tdiff_soften.png
[PIPE2D-1340] Add noise floor when running brutus Created: 20/Dec/23 Updated: 05/Feb/24 Resolved: 05/Feb/24 |
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| Status: | Done |
| Project: | DRP 2-D Pipeline |
| Component/s: | None |
| Affects Version/s: | None |
| Fix Version/s: | None |
| Type: | Task | Priority: | Normal |
| Reporter: | Masayuki Tanaka | Assignee: | ishigaki |
| Resolution: | Done | Votes: | 0 |
| Labels: | None | ||
| Remaining Estimate: | Not Specified | ||
| Time Spent: | Not Specified | ||
| Original Estimate: | Not Specified | ||
| Attachments: |
tdiff_soften.png
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| Epic Link: | Master FLUXSTD catalog |
| Reviewers: | Masayuki Tanaka |
| Description |
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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. |
| Comments |
| Comment by ishigaki [ 17/Jan/24 ] |
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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 err^2 = err0^2 + (s*flux)^2
where "s" is a softening parameter. 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. Based on this experiment, we decided to adopt s = 0.04 as a softening parameter for the noise floor.
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| Comment by ishigaki [ 05/Feb/24 ] |
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The noise floor will be implemented for the F-star catalog (version 3.3 or later). |