Index: trunk/doc/release.2015/ps1.analysis/Makefile =================================================================== --- trunk/doc/release.2015/ps1.analysis/Makefile (revision 41323) +++ trunk/doc/release.2015/ps1.analysis/Makefile (revision 41324) @@ -24,5 +24,6 @@ PDFPICS = \ pics/peaks.pdf \ -pics/FWHM.smooth.trend.ps1.pdf \ +pics/galplanecut.pdf \ +pics/FWHM.smooth.trend.v1.ps1.pdf \ pics/radial.profiles.pdf \ pics/moment.class.pdf \ Index: trunk/doc/release.2015/ps1.analysis/analysis.tex =================================================================== --- trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 41323) +++ trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 41324) @@ -595,5 +595,5 @@ Footprints & Y & Y & N & Y & \ref{sec:footprints} & All detections \\ Moments & Y & Y & Y & Y & \ref{sec:moments} & All detections \\ - PSF Model & Y & Y & Y & N$^2$ & \ref{sec:PSF.Model} & Uses bright, unsat. stars \\ + PSF Model & Y & Y & Y & N$^2$ & \ref{sec:PSF.Model} & Selected bright stars \\ Bright Star Profile & Y & Y & N & Y & \ref{sec:very.bright.star} & Saturated Stars \\ Radial Profiles v1 & Y & Y & N & Y & \ref{sec:radial.profile} & All detections \\ @@ -615,5 +615,5 @@ \hline \multicolumn{5}{l}{$^1$ Background subtraction is performed by {\tt ppSub} before calling {\tt psphot}} \\ -\multicolumn{5}{l}{$^2$ PSF modeling is perform by {\tt ppSub} on the input warps before calling {\tt psphot}} \\ +\multicolumn{5}{l}{$^2$ PSF modeling is performed by {\tt ppSub} on the input warps before calling {\tt psphot}} \\ \end{tabular} \end{center} @@ -961,4 +961,5 @@ \subsection{Initial Source Detection} +\label{sec:source.detection} \subsubsection{Peak Detection} @@ -1136,20 +1137,19 @@ \caption{\label{fig:moments.window} Example of the biases encountered when measuring the second moments. A simulated image - was generated using the PS1 PSF profile. Each panel corresponds - to a different value of $\sigma_w$, corresponding to the window - FWHM values as marked. The solid red line is the true FWHM of the - PSF used to generate the stars (1.4 arcsec in all cases). The - blue solid line is the FWHM of the window function. The gray dots - are the FWHM derived from the measured second moments for stars in - the image. The median of this distribution (mag $< -10$) is - listed as ``obs''. The ratio of the median FWHM to the FWHM of - the window function is listed as ``ratio'', while the ratio of the - median FWHM to the true stellar FWHM is listed as ``bias''. The - dotted blue line is the target (65\% of the window function). In - this example, we would choose $\sigma_w$ between 0.5 and 0.8 - arcseconds so the dotted blue line would match the bright end of - the gray dots. See discussion in the text for the choice of - target window. -} + was generated using the PS1 PSF profile. Panels (a) - (e) + corresponds to a different value of $\sigma_w$, corresponding to + the window FWHM values as marked. The solid red line is the true + FWHM of the PSF used to generate the stars (1.4 arcsec in all + cases). The blue solid line is the FWHM of the window function. + The gray dots are the FWHM derived from the measured second + moments for stars in the image. The median of this distribution + (mag $< -10$) is listed as ``obs''. The ratio of the median FWHM + to the FWHM of the window function is listed as ``ratio'', while + the ratio of the median FWHM to the true stellar FWHM is listed as + ``bias''. The dotted blue line is the target (65\% of the window + function). In this example, we would choose $\sigma_w$ between + 0.5 and 0.8 arcseconds (FWHM between 2.64 and 3.52 arcseconds), so + the dotted blue line would match the bright end of the gray dots. + See discussion in the text for the choice of target window. } \end{center} \end{figure} @@ -1458,6 +1458,7 @@ arcsec (blue). The red and blue points are individual pixel values. The black line shows the PSF model with radial trend of - the form $(1 + \kappa r^2 + r^{3.33})^{-1}$.} - + the form $(1 + \kappa r^2 + r^{3.33})^{-1}$. The models use a 1D + average of the 2D analytical portion of the PSF models fitted + to these specific stars in their standard analysis. } \end{center} \end{figure} @@ -1556,10 +1557,12 @@ \includegraphics[width=\hsize]{{\picdir/moment.class}.\plotext} \caption{\label{fig:moment.class} Illustration of PSF star selection - using the second moments in $X_{\rm ccd}$ and $Y_{\rm ccd}$ - directions. The dominant clump is located in this diagram. - Galaxies tend to have a range of sizes and thus spread out above - the stars. Cosmic rays also have a range of sizes, with one - dimension smaller than the PSF. The red circle represents the PSF - star candidates. } + using the second moments. \textadd{Each point represents the + second moments in the $X_{\rm ccd}$ and $Y_{\rm ccd}$ directions + for sources measured in one chip (XY32) from a particular PS\,1 + exposure (o6065g0428o)}. The dominant clump is located in this + diagram \textadd{to identify the stars.} Galaxies tend to have a range of + sizes and thus spread out above the stars. Cosmic rays also have + a range of sizes, with one dimension smaller than the PSF. The + red circle represents the PSF star candidates. } \end{center} \end{figure} @@ -1894,5 +1897,6 @@ sky radius. These values are saved in the \textmod{output FITS catalog files}, but not sent to the PSPS. The sky radius value is used below in the -calculation of the Kron magnitude. +calculation of the Kron magnitude. \note{used in both versions?} +\note{calculated for the second pass?} \subsubsection{Kron Magnitudes} @@ -2237,19 +2241,59 @@ After a first pass through the image, in which the brighter sources above a high threshold level have been detected, measured, and -subtracted, \ippprog{psphot} optionally begins a second pass at the image. In -this stage, the new peaks are detected on the image with the bright -sources subtracted. In this pass, the peak detection process uses the -variance image to test the validity of the individual peaks. All peaks -with a significance greater than a user-defined minimum threshold are -accepted as sources of potential interest. - -The sources which are measured in this faint-source stage are clearly -low significance detections. The PV3 threshold for the bright source -analysis is a signal-to-noise of 20. The flag bit -\code{PM_SOURCE_MODE2_PASS1_SRC} is raised for sources detected in -this initial analysis stage. The lower limit cutoff for the faint -source analysis in PV3 is a signal-to-noise of 5.0. Sources detected -in the faint source stage are fitted with the PSF model using the -linear, ensemble fitting process. +subtracted, \ippprog{psphot} optionally begins a second pass at the +image. \textadd{Some of the steps described in the previous sections + are repeated in this analysis, though with some modifications as + discussed below.} + +\textadd{The source detection steps described in + Section~\ref{sec:source.detection} are repeated. To start, the + sources detected in the previous steps are subtracted from the + image, and the variance enhanced by adding the variance predicted by + the model to the variance image, doubling the effective variance at + the location of previously detected sources. As in + Section~\ref{sec:peaks}, the image is smoothed, but in this pass it + is convolved with the PSF determined above, not a place-holder + Gaussian. The new peaks are detected on the smoothed image. The + peak detection process again uses the variance image to test the + significance of the individual peaks. All peaks with a significance + greater than a user-defined minimum threshold are accepted as + sources of potential interest. Footprints are again generated as in + Section~\ref{sec:footprints}.} + +\textadd{Next, moments are measured as in Section~\ref{sec:moments}. + In this pass, however, the size of the window function applied for + the measurement of the moments is fixed at the value determined from + the bright source analysis. All sources, including those measured + in the bright-source analysis (which are re-added to the image and + their variance reset), are then simultaneously fit for their flux + normalizations as in Section~\ref{sec:ensemble.fitting}. In this + step, the `best' model is used for each source, either a PSF model + or the unconvolved extended source model determined in + Section~\ref{sec:nonlinear.galaxy.model}. For the newly detected + sources, the PSF model is used, with the position set by the + centroids.} + +\textadd{After the flux-normalization is calculated, the moments + are used to calculate the preliminary Kron radius and flux (see + Section~\ref{sec:kron.mags}). These are in turn used to assess the + source sizes as in Section~\ref{sec:source.size}. However, the + non-linear fitting steps for the PSF model fits + (Section~\ref{sec:nonlinear.psf.model}) and the extended source + model fits (Section~\ref{sec:nonlinear.galaxy.model}) are not + performed for these faint sources. These steps are skipped for two + reasons: First, the non-linear fitting steps are costly in terms of + computation time and the faint sources usually far out-number the + brighter sources. Second, since these are faint sources they do not + have the signal-to-noise to constrain models with many additional + parameters. In addition, the positions (for PSF sources) are not + much improved using the non-linear fitting compared with the + non-parametric centroid measurement for these faint sources. + \note{show with a model}.} + +The PV3 threshold for the bright source analysis is a signal-to-noise +of 20. The flag bit \code{PM_SOURCE_MODE2_PASS1_SRC} is raised for +sources detected in this initial analysis stage. The lower limit +cutoff for the faint source analysis in PV3 is a signal-to-noise of +5.0. In the \ippprog{psphotStack} version of the code, the 5 filter images @@ -2333,6 +2377,6 @@ pointing compared to the next 17 images, after correction for a relative zero point, as a function of the instrumental magnitudes - above the detection threshold. Black dots are from stars for - which both measurements have {\tt PSF\_QF} $> 0.95$, while grey + above the detection threshold. Gray dots are from stars for + which both measurements have {\tt PSF\_QF} $> 0.95$, while light red dots have lower {\tt PSF\_QF} values. The top three panels (a) - (c) show histograms in three magnitude ranges for the magnitude @@ -3066,15 +3110,16 @@ \includegraphics[width=\hsize,clip]{\picdir/{galaxy.exp.complete}.\plotext} \includegraphics[width=\hsize,clip]{\picdir/{galaxy.dev.complete}.\plotext} - \caption{\label{fig:galaxy.complete} Top: Completeness curves for - simulated galaxies with Exponential profiles. Bottom: - Completeness curves for simulated galaxies with DeVaucouleur - profiles. The curves are shown as a function of the difference - between the injected instrumental magnitude of the galaxy and the - magnitude corresponding to the $5\sigma$ detection threshold for a - PSF-like source. The black curves shows the compleness for all - galaxies. The three colored curves show the completeness for - three major axis ranges. Compact galaxies are more likely to be - detected since peaks are detected after convolution with the - PSF. } + \caption{\label{fig:galaxy.complete} {\bf Panel (a):} Completeness + curves for simulated galaxies with Exponential profiles. {\bf + Panel (b):} Completeness curves for simulated galaxies with + DeVaucouleur profiles. The curves are shown as a function of the + difference between the injected instrumental magnitude of the + galaxy and the magnitude corresponding to the $5\sigma$ detection + threshold for a PSF-like source. The black curves shows the + compleness for all galaxies. The three colored curves show the + completeness for three major axis ranges. Compact galaxies are + more likely to be detected since peaks are detected after + convolution with the PSF. \textadd{The simulated images have seeing of + 1\arcsec, equal to pixels.}} \end{center} \end{figure} @@ -3084,8 +3129,12 @@ the Exponential and DeVaucouleur models, respectively. Both figures show the reliability of the measured magnitudes, major -and minor axis sizes, and ellipticities. For all recovered +and minor axis sizes, and \textadd{ellipticities, which we represent as +$\frac{R_{\rm Major} - R_{\rm Minor}}{R_{\rm Major} + R_{\rm + Minor}}$. Galaxies are grouped in 0.1 magnitude bins based +on their injected magnitudes. +For all recovered parameters, the standard deviation of the difference between the -measured parameter and the truth value is shown for all galaxies as a -function of magnitude, as well as for subsets in major-axis ranges. +measured parameter and the truth value is shown for all galaxies in +each magnitude bin, as well as for subsets in major-axis ranges.} The mean of the difference, illustrating any biases, is also given for all galaxies. The comparison for the major and minor axis sizes @@ -3106,6 +3155,19 @@ \begin{center} \includegraphics[width=\hsize,clip]{\picdir/{galaxy.exp.params}.\plotext} + \caption{\label{fig:exp.params} Parameter recovery for simulated - galaxies with Exponential profiles. } + galaxies with Exponential profiles. In each panel, we show + several statistics for the difference between the truth parameter + and the measured value for galaxies in a series of brightness + bins, ranging from 5 magnitudes to 0.5 magnitudes brighter than + the PSF $5-\sigma$ detection threshold. Statistics, as shown in + the legend, include the average difference, the standard deviation + for all galaxies in the bin, and the standard deviations for 3 + major axis ranges. Panel (a) through (d) show in order the + recovered magnitudes, ellipticity, major axis size; minor axis + size. Panels (e) and (f) show statistics for the major and minor + axis difference as a fraction of the truth value. The average + magnitude difference is plotted so that positive numbers mean the + fitted flux is brighter than the injected flux. } \end{center} \end{figure*} @@ -3116,5 +3178,6 @@ \includegraphics[width=\hsize,clip]{\picdir/{galaxy.dev.params}.\plotext} \caption{\label{fig:dev.params} Parameter recovery for simulated - galaxies with DeVaucouleur profiles. } + galaxies with DeVaucouleur profiles. See + Figure~\ref{fig:exp.params} for complete explanation.} \end{center} \end{figure*} Index: trunk/doc/release.2015/ps1.analysis/response.txt =================================================================== --- trunk/doc/release.2015/ps1.analysis/response.txt (revision 41323) +++ trunk/doc/release.2015/ps1.analysis/response.txt (revision 41324) @@ -77,5 +77,5 @@ state the same for galaxy astrometry, fluxes and colors. -**** +**** TBD A detail of the code is presented (variable names, etc) that imply @@ -96,5 +96,5 @@ that the photometric goals are achieved -**** see note section Forced PSF Phot +**** TBD see note section Forced PSF Phot - Sec 7, where the image differencing detections and photometry is used @@ -437,5 +437,5 @@ range. -**** TDB: was the turned on for PV3? +**** TBD: was the turned on for PV3? Sec 4.7: @@ -719,5 +719,5 @@ each of the sub-panels (a), (b), etc, and describe in the caption. -**** TBD: fixed for Figures 2, 5, 6 TBD: 8, 9, 10 +** fixed for Figures 2, 5, 6, 8, 9, 10 Figure 2: @@ -746,5 +746,5 @@ particular stars -**** TBD: NEED to examine how figure was created +** the lines are a 1D average of the PSF models fitted to these stars (added to caption) Figure 4: @@ -752,5 +752,5 @@ denoted by a point. -**** TBD +** updated the caption Figures 5 and 6: @@ -766,5 +766,5 @@ - Caption should specify the seeing of these images (not in the text either). -**** TBD +** added to caption and text Figures 8 and 9: @@ -774,5 +774,5 @@ in the text. The other 4 panels could refer to the explanation in Sec 5.5. -**** TBD +** captions update to be more informative. References: