Published May 15, 2009 | Version v1
Journal article

B-mode CMB polarization from patchy screening during reionization

  • 1. Kavli Institute for Cosmological Physics and Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637 (United States)
  • 2. Department of Physics, University of Chicago, Chicago, Illinois 60637 (United States)
  • 3. Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637 (United States)
  • 4. Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA (United Kingdom)

Description

B modes in CMB polarization from patchy reionization arise from two effects: generation of polarization from scattering of quadrupole moments by reionization bubbles and fluctuations in the screening of E modes from recombination. The scattering contribution has been studied previously, but the screening contribution has not yet been calculated. We show that on scales smaller than the acoustic scale (l > or approx. 300), the B-mode power from screening is larger than the B-mode power from scattering. The ratio approaches a constant ∼2.5 below the damping scale (l > or approx. 2000). On degree scales relevant for gravitational waves (l < or approx. 100), screening B modes have a white noise tail and are subdominant to the scattering effect. These results are robust to uncertainties in the modeling of patchy reionization.

Additional details

Publishing Information

Journal Title
Physical Review. D, Particles Fields
Journal Volume
79
Journal Issue
10
Journal Page Range
p. 107302-107302.4
ISSN
0556-2821
CODEN
PRVDAQ

INIS

Country of Publication
United States
Country of Input or Organization
International Atomic Energy Agency (IAEA)
INIS RN
41042704
Subject category
S72: PHYSICS OF ELEMENTARY PARTICLES AND FIELDS;
Descriptors DEI
FLUCTUATIONS; GRAVITATIONAL WAVES; NOISE; POLARIZATION; QUADRUPOLE MOMENTS; RECOMBINATION; RELICT RADIATION; SCATTERING; SCREENING; SIMULATION
Descriptors DEC
ELECTROMAGNETIC RADIATION; MICROWAVE RADIATION; RADIATIONS; VARIATIONS

Optional Information

Notes
(c) 2009 The American Physical Society