Index: trunk/doc/release.2015/ps1.calibration/calibration.tex
===================================================================
--- trunk/doc/release.2015/ps1.calibration/calibration.tex	(revision 41190)
+++ trunk/doc/release.2015/ps1.calibration/calibration.tex	(revision 41191)
@@ -132,5 +132,5 @@
 Type Ia supernovae to measure the history of the expansion of the
 universe.  The majority of the time (56\%) was spent on surveying the
-$\frac{3}{4}$ of the sky north of $-30\degree$ Declination with
+$\frac{3}{4}$ of the sky north of $-30$\degree Declination with
 \grizy\ filters in the so-called $3\pi$ Survey.  Another $\sim 25\%$
 of the time was concentrated on repeated deep observations of 10
@@ -1291,5 +1291,5 @@
   analysis are static in time; they supplement the flats from the
   ubercal analysis.  A total of 1.95 billion measurements were
-  extracted for this analysis.
+  extracted for this analysis.}
 
 We then used
@@ -2362,18 +2362,19 @@
 \mu^{\rm sol}_{b} & = & \frac{(U \cos(l) + V \sin(l)) \sin(b) - W \cos(b)}{d}
 \end{eqnarray}
-where $d$ is the distance and $l,b$ are the Galactic coordinates of the
-star. Note that the proper motion induced by
-the Galactic rotation is independent of distance while the reflex
-motion induced by the solar motion decreases with increasing
-distance.  Also note that this model assumes a flat rotation curve for
-objects in the thin disk; any reference stars which are part of 
-the halo population will have proper motions which are not 
-described by this model; the mostly random nature of the halo motions
-should act to increase the noise in the measurement, but should not
-introduce detectable motion biases.  Also, if the distance modulus is
-not well determined, we can assume the object is simply following the
-Galactic rotation curve and set a fixed proper motion.  If we do not
-have a distance modulus from the Green et al analysis, we assume a
-value of 500pc.  
+where $d$ is the distance and $l,b$ are the Galactic coordinates of
+the star. Note that the proper motion induced by the Galactic rotation
+is independent of distance while the reflex motion induced by the
+solar motion decreases with increasing distance.  Also note that this
+model assumes a flat rotation curve for objects in the thin disk.  Any
+reference stars which are part of the halo population will have proper
+motions which are not described by this model; the mostly random
+nature of the halo motions should act to increase the noise in the
+measurement, but should not introduce detectable motion biases.  Also,
+if the distance modulus is not well determined, we can assume the
+object is simply following the Galactic rotation curve and set a fixed
+proper motion.  If we do not have a distance modulus from the Green et
+al analysis, we assume a value of 500pc.
+
+\note{find the improvement by using 2MASS -- in the PS1 DRAVG pages}
 
 For the initial PV3 analysis, we again used the 2MASS coordinates as