Index: /trunk/doc/release.2015/ps1.detrend/detrend.tex =================================================================== --- /trunk/doc/release.2015/ps1.detrend/detrend.tex (revision 39857) +++ /trunk/doc/release.2015/ps1.detrend/detrend.tex (revision 39858) @@ -65,11 +65,11 @@ E.~A. Magnier,\altaffilmark{\IfA} P.~A. Price,\altaffilmark{\Princeton} +K.~C. Chambers,\altaffilmark{\IfA} H.~A. Flewelling,\altaffilmark{\IfA} M.~E. Huber,\altaffilmark{\IfA} +R.~H. Lupton,\altaffilmark{\Princeton} +A. Rest,\altaffilmark{\STSCI} W.~E. Sweeney,\altaffilmark{\IfA} J.~L. Tonry, \altaffilmark{\IfA} -K.~C. Chambers,\altaffilmark{\IfA} -R.~H. Lupton,\altaffilmark{\Princeton} -A. Rest,\altaffilmark{\STSCI} W.~M. Wood-Vasey,\altaffilmark{\Pitt} PS1 Builders @@ -128,5 +128,5 @@ This is the third in a series of seven papers describing the Pan-STARRS1 Surveys, -the data reduction techiques and the resulting data products. This paper (Paper III) +the data reduction techniques and the resulting data products. This paper (Paper III) describes the details of the pixel processing algorithms, including detrending, warping, and adding (to create stacked images) and subtracting @@ -139,6 +139,6 @@ %Magnier et al. 2017 (Paper II) %Pan-STARRS Data Processing Stages -\citet[][Paper II]{magnier2017c} -describes how the various data processing stages are organised and +\citet[][Paper II]{magnier2017a} +describes how the various data processing stages are organized and implemented in the Imaging Processing Pipeline (IPP), including details of the @@ -150,5 +150,5 @@ %Magnier et al. 2017 (Paper IV) %Pan-STARRS Pixel Analysis : Source Detection -\citet[][Paper IV]{magnier2017a} +\citet[][Paper IV]{magnier2017b} describes the details of the source detection and photometry, including point-spread-function and extended source fitting models, and the @@ -156,9 +156,7 @@ %Magnier et al. 2017 (Paper V) %Pan-STARRS Photometric and Astrometric Calibration -\citet[][Paper V]{magnier2017b} +\citet[][Paper V]{magnier2017c} describes the final calibration process, and the resulting photometric and astrometric quality. -The Pan-STARRS1 filters and photometric system has already been described -in detail in \cite{2012ApJ...750...99T}. %Flewelling et al. 2017 (Paper VI) %Pan-STARRS 1 Database and Data Products @@ -173,4 +171,6 @@ data products specific to that survey. The Medium Deep Survey is not part of Data Release 1. (DR1) +The Pan-STARRS1 filters and photometric system has already been described +in detail in \cite{2012ApJ...750...99T}. @@ -280,10 +280,11 @@ % Note taken verbatim from Ken's Paper 1. -\textit{Note: These papera are being placed on the arXiv.org to +\textit{Note: These papers are being placed on the arXiv.org to provide crucial support information at the time of the public release of Data Release 1 (DR1). We expect the arXiv versions to be - updated prior to submission and there could be significant - variations with the refereed papers. We apologize for the - inconvience.} + updated prior to submission to the Astrophysical Journal in January + 2017. Feedback and suggestions for additional information from early + users of the data products are welcome during the submission and + refereeing process.} % Discuss 2-phase/3-phase device differnces @@ -372,5 +373,5 @@ between exposures. -Both of these types of persistance trails are measured and optionally +Both of these types of persistence trails are measured and optionally repaired via the \ippprog{burntool} program. This program does an initial scan of the images, and identifies objects with pixel values @@ -380,5 +381,5 @@ that this is the functional form of this persistence effect. This also matches the expectation that a constant fraction of charge is -incompletely transfered at each shift beyond the persistence +incompletely transferred at each shift beyond the persistence threshold. Once this fit is done, the model can be subtracted from the image, and the location of the star is stored in a table along @@ -396,10 +397,10 @@ to expire. -The main concern with this method of correcting the persistance trails +The main concern with this method of correcting the persistence trails is that it is based on fits to the raw image data, which may have other signal sources not determined by the persistence effect. The presence of other stars or artifacts along the path of the burn can result in a poor model to be fit, resulting in either an over- or -under-subtraction of the persistance burn. For this reason, the image +under-subtraction of the persistence burn. For this reason, the image mask is marked with a value indicating that this correction has been applied. These pixels are not fully excluded, but they are marked as @@ -613,5 +614,5 @@ along the x-pixel axis binned along the full y-axis of the first row of cells. The raw data is shown, illustrating the positional -depenendence the dark signal has on the image values. In addition, +dependence the dark signal has on the image values. In addition, both the correct B-mode dark and incorrect A-mode dark have been applied to this image, showing that although both correct the bulk of @@ -687,5 +688,5 @@ video dark for older data simply as $VD_{2009} = D_{2009} - D_{Modern} + VD_{Modern}$ produces a satisfactory result that does not -oversubtract the amplifier glow. This is shown in figure +over subtract the amplifier glow. This is shown in figure \ref{fig:video_darks}, which shows video cells from before 2012-05-16, corrected with both the standard and video darks, with the early video @@ -706,5 +707,5 @@ % \end{subfigure} \end{minipage} - \caption{An example of the video dark model application to exposure o5677g0123o, OTA22 (2011-04-26, 43s \gps{} filter), which has a video cell located in cell xy16. The left panel shows the image data mosaicked to the OTA level, and has had the static mask applied, the overscan subtracted, the detector non-linearity corrected, and a regular dark applied. The right panel, shows the same exposure with a video dark applied instead of the standard dark. The main impact of this change is the improved correction of the corner glows, which are oversubtracted with the standard dark.} + \caption{An example of the video dark model application to exposure o5677g0123o, OTA22 (2011-04-26, 43s \gps{} filter), which has a video cell located in cell xy16. The left panel shows the image data mosaicked to the OTA level, and has had the static mask applied, the overscan subtracted, the detector non-linearity corrected, and a regular dark applied. The right panel, shows the same exposure with a video dark applied instead of the standard dark. The main impact of this change is the improved correction of the corner glows, which are over subtracted with the standard dark.} \label{fig:video_darks} \end{figure} @@ -1535,6 +1536,6 @@ distribution with a Gaussian. All pixels that were masked in the initial calculation are unmasked, and a histogram is again constructed -of the values, with a binsize set to $\sigma_{guess} / \left( N_{50} / -500 \right)$. With this binsize, we expect that a bin at $\pm 2 +of the values, with a bin size set to $\sigma_{guess} / \left( N_{50} / +500 \right)$. With this bin size, we expect that a bin at $\pm 2 \sigma$ will have approximately 50 input points, which gives a Poissonian signal to noise estimate around 7. In the case where @@ -1572,5 +1573,5 @@ disk as a $13\times{}13$ image with header entries listing the binning used. The full scale background image is then constructed by -binlinearly interpolating this binned model, and this is subtracted +bilinearly interpolating this binned model, and this is subtracted from the science image. Each object in the photometric catalog has a SKY and SKY\_SIGMA value that is the evaluation of this model at the @@ -1860,5 +1861,5 @@ Once individual exposures have been warped onto a common projection system, they can then be combined pixel-by-pixel regardless of their -original orientation. Creating a stacked image by coadding the +original orientation. Creating a stacked image by co-adding the individual warps increases the signal to noise, allowing for the detection of objects that would not be sufficiently significant to be measured from a single image. @@ -2201,5 +2202,5 @@ -Finally, a second pass at rejecting pixelsis conducted, by growing the +Finally, a second pass at rejecting pixels is conducted, by growing the current list to include pixels that are neighbors to many rejected pixels. The ISIS kernel used in the previous step is again used to @@ -2307,5 +2308,5 @@ frame is largely unmasked after combining inputs, with the only remaining masks falling on the cores of bright stars, and in small - regions around the brighest objects where the overlapping of + regions around the brightest objects where the overlapping of diffraction spike masks have removed all inputs.} @@ -2507,5 +2508,5 @@ %\czwdraft{Not happy with this.} -The Pan-STARRS1 PV3 processing has reduced an unprecidented volume of +The Pan-STARRS1 PV3 processing has reduced an unprecedented volume of image data, and has produced a catalog for the $3\Pi$ Survey containing hundreds of billions of individual measurements of