Difference between revisions of "Plan for next Galactic Phase-2sims"
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| − | Phase 2: Foreground modeling update | + | |
| + | == Phase 2: Foreground modeling update == | ||
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Will generate second set of PySM maps using: | Will generate second set of PySM maps using: | ||
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Phase-1 model = s1d1a1 | Phase-1 model = s1d1a1 | ||
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Model planned to be used = s3d4a2 | Model planned to be used = s3d4a2 | ||
This has the following components: | This has the following components: | ||
| − | Synchrotron, model = synchrotron3 (same MAMD spatial variation as ‘nominal’, but globally curved power law) | + | * Synchrotron, model = synchrotron3 (same MAMD spatial variation as ‘nominal’, but globally curved power law) |
| − | ThermalDust, model = dust4 (two components, using Finkbeiner/Meisner model) | + | * ThermalDust, model = dust4 (two components, using Finkbeiner/Meisner model) |
| − | SpinningDust, model = spdust2 (2% polarized AME) | + | * SpinningDust, model = spdust2 (2% polarized AME) |
The details are all described further in Thorne et al, https://arxiv.org/abs/1608.02841. The effects on the global spectrum are shown in this figure: | The details are all described further in Thorne et al, https://arxiv.org/abs/1608.02841. The effects on the global spectrum are shown in this figure: | ||
| − | [[File: | + | [[File:Pysm_freq.png|600px]] |
Next step underway is implementing Brandon Hensley’s new dust model into PySM code; Brandon and Ben are working on this. | Next step underway is implementing Brandon Hensley’s new dust model into PySM code; Brandon and Ben are working on this. | ||
Revision as of 12:23, 15 February 2017
Phase 2: Foreground modeling update
Will generate second set of PySM maps using: https://github.com/bthorne93/PySM_public
Phase-1 model = s1d1a1
Model planned to be used = s3d4a2
This has the following components:
- Synchrotron, model = synchrotron3 (same MAMD spatial variation as ‘nominal’, but globally curved power law)
- ThermalDust, model = dust4 (two components, using Finkbeiner/Meisner model)
- SpinningDust, model = spdust2 (2% polarized AME)
The details are all described further in Thorne et al, https://arxiv.org/abs/1608.02841. The effects on the global spectrum are shown in this figure:
Next step underway is implementing Brandon Hensley’s new dust model into PySM code; Brandon and Ben are working on this.
