https://pfspipe.ipmu.jp/jira This file is an XML representation of an issue en-us 8.3.4 803005 13-09-2019 https://pfspipe.ipmu.jp/jira/browse/PIPE2D-1340 DRP 2-D Pipeline <p>Add a noise floor to each filter when running brutus and see how the stellar parameter estimates changes for, e.g., SEGUE stars. The noise floor is meant to reduce effects of systematic zero-point errors and underestimated photometric uncertainties.</p> PIPE2D-1340

Add noise floor when running brutus

Task Normal Done Done ishigaki Masayuki Tanaka Wed, 20 Dec 2023 06:41:13 +0000 Sun, 4 Feb 2024 23:44:51 +0000 Sun, 4 Feb 2024 23:44:51 +0000 0 2 <p>The figure in the attachments above shows the median (left axis) and the dispersion (right axis) of the difference in the effective temperatures from photometry by brutus and from spectroscopy by SEGUE, after adding noises according to</p> <p>err^2 = err0^2 + (s*flux)^2</p> <p> </p> <p>where "s" is a softening parameter.  </p> <p>The comparison is made for a subset of the SEGUE sample. The dispersion is calculated based on the 25% and the 70% percentiles of the differences. The horizontal axis is the adopted value of s.</p> <p>Based on this experiment, we decided to adopt s = 0.04 as a softening parameter for the noise floor. </p> <p> </p> <p>   </p> <p>The noise floor will be implemented for the F-star catalog (version 3.3 or later).</p> Development Epic Link PIPE2D-1277 Rank 0|zzt0pj: Reviewers msyktnk