2015MNRAS.452..656V


Query : 2015MNRAS.452..656V

2015MNRAS.452..656V - Mon. Not. R. Astron. Soc., 452, 656-675 (2015/September-1)

Polarized radio filaments outside the Galactic plane.

VIDAL M., DICKINSON C., DAVIES R.D. and LEAHY J.P.

Abstract (from CDS):

We used data from the WMAP satellite at 23, 33 and 41 GHz to study the diffuse polarized emission over the entire sky. The emission originates mostly from filamentary structures with well-ordered magnetic fields. Some of these structures have been known for decades in radio continuum maps. Their origin is not clear and there are many filaments that are visible for the first time. We have identified and studied 11 filaments. The polarization fraction of some of them can be as high as 40 percent, which is a signature of a well-ordered magnetic field. The polarization spectral indices, averaged over 18 regions in the sky is β = -3.06±0.02, consistent with synchrotron radiation. There are significant variations in β over the sky (Δβ ~ 0.2). We explore the link between the large-scale filaments and the local interstellar medium, using the model of an expanding shell in the solar vicinity. We compared observed polarization angles with the predictions from the model and found good agreement. This strongly suggests that many large-scale filaments and loops are nearby structures. This is important in the context of the Galactic magnetic field as these structures are normally included in global models, neglecting the fact that they might be local. We also studied the level of contamination added by the diffuse filaments to the CMB (cosmic microwave background) polarization power spectra. We conclude that, even though these filaments present low radio brightness, a careful removal will be necessary for future all-sky CMB polarization analysis.

Abstract Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2015)

Journal keyword(s): polarization - radiation mechanisms: general - radiation mechanisms: non-thermal - ISM: magnetic fields - diffuse radiation - radio continuum: ISM

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME Loop III SR? 01 12 +78.3           ~ 83 1
2 NAME Loop V SNR 02 34 +79.9           ~ 6 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16252 1
4 M 1 SNR 05 34 32 +22 00.8           ~ 5956 1
5 NAME GUM Nebula ISM 07 43 -42.1           ~ 407 1
6 NAME Loop XI Rad 09 30 +06.           ~ 3 1
7 NAME North Polar Spur ISM 12 00 +00.0           ~ 339 1
8 NAME Loop XII Rad 12 26 -62.0           ~ 2 1
9 NAME Loop IV SNR 13 24 -13.6           ~ 56 1
10 NAME Loop 6 SR? 14 49 +85.8           ~ 4 1
11 NAME Loop I SR? 15 01 -38.7           ~ 355 2
12 NAME Loop IX Rad 15 18 -38.5           ~ 3 1
13 NAME Upper Sco-Cen As* 16 15 -24.2           ~ 1245 1
14 NAME dze Oph Cloud Cld 16 37 09 -10 34.0           ~ 107 0
15 NAME Loop X Rad 16 40 +13.           ~ 2 1
16 NAME Galactic Center Spur Rad 16 41 -39.1           ~ 16 1
17 NAME Loop VIIa Rad 17 04 -41.4           ~ 1 1
18 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13188 0
19 NAME Loop VIIb Rad 19 29 -38.0           ~ 10 1
20 SNR G093.2+06.7 SNR 20 52 25 +55 19.3           ~ 74 0
21 NAME Loop 2 SR? 23 25 +26.5           ~ 74 1
22 NAME Loop IIIs Rad 23 31 +38.           ~ 5 1

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2022.09.28-02:51:18

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