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Study of a giant Large Magellanic Cloud Supernova Remnant, Veliki (J0450.4-7050)

T0 review · 5 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read New radio maps enlarge supernova remnant Veliki to 150×81 pc and reveal an unusually flat radio spectrum pointing to a fully radiative shock.

desk verdict New MeerKAT/ASKAP imaging reveals a larger, still interesting LMC SNR, but the paper's flat-spectrum and radiative-phase interpretation rests on a spectral index that their own data contradict. read the letter →

arxiv 2506.15067 v1 pith:KDIPFPDA submitted 2025-06-18 astro-ph.HE

Z. J. Smeaton , M. D. Filipović , R. Z. E. Alsaberi , B. Arbutina , W. D. Cotton , E. J. Crawford , A. M. Hopkins , R. Kothes
show 7 more authors
D. Leahy J. L. Payne N. Rajabpour H. Sano M. Sasaki D. Urošević J. Th. van Loon
This is my paper · ORCID
classification astro-ph.HE PACS 95.85.Bh98.38.Mz
keywords ISM:supernovaremnantssupernovae:generalindividual:J0450-7050radiocontinuum:LargeMagellanicCloudspectralindexdiffuseshockaccelerationthermalbremsstrahlung
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper reports new high-resolution radio-continuum observations of the Large Magellanic Cloud supernova remnant J0450.4–7050, nicknamed Veliki, and re-examines its multi-frequency properties. It claims that Veliki is substantially larger than previously measured — 150×81 pc — making it one of the largest known supernova remnants, and that its integrated radio spectrum is unusually flat, $\alpha = -0.26 \pm 0.02$, with little spatial variation. The paper argues that the most likely explanation is an old, predominantly radiative remnant whose shocks have a high compression ratio $r \approx 6.8$, flattening the non-thermal spectrum, combined with a thermal bremsstrahlung contribution of about 58.6% at 1 GHz. If this interpretation is right, Veliki becomes a rare example of a giant, radiatively cooled supernova remnant and a direct test of diffuse shock acceleration outside the standard adiabatic shock limit.

What carries the argument

The load-bearing machinery is the radio spectral index itself plus two theoretical links. First, the integrated value $\alpha = -0.26 \pm 0.02$, derived from a 17-point power-law fit to flux densities spanning 88–8850 MHz, fixes the global emission law $S \propto \nu^{\alpha}$. Second, the diffuse-shock-acceleration (DSA) compression-ratio formula $\alpha = 3/(2(r-1))$ converts that index into $r \approx 6.8$, and a two-component spectral model (non-thermal synchrotron with $\alpha = -0.5$ plus optically thin thermal bremsstrahlung with $\alpha = -0.1$) assigns a 58.6% thermal fraction at 1 GHz. Radiative-shock theory, where the compression ratio can approach the square of the isothermal Mach number, supplies the physical justification for $r > 4$. These pieces, not any single image, carry the interpretive claim that Veliki is a fully radiative supernova remnant.

What would settle it

Re-fit the integrated spectrum after treating each survey's absolute flux calibration as a correlated systematic error, and also produce a matched-resolution spectral-index map that includes the 88–200 MHz low-frequency points; if the slope moves from $\alpha = -0.26$ to $\alpha \lesssim -0.35$ under either test, or the low-frequency map is uniformly steeper than the integrated value, the flat-spectrum case and the derived $r \approx 6.8$ and 58.6% thermal fraction would be refuted.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery is that Veliki is one of the largest known supernova remnants and its radio spectrum is flatter than standard shock acceleration predicts. Using 17 flux-density measurements spanning 88–8850 MHz, the authors obtain an integrated spectral index $\alpha = -0.26 \pm 0.02$, which corresponds, through the diffuse-shock-acceleration relation $\alpha = 3/(2(r-1))$, to a shock compression ratio $r \approx 6.8$ — well above the strong-shock limit $r = 4$ for an ideal adiabatic gas. They further model the spectrum as non-thermal synchrotron plus optically thin thermal bremsstrahlung and find that about 58.6% of the 1 GHz flux would need to be thermal to reproduce the flat index. Combined with a bright [SII]/H$\alpha$ shell and a soft X-ray interior, the paper concludes that Veliki is most likely a fully radiative supernova remnant, with the flat spectrum produced by the high compression ratio and thermal contamination, and its large size and high surface brightness explained by delayed cooling in the low-metallicity LMC environment and possibly a higher-than-normal explosion energy (about $8.6\times10^{51}$ erg).

Load-bearing premise

The load-bearing premise is that the single number $\alpha = -0.26 \pm 0.02$ accurately describes the whole remnant's radio emission, even though it is fitted to heterogeneous 88–8850 MHz flux densities with largely conventional 10–20% uncertainties and one strong outlier; if that number is off, the compression ratio and thermal fraction built on it collapse.

Editorial extensions

If this is right

  • Veliki's size and surface brightness place it outside the normal $\Sigma$–D evolutionary tracks, so if the interpretation is right it becomes a rare giant remnant formed by a delayed radiative transition in the low-metallicity LMC environment.
  • A compression ratio $r \approx 6.8$ means the shock has crossed the adiabatic $r = 4$ limit, making Veliki one of the clearest cases of diffuse shock acceleration operating in a fully radiative shock.
  • The 58.6% thermal fraction at 1 GHz should become visible as spectral flattening at higher frequencies, with any low-frequency turnover lying below 88 MHz; microwave and infrared measurements could test this directly.
  • If the fitted age of about 43,000 years and explosion energy of about $8.6\times10^{51}$ erg are correct, Veliki is a high-energy, evolved remnant rather than a typical middle-aged supernova remnant.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Beyond the paper, the flat-index claim could be checked independently by re-fitting the same 17 flux points with per-survey flux-scale nuisance parameters; if a correlated-error fit yields a steeper index, the radiative-shock and thermal-fraction story would lose its foundation.
  • Beyond the paper, the paper's dismissal of the steeper spectral-index map ($\alpha = -0.46 \pm 0.36$) as a frequency-range artifact could be tested by producing a matched-resolution map that includes the 88–200 MHz low-frequency points; a genuinely uniform flat map would strengthen the thermal-contamination story, while a steep map would point to calibration or resolution issues.
  • Beyond the paper, the southern radio filaments without optical counterparts may be ionised leakage rather than true shell material; targeted optical and infrared follow-up could decide whether Veliki's 150 pc extent is real or an upper limit, which would also change its position as a surface-brightness outlier.
  • Beyond the paper, if the molecular cloud near the north-western rim is truly interacting, future very-high-energy gamma-ray observations should detect hadronic emission; Veliki is a natural target for such observations once the LMC is covered at sufficient sensitivity.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

5 major / 5 minor

Summary. The paper presents new ASKAP and MeerKAT radio-continuum observations of the LMC supernova remnant J0450.4-7050 (nicknamed Veliki), together with archival MWA, MOST, optical, infrared, X-ray, H I, and CO data. The authors report a revised physical size of about 150 by 81 pc, an integrated radio spectral index of alpha = -0.26 +/- 0.02, low fractional polarization, and a roughly uniform spectral index map. Based on these results, they argue that Veliki is an old, predominantly radiative SNR whose flat spectrum arises from a high shock compression ratio (r about 6.8) combined with a thermal bremsstrahlung contribution of about 58.6% at 1 GHz. The interpretation is placed in the context of the LMC's low-metallicity, density-structured environment, and alternative scenarios such as a pulsar wind nebula, second-order Fermi acceleration, and molecular cloud interaction are considered and rejected.

Significance. The new high-resolution imaging and multi-wavelength comparison are a useful observational contribution to LMC SNR studies, and the measured size, morphology, polarimetry, and environmental analysis are of interest. If the flat integrated spectral index were robust, the paper would present a significant challenge to simple DSA expectations for evolved remnants. The authors are candid about several caveats, including the uncertain nature of the southern filaments and the heterogeneous flux-density measurements. However, the central quantitative conclusions rest on a spectral index whose robustness is not established and on a two-component spectral model that is mis-specified as written. As it stands, the radiative-shock/thermal-bremsstrahlung interpretation is not supported by the evidence presented.

major comments (5)
  1. [Sec. 3.3.1 and Table 1] The quoted integrated spectral index alpha = -0.26 +/- 0.02 is not robustly established. The fit combines 17 flux-density points with adopted 10-20% uncertainties and yields reduced chi^2 = 0.53, which means the errors are sufficiently generous that the formal +/- 0.02 underestimates systematic uncertainties. More directly, the data in Table 1 are not described by a single power law: the 944 to 1295 MHz pair gives alpha about -0.75, the 888 to 1295 MHz pair gives alpha about -0.33, and the 2300 to 8850 MHz range gives alpha about -0.3 to -0.5. The paper needs to quantify this scatter, for example with per-sub-band fits or an explicit curvature test, before using alpha = -0.26 as the foundation of the physical model.
  2. [Sec. 3.3.2] The dismissal of the spectral index map's average value alpha = -0.46 +/- 0.36 as an artifact of the 'smaller frequency range' is invalid: a single power law has the same slope in any frequency sub-range, with only the uncertainty changing. The discrepancy between the map and the integrated value therefore needs a quantitative explanation, such as calibration offsets between the ASKAP and MeerKAT images, missing extended flux at high resolution, or genuine spectral curvature.
  3. [Sec. 4.4.3] The two-component model is mis-specified as written. The statement 'alpha_total = alpha_thermal + alpha_non-thermal' is not the correct combination law for a composite spectrum; the effective spectral index is a flux-weighted average, alpha_eff = (S_th alpha_th + S_nt alpha_nt) / (S_th + S_nt). Because the 58.6% thermal fraction is derived from this model, it must be recomputed with the proper formula, or the intended formula must be stated unambiguously, and the uncertainty in the derived thermal fraction should be reported.
  4. [Sec. 4.4.3 and Sec. 4.4.4] The thermal-bremsstrahlung interpretation is internally inconsistent with the frequency dependence of the data. With a 58.6% thermal contribution at 1 GHz and alpha_th = -0.1, the spectrum should flatten at higher frequencies, approaching alpha about -0.1 as the thermal component dominates; instead, the 888-1300 MHz and 4.75-8.85 GHz sub-band slopes are steeper, approximately -0.3 to -0.75. This is not merely an absence of observable curvature; it is the opposite trend from the model's prediction.
  5. [Sec. 4.1 and Sec. 3.1] The revised size of 150 by 81 pc is presented as a headline result even though the authors state that the southern filaments may be leaked ionising radiation rather than physical shell material. Since the 'one of the largest SNRs' claim depends on including these filaments, the paper should either adopt a conservative shell size excluding ambiguous structures or provide a quantitative criterion, such as radio-optical morphological correspondence, for including them.
minor comments (5)
  1. [Sec. 4.4.3] The frequency range '88-8850 GHz' should be '88-8850 MHz'.
  2. [Sec. 3.1 and Sec. 4.2] The molecular cloud is called PGCC G272.62-35.35 in Sec. 3.1 and PGCC G282.62-35.35 in Sec. 4.2; the designation should be made consistent.
  3. [Fig. 9 caption] The surface brightness unit should be W m^-2 Hz^-1 sr^-1, not 'W m^-1 Hz^-2 sr^-1' as currently printed.
  4. [Abstract and Sec. 5] The phrase 'one of the lowest average radio spectral indices' is ambiguous; since alpha is negative, 'flattest' or 'least negative' would be clearer.
  5. [Secs. 3.5 and 4.4.4] The sign-convention footnotes are helpful, but the use of alpha = 0.26 in the compression-ratio equation may confuse readers; adopting one sign convention throughout would improve readability.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the flat spectral index is an observed fit, and the radiative-shock, compression-ratio, and thermal-fraction scenarios are model-dependent interpretations rather than re-labeled inputs.

full rationale

The paper's central quantities are not derived by construction. The integrated spectral index α = −0.26 ± 0.02 is measured from 17 flux densities with stated uncertainties (Sec. 3.3.1), not assumed. The compression ratio r ≈ 6.8 is obtained by inverting the standard DSA relation α = 3/(2(r−1)) (Sec. 4.4.4), a parameter-free external theoretical relation whose assumptions do not include the target result; this is an interpretation, not a circular reduction. The 58.6% thermal bremsstrahlung fraction (Sec. 4.4.3) is a best-fit two-component model parameter with assumed component indices (α_th = −0.1, α_nt = −0.5); although the fraction is algebraically tied to the observed α, the paper does not present it as an independent prediction or as a uniqueness proof, and it is explicitly labeled a rough estimate. The optical [SII]/Hα radiative-shell evidence (Sec. 4.3) is an independent input to the 'fully radiative SNR' conclusion. Self-citations (e.g., Filipović et al. 2022–2025 for flux-error and equipartition methods, Pavlović et al. 2018 for Σ-D tracks) are methodological or comparative and not load-bearing for the flat-spectrum claim. The paper itself flags the main caveats: the fit error 'likely underestimates the true uncertainty' (Sec. 3.3.1), the spectral index map is steeper (−0.46 ± 0.36) and dismissed as a frequency-range effect (Sec. 3.3.2), and no spectral curvature or turnover is seen (Sec. 4.4.3). These are robustness concerns, not circularity. No step reduces an output to an input by definition.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The paper's interpretive claims rest on assumed flux uncertainties, assumed component spectral indices for the thermal model, and adopted equipartition and evolution-model assumptions from the literature. No new physical entities are introduced. The thermal fraction and compression ratio are effectively rearrangements of the measured spectral index under theoretical priors, so the ledger is dominated by modeling assumptions rather than fitted constants.

free parameters (4)
  • Flux density uncertainty fractions = 10% (ASKAP/MeerKAT/MOST), 20% (MWA)
    Assumed uncertainties for integrated flux densities in Table 1; they directly affect the spectral index fit quality and the quoted error. The resulting reduced chi^2 of 0.53 suggests these uncertainties may be overestimated (Sec. 3.2 and Sec. 3.3.1).
  • Thermal component spectral index = -0.1
    Assumed for the two-component spectral model in Sec. 4.4.3; together with the non-thermal index and the measured total index, it determines the 58.6% thermal contribution at 1 GHz.
  • Non-thermal component spectral index = -0.5
    Assumed for the two-component spectral model in Sec. 4.4.3; it represents the standard DSA value for the non-thermal component.
  • Equipartition shock parameters = v=170 km/s, c_s=10 km/s, f=0.25, r=4, xi=4
    Assumed values used in the magnetic field estimate in Sec. 3.5; the resulting B field (20.0 or 68.9 microG) is used to support the high compression scenario.
assumptions (6)
  • domain assumption The distance to the LMC is ~50 kpc (Pietrzynski et al. 2019).
    Used to convert angular sizes to physical sizes and to compute luminosity and surface brightness (Sec. 3.1 and Sec. 3.3.1).
  • standard math The radio spectral index relates to the shock compression ratio via DSA theory, alpha = 3/(2(r-1)).
    Used in Sec. 4.4.4 to convert the measured alpha=-0.26 into r~6.8.
  • domain assumption The Leahy and Williams (2017) and Leahy et al. (2019) SNR evolution models apply to this remnant with the adopted X-ray temperature and emission measure.
    Used in Sec. 4.3.1 to derive explosion energy, age, and ambient density; the model details and assumptions are not reproduced in this paper.
  • domain assumption Equipartition between cosmic rays and magnetic fields holds for the magnetic field estimate.
    Adopted in Sec. 3.5 following Filipovic et al. (2023); the resulting field strength is model-dependent.
  • domain assumption The optical line ratios ([SII]/Halpha and Halpha brightness) trace radiative shocks and cooling.
    Used in Sec. 4.3 to classify Veliki as predominantly radiative based on the bright [SII]/Halpha shell.
  • domain assumption The ambient density around Veliki is ~0.3-0.5 cm^-3 as estimated by Williams et al. (2004).
    Used in Sec. 4.2 to discuss the environment; the new evolutionary models instead give densities an order of magnitude lower, which the paper attributes to intercloud vs cloud densities.

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Cite this review

Pith. "Pith review of Study of a giant Large Magellanic Cloud Supernova Remnant, Veliki (J0450.4-7050)." pith.science (2026). https://pith.science/paper/KDIPFPDA

@misc{pith2026250615067,
  author       = {Pith},
  title        = {Pith review of: Study of a giant Large Magellanic Cloud Supernova Remnant, Veliki (J0450.4-7050)},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/KDIPFPDA}},
  note         = {Machine review of arXiv:2506.15067}
}
abstract

We present a high-resolution radio-continuum view and a multi-frequency analysis of the Large Magellanic Cloud (LMC) Supernova Remnant (SNR) J0450.4-7050, which we give the nickname Veliki. These high-resolution observations reveal a larger extent than previously measured, making J0450.4-7050 one of the largest SNRs that we know of. Additionally, we observe a higher than expected radio surface brightness and an unusually flat spectral index ($\alpha = -0.26 \pm 0.02$), with little spectral variation over the remnant. We observe a bright H$\alpha$ shell indicating significant cooling over the remnant, but also an excess of [Oiii] on the eastern shock front. We investigate several theoretical scenarios to explain the emission and radio evolution of J0450.4-7050 in the context of the LMC environment, and determine that this is most likely an older, predominantly radiative, SNR with a higher shock compression ratio, which gives a flatter non-thermal spectrum, in combination with a thermal (bremsstrahlung) emission contribution.

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Works this paper leans on

111 extracted references · 66 canonical work pages

  1. [1]

    2023, MNRAS, 523, 5353

    Acharyya, A., Adam, R., Aguasca-Cabot, A., et al. 2023, MNRAS, 523, 5353

    2023

  2. [2]

    D., Camilo, F., Faerber, T., et al

    Anderson, L. D., Camilo, F., Faerber, T., et al. 2025, A&A, 693, A247

    2025

  3. [3]

    D., Kothes, R., Rosolowsky, E., et al

    Ball, B. D., Kothes, R., Rosolowsky, E., et al. 2023, MN- RAS, 524, 1396

    2023

  4. [4]

    Bell, A. R. 1978, Monthly Notices of the Royal Astronom- ical Society, 182, 147

    1978

  5. [5]

    P., Ghavamian, P., Sankrit, R., and Danforth, C

    Blair, W. P., Ghavamian, P., Sankrit, R., and Danforth, C. W. 2006, ApJS, 165, 480

    2006

  6. [6]

    2009, A&A, 498, 139

    Bocchino, F., Miceli, M., and Troja, E. 2009, A&A, 498, 139

    2009

  7. [7]

    M., Filipovic, M

    Bozzetto, L. M., Filipovic, M. D., Haberl, F., et al. 2015, Publication of Korean Astronomical Society, 30, 149

    2015

  8. [8]

    M., Filipovi´ c, M

    Bozzetto, L. M., Filipovi´ c, M. D., Sano, H., et al. 2023, MNRAS, 518, 2574 ‖http://www.atnf.csiro.au

    2023

Show all 111 references
  1. [9]

    M., Filipovi´ c, M

    Bozzetto, L. M., Filipovi´ c, M. D., Vukoti´ c, B., et al. 2017, ApJS, 230, 2

    2017

  2. [10]

    C., Smeaton, Z

    Bradley, A. C., Smeaton, Z. J., Tothill, N. F. H., et al. 2025, arXiv e-prints, in press (DOI: 10.48550/arXiv.2502.05299), arXiv:2502.05299

    2025 doi arXiv

  3. [11]

    L., Lazio, T

    Brogan, C. L., Lazio, T. J., Kassim, N. E., and Dyer, K. K. 2005, AJ, 130, 148

    2005

  4. [12]

    2024, A&A, 684, A150 ˇCajko, K

    Burger-Scheidlin, C., Brose, R., Mackey, J., et al. 2024, A&A, 684, A150 ˇCajko, K. O., Crawford, E. J., and Filipovi´ c, M. D. 2009, Serbian Astronomical Journal, 179, 55

    2024

  5. [13]

    and Lazarian, A

    Cho, J. and Lazarian, A. 2006, ApJ, 638, 811

    2006

  6. [14]

    2021, MN- RAS, 507, 4752

    Choudhury, S., de Grijs, R., Bekki, K., et al. 2021, MN- RAS, 507, 4752

    2021

  7. [15]

    D., Petre, R., and Snow- den, S

    Chu, Y.-H., Kim, S., Points, S. D., Petre, R., and Snow- den, S. L. 2000, AJ, 119, 2242

    2000

  8. [16]

    N., Little, A

    Clarke, J. N., Little, A. G., and Mills, B. Y. 1976, Aus- tralian Journal of Physics Astrophysical Supplement, 40, 1

    1976

  9. [17]

    2021, CARTA: Cube Analysis and Rendering Tool for Astronomy, As- trophysics Source Code Library, record ascl:2103.031

    Comrie, A., Wang, K.-S., Hsu, S.-C., et al. 2021, CARTA: Cube Analysis and Rendering Tool for Astronomy, As- trophysics Source Code Library, record ascl:2103.031

    2021

  10. [18]

    J., Filipovi´ c, M

    Crawford, E. J., Filipovi´ c, M. D., de Horta, A. Y., Stoot- man, F. H., and Payne, J. L. 2008, Serbian Astronom- ical Journal, 177, 61

    2008

  11. [19]

    Dimaratos, A., Cormier, D., Bigiel, F., and Madden, S. C. 2015, A&A, 580, A135

    2015

  12. [20]

    Dopita, M. A. and Sutherland, R. S. 1996, ApJS, 102, 161

    1996

  13. [21]

    1999, AJ, 118, 930

    Dubner, G., Giacani, E., Reynoso, E., et al. 1999, AJ, 118, 930

    1999

  14. [22]

    M., Braun, R., Winkler, P

    Dubner, G. M., Braun, R., Winkler, P. F., and Goss, W. M. 1991, AJ, 101, 1466

    1991

  15. [23]

    Fan, Z., Liu, S., and Fryer, C. L. 2010, MNRAS, 406, 1337

    2010

  16. [24]

    and Safi-Harb, S

    Ferrand, G. and Safi-Harb, S. 2012, Advances in Space Research, 49, 1313 Filipovi´ c, M. D., Bojiˇ ci´ c, I. S., Grieve, K. R., et al. 2021, MNRAS, 507, 2885 Filipovi´ c, M. D., Dai, S., Arbutina, B., et al. 2023, AJ, 166, 149 Filipovi´ c, M. D., Haberl, F., Winkler, P. F., et...

    2012

  17. [25]

    D., Smeaton, Z

    Filipovic, M. D., Smeaton, Z. J., Kothes, R., et al. 2025, arXiv e-prints, in press (DOI: 10.48550/arXiv.2505.04041), arXiv:2505.04041 19 Filipovi´ c, M. D. and Tothill, N. F. H. 2021, Principles of Multimessenger Astronomy, 2514-3433 (IOP Publish- ing) Filipovi´ c, M. D., Whi...

    2025 doi arXiv

  18. [26]

    D., White, G

    Filipovic, M. D., White, G. L., Jones, P. A., et al. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 112, The History of the Milky Way and Its Satellite System, ed. A. Burkert, D. H. Hartmann, and S. A. Majewski, 91

    1996

  19. [27]

    Q., Staveley-Smith, L., Hurley-Walker, N., et al

    For, B. Q., Staveley-Smith, L., Hurley-Walker, N., et al. 2018, MNRAS, 480, 2743

    2018

  20. [28]

    2009, ApJ, 705, 144

    Fukui, Y., Kawamura, A., Wong, T., et al. 2009, ApJ, 705, 144

    2009

  21. [29]

    M., Green, A

    Gaensler, B. M., Green, A. J., and Manchester, R. N. 1998, MNRAS, 299, 812

    1998

  22. [30]

    Galvin, T. J. and Filipovi´ c, M. D. 2014, Serbian Astro- nomical Journal, 189, 15

    2014

  23. [31]

    J., Filipovi´ c, M

    Galvin, T. J., Filipovi´ c, M. D., Crawford, E. J., et al. 2012, Ap&SS, 340, 133

    2012

  24. [32]

    J., Filipovi´ c, M

    Galvin, T. J., Filipovi´ c, M. D., Tothill, N. F. H., et al. 2014, Ap&SS, 353, 603

    2014

  25. [33]

    D., Alsaberi, R., et al

    Ghavam, M., Filipovi´ c, M. D., Alsaberi, R., et al. 2024, PASA, 41, e089

    2024

  26. [34]

    D., Camilo, F., et al

    Goedhart, S., Cotton, W. D., Camilo, F., et al. 2024, MNRAS, 531, 649

    2024

  27. [35]

    Green, D. A. 2025, Journal of Astrophysics and Astron- omy, 46, 14

    2025

  28. [36]

    2019, ASKAPsoft: ASKAP science data processor software

    Guzman, J., Whiting, M., Voronkov, M., et al. 2019, ASKAPsoft: ASKAP science data processor software

    2019

  29. [37]

    2014, in The X-ray Universe 2014, ed

    Haberl, F. 2014, in The X-ray Universe 2014, ed. J.-U. Ness, 4

    2014

  30. [38]

    Crawford, E. J. 2012, A&A, 537, L1

    2012

  31. [39]

    2009, in IAU Symposium, Vol

    Heald, G. 2009, in IAU Symposium, Vol. 259, Cosmic Magnetic Fields: From Planets, to Stars and Galaxies, ed. K. G. Strassmeier, A. G. Kosovichev, and J. E. Beckman, 591–602

    2009

  32. [40]

    M., Kapinska, A., Marvil, J., et al

    Hopkins, A. M., Kapinska, A., Marvil, J., et al. 2025, arXiv e-prints, in press (DOI: 10.48550/arXiv.2505.08271), arXiv:2505.08271

    2025 doi

  33. [41]

    W., Bunton, J

    Hotan, A. W., Bunton, J. D., Chippendale, A. P., et al. 2021, PASA, 38, e009

    2021

  34. [42]

    R., Hancock, P

    Hurley-Walker, N., Callingham, J. R., Hancock, P. J., et al. 2017, MNRAS, 464, 1146

    2017

  35. [43]

    2008, Experi- mental Astronomy, 22, 151

    Johnston, S., Taylor, R., Bailes, M., et al. 2008, Experi- mental Astronomy, 22, 151

    2008

  36. [44]

    J., Sasaki, M., Breitschwerdt, D., et al

    Kavanagh, P. J., Sasaki, M., Breitschwerdt, D., et al. 2020, A&A, 637, A12

    2020

  37. [45]

    N., and Sunyaev, R

    Chugai, N. N., and Sunyaev, R. A. 2023, MNRAS, 521, 5536

    2023

  38. [46]

    A., et al

    Kim, S., Staveley-Smith, L., Dopita, M. A., et al. 2003, ApJS, 148, 473

    2003

  39. [47]

    2006, ApJ, 653, 1145

    Kobayashi, C., Umeda, H., Nomoto, K., Tominaga, N., and Ohkubo, T. 2006, ApJ, 653, 1145

    2006

  40. [48]

    J., and Reich, W

    Kothes, R., Reich, P., Foster, T. J., and Reich, W. 2017, A&A, 597, A116 Laki´ cevi´ c, M., van Loon, J. T., Meixner, M., et al. 2015, ApJ, 799, 50

    2017

  41. [49]

    Vaneldik, J. F. 1989, MNRAS, 237, 277 Lazarevi´ c, S., Filipovi´ c, M. D., Koribalski, B. S., et al. 2024, Research Notes of the American Astronomical Society, 8, 107

    1989

  42. [50]

    2019, AJ, 158, 149

    Leahy, D., Wang, Y., Lawton, B., Ranasinghe, S., and Filipovi´ c, M. 2019, AJ, 158, 149

    2019

  43. [51]

    Leahy, D. A. 2017, ApJ, 837, 36

    2017

  44. [52]

    Leahy, D. A. and Filipovi´ c, M. D. 2022, ApJ, 931, 20

    2022

  45. [53]

    A., Ranasinghe, S., and Gelowitz, M

    Leahy, D. A., Ranasinghe, S., and Gelowitz, M. 2020, ApJS, 248, 16

    2020

  46. [54]

    Leahy, D. A. and Williams, J. E. 2017, AJ, 153, 239

    2017

  47. [55]

    L., Wang, J.-M., and Li, H

    Liu, S., Fan, Z.-H., Fryer, C. L., Wang, J.-M., and Li, H. 2008, ApJL, 683, L163

    2008

  48. [56]

    J., Filipovi´ c, M

    Luken, K. J., Filipovi´ c, M. D., Maxted, N. I., et al. 2020, MNRAS, 492, 2606

    2020

  49. [57]

    D., Vukoti´ c, B., et al

    Maggi, P., Filipovi´ c, M. D., Vukoti´ c, B., et al. 2019, A&A, 631, A127

    2019

  50. [58]

    J., et al

    Maggi, P., Haberl, F., Kavanagh, P. J., et al. 2016, A&A, 585, A162

    2016

  51. [59]

    2021, MNRAS, 504, 326

    Maitra, C., Haberl, F., Maggi, P., et al. 2021, MNRAS, 504, 326

    2021

  52. [60]

    Mathewson, D. S. and Clarke, J. N. 1973, ApJ, 180, 725

    1973

  53. [61]

    S., Ford, V

    Mathewson, D. S., Ford, V. L., Tuohy, I. R., et al. 1985, ApJS, 58, 197

    1985

  54. [62]

    X., Brooks, J

    McGee, R. X., Brooks, J. W., and Batchelor, R. A. 1972, Australian Journal of Physics, 25, 581

    1972

  55. [63]

    D., Indebetouw, R., et al

    Meixner, M., Gordon, K. D., Indebetouw, R., et al. 2006, AJ, 132, 2268

    2006

  56. [64]

    C., White, G

    Millar, W. C., White, G. L., and Filipovi´ c, M. D. 2012, Serbian Astronomical Journal, 184, 19

    2012

  57. [65]

    C., White, G

    Millar, W. C., White, G. L., Filipovi´ c, M. D., et al. 2011, Ap&SS, 332, 221

    2011

  58. [66]

    P., Hopkins, A

    Norris, R. P., Hopkins, A. M., Afonso, J., et al. 2011, PASA, 28, 215

    2011

  59. [67]

    P., Marvil, J., Collier, J

    Norris, R. P., Marvil, J., Collier, J. D., et al. 2021, PASA, 38, e046 O’Brien, A. N., Filipovi´ c, M. D., Crawford, E. J., et al. 2013, Ap&SS, 347, 159 Oni´ c, D. 2013, Ap&SS, 346, 3 Oni´ c, D. and Uroˇ sevi´ c, D. 2008, Serbian Astronomical Journal, 177, 67 Oni´ c, D., Uroˇ ...

    2021

  60. [68]

    G., Schlegel, E

    Pannuti, T. G., Schlegel, E. M., Filipovi´ c, M. D., et al. 2011, AJ, 142, 20

    2011

  61. [69]

    G., Swartz, D

    Pannuti, T. G., Swartz, D. A., Laine, S., et al. 2015, AJ, 150, 91 Pavlovi´ c, M. Z., Uroˇ sevi´ c, D., Arbutina, B., et al. 2018, Astrophys. J., 852, 84

    2015

  62. [70]

    L., White, G

    Payne, J. L., White, G. L., and Filipovi´ c, M. D. 2008, MNRAS, 383, 1175

    2008

  63. [71]

    L., White, G

    Payne, J. L., White, G. L., Filipovi´ c, M. D., and Pannuti, T. G. 2007, MNRAS, 376, 1793

    2007

  64. [72]

    M., van Loon, J

    Pennock, C. M., van Loon, J. T., Filipovi´ c, M. D., et al. 2021, MNRAS, 506, 3540

    2021

  65. [73]

    and Liu, S

    Petrosian, V. and Liu, S. 2004, ApJ, 610, 550 Pietrzy´ nski, G., Graczyk, D., Gallenne, A., et al. 2019, 20 Nature, 567, 200

    2004

  66. [74]

    L., Riedinger, J

    Pilbratt, G. L., Riedinger, J. R., Passvogel, T., et al. 2010, A&A, 518, L1

    2010

  67. [75]

    L., Swerdlyk, C

    Pineault, S., Landecker, T. L., Swerdlyk, C. M., and Re- ich, W. 1997, A&A, 324, 1152 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2016, A&A, 594, A28

    1997

  68. [76]

    and Leahy, D

    Ranasinghe, S. and Leahy, D. 2023, ApJS, 265, 53

    2023

  69. [77]

    Raymond, J. C. 1979, ApJS, 39, 1

    1979

  70. [78]

    Reynolds, S. P. 2008, ARA&A, 46, 89

    2008

  71. [79]

    Reynolds, S. P. and Ellison, D. C. 1992, ApJL, 399, L75

    1992

  72. [80]

    P., Gaensler, B

    Reynolds, S. P., Gaensler, B. M., and Bocchino, F. 2012, SSRv, 166, 231

    2012

  73. [81]

    and Petre, R

    Rho, J. and Petre, R. 1998, ApJL, 503, L167

    1998

  74. [82]

    Rolleston, W. R. J., Trundle, C., and Dufton, P. L. 2002, A&A, 396, 53

    2002

  75. [83]

    C., and Edgar, R

    Salvesen, G., Raymond, J. C., and Edgar, R. J. 2009, ApJ, 702, 327

    2009

  76. [84]

    2019, ApJ, 873, 40

    Sano, H., Matsumura, H., Nagaya, T., et al. 2019, ApJ, 873, 40

    2019

  77. [85]

    T., et al

    Sano, H., Yamane, Y., van Loon, J. T., et al. 2023, ApJ, 958, 53

    2023

  78. [86]

    K., Hughes, J

    Slane, P., Smith, R. K., Hughes, J. P., and Petre, R. 2002, ApJ, 564, 284

    2002

  79. [87]

    J., Filipovi´ c, M

    Smeaton, Z. J., Filipovi´ c, M. D., Koribalski, B. S., et al. 2024, Research Notes of the American Astronomical Society, 8, 158

    2024

  80. [88]

    2000, in Astronom- ical Society of the Pacific Conference Series, Vol

    Smith, C., Leiton, R., and Pizarro, S. 2000, in Astronom- ical Society of the Pacific Conference Series, Vol. 221,

    2000

  81. [89]

    2022, A&A, 664, A89

    Supan, L., Fischetto, G., and Castelletti, G. 2022, A&A, 664, A89

    2022

  82. [90]

    1950, Indagationes mathematicae, 12, 173

    Theil, H. 1950, Indagationes mathematicae, 12, 173

    1950

  83. [91]

    T., and Steinmetz, M

    Thornton, K., Gaudlitz, M., Janka, H. T., and Steinmetz, M. 1998, ApJ, 500, 95

    1998

  84. [92]

    Tian, W. W. and Leahy, D. 2005, A&A, 436, 187

    2005

  85. [93]

    J., Goeke, R., Bowman, J

    Tingay, S. J., Goeke, R., Bowman, J. D., et al. 2013, PASA, 30, e007

    2013

  86. [94]

    2025, A&A, 697, A200

    Tramacere, A., Campana, R., Massaro, E., et al. 2025, A&A, 697, A200

    2025

  87. [95]

    Turtle, A. J. and Amy, S. W. 1991, in IAU Symposium, Vol. 148, The Magellanic Clouds, ed. R. Haynes and D. Milne, 114

    1991

  88. [96]

    D., Funk, S., Tajima, H., and Tanaka, T

    Uchiyama, Y., Blandford, R. D., Funk, S., Tajima, H., and Tanaka, T. 2010, ApJL, 723, L122 Uroˇ sevi´ c, D. 2014, Ap&SS, 354, 541 Uroˇ sevi´ c, D. and Pannuti, T. G. 2005, Astroparticle Physics, 23, 577 Uroˇ sevi´ c, D., Pannuti, T. G., and Leahy, D. 2007, ApJL, 655, L41

    2010

  89. [97]

    2020, Physics and Evolution of Supernova Rem- nants

    Vink, J. 2020, Physics and Evolution of Supernova Rem- nants

    2020

  90. [98]

    2006, ApJL, 648, L33

    Vink, J., Bleeker, J., van der Heyden, K., et al. 2006, ApJL, 648, L33

    2006

  91. [99]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261 Vukoti´ c, B.,´Ciprijanovi´ c, A., Vuˇ ceti´ c, M. M., Oni´ c, D., and Uroˇ sevi´ c, D. 2019, Serbian Astronomical Journal, 199, 23 Vuˇ ceti´ c, M., Milanovi´ c, N., Uroˇ sevi´ c, D., et al. 2023,...

    2020

  92. [100]

    B., Lenc, E., Bell, M

    Wayth, R. B., Lenc, E., Bell, M. E., et al. 2015, PASA, 32, e025

    2015

  93. [101]

    White, R. L. and Long, K. S. 1991, ApJ, 373, 543

    1991

  94. [102]

    M., Chu, Y

    Williams, R. M., Chu, Y. H., Dickel, J. R., et al. 2004, ApJ, 613, 948

    2004

  95. [103]

    2011, ApJS, 197, 16

    Wong, T., Hughes, A., Ott, J., et al. 2011, ApJS, 197, 16

    2011

  96. [104]

    2017, ApJ, 850, 139

    Wong, T., Hughes, A., Tokuda, K., et al. 2017, ApJ, 850, 139

    2017

  97. [105]

    E., Griffith, M

    Wright, A. E., Griffith, M. R., Burke, B. F., and Ekers, R. D. 1994, ApJS, 91, 111

    1994

  98. [106]

    Xiao, L., F¨ urst, E., Reich, W., and Han, J. L. 2008, A&A, 482, 783

    2008

  99. [107]

    2016, ApJL, 820, L3

    Yamaguchi, H., Katsuda, S., Castro, D., et al. 2016, ApJL, 820, L3

    2016

  100. [108]

    D., Roper, Q., et al

    Yew, M., Filipovi´ c, M. D., Roper, Q., et al. 2018, PASA, 35, e015

    2018

  101. [109]

    D., Stupar, M., et al

    Yew, M., Filipovi´ c, M. D., Stupar, M., et al. 2021, MN- RAS, 500, 2336

    2021

  102. [110]

    2024, A&A, 692, A237

    Zangrandi, F., Jurk, K., Sasaki, M., et al. 2024, A&A, 692, A237

    2024

  103. [111]

    W., and Zuo, P

    Zhu, H., Tian, W. W., and Zuo, P. 2014, ApJ, 793, 95 21 22 Istra ivanje inovskog ostatka supernove u Velikom Magelanovom Oblaku: Veliki (J0450.4−7050) Z. J. Smeaton 1,M. D. Filipovi 1, R. Z. E. Alsaberi 2,1,B. Arbutina 3, W. D. Cotton 4,5, E. J. Crawford 1, A. M. Hopkins 6, R. ...

    2014

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