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| 20181029_beam_sidelobes_conviqt_simulation [2018/10/29 12:36] – zonca | 20181029_beam_sidelobes_conviqt_simulation [2018/12/11 14:56] (current) – kyoung | ||
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| ===== Configuration ===== | ===== Configuration ===== | ||
| - | * 1 pixel in band 12 at 154.80 GHz | + | |
| - | * 4 detectors, 0,90,45,135 degrees | + | * 4 detectors, 0,90,45,135 degrees |
| - | * realistic beams with center masked | + | * realistic beams with center masked |
| - | * boresight pointing | + | * boresight pointing |
| - | * PySM input sky | + | * PySM input sky |
| - | * 1 year | + | * 1 year |
| ===== Discussion and plots ===== | ===== Discussion and plots ===== | ||
| - | * [[Github issue with discussion|https:// | + | |
| - | * [[Github pull request with implementation|https:// | + | * [[https:// |
| - | * [[Notebook with map plots|https:// | + | * [[https:// |
| + | * Also scattered among daily updates on the systematic effects [[systematicswg|telecon page]] | ||
| + | |||
| + | ===== Summary plots ===== | ||
| + | |||
| + | * 4 pi beams, main beam is at the plot center: {{:: | ||
| + | * These beams had the central 10 deg peak removed and filled with the value of the neighboring pixels. This clipped beam was then used in conviqt. Original and clipped x-pol beam: {{:: | ||
| + | * Input Galaxy maps, smoothed to 10 deg: | ||
| + | * Ouput maps from Conviqt nside=512: | ||
| + | * Power spectrum of far sidelobe map masked with 43% Planck mask: | ||
| + | * Mask: | ||
| + | |||
| + | |||
| + | |||
| + | |||
| + | ===== Partial cleaning ===== | ||
| + | |||
| + | To give some idea of what level of removal is necessary I multiplied the sidelobe by a scaling factor, alpha, and added noise then recalculated the Cl' | ||
| + | |||
| + | Possible noise levels to compare sidelobes to: | ||
| + | * Depth for 1 year for 1 wafer is 0.1 uK deg. | ||
| + | * Depth for 5 year for 1 wafer is 0.05 uK deg. | ||
| + | * Depth for 5 year for all 6 wafers is 0.02 uK deg. | ||
| + | * Depth for the full mission is 0.01 uK deg. | ||
| + | |||
| + | Intensity of sidelobes, all units are uK, Q and U are the median and max of absolute value of Q, U: | ||
| + | | | ||
| + | | Masked map | Mean | 0.10 | 0.018 | 0.015 | | ||
| + | | ::: | Max | 0.21 | 0.12 | 0.11 | | ||
| + | | Full map | Mean | 0.28 | 0.022 | 0.014 | | ||
| + | | ::: | Max | 2.6 | 0.58 | 0.14 | | ||
| + | |||
| + | When looking at the masked map, which is what makes sense for B-modes as this is the cleanest 40% of the sky, the average polarized sidelobe level is less than the map noise. | ||
| + | |||
| + | * Power spectra for masked FSL, no noise added. {{:: | ||
| + | * Power spectra for masked FSL*0.6 + 0.05 uK deg noise: {{:: | ||
| + | * Power spectra for masked FSL*0.25 + 0.02 uK deg noise: {{:: | ||
| + | * Power spectra for masked FSL*0.10 + 0.01 uK deg noise: {{:: | ||
| + | |||
| + | For these power spectra I multiplied by the FSL map by alpha, added white noise where each map pixel value is drawn from a gaussian with sigma equal to the quoted noise level (scaled to appropriate pixel size, nside=512), and applied the galaxy mask. The power spectra are calculated using the healpy anafast function. | ||
| + | |||
| + | **Bottom line: | ||
| ===== Results location ===== | ===== Results location ===== | ||
| NERSC | NERSC | ||
| - | `/ | + | '' |
| tape | tape | ||
| - | `~zonca/ | + | '' |