B-mode contamination by synchrotron emission from 3-yr Wilkinson Microwave Anisotropy Probe data

By Andrew King, James E. Pringle. 2006

229 citations recorded by the source corpus.

We study the contamination of the B-mode of the cosmic microwave background polarization (CMBP) by Galactic synchrotron in the lowest emission regions of the sky. The 22.8-GHz polarization map of the 3-yr Wilkinson Microwave Anisotropy Probe (WMAP) data release is used to identify and analyse such regions. Two areas are selected with signal-to-noise ratio S/N 0.3). Such regions allow T/S similar to 10(-3) to be measured directly which approximately corresponds to the limit imposed by using a sky coverage of 15 per cent. This opens interesting perspectives on the investigation of the inflationary model space in lowest emission regions.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e5aeb6de5ebd8c3dec2da702f6ad28eaef881a06

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In Astronomy and Astrophysics

1. M. Volonteri
2. E. Barausse
3. L. Hernquist
4. S. Davis
5. M. Gaspari
6. Zoltán Haiman
7. Emanuele Berti
8. S. Oh

Citations in the corpus

• SELF-CONSISTENT MODELS OF THE AGN AND BLACK HOLE POPULATIONS: DUTY CYCLES, ACCRETION RATES, AND THE MEAN RADIATIVE EFFICIENCY (2007, result): “Our results are consistent with a scenario like the one of King & Pringle (2006) in which chaotic accretion spins down black holes because of counter-alignment with the accretion disk angular momentum, or with other mechanisms that reduce efficiencies below the MHD-simulation predictions.”
• Measuring Black Hole Spin Using X-Ray Reflection Spectroscopy (2013, background): “This suggests that the last mass doubling of these SMBHs occurred via coherent accretion and not chaotic accretion (King & Pringle 2006) or SMBH-SMBH major merger (Volonteri et al. 2005).”
• Raining on black holes and massive galaxies: the top-down multiphase condensation model (2016, background): “The relevance of chaotic collisions has been highlighted by King & Pringle (2006) and Nayakshin & King (2007).”
• Tearing up the disc: misaligned accretion on to a binary (2013, unknown): “Dynamical friction with background stars allows the two SMBHs to sink to the centre of the merged galaxy and form a bound pair (Begelman, Blandford & Rees 1980).”
• Powerful Outflows and Feedback from Active Galactic Nuclei (2015, background): “It is likely that the orientation of the accretion disc with respect to the host galaxy changes with each new episode of accretion (so–called chaotic accretion, King & Pringle 2006, King et al. 2008), tending to isotropize the long–term effect of momentum feedback.”
• The evolution of massive black holes and their spins in their galactic hosts (2012, background): “This is indeed what would be expected in a chaotic-accretion scenario, where the black-hole spinoscillates around a small non-zero value (King & Pringle 2006).”
• Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “If accretion proceeds via short-lived, uncorrelated episodes with co-rotating and counter-rotating material equally probable, spins tend to be small (King and Pringle, 2006, 2007, Moderski et al., 1998): counter-rotating material spins the black hole down more than co-rotating material spins it up,…”
• Four Quasars above Redshift 6 Discovered by the Canada-France High-z Quasar Survey (2007, background): “Forming such massive black holes within the first billion years of the universe provides a challenge to models of galaxy formation, black hole formation and black hole growth (Bromley et al. 2004; Yoo & Miralda-Escudé 2004; Shapiro 2005; Volonteri & Rees 2005; King & Pringle 2006).”
• On the diffusive propagation of warps in thin accretion discs (2010, background): “The dynamics of warped accretion can play a fundamental role in these cases,it in turn regulates the spin history of the growing SMBH and, asa consequence, its very ability to grow rapidly (King & Pringle 2006; King et al. 2008).”
• Chaotic cold accretion on to black holes (2013, background): “Regarding analytic calculations, King & Pringle (2006, 2007) and Nayakshin & King (2007) postulated that BHs may grow through a series of randomly oriented accretion events, via a succession of minor mergers.”
• Cosmological Black Hole Spin Evolution by Mergers and Accretion (2008, background): “King & Pringle (2006) suggest that accretion always proceeds via very small (and short) episodes, caused by fragmentation of the accretion disc where it becomes self-gravitating.”
• Black Hole Spin and Galactic Morphology (2007, result): “We expect therefore that bright quasars at z > 3 have large spins, in contrast with the suggestion of King & Pringle (2006).”
• THE RADIATIVE EFFICIENCY OF ACCRETION FLOWS IN INDIVIDUAL ACTIVE GALACTIC NUCLEI (2010, background): “If it grew through a series of independent events (minor mergers, episodic accretions), then a∗ will be close to zero (Hughes & Blandford 2003; Gammie et al. 2004; Volonteri et al. 2005; King & Pringle 2006; Berti & Volonteri 2008).”