35 cm observations of a sample of large supernova remnants

Reich, W.; Zhang, X; Fürst, E.

doi:10.1051/0004-6361:20030939

Cited by 50 publications

(69 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Using our λ6 cm flux density and those at lower frequencies (see Table 1), we calculated a spectral index of α = −0.59 ± 0.02, in agreement with that of Reich et al (2003).…”

Section: G1609+26 (Hb9)supporting

confidence: 66%

“…(1) Downes et al (1981), (2) Downes et al (1986), (3) Dubner et al (1998), (4) Kovalenko et al (1994), (5) Landecker et al (1990), (6) Kothes et al (2006b), (7) Tian & Leahy (2006b), (8) Castelletti et al (2003), (9) Mantovani et al (1985), (10) Velusamy et al (1976), (11) Wendker et al (1991), (12) Higgs et al (1977), (13) Pineault & Chastenay (1990), (14) Zhang et al (1997), (15) Higgs et al (1991), (16) Reich et al (2003), (17) Hirabayashi & Takahashi (1972), (18) Willis (1973), (19) …”

Section: G397−20 (W50)mentioning

confidence: 99%

“…HB9 has multiple fragmented shells and internal filamentary structures. Reich et al (2003) reported a spectral index of α = −0.57 ± 0.03 based on a TT-plot between 865 MHz data and 4750 MHz Effelsberg data. Kothes et al (2006b) compiled integrated flux densities at many frequencies and obtained a spectral index of α = −0.64 ± 0.02.…”

Section: G1609+26 (Hb9)mentioning

confidence: 99%

See 2 more Smart Citations

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…Using our λ6 cm flux density and those at lower frequencies (see Table 1), we calculated a spectral index of α = −0.59 ± 0.02, in agreement with that of Reich et al (2003).…”

Section: G1609+26 (Hb9)supporting

confidence: 66%

Section: G397−20 (W50)mentioning

confidence: 99%

Section: G1609+26 (Hb9)mentioning

confidence: 99%

See 1 more Smart Citation

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…The details of the 863 MHz and 1400 MHz Effelsberg maps are given by Reich et al (2003) and Uyanıker et al (1998Uyanıker et al ( , 1999, respectively. Relevant observational parameters of Effelsberg and DRAO data are summarized in Tables 1 and 2.…”

Section: Observationsmentioning

confidence: 99%

“…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

Self Cite

View full text Add to dashboard Cite

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.

show abstract

On the supernova remnants with flat radio spectra

Onić

2013

Astrophys Space Sci

View full text Add to dashboard Cite

A considerable fraction of Galactic supernova remnants (SNRs) characterize flat spectral indices ($\alpha<0.5$). There are several explanations of the flat radio spectra of SNRs in the present literature. The most of models involve a significant contribution of the second-order Fermi mechanism but some of them also discuss high compressions (>4), contribution of secondary electrons left over from the decay of charged pions, as well as the possibility of thermal contamination. In the case of expansion in high density environment, intrinsic thermal bremsstrahlung could theoretically shape the radio spectrum of an SNR and also account for observable curved -- "concave up" radio spectra of some Galactic SNRs. This model could also shed a light on the question of flat spectral indices determined in some Galactic SNRs. On the other hand, present knowledge of the radio continuum spectra (integrated flux densities at different frequencies) of SNRs prevent definite conclusions about the significance of proposed models so the question on flat spectral indices still remains open. New observations, especially at high radio continuum frequencies, are expected to solve these questions in the near future. Finally, as there is a significant connection between the majority of Galactic SNRs with flat integrated radio spectrum and their detection in $\gamma$-rays as well as detection of radiative recombination continua in their X-ray spectra, the analysis of high energy properties of these SNRs is very important.Comment: Accepted for publication in Astrophysics and Space Science. arXiv admin note: text overlap with arXiv:1207.2057 by other author

show abstract

35 cm observations of a sample of large supernova remnants

Cited by 50 publications

References 26 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Radio emission from the Cygnus Loop and its spectral characteristics

On the supernova remnants with flat radio spectra

Contact Info

Product

Resources

About