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| imagerteleconnotes20180206 [2018/02/07 13:47] – hanany | imagerteleconnotes20180206 [2018/02/07 15:54] (current) – wenxx181 | ||
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| ====== Telecon 20180206 ====== | ====== Telecon 20180206 ====== | ||
| - | Attending: | + | Attending: |
| Notes by : Karl/Qi \\ | Notes by : Karl/Qi \\ | ||
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| === Notes === | === Notes === | ||
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| + | Focal Plane Configuration | ||
| + | |||
| + | * Orientation of scan VS orientation of detector rows | ||
| + | * Kris repeated the concern again from last week; with the hexagone wafers and current scan strategy, is it important to align rows of detectors with direction of scan? | ||
| + | * multiple detectors on a row can scan over the same track if they are aligned with direction of scan | ||
| + | * Shaul pointed out that even now there are detectors are one row, every other column though | ||
| + | * It's not very clear if this matters | ||
| + | * Spin rate is dominant over precession, so scan direction is about straight from left to right as shown | ||
| + | * Shaul: each pixel has both polarizations; | ||
| + | * Jacques: arrangement of focal plane, cross scan sampling; shaul: we will take look into Jaques' | ||
| + | * Kris: faster precession, if compare 10 days to 10 hrs, gives better sky map coverage; however, if compare 10 hrs to 2 hrs, not sure if it makes a big difference | ||
| + | * Jacques: holes on sky map will affect systematics over the focal plane | ||
| + | * Shaul: fundamental questions have not be addressed, Q and U layout has not been done | ||
| + | * Q and U alignment is flexible within wafer | ||
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| + | * ADR | ||
| + | *shaul: current model has a tank next to focal plane for ADR, but it does not need to be there there | ||
| + | *Tom: PIPER ADR | ||
| + | *continuous ADR, 4 stages | ||
| + | *stage 1, attached to brown color plate, which attach the focal plane | ||
| + | *about 9'' | ||
| + | *For PICO, one more intermediate stage, stable temperature; | ||
| + | *0.1 K fluctuates between magging and demagging; Tom will look into it how large the fluctuation is for next week | ||
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| + | * Focal Plane | ||
| + | * change: 1)central wafer, split into three: F and GHI;2) 4mm space between edges of wafers based on different experiments (4.2mm for EBEX, 4-5mm for POLARBEAR, 5.5mm for BICEP) | ||
| + | * Shaul: let's make space to 5mm | ||
| + | * less F detectors, more GHI, same numbers for others | ||
| + | * wire bonding | ||
| + | * traditional: | ||
| + | * " | ||
| + | * readout | ||
| + | * for TDM, 4 mm^2; for FDM, mainly due to large capacitors, 50-80 mm^2 | ||
| + | * FGHI need some special packing, working on | ||
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| + | * sizes of mirrors | ||
| + | * we need to increase mirror sizes if we want to use more diffraction limited field of view | ||
| + | * dimensions are shown in the slides | ||
| + | |||
| + | Cosmic Rays | ||
| + | *Roger: signals long-time constant spikes | ||
| + | *TES for X-rays, they do not see it as a driven issue; worth looking into it | ||
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