2012/01/25 by Esfandiar Alizadeh, Christopher M. Hirata · 2 citations
Physics and Astronomy · #Anisotropy #Astrophysics #Cosmic microwave background #Cosmology and Gravitation Theories #Galaxy #Gravitational wave #Physics #Polarization (electrochemistry) #Pulsars and Gravitational Waves Research #Quadrupole #Quantum mechanics #Radio Astronomy Observations and Technology #Redshift #Reionization #Scattering #astro-ph.CO
paper · pdf · doi:10.1103/physrevd.85.123540
18 pages, 6 figures, to be submitted to PRD
arxiv created 2012/01/25 · openalex publication_date 2012/06/26 · arxiv updated 2013/05/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Thompson scattering of cosmic microwave background (CMB) photons off of free electrons during the reionization epoch induces a correlation between the distribution of galaxies and the polarization pattern of the CMB, the magnitude of which is proportional to the quadrupole moment of radiation at the time of scattering. Since the quadrupole moment generated by gravitational waves (GWs) gives rise to a different polarization pattern than that produced by scalar modes, one can put interesting constraints on the strength of GWs on large scales by cross correlating the small scale galaxy distribution and CMB polarization. We use this method together with Fisher analysis to predict how well future surveys can measure the tensor-to-scalar ratio r. We find that with a future CMB experiment with detector noise \ensuremathΔP=2 \ensuremathμK\mathrm\text\ensuremath-arcmin and a beam width \ensuremathθFWHM=2^\ensuremath' and a future galaxy survey with limiting magnitude I<25.6 one can measure the tensor-to-scalar ratio with an error \ensuremathσr\ensuremath≃0.09. To measure r\ensuremath≈0.01, however, one needs \ensuremathΔP\ensuremath≃0.5 \ensuremathμK\mathrm\text\ensuremath-arcmin and \ensuremathθFWHM\ensuremath≃1^\ensuremath'. We also investigate a few systematic effects, none of which turn out to add any biases to our estimators, but they increase the error bars by adding to the cosmic variance. The incomplete sky coverage has the most dramatic effect on our constraints on r for large sky cuts, with a reduction in signal-to-noise smaller than one would expect from the naive estimate ((S)/(N))2\ensuremath∝fsky. Specifically, we find a degradation factor of fdeg=0.32\ifmmode±\else\textpm\fi0.01 for a sky cut of |b|>10\ifmmode^∘\else\textdegree\fi (fsky=0.83) and fdeg=0.056\ifmmode±\else\textpm\fi0.004 for a sky cut of |b|>20\ifmmode^∘\else\textdegree\fi (fsky=0.66). Nonetheless, given that our method has different systematics than the more conventional method of observing the large scale B modes directly, it may be used as an important check in the case of a detection.