Closed moustakas closed 6 years ago
I'm planning on looking at this near-term (at least for bright stars)
@geordie666 Can you briefly summarize what has been incorporated in terms of the bright-star mask (or point to where this was discussed previously -- I can't seem to find it)?
Related: The BGS WG is finding a large excess of sources in the small-scale angular correlation function (at 17<r<20) that we've tracked down to Messier/NGC-sized contaminants. See here, for example -- with many thanks to @ekitanidis for producing these. If we could incorporate even a basic Messier/NGC/UGC mask into our target selection code (or, alternatively, imaginglss), that would be very helpful.
I think you're conflating two different bright star masks. The bright star mask to deal with large-scale structure is off-project. It would be a product of the science working groups. The bright star mask being built on-project (in the brightstar branch on desitarget https://github.com/desihub/desitarget/tree/brightstar) is to prevent saturation of adjacent fibers. If the goal of a mask is to remove potential LSS contaminants, then that would be a product of the science working groups. I believe Ashley Ross and the image validation working group or doing some work in that direction.
Note that there's no particular reason to apply masks for the purpose of science analyses a priori, other than to save some fibers in drastic cases. Such masks could be applied to targets after spectra have been taken in order to conduct science analyses. Such masks could, also, be applied in targeting, but then they'd have to be consistently applied again when studying, e.g., LSS. Whether to apply "science/LSS" masks during targeting or not is a decision for the science working groups.
On Fri, Jan 27, 2017 at 8:32 AM, John Moustakas notifications@github.com wrote:
@geordie666 https://github.com/geordie666 Can you briefly summarize what has been incorporated in terms of the bright-star mask (or point to where this was discussed previously -- I can't seem to find it)?
Related: The BGS WG is finding a large excess of sources in the small-scale angular correlation function (at 17<r<20) that we've tracked down to Messier/NGC-sized contaminants. See here https://desi.lbl.gov/trac/wiki/BrightGalaxyWG/TeleconNotes, for example -- with many thanks to @ekitanidis https://github.com/ekitanidis for producing these. If we could incorporate even a basic Messier/NGC/UGC mask into our target selection code (or, alternatively, imaginglss), that would be very helpful.
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A lot of progress has been made on this issue both on the imaging and the target selection side and I think we have a solid plan going forward. Closing this issue, which was more focused on discussion rather than a particular coding request.
Pasting from the thread [desi-targets 1068]:
@djschlegel suggests: