2013
DOI: 10.1093/mnras/stt1277
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Abstract: We investigate the dependence of residual rotation measure (RRM) on intervening absorption systems at cosmic distances by using a large sample of 539 SDSS quasars in conjunction with the available rotation measure catalog at around 21cm wavelength. We found an excess extragalactic contribution in standard deviation of observed RRM (σ rrm ) of about 8.11±4.83 rad m −2 in our sample with intervening Mg ii absorber as compare to the sample without Mg ii absorber. Our results suggest that intervening absorbers cou… Show more

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Cited by 20 publications
(37 citation statements)
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“…We have seen however that all modes grow together in the kinematic stage, and large-scale modes at k = 1-2 continue to grow at the same rapid rate even when the small-scale modes (k > 4) saturate. Note that it is the linear growth rate which has been important in discussions of the strength of the large-scale field in young galaxies (Kronberg et al 1992;Bernet et al 2008;Joshi & Chand 2013;Farnes et al 2014). Our present work does not really apply to galaxies, where shear is also important and the magnetic Prandtl number is large, but it highlights quite clearly that any estimate based on the value of α, or the value of |α∇Ω| 1/2 in models with differential rotation Ω (Beck et al 1996) must be irrelevant.…”
Section: The Very Limited Role Of α Effect Growth Ratesmentioning
confidence: 99%
“…We have seen however that all modes grow together in the kinematic stage, and large-scale modes at k = 1-2 continue to grow at the same rapid rate even when the small-scale modes (k > 4) saturate. Note that it is the linear growth rate which has been important in discussions of the strength of the large-scale field in young galaxies (Kronberg et al 1992;Bernet et al 2008;Joshi & Chand 2013;Farnes et al 2014). Our present work does not really apply to galaxies, where shear is also important and the magnetic Prandtl number is large, but it highlights quite clearly that any estimate based on the value of α, or the value of |α∇Ω| 1/2 in models with differential rotation Ω (Beck et al 1996) must be irrelevant.…”
Section: The Very Limited Role Of α Effect Growth Ratesmentioning
confidence: 99%
“…Implications on magnetic field measurements at high redshifts: Usually, one studies magnetic field properties in high redshift intervening objects by measuring the excess RM towards quasar absorption line systems: Mgii, damped Lyman-α (DLA), sub-DLA (see e.g., Oren & Wolfe 1995;Bernet et al 2008;Joshi & Chand 2013;Farnes et al 2014). It has been suggested that the sub-DLAs can originate from neutral gas that lies 20 kpc from the host galaxies and the absorbing gas is likely stripped via tidal interaction and/or ram pressure (Sembach et al 2001;Muzahid et al 2016).…”
Section: Implications On the Buildup Of Galactic Magnetic Fieldsmentioning
confidence: 99%
“…We first perform an analysis similar to that of Joshi & Chand (2013), and use our main sample to look for differences between the RMs and polarized fractions at 1.4 GHz of sources with N MgII =0, 1, and ≥ 2 MgII absorbers (irrespective of whether each source has a spectral index measurement). In order to test whether any differences are statistically significant, we calculate the empirical cumulative-distribution functions (ECDFs) and statistical measures for various aspects of our main sample, both with and without nonintrinsic MgII absorption systems along the line of the sight.…”
Section: Main Sample Analysismentioning
confidence: 99%
“…Conversely, when using RMs measured at lower frequencies, i.e. at 1.4 GHz, the correlation between RM and the presence of MgII absorbers is consistent with no signal (Bernet et al 2012), or with a weakly positive result at the 1.7σ level (Joshi & Chand 2013). This observed dichotomy between results at 1.4 GHz and 5 GHz has been used to suggest that the intervenors provide 'partial coverage', and obscure only a fraction of the background radio source (e.g.…”
Section: Introductionmentioning
confidence: 96%