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Magnetic field stre...
Magnetic field strength in cosmic web filaments
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- Carretti, Ettore (författare)
- Istituto nazionale di astrofisica (INAF)
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- Vacca, V. (författare)
- Istituto nazionale di astrofisica (INAF)
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- O'Sullivan, S. P. (författare)
- Dublin City University
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- Heald, G. H. (författare)
- Commonwealth Scientific and Industrial Research Organisation (CSIRO)
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- Horellou, Cathy, 1967 (författare)
- Chalmers tekniska högskola,Chalmers University of Technology
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- Rottgering, H. J. A. (författare)
- Universiteit Leiden (UL),Leiden University (UL)
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- Scaife, A. M. M. (författare)
- University of Manchester,The Alan Turing Institute
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- Shimwell, T. W. (författare)
- Universiteit Leiden (UL),Leiden University (UL),Netherlands Institute for Radio Astronomy (ASTRON)
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- Shulevski, A. (författare)
- Universiteit Leiden (UL),Leiden University (UL)
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- Stuardi, C. (författare)
- Universita di Bologna,University of Bologna,Istituto nazionale di astrofisica (INAF)
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- Vernstrom, T. (författare)
- Commonwealth Scientific and Industrial Research Organisation (CSIRO)
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(creator_code:org_t)
- 2022-02-14
- 2022
- Engelska.
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Ingår i: Monthly Notices of the Royal Astronomical Society. - : Oxford University Press (OUP). - 0035-8711 .- 1365-2966. ; 512:1, s. 945-959
- Relaterad länk:
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http://arxiv.org/pdf...
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https://research.cha...
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https://doi.org/10.1...
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Abstract
Ämnesord
Stäng
- We used the rotation measure (RM) catalogue derived from the LOFAR Two-metre Sky Survey Data Release 2 (LoTSS DR2) at 144MHz to measure the evolution with redshift of the extragalactic RM (RRM: Residual RM) and the polarization fraction (p) of sources in low-density environments. We also measured the same at 1.4 GHz by cross-matching with the NRAO VLA Sky Survey RM catalogue. We find that RRM versus redshift is flat at 144 MHz, but, once redshift-corrected, it shows evolution at high significance. Also, p evolves with redshift with a decrement by a factor of similar to 8 at z similar to 2. Comparing the 144-MHz and 1.4-GHz data, we find that the observed RRM and p are most likely to have an origin local to the source at 1.4 GHz, while a cosmic web filament origin is favoured at 144 MHz. If we attribute the entire signal to filaments, we infer a mean rest-frame RRM per filament of RRM0,f = 0.71 +/- 0.07 rad m(-2) and a magnetic field per filament of B-f = 32 +/- 3 nG. This is in agreement with estimates obtained with a complementary method based on synchrotron emission stacking, and with cosmological simulations if primordial magnetic fields are amplified by astrophysical source field seeding. The measurement of an RRM0, f supports the presence of diffuse baryonic gas in filaments. We also estimated a conservative upper limit of the filament magnetic turbulence of sigma(RRM0,f) = 0.039 +/- 0.001 rad m(-2), concluding that the ordered magnetic field component dominates in filaments.
Ämnesord
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
- NATURVETENSKAP -- Geovetenskap och miljövetenskap -- Geofysik (hsv//swe)
- NATURAL SCIENCES -- Earth and Related Environmental Sciences -- Geophysics (hsv//eng)
- NATURVETENSKAP -- Fysik -- Fusion, plasma och rymdfysik (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Fusion, Plasma and Space Physics (hsv//eng)
Nyckelord
- magnetic fields
- polarization
- methods: statistical
- intergalactic medium
- large-scale structure of the Universe
Publikations- och innehållstyp
- art (ämneskategori)
- ref (ämneskategori)
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Till lärosätets databas
- Av författaren/redakt...
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Carretti, Ettore
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Vacca, V.
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O'Sullivan, S. P ...
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Heald, G. H.
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Horellou, Cathy, ...
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Rottgering, H. J ...
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visa fler...
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Scaife, A. M. M.
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Shimwell, T. W.
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Shulevski, A.
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Stuardi, C.
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Vernstrom, T.
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visa färre...
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