Index: trunk/doc/release.2015/ps1.calibration/calibration.tex
===================================================================
--- trunk/doc/release.2015/ps1.calibration/calibration.tex	(revision 41240)
+++ trunk/doc/release.2015/ps1.calibration/calibration.tex	(revision 41276)
@@ -21,6 +21,6 @@
 %% NOTE: 2019 Feb versions of the figures are generated in /data/kukui.1/eugene/cal.paper.20190217
 
-%\def\picdir{pics}
-\def\picdir{.}
+\def\picdir{pics}
+%\def\picdir{.}
 
 % Pick a terse version of the title here;
@@ -106,9 +106,9 @@
 consistent zero points over the entire area surveyed, the \approx
 30,000 square degrees north of $\delta = -30$\degrees.  \textadd{Using external
-comparisons, we demonstrate that the resulting photometic system is
-consistent across the sky to between 7 and 12.4 millimags depending on
+comparisons, we demonstrate that the resulting photometric system is
+consistent across the sky to between 7 and 12.4 millimagnitudes depending on
 the filter.  For bright stars, the systematic error floor for
-individual measurementsis $(\sigma_g, \sigma_r, \sigma_i, \sigma_z,
-\sigma_y) = (14, 14, 15, 15, 18)$ millimags.}  The astrometric
+individual measurements is $(\sigma_g, \sigma_r, \sigma_i, \sigma_z,
+\sigma_y) = (14, 14, 15, 15, 18)$ millimagnitudes.}  The astrometric
 calibration compensates for similar systematic effects so that
 positions, proper motions, and parallaxes are reliable as well.  \textadd{The
@@ -385,5 +385,5 @@
 
 Coordinates and calibrated magnitudes of stars from the reference
-database are loaded by \ippprog{pasastro}.  A model for the positions of
+database are loaded by \ippprog{psastro}.  A model for the positions of
 the 60 chips in the focal plane is used to determine the expected
 astrometry for each chip based on the boresite coordinates and
@@ -488,7 +488,7 @@
   (changes from over time).  The spatial scale on which the
   astrometric deviations due to atmosphere are varying is related to
-  the isoplanetic patch size.  We note that, in the typical conditions
+  the isoplanatic patch size.  We note that, in the typical conditions
   at the \PSONE\ site, if the seeing is due to low-lying atmospheric
-  layers, the isoplanetic patch scale will be at most a few arcminutes
+  layers, the isoplanatic patch scale will be at most a few arcminutes
   \citep{1988ESOC...30..693B}, and smaller when the seeing comes from
   higher altitudes.}
@@ -886,5 +886,5 @@
 measurements of the same stars from different nights to tie nights
 together.  \textadd{This analysis relies on the chemical and
-  thermodynamic stability of the atmosphere during a photometic night
+  thermodynamic stability of the atmosphere during a photometric night
   so that the zero point and extinction slope are stable as a result.}
 Flat-field corrections are also determined as part of the minimization
@@ -916,5 +916,5 @@
   SDSS as an external reference, with standard deviations of (8.0,
   7.0, 9.0, 10.7, 12.4) millimags in (\grizy).  Internal comparisons
-  show the zero-points of indidual exposures to be consistent with the
+  show the zero-points of individual exposures to be consistent with the
   Ubercal solution with a standard deviation of 5 millimags.  The
   former is an upper limit on the overall system zero-point stability,
@@ -2395,5 +2395,5 @@
 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.  \textadd{We find that applying our Galactic rotatation model improves
+500pc.  \textadd{We find that applying our Galactic rotation model improves
 the systematic proper motion errors to some extent.  The standard
 deviation of the quasar proper motions (averaged on 12 arcminute
@@ -2452,5 +2452,5 @@
 astrometric analysis to provide a measurement which is robust against
 failures.  In addition to the detector effects artifacts which affect
-astrometry, the astrometric measurments may have non-Gaussian outliers
+astrometry, the astrometric measurements may have non-Gaussian outliers
 due to the high degree of structure in the astrometric transformations
 introduced by the camera optics and the atmosphere.  We have again
@@ -3118,5 +3118,5 @@
 Canada-France Imaging Survey, or CFIS, collaborations) is expected to
 release deep photometry in the {\it ugriz} bands for roughly 5000
-square degrees of the northern hemisphere with agressive photometric
+square degrees of the northern hemisphere with aggressive photometric
 precision goals.  This collaboration is in part motivated to support
 the Euclid satellite mission, which requires deep 8-band photometry to
@@ -3137,5 +3137,5 @@
 \textadd{Second, cross-comparisons between independent datasets are critical to
 reveal the limitations.  This lesson has appeared several times in our
-intestigations, in the comparison between Pan-STARRS and Gaia above,
+investigations, in the comparison between Pan-STARRS and Gaia above,
 between Pan-STARRS and SDSS \citep{2016ApJ...822...66F}, and in the
 comparison between Pan-STARRS and 2MASS \citep{2013ApJS..205...20M}.