LBNL-2016: Dark Energy / Gravity / Dark Matter

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Session Organizers: Robert Caldwell, Scott Dodelson, Cora Dvorkin

Break-out sessions:


4.1 Dark Energy and Modified Gravity

4.1.1 Models and parameters

4.1.2 CMB Dark Energy Observables Cluster abundance and mass Lensing Kinematic SZ

4.2 Dark Matter

4.2.1 Dark Matter Annihiliation

4.2.2 Non-standard Dark Matter Interactions Dark Matter-Baryon Scattering Dark Matter-Radiation Interaction

4.2.3 Ultralight axions

Plan for 40 minute DE/MG parallel session [DM will need ~20 min]


1) Reality check for our section: Are we missing anything important?

2) What are the open, provocative questions relevant to dark energy, gravity, dark matter?

9:15-9:35: Probes of DE/MG: 1 slide each explaining what they are aiming to do and what the open issues are that should be discussed at the plenary.

All: are we missing anything? Should ISW be included? [This could be an opportunity to present a slide on something you think is missing; please let us know in advance].

9:35-9:55: Forecasts: What space should we use for forecasts? Maybe move from simple [(w,w’)] to more complex [sigma_8(z)] to more complex [deviations from GR as a function of k,z: \mu,\Sigma] to EFT? Open discussion; please come ready to volunteer! We will try to identify a path forward, including who will do what.

9:55-10:15 Dark Matter

Goal: Present this plan in the plenary and highlight any open questions so the larger group can weigh in

[[Parallel Session Summary ]]

Dark Energy: Does the science book need to be restructured? Shall we divide it into top-level science case, science observables, instrumentation, foregrounds, survey configurations, external data, analysis/simulation, constraints / forecasts, results.

Shall we use the standard dark energy figure of merit or is there a better index to assess the experiment? For example, the standard FOM may not capture the range of CMB-S4-sensitive modified gravity or early dark energy behavior.

Are we settled with the systematics or issues of the observables, such as clusters and kSZ?

Cross correlations: how will the data be composed internally, and externally?

What external data will be in hand by the time of CMB-S4? How can they be used to bring out the most in CMB-S4? (data sets, as well as parameters)

What are the baseline experimental configurations and what are the timelines?

Dark Matter: Shall we reframe the dark matter section as a broad based complementary search for new dark matter phenomena?

What models should we feature or focus on?

What are the unique features of the experiment (angular scales, redshift, polarization) that we can use to shed light on dark matter?

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