Deep radio characterization of the supernova remnant G343.1-00.7

S. Loru; A. Ingallinera; C. Trigilio; G. Umana; D. Urošević B. Arbutina; D. Leahy; C. Bordiu; F. Bufano; I. U. Aalia; C. Buemi; F. Cavallaro; E. Egron; M. D. Filipović; L. Heino; A. M. Hopkins; S. Lazarević; P. Leto; A. Pellizzoni; S. F. Rahman; S. Riggi; A. C. Ruggeri; T. Zafar

arXiv · 2609.39731

Deep radio characterization of the supernova remnant G343.1-00.7

View original source ↗Read source document ↗Export metadata ↓

Abstract

Supernova remnants (SNRs) are extended radio sources whose morphology and evolution are shaped by the interaction of strong shocks with the surrounding medium. We combined the 0.944 GHz Australian Square Kilometre Array Pathfinder (ASKAP) image from the Evolutionary Map of the Universe (EMU) survey with 0.088-0.200 GHz MWA-GLEAM data to characterize the integrated radio spectrum of G343.1$-$00.7 and perform its first sensitive spatially resolved spectral analysis. We derived an integrated spectral index of $α=-0.50\pm0.01$, confirming the previously reported value with improved accuracy. We redefined the radio morphology of the remnant, providing the first morphological and spectral evidence that filamentary structures overlapping the nearby \hii\ G343.147$-$00.44 are associated with the SNR. Local brightness-brightness analysis revealed flatter-spectrum filaments along the south-eastern shell, consistent with a possible thermal bremsstrahlung contribution from radiative or partially radiative shocks. Comparison with \hi\ and CO data identified gas components kinematically consistent with the SNR distance, although no clear morphological evidence of interaction was found. The gas distribution around the \hii\ suggests an expanding \hi\ shell partially embedded within its parent molecular cloud. Theoretical models place G343.1$-$00.7 between the late Sedov and early pressure-driven phases, suggesting different evolutionary stages across the remnant. These results highlight the potential of high-resolution ASKAP observations for spatially resolved studies of poorly characterized SNRs in complex Galactic environments.

Explore related subjects

astro-ph.GA astro-ph.HE

Keep this discovery

Explore connections, maps & timelines

BibTeX RIS

S. Loru, A. Ingallinera, C. Trigilio, G. Umana, D. Urošević B. Arbutina, D. Leahy, C. Bordiu, F. Bufano, I. U. Aalia, C. Buemi, F. Cavallaro, E. Egron, M. D. Filipović, L. Heino, A. M. Hopkins, S. Lazarević, P. Leto, A. Pellizzoni, S. F. Rahman, S. Riggi, A. C. Ruggeri, T. Zafar. 2026-09-30. Deep radio characterization of the supernova remnant G343.1-00.7. https://arxiv.org/abs/2609.39731

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Spatio-Temporal Log-Gaussian Cox-Hawkes Processes with Inhibition and Excitation for Stochastic Star Formation

We establish a connection between the stochastic self-propagating star-formation (SSPSF) model and spatio-temporal point processes by showing that the SSPSF update law admits a conditional Poisson representation. Building on this connection, we propose a spatio-temporal log-Gaussian Cox-Hawkes process as a continuous point process model for stochastic star formation. The model represents star-formation events as point patterns driven jointly by deterministic galactic structure, latent spatio-temporal background variation, and dependence on past events. Its key feature is that the deterministic mean field, latent Gaussian random field, and history-dependent interaction field enter through a single log-intensity. This log-scale construction differs from additive Cox-Hawkes formulations and allows the history effect to be signed, past events may either increase or decrease future local intensity while the conditional intensity remains positive. The resulting framework provides an interpretable point-process model for representing latent clustering, self-excitation, local inhibition, and event-driven propagation in stochastic star formation. Further extensions replace the constant history coefficient with deterministic or random fields representing source influence, local response or both. Beyond linking SSPSF to spatio-temporal point-process theory, it offers a continuous stochastic formulation for analysing the propagation of star formation in galaxies and for interpreting observational surveys of star-forming regions within a unified statistical model.

astro-ph.GA↗

arXiv2026

The Einstein Gap: an unrecognised strong lensing feature in weak lensing mass density profiles

Magnification bias cross-correlations between galaxy clusters and high-redshift submillimetre galaxies have recently revealed a characteristic signal deficit at intermediate angular scales, termed the Einstein Gap, that appears consistently across all lens types and cannot be explained by any single theoretical mass density profile. In this work we identify for the first time the most plausible physical origin of this feature through a combination of observational tests and improved lensing simulations. Using galaxy clusters to characterise the satellite population and as the lens sample, we show that the gap is detected at high statistical significance, accounting for the full covariance of the stacked profile. Then, we demonstrate that the Einstein Gap is robust across three independent estimators of the angular cross-correlation function, strengthens as the positional smoothing is reduced, and scales systematically with the bright central galaxy stellar mass. Finally, we show that the projected radial distribution of satellite galaxies is smooth and continuous at all angular scales with no depression corresponding to the gap, disfavouring both a statistical artifact and a genuine absence of mass as its origin. An improved magnification bias simulator incorporating full ray-tracing via the lens equation and a NFW+Sersic mass density profile reproduces the observed signal deficit, strongly supporting that the Einstein Gap is a strong lensing feature: background sources within the Einstein radius are displaced outward, creating a characteristic empty annulus whose angular size scales. This feature is consistent with features visible in previously published weak-lensing profiles that were not, however, interpreted as a strong-lensing signature. Its identification opens new possibilities for constraining halo masses and concentrations from magnification bias measurements alone.

astro-ph.GA↗

arXiv2026

Starbursts hiding in the main sequence: a pathway toward quenching?

Star-forming galaxies spend most of their lifetimes on the star-forming main sequence, which establishes a tight empirical and statistical relation between stellar mass and star-formation rate. Occasional episodes of rapid star formation can push them temporarily above this sequence, turning them into starbursts. Yet some galaxies display starburst-like traits -- rapid, dense, and compact star formation -- while still remaining within the scatter of the main sequence. These "starbursts in the main sequence" (SBMSs) reveal the complexity and diversity of star formation modes, making them crucial for understanding how galaxies evolve and transition between different regimes. In this paper, we identify SBMSs in the cosmological simulation NewHorizon and follow their evolution across time to uncover their physical origins and the role of this special regime in shaping galaxy evolution. We explain the existence of SBMSs by a comparatively earlier assembly of their stellar mass, driven in particular by more frequent and repeated mergers as the other galaxies, as well as exceptionally productive starburst events triggered by these interactions. As a result, this regime appears preferentially -- though not exclusively -- in the most massive galaxies. The SBMS behavior is not continuous within individual galaxies but instead arises intermittently as a short-lived (~ 30 Myr) evolutionary mode. Nevertheless, such SBMS episodes exist throughout cosmic time across the galaxy population... [abridged]

astro-ph.GA↗