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Old and Bright: The Remarkable Radio Brightening of the Engine-driven SN 2012au Several Years After Explosion Signals the Birth of a PWN

T0 review · 2 major / 0 minor · reviewed 2026-06-26 · grok-4.3

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Pith's one-line read SN 2012au's late radio re-brightening is produced by a newborn pulsar wind nebula rather than shock interaction with circumstellar material.

desk verdict SN 2012au shows a clear late radio re-brightening at 6.7 years whose properties the authors attribute to a newborn PWN, but the case against an aspherical CSM origin rests on an unquantified assertion rather than a demonstrated inconsistency. read the letter →

arxiv 2606.20836 v1 pith:27CUIT3L submitted 2026-06-18 astro-ph.HE

Eli Wiston , Raffaella Margutti , A. J. Nayana , Brian D. Metzger , Kohta Murase , Dan Milisavljevic , Itai Sfaradi , Ryan Chornock
show 18 more authors
Deanne L. Coppejans Joe Bright Garrett K. Keating Giacomo Terreran Mattias Lazda Maria R. Drout Michael Stroh Lauren Rhodes Ben Margalit Jonathan Granot Fabio De Colle Michael Bietenholz Daichi Tsuna Samantha Wu Tanmoy Laskar Edo Berger Daniel Patnaude Collin T. Christy
This is my paper · ORCID
classification astro-ph.HE
keywords SN2012aupulsarwindnebularadiore-brighteningTypeIbsupernovaengine-drivenPWNemission
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

After matching standard forward-shock models for the first six years, SN 2012au develops a luminous radio re-brightening at 6.7 years with a rapidly evolving spectral peak, shallow slope, and hard electron index. The emitting region must be compact, slow-moving, and embedded in dense gas. Conventional shock-CSM models can reproduce the data only by invoking extreme and unmotivated circumstellar properties. Emission from adiabatic expansion of relic pair plasma inside a newly formed pulsar wind nebula accounts for the radio evolution and the continued absence of X-rays. The authors therefore identify SN 2012au as the clearest known example of a young pulsar wind nebula born inside a supernova.

What carries the argument

Emission from adiabatic expansion of relic pair plasma inside a newborn Pulsar Wind Nebula.

What would settle it

Very Long Baseline Interferometry measurements that either confirm or rule out a source size of order 10^16 cm expanding at less than or equal to 500 km/s at late times.

Watch

Extended reading notes

Core claim

The emergence of radiation from a newborn Pulsar Wind Nebula naturally explains the radio spectral evolution and high-energy limits, where the emission is governed by the adiabatic expansion of a relic pair plasma. We conclude that SN 2012au represents the most compelling candidate for a young, newborn PWN discovered to date, a scenario that can be directly tested with pending Very Long Baseline Interferometry observations.

Load-bearing premise

The radio properties cannot be produced by aspherical shock-CSM interaction without extreme and unmotivated circumstellar geometry, density, or mass.

Editorial extensions

If this is right

  • The late emission is produced by adiabatic expansion of relic pair plasma rather than ongoing particle acceleration at a shock.
  • No detectable X-ray emission is expected because high-energy radiation is either absorbed or intrinsically weak.
  • The radio source remains compact and slow-moving while embedded in gas denser than 10^4 cm^{-3}.
  • The electron spectrum is hard, with power-law index near 1.6.
  • Pending VLBI observations can directly test the PWN interpretation by resolving the source size and velocity.

Reading between the lines

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

  • If confirmed, late-time radio monitoring of other engine-driven supernovae could uncover additional young PWNe that are currently hidden.
  • Detection of more such objects would tighten constraints on the fraction of core-collapse events that leave behind rapidly rotating, strongly magnetized neutron stars.
  • The same adiabatic-pair-plasma mechanism may operate in other compact radio sources whose spectra harden at late times.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 0 minor

Summary. The paper presents multi-wavelength (radio to X-ray) observations of the engine-driven Type Ib SN 2012au over 13 years. Early emission (δt ≤ 190 d) is consistent with a forward shock in a wind-like CSM (ρ_CSM ∝ r^{-2}). At δt ≈ 6.7 yr a radio re-brightening is detected with a broad, rapidly evolving spectral peak, optically thin index F_ u ∝ u^{-0.31 ± 0.02}, implying a compact region (R ≲ 10^{16} cm), slow velocity (≲ 500 km s^{-1}), high density (≥ 10^4 cm^{-3}), and hard electron index p ≈ 1.6. No X-ray emission is seen at any epoch. The authors argue these properties cannot arise from aspherical shock-CSM interaction without extreme, unmotivated CSM parameters and instead attribute the emission to adiabatic expansion of relic pair plasma in a newborn PWN, testable with VLBI.

Significance. If the PWN interpretation is confirmed, the result would be significant as the first compelling identification of a young, newborn PWN in a supernova, with implications for central-engine activity and non-thermal particle populations in engine-driven events. The combination of radio spectral evolution, compactness, and X-ray non-detection provides a potential observational template.

major comments (2)
  1. [Abstract] Abstract: The central claim that 'in the context of aspherical shock-CSM interaction models, these observations imply extreme properties of the CSM (geometry, density, total mass) that lack clear astrophysical motivation' is presented without any quantitative derivation (e.g., minimum CSM mass, required density contrast, or solid angle) using the standard synchrotron formulas to match the observed radio luminosity, spectral peak evolution, and derived parameters (R, v, n, p). This exclusion of the CSM channel is therefore an assertion rather than a demonstrated inconsistency and is load-bearing for preferring the PWN scenario.
  2. [Abstract] Abstract and modeling sections: The reported parameters (p ≈ 1.6, R ≲ 10^{16} cm, v ≲ 500 km s^{-1}, n ≥ 10^4 cm^{-3}) are derived from the same late-time radio data used to motivate the PWN model; no independent, falsifiable prediction of the PWN scenario (e.g., expected light-curve shape or VLBI size evolution) is shown prior to comparison with the data, raising a circularity concern for the interpretation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and valuable comments on our manuscript. We respond to each major comment below and indicate the revisions we will make.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim that 'in the context of aspherical shock-CSM interaction models, these observations imply extreme properties of the CSM (geometry, density, total mass) that lack clear astrophysical motivation' is presented without any quantitative derivation (e.g., minimum CSM mass, required density contrast, or solid angle) using the standard synchrotron formulas to match the observed radio luminosity, spectral peak evolution, and derived parameters (R, v, n, p). This exclusion of the CSM channel is therefore an assertion rather than a demonstrated inconsistency and is load-bearing for preferring the PWN scenario.

    Authors: We agree that the abstract would be strengthened by explicitly referencing the quantitative analysis. In the main text (particularly in the discussion of the late-time emission), we apply the standard synchrotron formulas to show that reproducing the observed radio luminosity and the derived compact size, low velocity, and high density in an aspherical CSM interaction would require either a total CSM mass of several solar masses confined to a small solid angle or extreme density contrasts (factors of 10^3 or more) with no clear link to known progenitor mass-loss histories. To make this transparent in the abstract, we will revise it to include a concise mention of these calculations. revision: yes

  2. Referee: [Abstract] Abstract and modeling sections: The reported parameters (p ≈ 1.6, R ≲ 10^{16} cm, v ≲ 500 km s^{-1}, n ≥ 10^4 cm^{-3}) are derived from the same late-time radio data used to motivate the PWN model; no independent, falsifiable prediction of the PWN scenario (e.g., expected light-curve shape or VLBI size evolution) is shown prior to comparison with the data, raising a circularity concern for the interpretation.

    Authors: The emitting region parameters are obtained directly from the radio observations via synchrotron self-absorption modeling and are thus independent of the subsequent physical interpretation. These parameters then allow us to evaluate the plausibility of CSM versus PWN origins. While the PWN scenario is indeed applied after deriving the parameters, it provides a self-consistent explanation without requiring ad hoc adjustments. We recognize the referee's point regarding forward modeling and will add a new subsection in the revised manuscript that outlines specific, testable predictions of the PWN model, such as the expected temporal evolution of the source size measurable with VLBI and the anticipated radio light curve behavior at later times. revision: partial

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity; derivation remains self-contained

full rationale

The provided abstract and context show the paper fits standard synchrotron models to early radio/X-ray data to derive CSM parameters, then qualitatively contrasts late-time fitted values (R ≲ 10^16 cm, v ≲ 500 km/s, n ≥ 10^4 cm^{-3}, p ≈ 1.6) against aspherical CSM scenarios by asserting they require 'extreme properties lacking astrophysical motivation.' It proposes PWN as an alternative that 'naturally explains' the evolution without presenting equations that reduce the PWN conclusion to the fitted inputs by construction, nor any self-citation chains, uniqueness theorems imported from prior work, or ansatzes smuggled via citation. No load-bearing step equates a 'prediction' to a fit or renames a known result. The central claim is therefore an interpretive preference rather than a circular reduction, consistent with a score of 0.

Assumptions & free parameters 3 free parameters · 2 assumptions · 1 invented entities

The central claim rests on the observational characterization of the late-time component and the assertion that standard CSM models cannot accommodate the derived parameters without extreme assumptions.

free parameters (3)
  • electron power-law index p = 1.6
    Fitted to the observed optically thin spectral slope F_ν ∝ ν^{-0.31±0.02}
  • emitting region size R = ≲10^16 cm
    Inferred from the broad, rapidly evolving spectral peak
  • expansion velocity = ≲500 km/s
    Derived from the compact size and time since explosion
assumptions (2)
  • domain assumption The late-time radio emission is dominated by a single luminous component with the stated spectral properties
    Invoked to separate the re-brightening from earlier forward-shock emission
  • ad hoc to paper Aspherical shock-CSM interaction cannot produce the observed combination of compactness, slow velocity, and high density without astrophysically unmotivated CSM properties
    Used to rule out the conventional model in favor of the PWN interpretation
invented entities (1)
  • newborn Pulsar Wind Nebula
    purpose: Source of the late-time radio emission via adiabatic expansion of relic pair plasma
    Postulated to explain the radio spectral evolution and X-ray non-detection

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Cite this review

Pith. "Pith review of Old and Bright: The Remarkable Radio Brightening of the Engine-driven SN 2012au Several Years After Explosion Signals the Birth of a PWN." pith.science (2026). https://pith.science/paper/27CUIT3L

@misc{pith2026260620836,
  author       = {Pith},
  title        = {Pith review of: Old and Bright: The Remarkable Radio Brightening of the Engine-driven SN 2012au Several Years After Explosion Signals the Birth of a PWN},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/27CUIT3L}},
  note         = {Machine review of arXiv:2606.20836}
}
abstract

We present the results from an extensive broad-band (radio to X-rays) observing campaign of the engine-driven Type Ib SN 2012au in the first 13 years of evolution. The early-time (${\delta}t\leq{190}$ d) radio and X-ray evolution is well-described by conventional models of a forward shock interacting with a wind-like circumstellar medium ($\rho_{\rm{CSM}}\propto{r}^{-2}$). However, starting at $\delta{t}\approx{6.7}$ yr, we detect a significant radio re-brightening. This late-time emission is dominated by a luminous component characterized by a broad and rapidly evolving spectral peak and a shallow optically thin spectral slope, $F_{\nu}\propto{\nu}^{-0.31\pm0.02}$. These properties imply a compact emitting region ($R\lesssim{10}^{16}$ cm) expanding at a remarkably slow velocity ($\lesssim{500}$ km/s) into a high-density environment ($\geq{10}^4 \rm{cm}^{-3}$), accompanied by a hard electron power-law index $p\approx{1.6}$. No soft or hard X-ray emission is detected at any epoch, indicating that high-energy radiation is either strongly absorbed or intrinsically absent. In the context of aspherical shock-CSM interaction models, these observations imply extreme properties of the CSM (geometry, density, total mass) that lack clear astrophysical motivation. Instead, we show that the emergence of radiation from a newborn Pulsar Wind Nebula (PWN) naturally explains the radio spectral evolution and high-energy limits, where the emission is governed by the adiabatic expansion of a relic pair plasma. We conclude that SN 2012au represents the most compelling candidate for a young, newborn PWN discovered to date, a scenario that can be directly tested with pending Very Long Baseline Interferometry (VLBI) observations.

Figures

Figures reproduced from arXiv: 2606.20836 by the authors.

Figure 1
Figure 1. Left: Complete SN 2012au radio (i.e., meter-wave to mm-wave) dataset spanning ≈ 13 years of evolution. The early-time data (≲ 6 months) originate from Kamble et al. (2014), to which we add one unpublished epoch at δt = 190 d. Solid lines (yellow to red): best-fitting model of synchrotron emission powered by the deceleration of the explosion’s forward shock into a broken power law CSM-density model with a continuous … view at source ↗
Figure 2
Figure 2. The extrapolation of our best-fitting model(s) of §3.2.2 to late times δt ≥ 6 yr significantly under-predicts the detected emission (filled circles). Solid lines: extrapolation of the early-time (δt ≤ 190d) best-fitting model using a standard wind CSM density index s = 2, and electron energy distribution index p = 3. The dashed lines show how a model with shallower p = 2.01, and a slightly less steep density index s… view at source ↗
Figure 3
Figure 3. Late-time radio observations of SN 2012au (this paper), SN 1986J (Bietenholz & Bartel 2017), and SN 2001em (Chandra et al. 2020) show a qualitatively simi￾lar behavior, with an “inverted” SED at low frequencies. SN 2012au exhibits other notably unusual features: (i) The optically thick slope around νpk is unusually shal￾low: Fν ∝ ν 0.5 , compared to the expected Fν ∝ ν 5/2 or Fν ∝ ν 2 of the SSA regime (or even stee… view at source ↗
Figures from the paper (17 more)
Figure 4
Figure 4. Figure 4: A model-agnostic, two-component fit to the late-time (δt > 6 yr) SN 2012au data. The model is sum of a low￾frequency, single power-law component, and a high-frequency, broken power-law component, with a spectral break that may represent a cooling break. Dashed lines: t…
Figure 5
Figure 5. Figure 5: The best fitting values for Fν,brk and νbrk of the high frequency component as a function of time since explosion for the model-agnostic fit of §4.1. Both Fν,brk and νbrk follow consistent power law decays with time. a small clump of dense CSM, placed at some large rad…
Figure 6
Figure 6. Figure 6: Cartoon showing two different CSM configurations: (a) Spherically asymmetric torus-like CSM extending from a distance R = Rin to R = RT from the explosion site, with the shock interacting with a less dense medium at r > RT . The half opening angle of the torus θT is re…
Figure 7
Figure 7. Figure 7: Best-fitting model for a torus-like dense CSM viewed edge-on. While the model captures the overall SED behavior at δt = 8.4 yr and δt = 11.7 yr reasonably well, it under-predicts the δt = 7.6 yr epoch, while over-predicting the δt = 12.7 yr epoch. The cooling breaks, v…
Figure 8
Figure 8. Figure 8: Dynamical evolution of the shock (radius and velocity) expanding in a “torus-like” dense-CSM scenario (§5.1). The vertical gray dashed lines mark the epochs of our late-time radio observations. The red dot in each curve marks the transition radius, RT . a roughly const…
Figure 9
Figure 9. Figure 9: Best-fitting torus CSM density (ne) and shock properties (B and U) as a function of Rs in the con￾text of the “torus-like” dense CSM scenario viewed edge-on (§5.1.1). The sharp discontinuities in each curve correspond to when the shock reaches the discontinuity in the …
Figure 10
Figure 10. Figure 10: Best-fitting models for a small clump of dense CSM with filling factor fV = 5 × 10−8 at Rbrk,2 = 4.7 × 1017 cm through Rend = 1.2 × 1018 cm. Like the edge-on torus model, the data are well fit at δt = 8.4 yr and δt = 11.7 yr, while being under-predicted at δt = 7.6 yr…
Figure 11
Figure 11. Figure 11: The dynamical evolution of the shock radius (Rs), shock velocity (vs), and radius of the emitting region (Rc) for the CSM clump scenario. The different colored lines correspond to different volumetric filling factors of the dense material. The gray dashed lines corres…
Figure 12
Figure 12. Figure 12: The CSM density (ne) and shock properties (B and U) as a function of Rs for the dense CSM clump scenario. The different colored lines correspond to different volumetric filling factors composed of this dense material. count for the observed spectral cooling break at ν…
Figure 13
Figure 13. Figure 13: Late-time (δt > 6 yr) broadband SED of SN 2012au, compared to the Crab Nebula at s δt ∼ 1000 yr (using data compiled in Mac´ıas-P´erez et al. 2010). Both objects exhibit a shallow spectral index at radio frequencies, which steepens at some point in the mm-optical regi…
Figure 14
Figure 14. Figure 14: Motivated parameter space for the initial spin period, P0, and period derivative, P˙ 0, in the PWN emission scenario. The green region shows the reference range motivated by the optical rise time if the central engine contributed significantly to the optical luminosit…
Figure 15
Figure 15. Figure 15: Observed late-time radio SED of SN 2012au compared with a representative nascent PWN synchrotron model (Murase et al. 2016). The model is not a formal fit, but demonstrates that high-frequency radio emission from a young PWN can reach the observed luminosity scale onc…
Figure 16
Figure 16. Figure 16: Corner plots for the posteriors of the fit to the early time data δt ≤ 190 d described in §3.2.1. The data are well modeled by synchrotron emission originating from a blast wave propagating into a broken power-law density CSM, with a change in density indexes from s1 …
Figure 17
Figure 17. Figure 17: Corner plot for the posteriors of key parameters in the model agnostic fit of the late-time data shown in [PITH_FULL_IMAGE:figures/full_fig_p034_17.png]
Figure 18
Figure 18. Figure 18: Corner plot for the edge on torus-like dense CSM model in Section 5.1.1. The region at R < RT is characterized by extremely high densities (ρ1 ≈ 105 g/cm 3 ), needed to significantly decelerate the shock. At R = RT , there is a large drop in density to ρ2 = 10−12.56g/…
Figure 19
Figure 19. Figure 19: The best model fit for the dense torus viewed from a face-on perspective, described in Section 5.1.2. While the optically thin side of the observed SEDs is well modeled, the optically thick side is significantly overestimated by the model. In the face-on perspective, …
Figure 20
Figure 20. Figure 20: Corner plots for the small clump of dense CSM models models in Section 5.2. Plots (a) - (c) show the parameter space for fV = 5×10−6 through fV = 5×10−8 respectively. The factors related to the dynamics of the shock Rbrk,2, ρc, and Rend are all constant across differe…

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Works this paper leans on

150 extracted references · 135 canonical work pages

  1. [1]

    , keywords =

    Additional Evidence for a Pulsar Wind Nebula in the Heart of SN 1987A from Multiepoch X-Ray Data and MHD Modeling. , keywords =. doi:10.3847/1538-4357/ac679d , archivePrefix =. 2204.06804 , primaryClass =

    work page doi:10.3847/1538-4357/ac679d

  2. [2]

    High angular resolution ALMA images of dust and molecules in the SN 1987A ejecta

    High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta. , keywords =. doi:10.3847/1538-4357/ab4b46 , archivePrefix =. 1910.02960 , primaryClass =

    work page doi:10.3847/1538-4357/ab4b46 1910

  3. [3]

    , keywords =

    Indication of a Pulsar Wind Nebula in the Hard X-Ray Emission from SN 1987A. , keywords =. doi:10.3847/2041-8213/abdf5a , archivePrefix =. 2101.09029 , primaryClass =

    work page doi:10.3847/2041-8213/abdf5a

  4. [4]

    Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars

    Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars. , keywords =. doi:10.1093/mnras/stu247 , archivePrefix =. 1311.1519 , primaryClass =

    work page Pith review arXiv doi:10.1093/mnras/stu247

  5. [5]

    A Dynamical Model for the Evolution of a Pulsar Wind Nebula inside a Non-Radiative Supernova Remnant

    A Dynamical Model for the Evolution of a Pulsar Wind Nebula Inside a Nonradiative Supernova Remnant. , keywords =. doi:10.1088/0004-637X/703/2/2051 , archivePrefix =. 0904.4053 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/703/2/2051

  6. [6]

    K., & McKee, C

    Evolution of Nonradiative Supernova Remnants. , keywords =. doi:10.1086/313176 , adsurl =

    work page doi:10.1086/313176

  7. [7]

    X-rays from the location of the Bactrian Transient ASASSN-15lh

    X-Rays from the Location of the Double-humped Transient ASASSN-15lh. , keywords =. doi:10.3847/1538-4357/836/1/25 , archivePrefix =. 1610.01632 , primaryClass =

    work page Pith review arXiv doi:10.3847/1538-4357/836/1/25

  8. [8]

    Gamma-Ray and Hard X-Ray Emission from Pulsar-Aided Supernovae as a Probe of Particle Acceleration in Embryonic Pulsar Wind Nebulae

    Gammy-Ray and Hard X-Ray Emission from Pulsar-aided Supernovae as a Probe of Particle Acceleration in Embryonic Pulsar Wind Nebulae. , keywords =. doi:10.1088/0004-637X/805/1/82 , archivePrefix =. 1411.0619 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/805/1/82

Show all 150 references
  1. [9]

    , keywords =

    A burst in a wind bubble and the impact on baryonic ejecta: high-energy gamma-ray flashes and afterglows from fast radio bursts and pulsar-driven supernova remnants. , keywords =. doi:10.1093/mnras/stw1328 , archivePrefix =. 1603.08875 , primaryClass =

    doi arXiv

  2. [10]

    , keywords =

    ALMA and NOEMA constraints on synchrotron nebular emission from embryonic superluminous supernova remnants and radio-gamma-ray connection. , keywords =. doi:10.1093/mnras/stab2506 , archivePrefix =. 2105.05239 , primaryClass =

    doi

  3. [11]

    , keywords =

    Multi-messenger Tests for Fast-spinning Newborn Pulsars Embedded in Stripped-envelope Supernovae. , keywords =. doi:10.3847/0004-637X/818/1/94 , archivePrefix =. 1508.04393 , primaryClass =

    doi arXiv

  4. [12]

    , keywords =

    Radio emission from embryonic superluminous supernova remnants. , keywords =. doi:10.1093/mnras/stx2743 , archivePrefix =. 1704.00456 , primaryClass =

    doi arXiv

  5. [13]

    , keywords =

    Signatures of pulsars in the light curves of newly formed supernova remnants. , keywords =. doi:10.1093/mnras/stt680 , archivePrefix =. 1304.5326 , primaryClass =

    doi arXiv

  6. [14]

    , keywords =

    Results from a Systematic Survey of X-Ray Emission from Hydrogen-poor Superluminous SNe. , keywords =. doi:10.3847/1538-4357/aad2df , archivePrefix =. 1704.05865 , primaryClass =

    doi arXiv

  7. [16]

    , keywords =

    Ionization break-out from millisecond pulsar wind nebulae: an X-ray probe of the origin of superluminous supernovae. , keywords =. doi:10.1093/mnras/stt1922 , archivePrefix =. 1307.8115 , primaryClass =

    doi arXiv

  8. [17]

    , title =

    Vurm, Indrek and Metzger, Brian D. , title =. The Astrophysical Journal , abstract =. 2021 , month =. doi:10.3847/1538-4357/ac0826 , url =

    2021 doi

  9. [18]

    , title =

    Margalit, Ben and Berger, Edo and Metzger, Brian D. , title =. The Astrophysical Journal , abstract =. 2019 , month =. doi:10.3847/1538-4357/ab4c31 , url =

    2019 doi

  10. [19]

    arXiv e-prints , keywords =

    Particle Acceleration at Shocks: An Introduction. arXiv e-prints , keywords =. doi:10.48550/arXiv.2307.00284 , archivePrefix =. 2307.00284 , primaryClass =

    doi

  11. [20]

    , keywords =

    Late Emission from the Type Ib/c SN 2001em: Overtaking the Hydrogen Envelope. , keywords =. doi:10.1086/500539 , archivePrefix =. astro-ph/0510362 , primaryClass =

    doi arXiv

  12. [21]

    , keywords =

    HI4PI: A full-sky H I survey based on EBHIS and GASS. , keywords =. doi:10.1051/0004-6361/201629178 , archivePrefix =. 1610.06175 , primaryClass =

    doi arXiv

  13. [22]

    , keywords =

    Seven Years of SN 2014C: A Multiwavelength Synthesis of an Extraordinary Supernova. , keywords =. doi:10.3847/1538-4357/ac5fa6 , archivePrefix =. 2203.12747 , primaryClass =

    doi

  14. [23]

    , keywords =

    The radio re-brightening of the Type IIb SN 2001ig. , keywords =. doi:10.1017/pasa.2025.38 , archivePrefix =. 2502.01740 , primaryClass =

    2025 doi

  15. [24]

    , keywords =

    PS1-11aop: Probing the Mass-loss History of a Luminous Interacting Supernova Prior to Its Final Eruption with Multiwavelength Observations. , keywords =. doi:10.3847/1538-4357/ad9336 , archivePrefix =. 2410.15140 , primaryClass =

    doi

  16. [25]

    Bietenholz and Norbert Bartel , title =

    Michael F. Bietenholz and Norbert Bartel , title =. The Astrophysical Journal , abstract =. 2017 , month =. doi:10.3847/1538-4357/aa960b , url =

    2017 doi

  17. [26]

    doi:https://doi.org/10.1002/9783527618170.ch5 , url =

    BREMSSTRAHLUNG , booktitle =. doi:https://doi.org/10.1002/9783527618170.ch5 , url =. https://onlinelibrary.wiley.com/doi/pdf/10.1002/9783527618170.ch5 , year =

    doi

  18. [27]

    and Cia, Annalisa De and Gal-Yam, Avishay and Leloudas, Giorgos and Lunnan, Ragnhild and Perley, Daniel A

    Quimby, Robert M. and Cia, Annalisa De and Gal-Yam, Avishay and Leloudas, Giorgos and Lunnan, Ragnhild and Perley, Daniel A. and Vreeswijk, Paul M. and Yan, Lin and Bloom, Joshua S. and Cenko, S. Bradley and Cooke, Jeff and Ellis, Richard and Filippenko, Alexei V. and Kasliwal...

    2018 doi

  19. [28]

    Central Bureau Electronic Telegrams , year = 2012, month = mar, volume =

    Supernova 2012au in NGC 4790 = Psn J12545218-1014502. Central Bureau Electronic Telegrams , year = 2012, month = mar, volume =

    2012

  20. [29]

    , keywords =

    Radio Observations Reveal a Smooth Circumstellar Environment Around the Extraordinary Type Ib Supernova 2012au. , keywords =. doi:10.1088/0004-637X/797/1/2 , adsurl =

    doi

  21. [30]

    and Fransson, Claes

    Chevalier, Roger A. and Fransson, Claes. Thermal and Non-thermal Emission from Circumstellar Interaction. Handbook of Supernovae. 2017. doi:10.1007/978-3-319-21846-5_34

    2017 doi

  22. [31]

    , keywords =

    Synchrotron Self-Absorption in Radio Supernovae. , keywords =. doi:10.1086/305676 , adsurl =

    doi

  23. [32]

    and Terreran, Giacomo and Coppejans, Deanne L

    Stroh, Michael C. and Terreran, Giacomo and Coppejans, Deanne L. and Bright, Joe S. and Margutti, Raffaella and Bietenholz, Michael F. and De Colle, Fabio and DeMarchi, Lindsay and Duran, Rodolfo Barniol and Milisavljevic, Danny and Murase, Kohta and Paterson, Kerry and Willia...

    2021 doi

  24. [33]

    , keywords =

    Evidence for a Pulsar Wind Nebula in the Type Ib Peculiar Supernova SN 2012au. , keywords =. doi:10.3847/2041-8213/aadd4e , archivePrefix =. 1809.01141 , primaryClass =

    doi arXiv

  25. [34]

    , keywords =

    SN 2012au: A Golden Link between Superluminous Supernovae and Their Lower-luminosity Counterparts. , keywords =. doi:10.1088/2041-8205/770/2/L38 , archivePrefix =. 1304.0095 , primaryClass =

    doi arXiv

  26. [35]

    , keywords =

    A Luminous and Fast-expanding Type Ib Supernova SN 2012au. , keywords =. doi:10.1088/2041-8205/772/2/L17 , archivePrefix =. 1306.5490 , primaryClass =

    doi arXiv

  27. [36]

    Alburger, D. E. and Warburton, E. K. and Tao, Z. , journal =. Half-life of ^. 1989 , month =. doi:10.1103/PhysRevC.40.2789 , url =

    1989 doi

  28. [37]

    da Cruz, M. T. F. and Chan, Y. and Larimer, R.-M. and Lesko, K. T. and Norman, E. B. and Stokstad, R. G. and Wietfeldt, F. E. and. Half-life of ^. Phys. Rev. C , volume =. 1992 , month =. doi:10.1103/PhysRevC.46.1132 , url =

    1992 doi

  29. [38]

    , keywords =

    Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au. , keywords =. doi:10.1093/mnras/stab1889 , archivePrefix =. 2106.15856 , primaryClass =

    doi

  30. [39]

    American Astronomical Society Meeting Abstracts , year = 2023, series =

    Asymmetry and Clumps and Jets! Oh My!: Revealing the Changing Structure of Type-Ib SN 2012au. American Astronomical Society Meeting Abstracts , year = 2023, series =

    2023

  31. [40]

    Astronomical Data Analysis Software and Systems XVI , year = 2007, series =

    CASA Architecture and Applications. Astronomical Data Analysis Software and Systems XVI , year = 2007, series =

    2007

  32. [41]

    ascl:1502.007 , adsurl =

    PyBDSF: Python Blob Detection and Source Finder. ascl:1502.007 , adsurl =

  33. [42]

    Ionospheric calibration of low frequency radio interferometric observations using the peeling scheme. I. Method description and first results. , keywords =. doi:10.1051/0004-6361/200811094 , archivePrefix =. 0904.3975 , primaryClass =

    doi arXiv

  34. [43]

    First alternative data release TGSS ADR1

    The GMRT 150 MHz all-sky radio survey. First alternative data release TGSS ADR1. , keywords =. doi:10.1051/0004-6361/201628536 , archivePrefix =. 1603.04368 , primaryClass =

    doi arXiv

  35. [44]

    Offringa, A. R. and McKinley, B. and Hurley-Walker and others , title =. 2014 , doi =

    2014

  36. [45]

    AIPS: Astronomical Image Processing System

  37. [46]

    , keywords =

    The radio and X-ray emission from type II supernovae. , keywords =. doi:10.1086/160167 , adsurl =

    doi

  38. [47]

    , keywords =

    Asymmetric Envelope Expansion of Supernova 1987A. , keywords =. doi:10.1086/167545 , adsurl =

    doi

  39. [48]

    The Astrophysical Journal , abstract =

    Granot, Jonathan and Sari, Re’em , title =. The Astrophysical Journal , abstract =. 2002 , month =. doi:10.1086/338966 , url =

    2002 doi

  40. [49]

    and Fransson, Claes , title =

    Chevalier, Roger A. and Fransson, Claes , title =. The Astrophysical Journal , abstract =. 2006 , month =. doi:10.1086/507606 , url =

    2006 doi

  41. [50]

    2025 , eprint=

    Systematic Investigation into Radio Supernovae with Markov Chain Monte Carlo Analysis: Implications for Massive Stars' Mass Loss and Shock Acceleration Physics , author=. 2025 , eprint=

    2025

  42. [51]

    The Astrophysical Journal Letters , abstract =

    Yang, Yuan-Pei and Zhang, Bing , title =. The Astrophysical Journal Letters , abstract =. 2018 , month =. doi:10.3847/2041-8213/aada4f , url =

    2018 doi

  43. [52]

    and McKee, Christopher F

    Matzner, Christopher D. and McKee, Christopher F. , title =. The Astrophysical Journal , abstract =. 1999 , month =. doi:10.1086/306571 , url =

    1999 doi

  44. [53]

    , keywords =

    The interaction of core-collapse supernova ejecta with a companion star. , keywords =. doi:10.1051/0004-6361/201526757 , archivePrefix =. 1509.03633 , primaryClass =

    doi arXiv

  45. [54]

    Physics of Fluids A: Fluid Dynamics , volume =

    Waxman, Eli and Shvarts, Dov , title =. Physics of Fluids A: Fluid Dynamics , volume =. 1993 , month =. doi:10.1063/1.858668 , url =

    1993 doi

  46. [55]

    Nonthermal processes in galactic and extragalactic sources

    Radio astrophysics. Nonthermal processes in galactic and extragalactic sources

  47. [56]

    , keywords =

    Seven Years of Coordinated Chandra-NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor. , keywords =. doi:10.3847/1538-4357/ac8b14 , archivePrefix =. 2206.00842 , primaryClass =

    doi

  48. [57]

    2025 , eprint=

    The First Radio-Bright Off-Nuclear TDE 2024tvd Reveals the Fastest-Evolving Double-Peaked Radio Emission , author=. 2025 , eprint=

    2025

  49. [58]

    and Chugai, Nikolai and Milisavljevic, Dan and Fransson, Claes , title =

    Chandra, Poonam and Chevalier, Roger A. and Chugai, Nikolai and Milisavljevic, Dan and Fransson, Claes , title =. The Astrophysical Journal , abstract =. 2020 , month =. doi:10.3847/1538-4357/abb460 , url =

    2020 doi

  50. [59]

    VizieR Online Data Catalog: 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)

    1998

  51. [60]

    2026 , eprint=

    VLBI Observations of SN 2012au Reveal a Compact Radio Source a Decade Post Explosion , author=. 2026 , eprint=

    2026

  52. [61]

    , title =

    Margalit, Ben and Metzger, Brian D. , title =. The Astrophysical Journal Letters , abstract =. 2018 , month =. doi:10.3847/2041-8213/aaedad , url =

    2018 doi

  53. [62]

    and Soderberg, Alicia M

    Drout, Maria R. and Soderberg, Alicia M. and Gal-Yam, Avishay and Cenko, S. Bradley and Fox, Derek B. and Leonard, Douglas C. and Sand, David J. and Moon, Dae-Sik and Arcavi, Iair and Green, Yoav , title =. The Astrophysical Journal , abstract =. 2011 , month =. doi:10.1088/00...

    2011 doi

  54. [63]

    Particle acceleration in interstellar shocks , journal=

    Uro. Particle acceleration in interstellar shocks , journal=. 2019 , month=. doi:10.1007/s10509-019-3669-y , url=

    2019 doi

  55. [64]

    and Slane, Patrick O

    Gelfand, Joseph D. and Slane, Patrick O. and Temim, Tea , title =. The Astrophysical Journal , abstract =. 2015 , month =. doi:10.1088/0004-637X/807/1/30 , url =

    2015 doi

  56. [65]

    Pulsar Wind Nebulae

    Slane, Patrick. Pulsar Wind Nebulae. Handbook of Supernovae. 2017. doi:10.1007/978-3-319-21846-5_95

    2017 doi

  57. [66]

    , keywords =

    The Keck Low-Resolution Imaging Spectrometer. , keywords =. doi:10.1086/133562 , adsurl =

    doi

  58. [67]

    , keywords =

    DAOPHOT - A computer program for crowded-field stellar photometry. , keywords =. doi:10.1086/131977 , adsurl =

    doi

  59. [68]

    , eprint =

    The Sloan Digital Sky Survey: Technical Summary. , eprint =. doi:10.1086/301513 , adsurl =

    doi

  60. [69]

    , archivePrefix = "arXiv", eprint =

    Setting UBVRI Photometric Zero-Points Using Sloan Digital Sky Survey ugriz Magnitudes. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-6256/135/1/264 , adsurl =

    doi

  61. [70]

    , keywords =

    The Evolution and Structure of Pulsar Wind Nebulae. , keywords =. doi:10.1146/annurev.astro.44.051905.092528 , archivePrefix =. astro-ph/0601081 , primaryClass =

    doi arXiv

  62. [71]

    Macías-Pérez, J. F. and Mayet, F. and Aumont, J. and Désert, F.-X. , title =. The Astrophysical Journal , abstract =. 2010 , month =. doi:10.1088/0004-637X/711/1/417 , url =

    2010 doi

  63. [72]

    and Charles, Philip A

    Seward, Frederick D. and Charles, Philip A. , year=. Neutron stars, pulsars, pulsar wind nebulae, and more supernova remnants , booktitle=

  64. [73]

    and Hallinan, Gregg , title =

    Dong, Dillon Z. and Hallinan, Gregg , title =. The Astrophysical Journal , abstract =. 2023 , month =. doi:10.3847/1538-4357/acc06c , url =

    2023 doi

  65. [74]

    , keywords =

    Evolution of pulsar-driven supernova remnants. , keywords =. doi:10.1086/161831 , adsurl =

    doi

  66. [75]

    and Berger, Edo and Margalit, Ben , title =

    Metzger, Brian D. and Berger, Edo and Margalit, Ben , title =. The Astrophysical Journal , abstract =. 2017 , month =. doi:10.3847/1538-4357/aa633d , url =

    2017 doi

  67. [76]

    Monthly Notices of the Royal Astronomical Society , volume =

    Smeaton, Zachary J and Filipović, Miroslav D and Lazarević, Sanja and Alsaberi, Rami Z E and Ahmad, Adeel and Araya, Miguel and Ball, Brianna D and Bordiu, Cristobal and Buemi, Carla S and Bufano, Filomena and Dai, Shi and Haberl, Frank and Hopkins, Andrew M and Ingallinera, A...

    2024 doi

  68. [77]

    , keywords =

    Testing a stochastic acceleration model of pulsar wind nebulae: early evolution of a wind nebula associated with SN 1986J. , keywords =. doi:10.1093/mnras/stad2504 , archivePrefix =. 2308.08809 , primaryClass =

    doi

  69. [78]

    , keywords =

    Supernova 1987A: Six Weeks Later. , keywords =. doi:10.1086/165908 , adsurl =

    doi

  70. [79]

    Hurley , abstract =

    K. Hurley , abstract =. Magnetars , journal =. 2011 , note =. doi:https://doi.org/10.1016/j.physe.2010.07.028 , url =

    2011 doi

  71. [80]

    Frail, D. A. and Scharringhausen, B. R. , title =. The Astrophysical Journal , abstract =. 1997 , month =. doi:10.1086/303943 , url =

    1997 doi

  72. [81]

    , keywords =

    Toward nebular spectral modeling of magnetar-powered supernovae. , keywords =. doi:10.1051/0004-6361/202245406 , archivePrefix =. 2211.04502 , primaryClass =

    doi

  73. [82]

    , keywords =

    Unveiling the engines of fast radio bursts, superluminous supernovae, and gamma-ray bursts. , keywords =. doi:10.1093/mnras/sty2417 , archivePrefix =. 1806.05690 , primaryClass =

    doi arXiv

  74. [83]

    On the Nature of Pulsars. I. Theory. , year = 1969, month = sep, volume =. doi:10.1086/150160 , adsurl =

    1969 doi

  75. [84]

    The Astrophysical Journal , abstract =

    Kasen, Daniel and Bildsten, Lars , title =. The Astrophysical Journal , abstract =. 2010 , month =. doi:10.1088/0004-637X/717/1/245 , url =

    2010 doi

  76. [85]

    The Astrophysical Journal Letters , abstract =

    Kashiyama, Kazumi and Murase, Kohta , title =. The Astrophysical Journal Letters , abstract =. 2017 , month =. doi:10.3847/2041-8213/aa68e1 , url =

    2017 doi

  77. [86]

    , keywords =

    Superluminous supernovae: ^ 56 Ni power versus magnetar radiation. , keywords =. doi:10.1111/j.1745-3933.2012.01329.x , archivePrefix =. 1208.1214 , primaryClass =

    2012 doi

  78. [87]

    , keywords =

    Time-dependent Force-free Pulsar Magnetospheres: Axisymmetric and Oblique Rotators. , keywords =. doi:10.1086/507518 , archivePrefix =. astro-ph/0603147 , primaryClass =

    doi arXiv

  79. [88]

    , keywords =

    The luminous late-time emission of the type-Ic supernova iPTF15dtg - evidence for powering from a magnetar?. , keywords =. doi:10.1051/0004-6361/201833688 , archivePrefix =. 1806.10000 , primaryClass =

    doi arXiv

  80. [89]

    , keywords =

    Stripped-envelope supernova light curves argue for central engine activity. , keywords =. doi:10.1038/s41586-024-07262-x , archivePrefix =. 2404.10846 , primaryClass =

    doi

  81. [90]

    Lin, W. L. and Wang, X. F. and Wang, L. J. and Dai, Z. G. , title =. The Astrophysical Journal Letters , abstract =. 2020 , month =. doi:10.3847/2041-8213/abc254 , url =

    2020 doi

  82. [91]

    Fransson and M

    C. Fransson and M. J. Barlow and P. J. Kavanagh and J. Larsson and O. C. Jones and B. Sargent and M. Meixner and P. Bouchet and T. Temim and G. S. Wright and J. A. D. L. Blommaert and N. Habel and A. S. Hirschauer and J. Hjorth and L. Lenkić and T. Tikkanen and R. Wesson and A...

    2024 doi

  83. [92]

    , keywords =

    A Radio Source Coincident with the Superluminous Supernova PTF10hgi: Evidence for a Central Engine and an Analog of the Repeating FRB 121102?. , keywords =. doi:10.3847/2041-8213/ab18a5 , archivePrefix =. 1901.10479 , primaryClass =

    doi

  84. [93]

    2024 , DOI =

    Dessart, Luc , URL =. 2024 , DOI =

    2024

  85. [94]

    , keywords =

    The Observed Phase Space of Mass-loss History from Massive Stars Based on Radio Observations of a Large Supernova Sample. , keywords =. doi:10.3847/1538-4357/ad9e93 , archivePrefix =. 2501.14028 , primaryClass =

    doi

  86. [95]

    Monthly Notices of the Royal Astronomical Society , volume =

    Rose, Kovi and Horesh, Assaf and Murphy, Tara and Kaplan, David L and Sfaradi, Itai and Ryder, Stuart D and Aloisi, Robert J and Dobie, Dougal and Driessen, Laura and Fender, Rob and Green, David A and Leung, James K and Lenc, Emil and Qiu, Hao and Williams-Baldwin, David , ti...

    2024 doi

  87. [96]

    , keywords =

    Data Characterization Using Artificial-Star Tests: Performance Evaluation. , keywords =. doi:10.1086/658162 , archivePrefix =. 1011.3892 , primaryClass =

    doi arXiv

  88. [97]

    10.1051/0004-6361:20021134

    The late-time radio spectrum of SN 1993J , DOI= "10.1051/0004-6361:20021134", url= "https://doi.org/10.1051/0004-6361:20021134", journal =

    doi

  89. [98]

    , keywords =

    First Multimessenger Observations of a Neutron Star Merger. , keywords =. doi:10.1146/annurev-astro-112420-030742 , archivePrefix =. 2012.04810 , primaryClass =

    2012 doi

  90. [99]

    , keywords =

    Self-similar solutions for the interaction of stellar ejecta with an external medium. , keywords =. doi:10.1086/160126 , adsurl =

    doi

  91. [100]

    , keywords =

    The Interaction of Supernovae with Circumstellar Bubbles. , keywords =. doi:10.1086/167802 , adsurl =

    doi

  92. [101]

    , title =

    Rhoads, James E. , title =. The Astrophysical Journal , abstract =. 1997 , month =. doi:10.1086/310876 , url =

    1997 doi

  93. [102]

    , year = 1993, month = nov, volume =

    Structure of the radio remnant of supernova 1987A. , year = 1993, month = nov, volume =. doi:10.1038/366136a0 , adsurl =

    1993 doi

  94. [103]

    , keywords =

    Radio Emission from Supernova SN 1986J in NGC 891. , keywords =. doi:10.1086/167546 , adsurl =

    doi

  95. [104]

    Advances in Space Research , year = 2008, month = jan, volume =

    The evolution of the central component in SN 1986J. Advances in Space Research , year = 2008, month = jan, volume =. doi:10.1016/j.asr.2006.12.004 , adsurl =

    2008 doi

  96. [105]

    Supernova 1986J Very Long Baseline Interferometry. II. The Evolution of the Shell and the Central Source. , keywords =. doi:10.1088/0004-637X/712/2/1057 , archivePrefix =. 1002.0304 , primaryClass =

    doi arXiv

  97. [106]

    SN 1986J VLBI. III. The Central Component Becomes Dominant. , keywords =. doi:10.3847/1538-4357/aa67a0 , archivePrefix =. 1701.08447 , primaryClass =

    doi arXiv

  98. [107]

    , keywords =

    The Radio Luminosity-risetime Function of Core-collapse Supernovae. , keywords =. doi:10.3847/1538-4357/abccd9 , archivePrefix =. 2011.11737 , primaryClass =

    2011 doi

  99. [108]

    and Williams, G

    DeSoto, Sabrina and Hoffman, Jennifer L. and Williams, G. Grant and Bilinski, Christopher and Leonard, Douglas C. and Milne, Peter A. and Pickens, Christopher and Shrestha, Manisha and Smith, Nathan and Smith, Paul S. , title =. The Astrophysical Journal , abstract =. 2025 , m...

    2025 doi

  100. [109]

    , keywords =

    Radio Emission from Supernovae and Gamma-Ray Bursters. , keywords =. doi:10.1146/annurev.astro.40.060401.093744 , adsurl =

    doi

  101. [110]

    , keywords =

    Off-Axis Afterglow Emission from Jetted Gamma-Ray Bursts. , keywords =. doi:10.1086/340991 , archivePrefix =. astro-ph/0201322 , primaryClass =

    doi arXiv

  102. [111]

    SN 1993J VLBI. IV. A Geometric Distance to M81 with the Expanding Shock Front Method. , keywords =. doi:10.1086/521326 , archivePrefix =. 0707.0881 , primaryClass =

    doi arXiv

  103. [112]

    , keywords =

    Radio Emission and Particle Acceleration in SN 1993J. , keywords =. doi:10.1086/306531 , archivePrefix =. astro-ph/9807030 , primaryClass =

    doi arXiv

  104. [113]

    , keywords =

    Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies. , keywords =. doi:10.3847/1538-4357/ab0d81 , archivePrefix =. 1903.02457 , primaryClass =

    1903 doi arXiv

  105. [114]

    , keywords =

    Joining Radio with X-Rays: A Revised Model for SN 1993J. , keywords =. doi:10.1088/0004-637X/813/1/43 , archivePrefix =. 1509.04533 , primaryClass =

    doi arXiv

  106. [115]

    Radio emission of SN1993J: the complete picture. II. Simultaneous fit of expansion and radio light curves. , keywords =. doi:10.1051/0004-6361/201014517 , archivePrefix =. 1007.1224 , primaryClass =

    doi arXiv

  107. [116]

    , keywords =

    Circumstellar Interaction in SN 1993J. , keywords =. doi:10.1086/177119 , adsurl =

    doi

  108. [117]

    Jansky Very Large Array Sky Survey (VLASS)

    The Karl G. Jansky Very Large Array Sky Survey (VLASS). Science Case and Survey Design. , keywords =. doi:10.1088/1538-3873/ab63eb , archivePrefix =. 1907.01981 , primaryClass =

    1907 doi

  109. [118]

    and BANYER, JAY and BELL, MARTIN E

    MURPHY, TARA and CHATTERJEE, SHAMI and KAPLAN, DAVID L. and BANYER, JAY and BELL, MARTIN E. and BIGNALL, HAYLEY E. and BOWER, GEOFFREY C. and CAMERON, ROBERT A. and COWARD, DAVID M. and CORDES, JAMES M. and et al. , year=. VAST: An ASKAP Survey for Variables and Slow Transient...

    2012 doi

  110. [119]

    Supernova explosions in the universe

    Burrows, A. Supernova explosions in the universe. Nature. 2000. doi:10.1038/35001501

    2000 doi

  111. [120]

    Monthly Notices of the Royal Astronomical Society , volume =

    Wang, Tianshu and Vartanyan, David and Burrows, Adam and Coleman, Matthew S B , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2022 , month =. doi:10.1093/mnras/stac2691 , url =

    2022 doi

  112. [121]

    10.1051/0004-6361:20066187

    Kinematics of the Local Universe* - XIII. 21-cm line measurements of 452 galaxies with the Nançay radiotelescope, JHK Tully-Fisher relation, and preliminary maps of the peculiar velocity field , DOI= "10.1051/0004-6361:20066187", url= "https://doi.org/10.1051/0004-6361:2006618...

    doi

  113. [122]

    , keywords =

    The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of a Strongly Magnetized Neutron Star. , keywords =. doi:10.1086/520054 , archivePrefix =. 0705.2713 , primaryClass =

    doi arXiv

  114. [123]

    , keywords =

    Bright Supernovae from Magnetar Birth. , keywords =. doi:10.1088/2041-8205/719/2/L204 , archivePrefix =. 0911.0698 , primaryClass =

    doi arXiv

  115. [124]

    , keywords =

    The diversity of transients from magnetar birth in core collapse supernovae. , keywords =. doi:10.1093/mnras/stv2224 , archivePrefix =. 1508.02712 , primaryClass =

    doi arXiv

  116. [125]

    , keywords =

    The Most Luminous Supernovae. , keywords =. doi:10.3847/2041-8205/820/2/L38 , archivePrefix =. 1602.04865 , primaryClass =

    doi arXiv

  117. [126]

    , keywords =

    Magnetar-powered ordinary Type IIP supernovae. , keywords =. doi:10.1093/mnras/stx2004 , archivePrefix =. 1704.06682 , primaryClass =

    doi arXiv

  118. [127]

    , keywords =

    Dynamics and observational signatures of core-collapse supernovae with central engines: hydrodynamics simulations with Monte Carlo post-processing. , keywords =. doi:10.1093/mnras/stag306 , adsurl =

    doi

  119. [128]

    The Astrophysical Journal , abstract =

    Nicholl, Matt and Guillochon, James and Berger, Edo , title =. The Astrophysical Journal , abstract =. 2017 , month =. doi:10.3847/1538-4357/aa9334 , url =

    2017 doi

  120. [129]

    10.1051/0004-6361/201732402

    A magnetar model for the hydrogen-rich super-luminous supernova iPTF14hls , DOI= "10.1051/0004-6361/201732402", url= "https://doi.org/10.1051/0004-6361/201732402", journal =

    doi

  121. [130]

    The evolution of nonthermal supernova remnants. II. Can radio supernovae become plerions ?. , keywords =. doi:10.1086/162484 , adsurl =

    doi

  122. [131]

    , keywords =

    Inhomogeneities in Type Ib/c Supernovae: An Inverse Compton Scattering Origin of the X-Ray Emission. , keywords =. doi:10.1088/0004-637X/769/1/65 , archivePrefix =. 1303.4254 , primaryClass =

    doi arXiv

  123. [132]

    , keywords =

    Inhomogeneities and the Modeling of Radio Supernovae. , keywords =. doi:10.3847/1538-4357/aa6cad , archivePrefix =. 1704.05283 , primaryClass =

    doi arXiv

  124. [133]

    , keywords =

    The dense and non-homogeneous circumstellar medium revealed in radio wavelengths around the Type Ib SN 2019oys. , keywords =. doi:10.1051/0004-6361/202348761 , archivePrefix =. 2312.00131 , primaryClass =

    doi

  125. [134]

    , keywords =

    Modeling of Radio Supernovae: Including the Effects of Inhomogeneities and Radiative Cooling. , keywords =. doi:10.3847/1538-4357/ad1109 , archivePrefix =. 2311.18516 , primaryClass =

    doi

  126. [135]

    , keywords =

    HST Observations of the Ring around SN 1987A. , keywords =. doi:10.1086/175213 , adsurl =

    doi

  127. [136]

    , keywords =

    Evidence for a possible black hole remnant in the Type IIL Supernova 1979C. , keywords =. doi:10.1016/j.newast.2010.09.004 , archivePrefix =. 0912.1571 , primaryClass =

    2010 doi arXiv

  128. [137]

    , keywords =

    X-Ray Observations of Old Nearby Supernovae Constraints on Compact Object Populations and Late Interaction. , keywords =. doi:10.3847/1538-4357/ae1d7c , archivePrefix =. 2511.03539 , primaryClass =

    doi

  129. [138]

    , keywords =

    Radio Studies of Supernovae 1979C, 1986J, and 2006X with LOFAR. , keywords =. doi:10.3847/1538-4357/ae2fbf , archivePrefix =. 2512.17520 , primaryClass =

    doi

  130. [139]

    , keywords =

    On the Maximum Pair Multiplicity of Pulsar Cascades. , keywords =. doi:10.3847/1538-4357/aaf050 , archivePrefix =. 1803.08924 , primaryClass =

    doi arXiv

  131. [140]

    and Arons, Jonathan , title =

    Hibschman, Johann A. and Arons, Jonathan , title =. The Astrophysical Journal , abstract =. 2001 , month =. doi:10.1086/321378 , url =

    2001 doi

  132. [141]

    , year = 1969, month = aug, volume =

    Pulsar Electrodynamics. , year = 1969, month = aug, volume =. doi:10.1086/150119 , adsurl =

    1969 doi

  133. [142]

    Monthly Notices of the Royal Astronomical Society , volume =

    Cehula, Jakub and Thompson, Todd A and Metzger, Brian D , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2024 , month =. doi:10.1093/mnras/stae358 , url =

    2024 doi

  134. [143]

    and Cehula, Jakub and Burns, Eric and Goldberg, Jared A

    Patel, Anirudh and Metzger, Brian D. and Cehula, Jakub and Burns, Eric and Goldberg, Jared A. and Thompson, Todd A. , title =. The Astrophysical Journal Letters , abstract =. 2025 , month =. doi:10.3847/2041-8213/adc9b0 , url =

    2025 doi

  135. [144]

    Monthly Notices of the Royal Astronomical Society , volume =

    Svensson, Roland , title =. Monthly Notices of the Royal Astronomical Society , volume =. 1987 , month =. doi:10.1093/mnras/227.2.403 , url =

    1987 doi

  136. [145]

    Tody, Doug , title =. Proc. SPIE Instrumentation in Astronomy VI , editor =. 1986 , doi =

    1986

  137. [146]

    SNooPy: TypeIa supernovae analysis tools

  138. [147]

    , keywords =

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    doi arXiv

  139. [148]

    , keywords =

    emcee: The MCMC Hammer. , keywords =. doi:10.1086/670067 , archivePrefix =. 1202.3665 , primaryClass =

    doi arXiv

  140. [149]

    and Craig, William W

    Harrison, Fiona A. and Craig, William W. and Christensen, Finn E. and Hailey, Charles J. and Zhang, William W. and Boggs, Steven E. and Stern, Daniel and Cook, W. Rick and Forster, Karl and Giommi, Paolo and Grefenstette, Brian W. and Kim, Yunjin and Kitaguchi, Takao and Kogli...

    2013 doi

  141. [150]

    Observatory Operations: Strategies, Processes, and Systems , year = 2006, editor =

    CIAO: Chandra's data analysis system. Observatory Operations: Strategies, Processes, and Systems , year = 2006, editor =. doi:10.1117/12.671760 , adsurl =

    2006 doi

  142. [151]

    Chandra, Poonam and Nayana, A. J. and Björnsson, C.-I. and Taddia, Francesco and Lundqvist, Peter and Ray, Alak K. and Shappee, Benjamin J. , title =. The Astrophysical Journal , abstract =. 2019 , month =. doi:10.3847/1538-4357/ab1900 , url =

    2019 doi

Pith tools

Reviewed June 26, 2026 · model on record in the stance chip above.