The radio SNR G65.1+0.6 and its associated pulsar J1957+2831

Abstract

New images of the radio Supernova Remnant (SNR) G65.1+0.6 are presented, based on the 408 MHz and 1420 MHz continuum emission and the HI-line emission data of the Canadian Galactic Plane Survey (CGPS). A large shell-like structure seen in the 2695 MHz Effelsberg map appears to have nonthermal spectral index. HI observations show structures associated with the SNR G65.1+0.6 in the radial velocity range of −20 to −26 km s −1 and suggest a distance of 9.2 kpc for the SNR. The estimated Sedov age for G65.1+0.6 is 4−14 × 10 4 yr. The pulsar (PSR) J1957+2831 is possibly associated with G65.1+0.6, with consistent distance and kinematic age estimate, but different characteristic age than the SNR. The EGRET source 3EG J1958+2909 and γ-ray source 2CG 065+00 are also near the eastern edge of the SNR but do not agree in position with the pulsar and are likely not associated with the SNR. The SNR's flux densities at 408 MHz (8.6 ± 0.8 Jy), 1420 MHz (4.9 ± 0.5 Jy) and 2695 MHz (3.3 ± 0.5 Jy) have been corrected for flux densities from compact sources within the SNR. The integrated flux density based spectral index (S ν ∝ ν −α ) between 1420 MHz and 408 MHz is 0.45 ± 0.11 and agrees with the T-T plot spectral index of 0.34 ± 0.20. The nearby SNR DA495 has a T-T plot spectral index of 0.50 ± 0.01.

A Sino-Germanλ6 cm polarization survey of the Galactic plane

“…We also calculated the λ21 cm integrated flux density from the Effelsberg λ21 cm survey to be S 21 cm = 5.4 ± 0.6 Jy. This value is consistent with those quoted by Landecker et al (1990) and Tian & Leahy (2006b) from the CGPS, which used the Effelsberg λ21 cm survey for missing zero-spacings. Using these flux densities together with the flux densities at 408 MHz Kothes et al 2006b;Tian & Leahy 2006b) and other bands (see references in Table 1), we obtained a radio spectral index of α = −0.45 ± 0.04 (see Fig.…”

“…(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) …”

“…It shows strong southern shell emission, while its emission in the north is rather diffuse. Tian & Leahy (2006b) analyzed CGPS H i data and proposed a SNR distance of 9.2 kpc. Polarization from the southern Fig.…”

G64.5+0.9: a new shell supernova remnant with unusual central emission

“…As the arc resembles part of a ring and lies in the Galactic plane, it was identified as a possible supernova remnant (SNR). Tian & Leahy (2006) also noted this structure in Canadian Galactic Plane Survey (CGPS; Taylor et al 2003) data with similar sensitivity to but poorer resolution than the NVSS data, and proposed it as a possible SNR. It has now been observed with the VLA and the newly commissioned Arcminute Microkelvin Imager (AMI; see AMI Consortium: Zwart et al 2008).…”

Radio spectrum variations in supernova remnants

“…SNR G126.2+1.6 ( [15]) and SNR G65.1+0.6 ( [16]) are dominated by background point sources so their radio spectra were not correctly determined until background source correction. In SNR with compact sources at their center, the radio spectrum of the SNR needs to be corrected for flux from the central source (e.g [17]).…”