Index: trunk/doc/release.2015/ps1.analysis/analysis.tex =================================================================== --- trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 39839) +++ trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 39845) @@ -410,5 +410,5 @@ The variance image, if not supplied is constructed by default from the flux image using the configuration supplied values of \code{GAIN} and -\code{READ\_NOISE} to calculate the appropriate Poisson statistics for +\code{READ_NOISE} to calculate the appropriate Poisson statistics for each pixel. In this case, the image is assumed to represent the readout from a single detector, with well-defined gain and read noise @@ -444,5 +444,5 @@ image. The background image and the background standard deviation image are kept in memory from which the values of \code{SKY} and -\code{SKY\_SIGMA} are calculated for each object in the output catalog. +\code{SKY_SIGMA} are calculated for each object in the output catalog. \subsection{Initial Object Detection} @@ -458,6 +458,6 @@ the covariance, if known. At this stage, the goal is only to detect the brighter sources, above a user defined S/N limit (configuration -keyword: \code{PEAKS\_NSIGMA\_LIMIT}). A maximum of -\code{PEAKS\_NMAX} are found at this stage. The detection efficiency +keyword: \code{PEAKS_NSIGMA_LIMIT}). A maximum of +\code{PEAKS_NMAX} are found at this stage. The detection efficiency for the brighter sources is not strongly dependent on the form of this smoothing function. @@ -546,5 +546,5 @@ {\em key col} for this peak (as used in topographic descriptions of a mountain). If the key col for a given peak is less than -\code{FOOTPRINT\_CULL\_NSIGMA\_DELTA} (4.0) sigmas below the peak of +\code{FOOTPRINT_CULL_NSIGMA_DELTA} (4.0) sigmas below the peak of interest, the peak is considered to be {\em locally insignificant} and removed from the list of possible detections. In the vicinity of a @@ -581,9 +581,9 @@ 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 +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 measured as defined below. @@ -615,5 +615,5 @@ If the measured centroid coordinates ($x_0, y_0$) differs from the -peak coordinates be a large amount (\code{MOMENT\_RADIUS}), then the +peak coordinates be a large amount (\code{MOMENT_RADIUS}), then the peak is identified as being of poor quality and is rejected. In both of these cases, it is likely that the `peak' was identified in a @@ -638,6 +638,6 @@ limited at the low and high ends by $R_{\rm min} < M_r < R_{\rm max}$ where $R_{\rm min}$ is the first radial moment of the PSF stars, or -0.75$\times$ \code{MOMENTS\_GAUSS\_SIGMA} if that cannot be -determined. $R_{\rm max}$ is set to \code{PSF\_MOMENTS\_RADIUS}, the +0.75$\times$ \code{MOMENTS_GAUSS_SIGMA} if that cannot be +determined. $R_{\rm max}$ is set to \code{PSF_MOMENTS_RADIUS}, the size of the moments aperture. @@ -731,5 +731,5 @@ registered as part of the model function code. Another function is then used to return the appropriate function for a specific model -type. For example, the \code{psModelLookup\_GetFunction} will return +type. For example, the \code{psModelLookup_GetFunction} will return the \code{psModelLookup} function for a given model type. This mechanism makes it very easy to add new model functions into the @@ -756,5 +756,5 @@ their peaks, as well as an approximate signal-to-noise ratio. All objects with a S/N ratio greater than a user-defined parameter -(\code{PSF\_SHAPE\_NSIGMA} ???) are selected by PSPhot, though objects +(\code{PSF_SHAPE_NSIGMA} ???) are selected by PSPhot, though objects which have more than a certain number of saturated pixels are excluded at this stage. PSPhot then examines the 2-D plane of $\sigma_x, @@ -1014,5 +1014,5 @@ PSPhot will use the user-selected galaxy model to attempt the galaxy -model fits. In the configuration system, the keyword \code{GAL\_MODEL} +model fits. In the configuration system, the keyword \code{GAL_MODEL} is set to the model of interest. All suspected extended objects are fitted with the model, allowing all of the parameters to float. The @@ -1146,7 +1146,7 @@ value for the ApResid scatter is then used by PSPhot as the best PSF model for this image. The number of models to be tested is specified -by the configuration keyword \code{PSF\_MODEL\_N}. The configuration -variables \code{PSF\_MODEL\_0}, \code{PSF\_MODEL\_1}, through -\code{PSF\_MODEL\_N - 1} specify the names of the models which should be +by the configuration keyword \code{PSF_MODEL_N}. The configuration +variables \code{PSF_MODEL_0}, \code{PSF_MODEL_1}, through +\code{PSF_MODEL_N - 1} specify the names of the models which should be tested. @@ -1198,13 +1198,14 @@ The surface brightness values are sampled at a number of radial -annuli, with the radii defined in the configuration ({\tt - RADIAL.ANNULAR.BINS.LOWER \& RADIAL.ANNULAR.BINS.UPPER}). For each -source, the resulting surface brightness profile is saved in the -output cmf-file as an N-element value in the FITS table ({\tt - PROF\_SB}). The flux at each radial position and the fill-factor -(fraction of pixels used to the total possible) as also saved as -equal-length vectors in the FITS table ({\tt PROF\_FLUX and - PROF\_FILL}). The values of the radial bins are saved in the cmf -header ({\tt RMIN\_NN, RMAX\_NN}). +annuli, with the radii defined in the configuration +(\code{RADIAL.ANNULAR.BINS.LOWER} \& +\code{RADIAL.ANNULAR.BINS.UPPER}). For each source, the resulting +surface brightness profile is saved in the output cmf-file as an +N-element value in the FITS table (\code{PROF_SB}). The flux at each +radial position and the fill-factor (fraction of pixels used to the +total possible) as also saved as equal-length vectors in the FITS +table (\code{PROF_FLUX} and \code{PROF_FILL}). The values of the +radial bins are saved in the cmf header (\code{RMIN_NN}, +\code{RMAX_NN}). \note{these profiles are not saved in PSPS}