Radio Polarimetric Imaging of the Interstellar Medium: Magnetic Field and Diffuse Ionized Gas Structure near the W3/W4/W5/HB 3 Complex

Gray, A. D.; Landecker, T. L.; Dewdney, P. E.; Taylor, A. R.; Willis, A.; Normandeau, M.

doi:10.1086/306934

Cited by 55 publications

(85 citation statements)

References 25 publications

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“…7) appears to be depolarized by a different amount and the distribution is mottled for our 9. 5 beam, although we see less fine structures when compared to the 1.4 GHz map of Gray et al (1999).…”

Section: W5 ( = 137mentioning

confidence: 50%

“…• 1) and the "lens" Faraday Screen W3/W4/W5 are prominent H ii regions forming a chain together with the SNR HB3 in the Perseus arm about 2 kpc away. Gray et al (1999) used the DRAO Synthesis Telescope and obtained 1 resolution radio images of both total intensity and polarized emission of this field at 1.4 GHz. We limit our discussion to W5 in the following.…”

Section: W5 ( = 137mentioning

confidence: 99%

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A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Reich²,

Han

et al. 2010

A&A

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Context. Linearly polarized Galactic synchrotron emission provides valuable information about the properties of the Galactic magnetic field and the interstellar magneto-ionic medium, when Faraday rotation along the line of sight is properly taken into account. Aims. We aim to survey the Galactic plane at λ6 cm including linear polarization. At such a short wavelength Faraday rotation effects are in general small and the Galactic magnetic field properties can be probed to larger distances than at long wavelengths. Methods. The Urumqi 25-m telescope is used for a sensitive λ6 cm survey in total and polarized intensities. WMAP K-band (22.8 GHz) polarization data are used to restore the absolute zero-level of the Urumqi U and Q maps by extrapolation. Results. Total intensity and polarization maps are presented for a Galactic plane region of 129 • ≤ ≤ 230 • and |b| ≤ 5 • in the anti-centre with an angular resolution of 9. 5 and an average sensitivity of 0.6 mK and 0.4 mK T B in total and polarized intensity, respectively. We briefly discuss the properties of some extended Faraday Screens detected in the λ6 cm polarization maps. Conclusions. The Sino-German λ6 cm polarization survey provides new information about the properties of the magnetic ISM. The survey also adds valuable information for discrete Galactic objects and is in particular suited to detect extended Faraday Screens with large rotation measures hosting strong regular magnetic fields.

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Section: W5 ( = 137mentioning

confidence: 50%

Section: W5 ( = 137mentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Reich²,

Han

et al. 2010

A&A

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“…However, by comparing high Galactic latitude fields with observations of the Galactic plane at 1.4 GHz Gray et al (1999) find that the magneto-ionic medium which induces the Faraday rotation on polarised emission appears to be concentrated in the disc component of the Galaxy (b < ∼ 10 • ). This would imply that higher latititude observations of synchrotron polarised emission at low frequencies and for similar angular resolution may yield steeper angular power spectra.…”

Section: Comparison With Previous Results and Discussionmentioning

confidence: 95%

Towards a model of full-sky Galactic synchrotron intensity and linear polarisation: A re-analysis of the Parkes data

Giardino

Banday

Górski

et al. 2002

A&A

133

198

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Abstract. We have analysed the angular power spectra of the Parkes radio continuum and polarisation survey of the Southern galactic plane at 2.4 GHz. We have found that in the multipole range l = 40−250 the angular power spectrum of the polarised intensity is well described by a power-law spectrum with fitted spectral index αL = 2.37 ± 0.21. In the same multipole range the angular power spectra of the E and B components of the polarised signal are significantly flatter, with fitted spectral indices respectively of αE = 1.57 ± 0.12 and αB = 1.45 ± 0.12. Temperature fluctuations in the E and B components are mostly determined by variations in polarisation angle. We have combined these results with other data from available radio surveys in order to produce a full-sky toy model of Galactic synchrotron intensity and linear polarisation at high frequencies (ν > ∼ 10 GHz). This can be used to study the feasibility of measuring the Cosmic Microwave Background polarisation with forthcoming experiments and satellite missions.

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“…A substantial increase in angular resolution has been provided by aperture-synthesis telescopes, and observations of the Galactic polarized emission with angular resolutions from one to a few arcminutes have been made in recent years (Wieringa et al 1993;Gray et al 1998Gray et al , 1999Haverkorn et al 2000;Gaensler et al 2001;Uyanıker & Landecker 2002;Uyanıker et al 2003;Haverkorn et al 2003aHaverkorn et al ,b,c, 2006. These observations have revealed much about Faraday rotation in the ISM, but interpretation has been hampered by the lack of information on the biggest structures 1 .…”

Section: Introductionmentioning

confidence: 99%

A Survey of the polarized emission from the Galactic plane at 1420 MHz with arcminute angular resolution

Landecker¹,

Reich

Reid³

et al. 2010

A&A

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111

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Context. Observations of polarized emission are a significant source of information on the magnetic field that pervades the interstellar medium of the Galaxy. Despite the acknowledged importance of magnetic fields in interstellar processes, our knowledge of field configurations on all scales is seriously limited. Aims. This paper describes an extensive survey of polarized Galactic emission at 1.4 GHz that provides data with arcminute resolution and complete coverage of all structures from the broadest angular scales to the resolution limit, giving information on the magnetoionic medium over a wide range of interstellar environments. • 5. This is the first extensive polarization survey to present aperture-synthesis data combined with data from single antennas, and the techniques developed to achieve this combination are described. Results. The appearance of the extended polarized emission at 1.4 GHz is dominated by Faraday rotation along the propagation path, and the diffuse polarized sky bears little resemblance to the total-intensity sky. There is extensive depolarization, arising from vector averaging on long lines of sight, from H ii regions, and from diffuse ionized gas seen in Hα images. Preliminary interpretation is presented of selected polarization features on scales from parsecs (the planetary nebula Sh 2-216) to hundreds of parsecs (a superbubble GSH 166−01−17), to kiloparsecs (polarized emission in the direction of Cygnus X).

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Radio Polarimetric Imaging of the Interstellar Medium: Magnetic Field and Diffuse Ionized Gas Structure near the W3/W4/W5/HB 3 Complex

Cited by 55 publications

References 25 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Towards a model of full-sky Galactic synchrotron intensity and linear polarisation: A re-analysis of the Parkes data

A Survey of the polarized emission from the Galactic plane at 1420 MHz with arcminute angular resolution

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