Supernova remnant G46.8–0.3: A new case of interaction with molecular material

Abstract

Although the Galactic supernova remnant (SNR) G46.8–0.3 has been known for more than 50 yr, no specific studies of this source or its environment have been published to date. To make progress on this matter, we measured new flux densities from radio surveys and combined them with previous estimates carefully collected from the literature to create an improved and fully populated version of the integrated radio spectrum for G46.8–0.3. The resulting spectrum exhibits a featureless power-law form with an exponent α = −0.535 ± 0.012. The lack of a spectral turnover at the lowest radio frequencies, which is observable in many other SNRs, excludes the presence of abundant ionised gas either proximate to the SNR itself or along its line of sight. The analysis of local changes in the radio spectral index across G46.8–0.3 suggests a tendency to slightly steepen approximately at 1 GHz. Even if this steepening is real, it does not impact the integrated spectrum of the source. Deeper imaging of the radio structures of G46.8–0.3 and spectral maps constructed from matched raw data are needed to provide new insights into the local spectral properties of the remnant. On the basis of the spectral properties of the atomic gas, we placed the remnant at 8.7 ± 1.0 kpc and we revisited the distance to the nearby H ii region G046.495–00.241 to 7.3 ± 1.2 kpc. From evolutionary models and our distance estimate, we conclude that G46.8–0.3 is a middle-aged (~1 × 104 yr) SNR. Furthermore, we recognise several 12CO and 13CO molecular structures in the proximity of the remnant. We used combined CO-H i profiles to derive the kinematic distances to these features and characterise their physical properties. We provide compelling evidence for environmental molecular clouds physically linked to G46.8–0.3 at its centre, on its eastern edge, and towards the northern and southwestern rims on the far side of the SNR shell. Our study of the molecular matter does not confirm that the remnant is embedded in a molecular cavity as previously suggested. G46.8–0.3 shows a line-of-sight coincidence with the γ-ray source 4FGL J1918.1+1215c detected at GeV energies by the space telescope Fermi. A rough analysis based on the properties of the interstellar matter close to G46.8–0.3 indicates that the GeV γ-ray photons detected in the direction to the SNR can be plausibly attributed to hadronic collisions and/or bremsstrahlung radiation.

Polarized Emission from Four Supernova Remnants in the THOR Survey

“…From H 2 infrared emission lines, Lee et al (2020) found a V LSR of 44 ± 1 km s −1 and obtained a kinematic distance of 5.4 ± 0.1 kpc, which are both consistent with values from H I. With combined CO-H I profiles, Supan et al (2022) provided evidence for environmental molecular clouds that are physically linked to the remnant at its center, the lower edge, and toward the bright regions on the top-left and lower-right rims on the far side of the SNR shell. Sun et al (2011a) observed SNR G46.8 − 0.3 at λ6 cm to be 8% polarized with an integrated polarized flux density of 595 ± 32 mJy and a spectral index of −0.54 ± 0.02 at ¢ 9.5 resolution.…”

“…Lee et al (2019) observed H 2 line emission associated with the edges of regions of bright synchrotron emission for G43.3−0.2 and G39.2−0.3, which indicate a collision between the SNR shock and a dense molecular cloud. Similarly for G46.8−0.3, Supan et al (2022) observed an interaction between the forward shock and dense molecular clouds in the center of the SNR and the brightest regions along the edges. For each polarized SNR in this study, we associate depolarization in regions with bright Stokes I with an interaction between the SNR shock and nearby molecular clouds.…”

A Systematic Study of Associations between Supernova Remnants and Molecular Clouds

“…Therefore, the remnant may be associated with either the +19.4 or +59.3 km s −1 components. Note that there is H I absorption at the tangent point velocity toward this SNR detected by Sato (1979), Ranasinghe & Leahy (2018b), and Supan et al (2022), indicating that the SNR is at a far kinematic distance. The far kinematic distance of the +19.4 km s −1 component is estimated as 10.1 ± 0.6 kpc, and the kinematic distance of the +59.3 km s −1 component is estimated as 6.9 ± 0.5 kpc.…”

Polarized Emission From Four Supernova Remnants In The THOR Survey

“…From H 2 infrared emission lines, Lee et al (2020) find a V LSR of 44 ± 1 km s −1 and obtain a kinematic distance to be 5.4±0.1 kpc which are consistent with values from HI. With combined CO-HI profiles, Supan et al (2022) provide evidence for environmental molecular clouds that are physically linked to the remnant at its centre, the lower edge, and towards the bright regions on the top-left and lower-right rims on the far side of the SNR shell. Sun et al (2011a) observed SNR G46.8−0.3 at λ6 cm to be 8% polarized with an integrated polarized flux density of 595±32 mJy and a spectral index of −0.54 ± 0.02 at 9.…”

“…Since we do not detect polarized emission from the brightest parts of the SNRs at λ21 cm, polarization observations at λ6 cm would confirm that depolarization in the bright regions is wavelength-dependent. Lee et al (2019) G46.8−0.3, Supan et al (2022) observe an interaction between the forward shock and dense molecular clouds in the centre of the SNR and the brightest regions along the edges. For each polarized SNR in this study, we associate depolarization in regions with bright Stokes I with an interaction between the SNR shock and nearby molecular clouds.…”