High-resolution Near-infrared Spectroscopic Study of Galactic Supernova Remnants. I. Kinematic Distances

Lee, Yong-Hyun; Koo, Bon‐Chul; Lee, Jae‐Joon

doi:10.3847/1538-3881/abc00e

Cited by 16 publications

(38 citation statements)

References 89 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The velocity is roughly consistent with the H I absorption studies (Brogan & Troland 2001;Ranasinghe & Leahy 2018). Most recently, Lee et al (2020) performed near-infrared spectroscopy of shocked H 2 emission toward four strips on W49B. The authors found that a central velocity of shocked H 2 is ∼64 km s −1 and then concluded that the molecular cloud at ∼60 km s −1 located toward the center and the southwest shell of W49B is likely associated with the SNR.…”

supporting

confidence: 77%

“…The SNR is thought to be lying on the far-side of the Galaxy from us (e.g., Lockhart & Goss 1978;Brogan & Troland 2001). The small apparent diameter of ∼3 -5 is consistent with the larger distance of ∼7.5-11.3 kpc (Zhu et al 2014;Ranasinghe & Leahy 2018;Lee et al 2020) and its young age (5- Figure 1. Intensity map of Chandra broad-band X-rays (E: 0.5-7.0 keV, e.g., Lopez et al 2013b) superposed on the VLA radio continuum contours at 20 cm obtained from MAGPIS (Helfand et al 2006).…”

mentioning

confidence: 70%

“…Figure 2 shows integrated intensity maps of 12 CO(J = 2-1) and 13 CO(J = 2-1) for three velocity ranges of 1-15 km s −1 (hereafter "10 km s −1 cloud"), 38-47 km s −1 (hereafter "40 km s −1 cloud"), and 57-67 km s −1 (hereafter "60 km s −1 cloud") as previously mentioned in several papers (e.g., Zhu et al 2014;Kilpatrick et al 2016;Lee et al 2020). The kinematic distance of molecular cloud is ∼11 kpc for the 10 km s −1 cloud; ∼9 kpc for the 40 km s −1 cloud 1 ; and ∼7 kpc for the 60 km s −1 cloud (Sofue et al 2020).…”

Section: Overview Of X-ray Radio Continuum and Co Distributionsmentioning

confidence: 87%

“…DISCUSSION 4.1. Molecular Clouds Associated with W49B Previous studies proposed three candidates of molecular clouds which are interacting with the SNR W49B: namely the 10 km s −1 cloud, 40 km s −1 cloud, and the 60 km s −1 cloud (Zhu et al 2014;Kilpatrick et al 2016;Lee et al 2020). Their claim is mainly based on three elements: (1) a line-broadening feature of CO emission at ∼10 km s −1 , (2) a wind-bubble like morphology of CO cloud at ∼40 km s −1 , and (3) a central velocity of shocked H 2 line emission at ∼64 km s −1 .…”

Section: Physical Conditions Of the Molecular Cloudsmentioning

confidence: 99%

“…The total mass of shocked H 2 is estimated to 14-550 M . Subsequent radio observations using CO line emission revealed three molecular clouds at velocities of ∼10, ∼40, and ∼60 km s −1 , which are possibly associated with the SNR (e.g., Zhu et al 2014;Kilpatrick et al 2016;Lee et al 2020). Zhu et al (2014) argued that the molecular cloud at ∼40 km s −1 is interacting with W49B because of its wind-bubble like morphology.…”

mentioning

confidence: 99%

See 4 more Smart Citations

ALMA CO Observations of the Mixed-Morphology Supernova Remnant W49B: Efficient Production of Recombining Plasma and Hadronic Gamma-rays via Shock-Cloud Interactions

Sano,

Yoshiike,

Yamane

et al. 2021

Preprint

View full text Add to dashboard Cite

We carried out new CO(J = 2-1) observations toward the mixed-morphology supernova remnant (SNR) W49B with the Atacama Large Millimeter/submillimeter Array (ALMA). We found that CO clouds at ∼10 km s −1 show a good spatial correspondence with synchrotron radio continuum as well as an X-ray deformed shell. The bulk mass of molecular clouds accounts for the western part of the shell, not for the eastern shell where near-infrared H 2 emission is detected. The molecular clouds at ∼10 km s −1 show higher kinetic temperature of ∼20-60 K, suggesting that modest shock-heating occurred. The expanding motion of the clouds with ∆V ∼6 km s −1 was formed by strong winds from the progenitor system. We argue that the barrel-like structure of Fe rich ejecta was possibly formed not only by an asymmetric explosion, but also by interactions with dense molecular clouds. We also found a negative correlation between the CO intensity and the electron temperature of recombining plasma, implying that the origin of the high-temperature recombining plasma in W49B can be understood as the thermal conduction model. The total energy of accelerated cosmic-ray protons W p is estimated to be ∼2 × 10 49 erg by adopting an averaged gas density of ∼650 ± 200 cm −3 . The SNR age-W p diagram indicates that W49B shows one of the highest in-situ values of W p in the gamma-ray bright SNRs.

show abstract

supporting

confidence: 77%

mentioning

confidence: 70%

Section: Overview Of X-ray Radio Continuum and Co Distributionsmentioning

confidence: 87%

Section: Physical Conditions Of the Molecular Cloudsmentioning

confidence: 99%

mentioning

confidence: 99%

See 3 more Smart Citations

ALMA CO Observations of the Mixed-Morphology Supernova Remnant W49B: Efficient Production of Recombining Plasma and Hadronic Gamma-rays via Shock-Cloud Interactions

Sano,

Yoshiike,

Yamane

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

Thermal radio absorption as a tracer of the interaction of SNRs with their environments

Castelletti

Supán

Peters

et al. 2021

A&A

View full text Add to dashboard Cite

We present new images and continuum spectral analysis for 14 resolved Galactic supernova remnants (SNRs) selected from the 74 MHz Very Large Array Low-Frequency Sky Survey Redux (VLSSr). We combine new integrated measurements from the VLSSr with, when available, flux densities extracted from the Galactic and Extragalactic All-Sky Murchison Widefield Array Survey and measurements from the literature to generate improved integrated continuum spectra sampled from ~15 MHz to ~217 GHz. We present the VLSSr images. When possible we combine them with publicly available images at 1.4 GHz, to analyse the resolved morphology and spectral index distribution across each SNR. We interpret the results and look for evidence of thermal absorption caused by ionised gas either proximate to the SNR itself, or along its line of sight. Three of the SNRs, G4.5+6.8 (Kepler), G28.6−0.1, and G120.1+1.4 (Tycho), have integrated spectra which can be adequately fit with simple power laws. The resolved spectral index map for Tycho confirms internal absorption which was previously detected by the Low Frequency Array, but it is insufficient to affect the fit to the integrated spectrum. Two of the SNRs are pulsar wind nebulae, G21.5−0.9 and G130.7+3.1 (3C 58). For those we identify high-frequency spectral breaks at 38 and 12 GHz, respectively. For the integrated spectra of the remaining nine SNRs, a low frequency spectral turnover is necessary to adequately fit the data. In all cases we are able to explain the turnover by extrinsic thermal absorption. For G18.8+0.3 (Kes 67), G21.8−0.6 (Kes 69), G29.7−0.3 (Kes 75), and G41.1−0.3 (3C 397), we attribute the absorption to ionised gas along the line of sight, possibly from extended H II region envelopes. For G23.3−0.3 (W41) the absorption can be attributed to H II regions located in its immediate proximity. Thermal absorption from interactions at the ionised interface between SNR forward shocks and the surrounding medium were previously identified as responsible for the low frequency turnover in SNR G31.9+0.0 (3C 391); our integrated spectrum is consistent with the previous results. We present evidence for the same phenomenon in three additional SNRs G27.4+0.0 (Kes 73), G39.2–0.3 (3C 396), and G43.3–0.2 (W49B), and derive constraints on the physical properties of the interaction. This result indicates that interactions between SNRs and their environs should be readily detectable through thermal absorption by future low frequency observations of SNRs with improved sensitivity and resolution.

show abstract

QUIJOTE scientific results – V. The microwave intensity and polarization spectra of the Galactic regions W49, W51 and IC443

Tramonte

Génova-Santos

Rubiño-Martín

et al. 2023

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present new intensity and polarization maps obtained with the QUIJOTE experiment towards the Galactic regions W49, W51 and IC443, covering the frequency range from 10 to 20 GHz at $\sim 1\, \text{deg}$ angular resolution, with a sensitivity in the range 35–79 $\mu \text{K}\, \text{beam}^{-1}$ for total intensity and 13–23 $\mu \text{K}\, \text{beam}^{-1}$ for polarization. For each region, we combine QUIJOTE maps with ancillary data at frequencies ranging from 0.4 to 3000 GHz, reconstruct the spectral energy distribution and model it with a combination of known foregrounds. We detect anomalous microwave emission (AME) in total intensity towards W49 at 4.7σ and W51 at 4.0σ with peak frequencies $\nu _{\rm AME}=(20.0\pm 1.4)\, \text{GHz}$ and $\nu _{\rm AME}=(17.7\pm 3.6)\, \text{GHz}$, respectively; this is the first detection of AME towards W51. The contamination from ultracompact H ii regions to the residual AME flux density is estimated at 10 per cent in W49 and 5 per cent in W51, and does not rule out the AME detection. The polarized SEDs reveal a synchrotron contribution with spectral indices αs = −0.67 ± 0.10 in W49 and αs = −0.51 ± 0.07 in W51, ascribed to the diffuse Galactic emission and to the local supernova remnant, respectively. Towards IC443 in total intensity we measure a broken power-law synchrotron spectrum with cut-off frequency $\nu _{\rm 0,s}=(114\pm 73)\, \text{GHz}$, in agreement with previous studies; our analysis, however, rules out any AME contribution which had been previously claimed towards IC443. No evidence of polarized AME emission is detected in this study.

show abstract

High-resolution Near-infrared Spectroscopic Study of Galactic Supernova Remnants. I. Kinematic Distances

Cited by 16 publications

References 89 publications

ALMA CO Observations of the Mixed-Morphology Supernova Remnant W49B: Efficient Production of Recombining Plasma and Hadronic Gamma-rays via Shock-Cloud Interactions

ALMA CO Observations of the Mixed-Morphology Supernova Remnant W49B: Efficient Production of Recombining Plasma and Hadronic Gamma-rays via Shock-Cloud Interactions

Thermal radio absorption as a tracer of the interaction of SNRs with their environments

QUIJOTE scientific results – V. The microwave intensity and polarization spectra of the Galactic regions W49, W51 and IC443

Contact Info

Product

Resources

About