Changeset 39855

Timestamp:

Dec 14, 2016, 5:22:30 AM (10 years ago)

Author:

eugene

Message:

updates

Location:

trunk/doc/release.2015

Files:

• ps1.analysis/analysis.tex (modified) (3 diffs)
• ps1.calibration/calibration.tex (modified) (1 diff)

trunk/doc/release.2015/ps1.analysis/analysis.tex

@@ -573 +573 @@
   this}.
 
-To choose the value of $sigma_W$, we try values of (1, 2, 3, 4.5, 6,
-9, 12, 18) pixels.  For each of these values, we then select candidate
-PSF stars based on the distribution of the measured $\sigma_{x,x},
-\sigma_{y,y}$ values.  For each test value of $\sigma_w$, determine
-the ratio $f = \frac{\sigma_{x,x} + \sigma{y,y}}{2 \sigma_w}$, i.e.,
-the ratio of the window size to the observed PSF size.  We interpolate
-to find a value of $\sigma_W$ for which $f$ is expected to be 0.65.
-\note{what is the expected ratio of $\sigma_x$ to the true value?}.
-We call this value the \code{MOMENTS_GAUSS_SIGMA}.  We use an
-aperture with a radius of \code{PSF_MOMENTS_RADIUS} = 4$\times$
-\code{MOMENTS_GAUSS_SIGMA} to select the pixels for the measurement.
+To choose the value of $\sigma_W$, we try values of (1, 2, 3, 4.5, 6,
+9, 12, 18) pixels \note{list arcseconds}.  For each of these values,
+we then select candidate PSF stars based on the distribution of the
+measured $\sigma_{x,x}, \sigma_{y,y}$ values.  For each test value of
+$\sigma_w$, determine the ratio $f = \frac{\sigma_{x,x} +
+  \sigma{y,y}}{2 \sigma_w}$, i.e., the ratio of the window size to the
+observed PSF size.  We interpolate to find a value of $\sigma_W$ for
+which $f$ is expected to be 0.65.  \note{what is the expected ratio of
+  $\sigma_x$ to the true value?}.  We call this value the
+\code{MOMENTS_GAUSS_SIGMA}.  We use an aperture with a radius of
+\code{PSF_MOMENTS_RADIUS} = 4$\times$ \code{MOMENTS_GAUSS_SIGMA} to
+select the pixels for the measurement.
 
 Once \code{PSF_MOMENTS_SIGMA} has been determined, moments are
@@ -689 +690 @@
 \sigma_{xy} & = & f_3(x,y) \\
 \end{eqnarray}
+
+\note{PV3 config values: we used 6x6 map not 3x3 (PV2) or 3rd order
+  polynomial (PV1)}
 
 PSPhot uses a single structure to represent the object model and
@@ -1597 +1601 @@
 
 \end{document}
+
+Figures Needed for this document:
+
+* illustration of peak & col for footprint
+* measured moments vs gauss window size for PS1 profile
+* PS1 PSF profiles (good and bad seeing)
+* Mxx vs Myy plane for selecting PSF stars (etc)
+* example of a very bright star, subtracted?
+* CR masking example?
+* aperture - PSF model example
+* make of the sky with galaxy region illustrated?
+
+* plots showing the quality of the data?
+
+Tables needed:
+
+* table of mask image bit values
+* table of models?

trunk/doc/release.2015/ps1.calibration/calibration.tex

@@ -1168 +1168 @@
 \begin{verbatim}
  Plots:
-* bright-end astrometry residuals
-* bright-end photometry residuals
-* photometry residuals vs camera
+* illustration of the astrometric models (schematic)
+* astrometry cross-correlation example?
+* zero point history, including / excluding ubercal? (from Eddie)
+* applied flat-field images [FITS -> png]
+* Koppenhoffer plots [from presentations]
+* DCR plots [exist]
+* astrometric flat fields [FITS -> png]
+* PV3 vs Gaia [exit]
+* PV3 quasar motions [** need to extract **]
+* bright-end astrometry residuals [running cdhist code, but is the density too low?]
+* bright-end photometry residuals [running cdhist code, but is the density too low?]
 
 \end{verbatim}