TY - JOUR
T1 - Weighing the universe with the cosmic microwave background
AU - Jungman, Gerard
AU - Kamionkowski, Marc
AU - Kosowsky, Arthur
AU - Spergel, David N.
PY - 1996
Y1 - 1996
N2 - Variations in Ω, the total density of the Universe, leave an imprint on the power spectrum of temperature fluctuations in the cosmic microwave background (CMB). We evaluate the precision with which Ω can be determined by a CMB map as a function of sky coverage, pixel noise, and beam size. Assuming only that the primordial density perturbations were adiabatic and with no prior information on the values of any other cosmological parameters, a full-sky CMB map at 0.5° angular resolution and a noise level of 15 ΩK per pixel can determine Ω with a standard error of 5%. If all other cosmological parameters are fixed, Ω can be measured to better than 1%.
AB - Variations in Ω, the total density of the Universe, leave an imprint on the power spectrum of temperature fluctuations in the cosmic microwave background (CMB). We evaluate the precision with which Ω can be determined by a CMB map as a function of sky coverage, pixel noise, and beam size. Assuming only that the primordial density perturbations were adiabatic and with no prior information on the values of any other cosmological parameters, a full-sky CMB map at 0.5° angular resolution and a noise level of 15 ΩK per pixel can determine Ω with a standard error of 5%. If all other cosmological parameters are fixed, Ω can be measured to better than 1%.
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U2 - 10.1103/PhysRevLett.76.1007
DO - 10.1103/PhysRevLett.76.1007
M3 - Article
C2 - 10061610
AN - SCOPUS:4243708143
SN - 0031-9007
VL - 76
SP - 1007
EP - 1010
JO - Physical review letters
JF - Physical review letters
IS - 7
ER -