A 1.4 GHz radio continuum and polarization survey at medium 
Galactic latitudes

Uyanıker, B.; Fürst, E.; Reich, W.; Reich, P.; Wielebinski, R.

doi:10.1051/aas:1999494

Cited by 111 publications

(145 citation statements)

References 13 publications

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“…We obtained integrated flux densities of a number of SNRs (see Table 1) from the Effelsberg λ11 cm survey (Fürst et al 1990;Reich et al 1990a), λ21 cm survey (Reich et al 1990b(Reich et al , 1997, and the λ21 cm Effelsberg Medium Latitude Survey (EMLS) (Uyanıker et al 1999) within the same boundary as used for the λ6 cm integration.…”

Section: Resultsmentioning

confidence: 99%

“…The brightness-temperature spectral index from the TTplot (Fig. 6) using the Urumqi λ6 cm and Effelsberg Medium Latitude Survey (EMLS) λ21 cm data (Uyanıker et al 1999) is β = −2.05 ± 0.07 for the western filament (W-fila) and β = −2.05 ± 0.01 for the eastern filament (E-fila) (Fig. 6).…”

Section: G822+53 (W63)mentioning

confidence: 99%

“…Therefore, we discounted these two filaments in the flux density integration and got S 6 cm = 48.5 ± 4.9 Jy. We also calculated the integrated flux density at λ21 cm for the same area from the EMLS (Uyanıker et al 1999), S 21 cm = 93.1 ± 9.5 Jy. Combining all available flux densities, we obtained a spectral index of α = −0.44 ± 0.04.…”

Section: G822+53 (W63)mentioning

confidence: 99%

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A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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Context.Observations of large supernova remnants (SNRs) at high frequencies are rare, but provide valuable information about their physical properties. Aims. The total intensity and polarization properties of 16 large SNRs in the Galactic plane are investigated based on observations of the Urumqi λ6 cm polarization survey of the Galactic plane with an angular resolution of 9. 5. Methods. We extracted total intensity and linear polarization maps of large SNRs from the Urumqi λ6 cm survey, obtained their integrated flux densities, and derived the radio spectra by using these flux densities together with previously published flux densities at various frequencies. In particular, Effelsberg λ11 cm and λ21 cm survey data were used to calculate integrated flux densities. The λ6 cm polarization data also delineate the magnetic field structures of the SNRs. Results. We present the first total intensity maps at λ6 cm for SNRs G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06) and the first polarization measurements at λ6 cm for SNRs G82.2+5.3 (W63), G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06). Most of the newly derived integrated radio spectra are consistent with previous results. The new flux densities obtained from the Urumqi λ6 cm, Effelsberg λ11 cm and λ21 cm surveys are crucial to determine the spectra of SNR G65.1+0.6, G69.0+2.7 (CTB 80), G93.7−0.2, and G114.3+0.3. We find that G192.8−1.1 (PKS 0607+17) consists of background sources, H ii regions, and extended diffuse emission of thermal nature, and conclude that G192.8−1.1 is not a SNR.

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Section: Resultsmentioning

confidence: 99%

Section: G822+53 (W63)mentioning

confidence: 99%

Section: G822+53 (W63)mentioning

confidence: 99%

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A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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“…• 5) from the survey of Uyanıker et al (1999) at 1.4 GHz. By averaging the derived spectral indices for the polarised emission from all twenty fields they obtain α L,l=100−800 = 1.8 ± 0.3.…”

Section: Comparison With Previous Results and Discussionmentioning

confidence: 99%

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

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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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“…5 we analyze and discuss the results of the spectral analysis along with a brief theoretical background on that issue, and compare our results with previous investigations. Haslam et al (1982), b) Reich & Reich (1988), c) Reich et al (2003), d) Uyanıker et al (1998), e) Uyanıker et al (1999), f) Uyanıker et al (2002). Landecker et al (2000).…”

Section: Introductionmentioning

confidence: 99%

Radio emission from the Cygnus Loop and its spectral characteristics

Uyanıker

Reich

Yar

et al. 2004

A&A

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Abstract. We present a new sensitive 2675 MHz radio continuum map of the Cygnus Loop, which is used in conjunction with 408 MHz, 863 MHz and 1420 MHz maps from both the Effelsberg 100-m telescope and the DRAO Synthesis Telescope for a spectral analysis. Between 408 MHz and 2675 MHz we find an overall integrated spectral index of α = −0.42 ± 0.06 (S ∼ ν α ), close to previous results. There is no indication of a spectral break in the integrated spectrum. Spatially highly varying and rather strong spectral curvature was previously reported, but is not confirmed on the basis of new, higher sensitivity observations. We found spectral variations across the Cygnus Loop reaching up to ∆α = 0.2 from a TT-plot analysis. The flattest spectra are seen towards enhanced emission areas. Spectral index maps produced between different frequency pairs, as well as all four maps, revealed that there are at least three flat spectrum regions. In regions interior to the high emission filaments, we have detected at least two spectral components across the whole object with α = −0.4 and α = −0.6 towards northern and southern parts of the object, respectively.

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A 1.4 GHz radio continuum and polarization survey at medium Galactic latitudes

Cited by 111 publications

References 13 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

Radio emission from the Cygnus Loop and its spectral characteristics

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