G51.04+0.07 and its environment: Identification of a new Galactic supernova remnant at low radio frequencies

Supán, L.; Castelletti, G.; Peters, Wendy; Kassim, N. E.

doi:10.1051/0004-6361/201832995

Cited by 10 publications

(5 citation statements)

References 53 publications

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“…The candidate G51.21+0.11 was identified by Anderson et al (2017) in the THOR survey. Further studies by Supan et al (2018) and Dokara et al (2018) have shown evidence of nonthermal emission arising from two distinct regions in this complex. Dokara et al (2018) classify it as two separate SNRs, G51.04+0.07 and G51.26+0.11.…”

Section: New Snr Candidates With Polarized Emissionmentioning

confidence: 91%

A global view on star formation: The GLOSTAR Galactic plane survey

Dokara

Brunthaler

Menten

et al. 2021

A&A

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Context. The properties of the population of Galactic supernova remnants (SNRs) are essential to our understanding of the dynamics of the interstellar medium (ISM) in the Milky Way. However, the completeness of the catalog of Galactic SNRs is expected to be only ~30%, with on order 700 SNRs yet to be detected. Deep interferometric radio continuum surveys of the Galactic plane help in rectifying this apparent deficiency by identifying low surface brightness SNRs and compact SNRs that have not been detected in previous surveys. However, SNRs are routinely confused with H II regions, which can have similar radio morphologies. Radio spectral index, polarization, and emission at mid-infrared (MIR) wavelengths can help distinguish between SNRs and H II regions. Aims. We aim to identify SNR candidates using continuum images from the Karl G. Jansky Very Large Array GLObal view of the STAR formation in the Milky Way (GLOSTAR) survey. Methods. GLOSTAR is a C-band (4–8 GHz) radio wavelength survey of the Galactic plane covering 358° ≤ l ≤ 60°, |b|≤ 1°. The continuum images from this survey, which resulted from observations with the most compact configuration of the array, have an angular resolution of 18″. We searched for SNRs in these images to identify known SNRs, previously identified SNR candidates, and new SNR candidates. We study these objects in MIR surveys and the GLOSTAR polarization data to classify their emission as thermal or nonthermal. Results. We identify 157 SNR candidates, of which 80 are new. Polarization measurements provide evidence of nonthermal emission from nine of these candidates. We find that two previously identified candidates are filaments. We also detect emission from 91 of the 94 known SNRs in the survey region. Four of these are reclassified as H II regions following detection in MIR surveys. Conclusions. The better sensitivity and resolution of the GLOSTAR data have led to the identification of 157 SNR candidates, along with the reclassification of several misidentified objects. We show that the polarization measurements can identify nonthermal emission, despite the diffuse Galactic synchrotron emission. These results underscore the importance of higher resolution and higher sensitivity radio continuum data in identifying and confirming SNRs.

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Section: New Snr Candidates With Polarized Emissionmentioning

confidence: 91%

A global view on star formation: The GLOSTAR Galactic plane survey

Dokara

Brunthaler

Menten

et al. 2021

A&A

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“…G51.21+0.11 was classified as an SNR candidate by Anderson et al (2017) using the combination of 1-2 GHz continuum data from The HI, OH, Recombination line survey of the Milky Way (THOR) and 1.4 GHz Very Large Array Galactic Plane Survey continuum data and observed by Driessen et al (2018) using the LOw Frequency ARray. Following studies identified it as a complex of two separate SNRs: the compact SNR G51.04+0.07 (Supan et al 2018) and the shell-type SNR G51.26+0.11 (Dokara et al 2018). Evidence of nonthermal emission from the two distinct regions in this complex was also provided (Supan et al 2018;Dokara et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Following studies identified it as a complex of two separate SNRs: the compact SNR G51.04+0.07 (Supan et al 2018) and the shell-type SNR G51.26+0.11 (Dokara et al 2018). Evidence of nonthermal emission from the two distinct regions in this complex was also provided (Supan et al 2018;Dokara et al 2018). Figure 1 displays the radio emission from the complex in the 80-300 MHz 15,25,35,45 and 55 K km s −1 in the velocity range of +52 -+58 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

A Study of GeV Gamma-ray Emission toward Supernova Remnant G51.26+0.11 and Its Molecular Environment

Zhong¹,

Zhang²,

Chen³

et al. 2023

Preprint

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We reanalyze the Fermi-LAT GeV 𝛾-ray emission in the region of supernova remnant (SNR) G51.26+0.11 and investigate its interstellar molecular environment with the CO-line data. At GeV energies, based on 13.2 years of Fermi-LAT data, the extended 𝛾-ray emission observed in this region is resolved into a uniform-disk source ('Src A') with a significance of 19.5𝜎 and a point source (4FGL J1924.3+1628) with a significance of 4.2𝜎 in 0.2-500 GeV. With an angular radius of ∼ 0.17 • , 'Src A' overlaps with SNR G51.26+0.11 significantly in the line of sight. On the other hand, the morphological coincidence between the SNR and the ∼ +54 km s −1 molecular clouds (MCs) together with the asymmetric or broad 12 CO line profiles near the SNR boundary provides evidence for the very likely SNR-MC interaction. The SNR-MC interaction and the H I absorption features indicate that SNR G51.26+0.11 is located at a kinematic distance of 6.2 ± 0.5 kpc. Combined with the results from the multi-wavelength analysis, the 𝛾-ray emission of the SNR ('Src A') can be naturally explained by a hadronic model with a soft power-law proton spectrum of index ∼ 2.25.

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“…Green (2019) gives the current total of Galactic SNRs as 294. While the predicted total number of Galactic SNRs is a few thousand (Supan et al 2018;Ranasinghe & Leahy 2022), observations and identification of SNRs are greatly affected by selection effects.…”

Section: Introductionmentioning

confidence: 99%

A Statistical Analysis of Galactic Radio Supernova Remnants

Ranasinghe

Leahy

2023

ApJS

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We present a revised table of 390 Galactic radio supernova remnants (SNRs) and their basic parameters. Statistical analyses are performed on SNR diameters, ages, spectral indices, Galactic heights, and spherical symmetries. Furthermore, the accuracy of distances estimated using the Σ–D relation is examined. The arithmetic mean of the Galactic SNR diameters is 30.5 pc with standard error 1.7 pc and standard deviation 25.4 pc. The geometric mean and geometric standard deviation factor of Galactic SNR diameters is 21.9 pc and 2.4, respectively. We estimate ages of 97 SNRs and find a supernova (SN) birth rate lower than, but within 2σ of, currently accepted values for the SN birth rate. The mean spectral index of shell-type SNRs is −0.51 ± 0.01 and no correlations are found between spectral indices and the SNR parameters of molecular cloud association, SN type, diameter, Galactic height, and surface brightness. The Galactic height distribution of SNRs is best described by an exponential distribution with a scale height of 48 ± 4 pc. The spherical symmetry measured by the ovality of radio SNRs is not correlated to any other SNR parameters considered here or to explosion type.

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G51.04+0.07 and its environment: Identification of a new Galactic supernova remnant at low radio frequencies

Cited by 10 publications

References 53 publications

A global view on star formation: The GLOSTAR Galactic plane survey

A global view on star formation: The GLOSTAR Galactic plane survey

A Study of GeV Gamma-ray Emission toward Supernova Remnant G51.26+0.11 and Its Molecular Environment

A Statistical Analysis of Galactic Radio Supernova Remnants

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