Difference between revisions of "SLAC-2017:FSM Small angular scales"

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* Marcelo Alvarez - extragalactic sims
 
* Marcelo Alvarez - extragalactic sims
 
* Kevin Huffenberger (remote, 5 min) - Foregrounds and Atm noise for tSZ science [[Media:huffenberger_src_atm_sz.pdf|slides]]
 
* Kevin Huffenberger (remote, 5 min) - Foregrounds and Atm noise for tSZ science [[Media:huffenberger_src_atm_sz.pdf|slides]]
* Simone Ferraro - foregrounds for kSZ
+
* Simone Ferraro - foregrounds for kSZ [[Media:Foregrounds_ferraro.pdf | slides]]
 
* Lindsay Bleem - more on sims
 
* Lindsay Bleem - more on sims
  

Revision as of 15:42, 28 February 2017

Back to SLAC-2017 main page

Foregrounds, Systematics and Modeling: Small Angular Scales

Post session talks here.

Questions To be addressed for each small-scale science ‘probe’ (TT/TE/EE, lensing, tSZ/kSZ) towards defining measurement requirements - to start discussion/for context


How large do the large telescopes need to be?

  • Current status: studies indicate 5m is sufficient for lensing (mnu and delensing) and high-ell TE/EE science (Neff), but may not be enough for cluster-derived science. Extra resolution doesn’t seem needed for cleaning TE/EE and lensing.
  • To-do—push forward cluster forecasts (see lunchtime discussion).


Can we achieve science requirements given realistic atmospheric noise?

  • Current status: realistic atmospheric noise consistent with Chilean observations without HWP has now been modeled and included in fisher forecasts for high-ell and lensing science. Neff/mnu parameters are not degraded.
  • To-do: include multi-freq realistic atmospheric noise in tSZ/kSZ forecasts, include South Pole noise curves. Establish agreement on atmospheric noise model being used by everyone.


How many/which wavelengths do we need in the large telescopes?

(1) for TE/EE 2-pt for Neff

  • Current status: indicates that three is sufficient, based on new power spectrum simulations.
  • To-do: check impact of Galactic contamination

(2) for lensing (mnu/delensing) to avoid EB lensing bias

  • Current status: perhaps only 90/150/220 needed, but work underway to test effect on lensing of expected non-Gaussian dust foregrounds. Might need synchrotron channels.
  • To-do: continue this work, test other sims.

(3) for tSZ/kSZ (mnu/w/patchy-tau/growth/feedback)

  • Current status: at least 90, 150, 220 for tSZ. Suspect 270 GHz will be beneficial but assess expected noise levels. More frequencies would help separate kSZ, especially in power spectrum for reionization.
  • To-do: run cluster forecasts (for counts, tSZ power spectrum, y-maps, kSZ signal) on extragalactic sims


What are our systematic requirements for the 2pt and 4pt functions?



Some people who have things to say on these topics:


  • Matthew Hasselfield - atmospheric noise model for large telescopes

Neff (TE/EE)-Discussion of Systematics and Foregrounds

  • Dan Green - Overview + Beams/Pointing - slides

Lensing-related

  • Alex van Engelen - Impact of polarized dust on lensing
  • Mat M. / Colin H. - Multigrequency cleaning and extra spatial filtering
  • Yuuki Omori - Biases from extragalatic sources in temperature lensing

Cluster-related

  • Marcelo Alvarez - extragalactic sims
  • Kevin Huffenberger (remote, 5 min) - Foregrounds and Atm noise for tSZ science slides
  • Simone Ferraro - foregrounds for kSZ slides
  • Lindsay Bleem - more on sims

Notes from session

Take notes here.

Action items/Next steps

Summarize action items here