CMB-S4: Dark Radiation Anisotropy Flowdown Team (DRAFT) tool

Articles to cite:

If you use results from this repository, please cite the following articles.

• ILC residuals:
  • Raghunathan and Omori, 2023, arXiv:2304.09166.
• Fisherlens:
  • Green, Meyers, van Engelen 2016, arXiv: 1609.08143.
  • Hotinli, et al. 2023, arXiv: 2111.15036.
• This tool also uses results from the following:
  • Extragalacitc foreground modelling: Reichardt et al. 2021, arXiv: 2002.06197.
  • Galactic foreground modelling: https://pysm3.readthedocs.io/en/latest/

Results:

• ILC curves:
  • Look into this link.
    • File name:
      • Without galactic foregrounds: [expname]galaxy0[bands]_TT-EE_lmax6500_for7years.npy
      • With galactic foregrounds: [expname]galaxy0[bands]_TT-EE_galmask[0_or_1_or_2]_lmax6500_for7years.npy
        • Galactic foregrounds masks can be found here: planck_gal_fg_mask_with_cmbs4_footprint
        • 0 - GAL070 + CMB-S4 footprint.
        • 1 - GAL080 + CMB-S4 footprint.
        • 2 - GAL090 + CMB-S4 footprint.
    • S4-Wide (Chilean LAT): This is for the latest noise specs from PBDR (as of Oct 2023).
    • S4-Ultra deep (South Pole LAT: This is for the latest noise specs from PBDR (as of Oct 2023).
    • S4-Wide (Chilean LAT) achevied performance: This is best performance that can be acheived.
    • Look into read_ilc_residuals.py script to read ILC curves.
    • Look into read_lensing_noise.py script to lensing noise curves.

CMB-S4 instrument/noise specs:

Executing the script:

• Please look into (this README)(https://github.com/sriniraghunathan/DRAFT/blob/master/scripts/README.md)

Overview:

• Optimally combines data from different bands using noise + foreground signals in different bands.
  • Supports standard / constrained / partial internal linear combinations.
• Combines delensed CMB spectra and lensing spectra to forecast cosmological parameter constraints using Fisher formalism.
  • Delensing reference: Green, Meyers, van Engelen 2016, arXiv: 1609.08143.
  • Fisher code repo (yet to be integrated into this repo).
• Estimates biases in cosmological parameters due to residual foregrounds also using Fisher formalism.
  • References: Huterer & Takada 2004, arXiv: 0412142; Loverde, Hui, & Gaztanaga 2006, arXiv: 0611539; Amara & Réfrégier 2007, arXiv: 0710.5171.

Foreground modelling:

• Extragalactic foregrounds: Radio, CIB, tSZ and kSZ power spectra from SPT measurements (George et al. 2015, arXiv: 1408.3161 and Reichardt et al. 2020, arXiv: 2002.06197).
  • Assumed polarisation fractions: CIB = 2%; Radio = 3%; tSZ/kSZ = 0. But these are configurable. Look into params.ini.
• Galactic foregrounds: Dust and Synchrotron power spectra obtained from pySM3 simulations.

Contributors:

Joel Meyers, Cynthia Trendafilova, and Benjamin Wallisch.