Difference between revisions of "UCSD-2019: Analysis/Pipeline Working Group: Maps to C ell"
From CMB-S4 wiki
Jump to navigationJump to search (→Charge) |
(→Charge) |
||
| Line 2: | Line 2: | ||
== Charge == | == Charge == | ||
| + | |||
| + | '''Note that "Maps to Cl" is actually shorthand for "Maps to Cl to Parameters" or "Maps to Parameters from (non-low-ell-BB) Power Spectra." This is important for understanding the charge and defining the responsibilities of this group.''' | ||
The charge from the meeting SOC is twofold (see https://docs.google.com/document/d/1KtRif7_BPi3gACMkIA7__AWK63iUJiljN6UlKI41MS0/edit for the exact charge). One part is a set of general instructions for all analysis working groups: | The charge from the meeting SOC is twofold (see https://docs.google.com/document/d/1KtRif7_BPi3gACMkIA7__AWK63iUJiljN6UlKI41MS0/edit for the exact charge). One part is a set of general instructions for all analysis working groups: | ||
Revision as of 14:33, 11 October 2019
Contents
Charge
Note that "Maps to Cl" is actually shorthand for "Maps to Cl to Parameters" or "Maps to Parameters from (non-low-ell-BB) Power Spectra." This is important for understanding the charge and defining the responsibilities of this group.
The charge from the meeting SOC is twofold (see https://docs.google.com/document/d/1KtRif7_BPi3gACMkIA7__AWK63iUJiljN6UlKI41MS0/edit for the exact charge). One part is a set of general instructions for all analysis working groups:
- Identify key decisions that must be made (and justified) prior to CD-1,
- Make progress on (or actually make) those decisions,
- Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,
- Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.
The other part is a set of specific questions to support other working groups / WBSs as we move to the next level of design. Our questions are:
- How are we calibrating beams to meet high-ell science requirements? Can we use high S/N point sources alone?
- How does the galaxy impact Neff inference?
- Does this drive frequency coverage?
- Is there a path to realistically achieve both the necessary cadence for transients and the necessary sky coverage for light relics goals?
- What are the necessary analysis tools to answer these questions?
Agenda
Remote attendance
