A Guide to Designing Future Ground-based CMB Experiments

Technical Report · Tue Feb 18 00:00:00 EST 2014

DOI:https://doi.org/10.2172/1335486· OSTI ID:1335486

Wu, W. L.K. ^[1]; Errard, J. ^[2]; Dvorkin, C. ^[3]; Kuo, C. L. ^[1]; Lee, A. T. ^[4]; McDonald, P. ^[5]; Slosar, A. ^[6]; Zahn, O. ^[7]

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1. Stanford Univ., CA (United States); Kavli Inst. for Particle Astrophysics and Cosmology, Menlo, Park, CA (United States)
2. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Univ. of California, Berkeley, CA (United States)
3. Inst. for Advanced Study, Princeton, NJ (United States)
4. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
5. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
6. Brookhaven National Lab. (BNL), Upton, NY (United States)
7. Univ. of California, Berkeley and Lawrence Berkeley National Lab. (LBNL), CA (United States)

In this follow-up work to the High Energy Physics Community Summer Study 2013 (HEP CSS 2013, a.k.a. Snowmass), we explore the scientific capabilities of a future Stage-IV Cosmic Microwave Background polarization experiment (CMB-S4) under various assumptions on detector count, resolution, and sky coverage. We use the Fisher matrix technique to calculate the expected uncertainties in cosmological parameters in vΛCDM that are especially relevant to the physics of fundamental interactions, including neutrino masses, effective number of relativistic species, dark-energy equation of state, dark-matter annihilation, and inflationary parameters. To further chart the landscape of future cosmology probes, we include forecasted results from the Baryon Acoustic Oscillation (BAO) signal as measured by DESI to constrain parameters that would benefit from low redshift information. We find the following best 1-σ constraints: σ(M_v ) = 15 meV, σ(N_eff ) = 0.0156, Dark energy Figure of Merit = 303, σ(p_ann) = 0.00588 x 3 x 10^-26 cm³/s/GeV, σ( Ω_K) = 0.00074, σ(n_s) = 0.00110, σ( α_s) = 0.00145, and σ(r) = 0.00009. We also detail the dependences of the parameter constraints on detector count, resolution, and sky coverage.

• Research Organization: Brookhaven National Lab. (BNL), Upton, NY (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP)
• DOE Contract Number: SC00112704
• OSTI ID: 1335486
• Report Number(s): BNL-112170-2014-IR; KA2301020; TRN: US1700841
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
EXPERIMENT PLANNING
ANNIHILATION
EQUATIONS OF STATE
RELICT RADIATION
NONLUMINOUS MATTER
NEUTRINOS
LIMITING VALUES
DESIGN
RESOLUTION
COSMOLOGY
MASS
MATRICES
POLARIZATION
COSMOLOGICAL INFLATION
FUNDAMENTAL INTERACTIONS