ axis of the target system.  The
-higher two terms may represent magnitude and color terms.
+higher two terms may represent color and magnitude terms.
 \begin{verbatim}
 typedef struct {
@@ -3479,7 +3479,7 @@
 There is one of these structures for each of the two output
 dimensions.  In this structure, the highest two dimensions could
-represent a magnitude and a color.  As an example, consider the simple
+represent a color and magnitude.  As an example, consider the simple
 transformation from one linear coordinate frame ($x,y$), e.g., on a
-CCD, of an object with magnitude and color ($m,c$) to a second frame
+CCD, of an object with color and magnitude ($c,m$) to a second frame
 ($p,q$), e.g., the focal plane. If we have only first order terms in
 the transformation \code{psPlaneDistort T}, the new coordinates
@@ -3488,7 +3488,7 @@
 \begin{verbatim}
 p = T.x->coeff[0][0][0][0] + x*T.x->coeff[1][0][0][0] + y*T.x->coeff[0][1][0][0] 
-  + m*T.x->coeff[0][0][1][0] + c*T.x->coeff[0][0][0][1]
+  + c*T.x->coeff[0][0][1][0] + m*T.x->coeff[0][0][0][1]
 q = T.y->coeff[0][0][0][0] + x*T.y->coeff[1][0][0][0] + y*T.y->coeff[0][1][0][0] 
-  + m*T.y->coeff[0][0][1][0] + c*T.y->coeff[0][0][0][1]
+  + c*T.y->coeff[0][0][1][0] + m*T.y->coeff[0][0][0][1]
 \end{verbatim}
 %