Python plotting routines for MAGPHYS high (v2) and MAGPHYS+photoz are available here (click `read more' to get link to show). Please let me know if there are bugs or other issues using these.
MAGPHYS is a spectral energy distribution code that allows the user to derive key physical properties of galaxies from their ultraviolet-to-radio observations. The code continues to be maintained on the main MAGPHYS site , and you can find more information about the spectral energy distribution modelling here (2008 MNRAS article describing the original model) and here (2015 ApJ article describing the high-z extension). This blog is maintained by Elisabete da Cunha and was created to update users on code upgrades, bug fixes, etc., as well as to provide a platform for the user community to leave comments and questions and for users to interact with each other. The blog also serves as a repository for the answers to common user questions (see FAQs ).
A correction that was made a while ago but I thought I'd point out for those who did not notice the update on the filter file. Will try to update in real time now that we have a MAGPHYS user blog! The Herschel PACS and SPIRE response functions originally introduced in the MAGPHYS filter file were in the wrong units (filters #169 to #174). The effect on SED fits is small, but can be noticeable at the level of a few K for the coldest dust component. Thanks very much to Steve Maddox and Loretta Dunne for spotting this! I updated the filter file with the correct response functions in Nov 2016. The new PACS and SPIRE filters are #441 to #446 in the filter file and they are labelled "recommended": those are the ones that should be used for Herschel point source fits. Please note that for extended sources we include recommended SPIRE response functions (#447 to #449) provided by Steve Maddox.
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