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trunk/doc/release.2015/ps1.detrend/detrend.tex (modified) (19 diffs)
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trunk/doc/release.2015/ps1.detrend/detrend.tex
r39854 r39858 65 65 E.~A. Magnier,\altaffilmark{\IfA} 66 66 P.~A. Price,\altaffilmark{\Princeton} 67 K.~C. Chambers,\altaffilmark{\IfA} 67 68 H.~A. Flewelling,\altaffilmark{\IfA} 68 69 M.~E. Huber,\altaffilmark{\IfA} 70 R.~H. Lupton,\altaffilmark{\Princeton} 71 A. Rest,\altaffilmark{\STSCI} 69 72 W.~E. Sweeney,\altaffilmark{\IfA} 70 73 J.~L. Tonry, \altaffilmark{\IfA} 71 K.~C. Chambers,\altaffilmark{\IfA}72 R.~H. Lupton,\altaffilmark{\Princeton}73 A. Rest,\altaffilmark{\STSCI}74 74 W.~M. Wood-Vasey,\altaffilmark{\Pitt} 75 75 PS1 Builders … … 128 128 This is the third in a series of seven papers describing the Pan-STARRS1 129 129 Surveys, 130 the data reduction tech iques and the resulting data products. This paper (Paper III)130 the data reduction techniques and the resulting data products. This paper (Paper III) 131 131 describes the details of the pixel processing algorithms, including 132 132 detrending, warping, and adding (to create stacked images) and subtracting … … 139 139 %Magnier et al. 2017 (Paper II) 140 140 %Pan-STARRS Data Processing Stages 141 \citet[][Paper II]{magnier2017 c}142 describes how the various data processing stages are organi sed and141 \citet[][Paper II]{magnier2017a} 142 describes how the various data processing stages are organized and 143 143 implemented 144 144 in the Imaging Processing Pipeline (IPP), including details of the … … 150 150 %Magnier et al. 2017 (Paper IV) 151 151 %Pan-STARRS Pixel Analysis : Source Detection 152 \citet[][Paper IV]{magnier2017 a}152 \citet[][Paper IV]{magnier2017b} 153 153 describes the details of the source detection and photometry, including 154 154 point-spread-function and extended source fitting models, and the … … 156 156 %Magnier et al. 2017 (Paper V) 157 157 %Pan-STARRS Photometric and Astrometric Calibration 158 \citet[][Paper V]{magnier2017 b}158 \citet[][Paper V]{magnier2017c} 159 159 describes the final calibration process, and the resulting photometric and 160 160 astrometric quality. 161 The Pan-STARRS1 filters and photometric system has already been described162 in detail in \cite{2012ApJ...750...99T}.163 161 %Flewelling et al. 2017 (Paper VI) 164 162 %Pan-STARRS 1 Database and Data Products … … 173 171 data products specific to that survey. The Medium Deep Survey is not part 174 172 of Data Release 1. (DR1) 173 The Pan-STARRS1 filters and photometric system has already been described 174 in detail in \cite{2012ApJ...750...99T}. 175 175 176 176 … … 280 280 281 281 % Note taken verbatim from Ken's Paper 1. 282 \textit{Note: These paper aare being placed on the arXiv.org to282 \textit{Note: These papers are being placed on the arXiv.org to 283 283 provide crucial support information at the time of the public 284 284 release of Data Release 1 (DR1). We expect the arXiv versions to be 285 updated prior to submission and there could be significant 286 variations with the refereed papers. We apologize for the 287 inconvience.} 285 updated prior to submission to the Astrophysical Journal in January 286 2017. Feedback and suggestions for additional information from early 287 users of the data products are welcome during the submission and 288 refereeing process.} 288 289 289 290 % Discuss 2-phase/3-phase device differnces … … 372 373 between exposures. 373 374 374 Both of these types of persist ance trails are measured and optionally375 Both of these types of persistence trails are measured and optionally 375 376 repaired via the \ippprog{burntool} program. This program does an 376 377 initial scan of the images, and identifies objects with pixel values … … 380 381 that this is the functional form of this persistence effect. This 381 382 also matches the expectation that a constant fraction of charge is 382 incompletely transfer ed at each shift beyond the persistence383 incompletely transferred at each shift beyond the persistence 383 384 threshold. Once this fit is done, the model can be subtracted from 384 385 the image, and the location of the star is stored in a table along … … 396 397 to expire. 397 398 398 The main concern with this method of correcting the persist ance trails399 The main concern with this method of correcting the persistence trails 399 400 is that it is based on fits to the raw image data, which may have 400 401 other signal sources not determined by the persistence effect. The 401 402 presence of other stars or artifacts along the path of the burn can 402 403 result in a poor model to be fit, resulting in either an over- or 403 under-subtraction of the persist ance burn. For this reason, the image404 under-subtraction of the persistence burn. For this reason, the image 404 405 mask is marked with a value indicating that this correction has been 405 406 applied. These pixels are not fully excluded, but they are marked as … … 613 614 along the x-pixel axis binned along the full y-axis of the first row 614 615 of cells. The raw data is shown, illustrating the positional 615 depen endence the dark signal has on the image values. In addition,616 dependence the dark signal has on the image values. In addition, 616 617 both the correct B-mode dark and incorrect A-mode dark have been 617 618 applied to this image, showing that although both correct the bulk of … … 687 688 video dark for older data simply as $VD_{2009} = D_{2009} - D_{Modern} 688 689 + VD_{Modern}$ produces a satisfactory result that does not 689 over subtract the amplifier glow. This is shown in figure690 over subtract the amplifier glow. This is shown in figure 690 691 \ref{fig:video_darks}, which shows video cells from before 2012-05-16, 691 692 corrected with both the standard and video darks, with the early video … … 706 707 % \end{subfigure} 707 708 \end{minipage} 708 \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.}709 \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.} 709 710 \label{fig:video_darks} 710 711 \end{figure} … … 1535 1536 distribution with a Gaussian. All pixels that were masked in the 1536 1537 initial calculation are unmasked, and a histogram is again constructed 1537 of the values, with a bin size set to $\sigma_{guess} / \left( N_{50} /1538 500 \right)$. With this bin size, we expect that a bin at $\pm 21538 of the values, with a bin size set to $\sigma_{guess} / \left( N_{50} / 1539 500 \right)$. With this bin size, we expect that a bin at $\pm 2 1539 1540 \sigma$ will have approximately 50 input points, which gives a 1540 1541 Poissonian signal to noise estimate around 7. In the case where … … 1572 1573 disk as a $13\times{}13$ image with header entries listing the binning 1573 1574 used. The full scale background image is then constructed by 1574 bi nlinearly interpolating this binned model, and this is subtracted1575 bilinearly interpolating this binned model, and this is subtracted 1575 1576 from the science image. Each object in the photometric catalog has a 1576 1577 SKY and SKY\_SIGMA value that is the evaluation of this model at the … … 1860 1861 Once individual exposures have been warped onto a common projection 1861 1862 system, they can then be combined pixel-by-pixel regardless of their 1862 original orientation. Creating a stacked image by co adding the1863 original orientation. Creating a stacked image by co-adding the 1863 1864 individual warps increases the signal to noise, allowing for the 1864 1865 detection of objects that would not be sufficiently significant to be measured from a single image. … … 2201 2202 2202 2203 2203 Finally, a second pass at rejecting pixels is conducted, by growing the2204 Finally, a second pass at rejecting pixels is conducted, by growing the 2204 2205 current list to include pixels that are neighbors to many rejected 2205 2206 pixels. The ISIS kernel used in the previous step is again used to … … 2307 2308 frame is largely unmasked after combining inputs, with the only 2308 2309 remaining masks falling on the cores of bright stars, and in small 2309 regions around the brigh est objects where the overlapping of2310 regions around the brightest objects where the overlapping of 2310 2311 diffraction spike masks have removed all inputs.} 2311 2312 … … 2507 2508 %\czwdraft{Not happy with this.} 2508 2509 2509 The Pan-STARRS1 PV3 processing has reduced an unprec idented volume of2510 The Pan-STARRS1 PV3 processing has reduced an unprecedented volume of 2510 2511 image data, and has produced a catalog for the $3\Pi$ Survey 2511 2512 containing hundreds of billions of individual measurements of
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