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| ====== Telecon 20171212 ====== | ====== Telecon 20171212 ====== | ||
| - | Attending: | + | Attending: |
| Notes by : Karl \\ | Notes by : Karl \\ | ||
| === Agenda=== | === Agenda=== | ||
| + | * No telecon next week | ||
| * Preparations for TeamX (JPL + UMN, led by Brian/Amy) | * Preparations for TeamX (JPL + UMN, led by Brian/Amy) | ||
| - | * Cosmic Rays (Jeff Filippini) | + | * Cosmic Rays (Jeff Filippini) |
| - | * GRASP (Brad Johnson) | + | * GRASP (Brad) |
| - | * Focal plane model V3.0 (Young) | + | * {{:: |
| === Notes:=== | === Notes:=== | ||
| + | |||
| + | No telecon next week (TeamX meeting) | ||
| + | |||
| + | Preparations for TeamX (JPL + UMN, led by Brian/Amy) | ||
| + | * Brian making a list of files TeamX needs. | ||
| + | * CodeV files. | ||
| + | * prep a 1.6 m and 1.2 m versions. | ||
| + | * 1.4 m with coma-correction and without. | ||
| + | * Kevin' | ||
| + | * Will get files/ | ||
| + | * Shaul will ensure Roger has a wire count for FDM. | ||
| + | * Cryogenics, ADR cooling power 10 uW. Kevin made a model that works for this. | ||
| + | * Roger estimated FP mass, for 12-15k detectors estimate 7-8 kg. | ||
| + | * in EPIC-IM a 1.5 m focal plane was 26 kg. | ||
| + | * Core had similar focal plane size with waveguides and was 8 kg. | ||
| + | |||
| + | Cosmic Rays (Jeff Filippini) B-mode from Space slides | ||
| + | * first 2-3 slides are intro to problem. | ||
| + | * Antarctic balloons good approximation of space at L2 | ||
| + | * impact rate set by area, deposition energy set by thickness. | ||
| + | * Planck issue was wafer hits. long time constant (seconds) and high rate (few Hz) | ||
| + | * new space mission, wafers hit at 100 Hz. need short time constants. need bolometers unresponsive to cosmic ray hits on wafers. | ||
| + | * should be able to absorb ballistic phonons and cool to thermal if wafer is coated in a superconductor (or normal metal). | ||
| + | * then heatsink wafer well. | ||
| + | * if crosstalk of cosmic ray hits is nonlinear. | ||
| + | * consider hits to readout electronics as well. LC resonators could shift. SQUIDs respond. etc. | ||
| + | * Shaul: anyone planning to test this? like the phonon down-conversion? | ||
| + | * Jeff yes, in progess. and Berkeley is also testing this month. | ||
| + | * SPIDER data. low coincidence rate, so no long distance propogation across wafer. | ||
| + | * in lab tests see ~ 8 ms time constants. See saturated TES at high energies. | ||
| + | * saw ' | ||
| + | * Think about what readout does when large energy depositions. | ||
| + | * Jeff: No evidence for bolometer response to cosmic rays hitting wafer. | ||
| + | * Shaul: what are 1st priorities to look for in EBEX data? | ||
| + | * Jeff: Coincidence is good. | ||
| + | * Shaul: Why does SPIDER see no long glitches? | ||
| + | * Jeff: Better heat sinking. easier at 300 mK. | ||
| + | * Shaul: 100 mK measurements would be nice. Really show the problem or not. | ||
| + | * Jeff: 100 mK is planned at JPL. | ||
| + | |||
| + | GRASP (Brad) | ||
| + | * Running, but Brad can't attend so topic delayed to next telecon. | ||
| + | |||
| + | Focal plane model, V3.0 (Young) | ||
| + | * Focal plane with pixels and hexagonal wafers is laid out. | ||
| + | * New sensitivity is 0.62 uK arcmin. | ||
| + | * Version posted on wiki. | ||
| + | * Toki: are all arrays < 150 mm wafer? | ||