Campuses:
This shows you the differences between two versions of the page.
| Both sides previous revisionPrevious revisionNext revision | Previous revision | ||
| systematicswg:telecons:2018-04-18:start [2018/04/18 11:33] – bcrill | systematicswg:telecons:2018-04-18:start [2018/04/18 12:08] (current) – bcrill | ||
|---|---|---|---|
| Line 17: | Line 17: | ||
| * initial results: look at the pointings only to see how well the dipole is measured vs. time. | * initial results: look at the pointings only to see how well the dipole is measured vs. time. | ||
| * There are some time periods where PICO only scans along the dipole equator thus seeing no dipole signal but these only last a few days (compare with Planck where these dead periods lasted many weeks). | * There are some time periods where PICO only scans along the dipole equator thus seeing no dipole signal but these only last a few days (compare with Planck where these dead periods lasted many weeks). | ||
| - | + | * 6 hour bins were chosen, but other time periods could be chosen. | |
| + | * DaCapo run on 2-year mission for 1 detector: calibrating in 6 hour signal chunks. | ||
| + | * Maurizio would like to do naive component separation, i.e. be a little bit fancier than masking the sky. | ||
| + | * noise: white + 1/f noise (as described in the [[https:// | ||
| + | * input sky: using pysm at 90 GHz. no kinetic dipole. | ||
| + | * What is the actual deliverable here? These results set limits on how well dipole calibration on short time scales can mitigate systematic errors: perhaps revisit the systematics list in light of these results to see which are actually mitigated. | ||
| + | * Correlated noise post re-calibration | ||
| + | * next week: | ||