Pith. sign in

REVIEW 4 major objections 4 minor 169 references

This paper claims that the TeV tail of the magnetar region CXOU J1714–3810 is hadronic, powered by protons in SNR CTB 37B, and that a 50-hour exposure with the next-generation Cherenkov observatory can confirm it.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 21:47 UTC pith:AOS34JMU

load-bearing objection Competent, honest SED modeling of CTB 37B with a weak but not absurd hadronic preference; the useful part is the CTAO forecast, and the load-bearing X-ray upper limit needs scrutiny. the 4 major comments →

arxiv 2607.15955 v1 pith:AOS34JMU submitted 2026-07-17 astro-ph.HE astro-ph.SRhep-ph

Non-thermal emission from the vicinity of the magnetar CXOU J171405.7-381031

Manoel F. Sousa , Rita. C. Anjos This is my paper
classification astro-ph.HE astro-ph.SRhep-ph
keywords magnetarCXOU J1714-3810CTB 37Bsupernova remnantgamma-ray SEDlepto-hadronic modelpion decayCTAO simulation
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper tries to establish that the gamma-ray emission from the environment of the magnetar CXOU J1714–3810, inside supernova remnant CTB 37B, is best described by a mixture of electrons and protons, with inverse-Compton scattering dominating at GeV energies and neutral-pion decay from proton–proton collisions producing the highest-energy TeV photons. The purely leptonic model reproduces the spectrum up to about 10 TeV but underestimates the highest-energy TeV data point, while a lepto-hadronic model with an exponential-cutoff power-law particle distribution and a proton cutoff near 123 TeV fits it better. This requires a large proton energy budget, roughly 10^51 erg, which drops to a plausible fraction of supernova kinetic energy if the remnant is interacting with a dense molecular cloud at 5–10 cm^-3. The paper also finds that a magnetar-wind-nebula origin is morphologically disfavored, and simulates that a 50-hour observing campaign with the next-generation Cherenkov telescope array will measure the proton cutoff and distinguish the scenarios.

Core claim

Within the SNR framework for CTB 37B, the best fit to the multiwavelength spectral energy distribution is the lepto-hadronic model with an electron-to-proton normalization ratio of 10^-2, electron spectral index about 2.2 with a cutoff near 3 TeV, and proton spectral index about 2.0 with a cutoff near 123 TeV. In this model, inverse-Compton scattering of infrared and cosmic-microwave-background photons dominates the GeV band, while neutral-pion decay dominates above about 10 TeV, matching the observed TeV spectrum where the purely leptonic model falls short. The required total proton energy is about 1.2 × 10^51 erg, comparable to the canonical kinetic energy of a core-collapse supernova; if

What carries the argument

The central machinery is a one-zone radiative model fitted to the broadband SED with Markov Chain Monte Carlo sampling, using exponential-cutoff power-law (ecpl) and log-parabolic distributions for the electron and proton populations and a fixed electron-to-proton normalization ratio of 10^-2. The decomposition of the emission into synchrotron, inverse-Compton, and neutral-pion-decay channels against the radio-to-TeV data, together with the X-ray upper limit that pins the electron cutoff near 3 TeV, is what allows the proton cutoff to be inferred at about 123 TeV. The forecasting component uses three-dimensional likelihood analysis with the next-generation observatory's response functions to

Load-bearing premise

The hadronic preference rests on treating the measured 2–10 keV thermal X-ray flux as an upper limit on any non-thermal synchrotron component; if there is an unresolved non-thermal X-ray contribution, the leptonic model could account for the TeV tail and the need for about 10^51 erg in protons would disappear.

What would settle it

A non-thermal X-ray detection from the CTB 37B shell at the level predicted by an unbroken electron spectrum, or a 50-hour observation with the next-generation Cherenkov observatory showing that the spectrum above about 5 TeV steepens sharply rather than persisting as a hard power-law tail up to tens of TeV, would falsify the claim of a hadronic origin for the highest-energy emission.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If the lepto-hadronic interpretation is correct, CTB 37B is actively accelerating protons to hundreds of TeV, making the remnant a Galactic cosmic-ray source.
  • The large proton energy budget either points to an unusually energetic, possibly magnetar-powered, supernova explosion or to a dense ambient medium that enhances pion production.
  • A 50-hour observation with the next-generation Cherenkov observatory will measure the proton cutoff energy and cleanly separate the leptonic and lepto-hadronic scenarios by the spectral shape above about 5 TeV.
  • The magnetar itself is not required to power the TeV emission; the supernova remnant's forward shock suffices as the accelerator.
  • A magnetar-wind-nebula contribution is not fully excluded but would be confined to a small, compact angular region near the magnetar with flux at most comparable to the remnant's.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If an unresolved non-thermal X-ray component lurks beneath the thermal flux adopted as an upper limit, the electron cutoff would not need to be as low as 3 TeV, and a purely leptonic inverse-Compton model could plausibly match the highest-energy TeV data point, removing the need for 10^51 erg in protons.
  • The proton energy budget scales with the square of the assumed distance; adopting the closer 7 kpc distance instead of 13.2 kpc would lower the required energy by roughly a factor of 3.5, substantially easing the tension with canonical supernova energies.
  • The electron-to-proton ratio is fixed at 10^-2 rather than fitted; allowing it to vary could shift the inferred proton cutoff and the statistical preference between the leptonic and lepto-hadronic models, a testable extension of the analysis.
  • The morphological argument—TeV extension of about 21 pc versus a predicted wind-nebula diffusion size of about 4–6 pc—could serve more generally as a diagnostic for distinguishing supernova-remnant from wind-nebula origins in other magnetar associations.

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

4 major / 4 minor

Summary. This paper presents a multiwavelength SED modeling study of the region around the magnetar CXOU J171405.7–381031 / SNR CTB 37B. The authors fit radio-to-TeV data with purely leptonic and lepto-hadronic one-zone models, using exponential cutoff power-law and log-parabolic particle distributions, and constrain parameters with MCMC in Naima. Model configurations are compared with the Bayesian Information Criterion. In the SNR scenario, the leptonic-ecpl model reproduces the overall spectral shape but underestimates the highest-energy H.E.S.S. point; the lepto-hadronic-ecpl model with fixed K_ep=10^-2 adds a pion-decay component above about 10 TeV, at the cost of Wp ≈ 1.2×10^51 erg. The authors also explore a magnetar wind nebula scenario, which is disfavored on morphological grounds, and simulate 50-h CTAO observations to show that the two SNR scenarios differ in the multi-TeV tail.

Significance. If the hadronic preference were robust, this would be a useful identification of a hadronic component in a magnetar-associated SNR and would provide a concrete CTAO strategy for testing the proton cutoff. Strengths of the paper include its reproducible use of public tools (Naima, Gammapy), MCMC-derived parameter uncertainties, BIC comparisons, and explicit simulated CTAO flux points. However, as detailed below, the central preference for a hadronic tail is currently conditional on a restrictive X-ray upper limit, a post hoc choice of K_ep, and essentially a single high-energy data point. The conclusions are plausible but not yet established at the level claimed by the abstract and title.

major comments (4)
  1. [§3.1] The X-ray upper-limit treatment is load-bearing. The text states: 'the observed thermal X-ray flux in the 2–10 keV range ... is adopted as an upper limit on any potential non-thermal component.' This caps the non-thermal synchrotron component at the thermal flux rather than at the total observed 2–10 keV flux. If an unresolved non-thermal power-law component is present below the thermal emission, the true constraint is larger. This assumption forces E_e,cut ≈ 3 TeV and truncates the leptonic IC tail above ~10 TeV—exactly the band where the purely leptonic model falls below H.E.S.S. and where the pion-decay component is introduced. A re-analysis that uses the total 2–10 keV flux as the upper limit, or that frees a non-thermal X-ray normalization, could allow the leptonic model to match the highest-energy H.E.S.S. point and remove the need for hadronic emission. The paper itself acknowledg
  2. [§2 / §3.1] The distance is not reconciled. Section 2 quotes d = 7 kpc (Caswell et al. 1975; Aharonian et al. 2008a) for the SNR age and the magnetar's transverse velocity, while §3.1 adopts d = 13.2 kpc (Tian & Leahy 2012) for the physical radius and the SED modeling. Since the inferred proton energy scales approximately as d^2 for fixed observed flux, this choice changes Wp by a factor of roughly (13.2/7)^2 ≈ 3.6. The sentence in §4.2 that 'this energy estimate scales inversely with the square of the source distance' is also incorrect: W_p ∝ d^2, not d^-2. The paper should justify one distance or show that Wp, W_e, and the particle cutoffs are insensitive to the adopted value.
  3. [§3.1 / Table 1] The statistical comparison between the two main SNR models is incomplete and the K_ep selection is not penalized. The lepto-hadronic analysis fixes K_ep = 10^-2 after exploring alternatives, stating that this 'yielded the optimal fit to the observational data' (§3.1). This post hoc choice on the same data is not included in the BIC as a free parameter, so the model comparison for the lepto-hadronic scenario overstates support. Moreover, Table 1 lists BIC = 47.92 for the Leptonic-ecpl model and BIC = 49.91 for the Lepto-hadronic-ecpl model; the paper never directly compares these two. By the paper's own BIC scale, the purely leptonic model is weakly preferred (ΔBIC ≈ 2). The claimed improvement above ~10 TeV rests on the highest-energy H.E.S.S. point, but no per-point residual or chi-square contribution is reported. Please quantify how the fit changes with and without that point, and trea
  4. [§4.3] The magnetar wind nebula energy-budget calculation is internally inconsistent. The text computes E_sd ≈ 2.6×10^45 erg by effectively multiplying the present spin-down luminosity by the characteristic age, and then argues this is 'several orders of magnitude' below the required electron energy. But for a spin-down-powered system, the integrated energy release over the spin-down history is not E_dot_now × age; it is the difference between the initial and current rotational energies. If P0 < 0.01 s, as invoked later in the same section, the initial reservoir is ≈ 2×10^50 erg and the integrated release is of that order (minus the current rotational energy), not 10^45–10^46 erg. The statement 'Even assuming that the magnetar has the same age as the associated SNR, this value increases to E_sd ≈ 4.2×10^46 erg' is also not a valid spindown integration. This quantitative argument should be corre
minor comments (4)
  1. [Eq. (1)–(2)] The reference energy E0 in the particle spectral formulas is not specified. Since K_ep is defined relative to 1 TeV, please state E0 explicitly (presumably 1 TeV) in the equations or the text.
  2. [Fig. 6] The text mentions significance contours reaching 'approximately 8σ, 13σ, and 16σ' and later gives a detection significance of ~27σ. Clarify whether the latter is a cumulative source significance and how it relates to the quoted contour levels.
  3. [§5] The phrase 'CTAO prediction' is used for what is in fact a forward simulation based on the fitted models. Consider using 'simulated observation' or 'projected spectrum' throughout to avoid overstating the predictive content.
  4. [§3.2] The PWN scenario uses the magnetar X-ray flux (Gotthelf et al. 2019) as an upper limit for nebular emission, but the text does not explain how the point-source magnetar flux relates to an extended nebular component. A brief justification would help.

Circularity Check

0 steps flagged

No circular derivation: the hadronic preference is an in-sample fit outcome, and the CTAO forecast is a forward simulation; only mild post-hoc parameter selection and non-load-bearing self-citations.

full rationale

The paper's central comparison is an open SED fit: particle-distribution parameters are sampled with MCMC/Naima against external radio, X-ray, GeV, and TeV data, and the leptonic vs lepto-hadronic comparison is made with BIC (Section 3.1, Table 1). This is not a derivation of the data from the conclusion. The strongest claim ('lepto-hadronic model ... yields a more complete description of the spectrum, particularly above ~10 TeV') is a description of the best fit, not an out-of-sample prediction. K_ep=10^-2 is selected by optimizing the same data ('Although alternative values of K_ep were explored, a ratio of 10^-2 yielded the optimal fit to the observational data'), so the hadronic preference is partly a post-hoc choice; however, the paper frames it as model comparison, and the statement is not presented as an independent prediction. The X-ray upper-limit treatment that forces E_e,cut~3 TeV is an explicit modeling assumption, and the authors themselves note 'the results depend on the adopted upper limits for the non-thermal X-ray emission' (Conclusions). That is a dependence/uncertainty, not circularity. The CTAO section simulates observations from the fitted models with Gammapy and explicitly states 'The reconstructed spectral flux points closely reproduce the input spectral models' — a sensitivity forecast, not a validation loop. Self-citations (Sousa et al. 2025; Costa et al. 2024) supply prior context and methodology but are not load-bearing for the fit. Overall, the derivation chain is self-contained against external data; no step equates its output to its input by construction.

Axiom & Free-Parameter Ledger

8 free parameters · 7 axioms · 0 invented entities

The central claim rests on standard radiative physics, on domain assumptions about the environment (density, photon fields, distance), and on post hoc choices (K_ep, upper-limit treatment). No new particles, forces, or entities are introduced.

free parameters (8)
  • Electron spectral index Γ_e = 2.18±0.04 (leptonic-ecpl); 2.88±0.04 (leptonic-lp)
    MCMC-fitted slope of the electron energy distribution; sets the broadband SED shape.
  • Electron cutoff energy E_e,cut = 3.17±0.56 TeV (leptonic-ecpl)
    MCMC-fitted; strongly constrained by the X-ray upper limit; critical for suppressing the leptonic TeV tail.
  • Magnetic field B = 27.6±2.9 µG (SNR leptonic-ecpl); 16.7±1.7 µG (leptonic-lp); 5–11 µG (MWN)
    MCMC-fitted from the synchrotron normalization; unusually low for a young SNR and directly affects electron cooling and cutoff.
  • Electron-to-proton ratio K_ep = 10^-2 (fixed after exploration)
    Selected post hoc as the 'optimal fit'; directly sets the proton normalization and therefore Wp, the key energy-budget tension.
  • Proton spectral index Γ_p = 2.04±0.32 (lepto-hadronic-ecpl); 0.12±0.72 (lepto-hadronic-lp)
    MCMC-fitted; the lp variant requires an unphysical hard index, used to discard that model.
  • Proton cutoff energy E_p,cut = 122.8±90.2 TeV (lepto-hadronic-ecpl)
    MCMC-fitted but weakly constrained; the CTAO forecast targets this parameter.
  • Log-parabolic curvature β_e, β_p = β_e=0.085–0.29; β_p=0.673
    Fitted for the lp variants; these variants are statistically disfavored or physically inconsistent.
  • Flux normalizations Φ_0 = Not tabulated directly; W_e and W_p reported in Table 1
    MCMC normalization parameters that set the absolute particle energies.
axioms (7)
  • standard math Standard radiative formulas for synchrotron, inverse Compton, and pp→π0→γγ emission (Rybicki & Lightman 1979; Blumenthal 1970; Kelner et al. 2006) are correct and applicable.
    Invoked throughout §3 via the Naima framework; no derivation is repeated and no alternative radiative model is considered.
  • domain assumption One-zone, stationary, homogeneous emission region; no time-dependent cooling or spatial structure.
    Acknowledged in Conclusions as a simplification; affects the physical interpretation of spectral indices and cutoffs.
  • domain assumption Ambient gas density n=0.5 cm^-3 as inferred from X-ray data is representative for the SNR shell.
    Used for the hadronic normalization; the paper later replaces it with n=5–10 cm^-3 to reduce Wp, showing sensitivity to this input (§4.2).
  • domain assumption Target photon fields are CMB + IR (T=30 K, u=1 eV cm^-3) + optical (T=6000 K, u=1 eV cm^-3) from Porter et al. (2006).
    IR/optical energy densities are assumed, not measured along this specific line of sight; IC flux scales with these.
  • domain assumption Distance to CTB 37B is 13.2 kpc for the modeling.
    Adopted from Tian & Leahy (2012) in §3.1, while §2 uses 7 kpc for age and velocity estimates; physical radii, energy budgets, and MWN size arguments all scale with distance.
  • domain assumption The 2–10 keV thermal X-ray flux is an upper limit on any non-thermal synchrotron component.
    States that no significant non-thermal X-ray emission has been detected (§3.1); this assumption forces the low electron cutoff and is the pivot for the hadronic preference.
  • ad hoc to paper K_ep = 10^-2 is the appropriate electron-to-proton normalization.
    Chosen after exploring alternatives because it yielded the optimal fit (§3.1); not derived from acceleration theory or independent constraints.

pith-pipeline@v1.3.0-alltime-deepseek · 23024 in / 15483 out tokens · 158597 ms · 2026-08-01T21:47:28.448609+00:00 · methodology

0 comments
read the original abstract

Magnetars are neutron stars with ultra-strong magnetic fields ($B \sim 10^{14}$-$10^{15}$ G) and are promising candidates for high-energy particle acceleration. We present a multiwavelength analysis of the region surrounding CXOU J171405.7-381031, a magnetar associated with the supernova remnant (SNR) CTB 37B. The broadband spectral energy distribution spanning radio to TeV energies is modeled using leptonic and lepto-hadronic scenarios, with particle populations constrained using Markov Chain Monte Carlo techniques. Within an SNR framework, both scenarios provide acceptable descriptions of the gamma-ray data. The purely leptonic model reproduces the overall spectral shape but slightly underestimates the highest-energy flux measured by H.E.S.S., whereas a lepto-hadronic interpretation offers an improved description above $\sim 10$ TeV, with inverse-Compton scattering dominating the GeV emission and neutral-pion decay contributing at the highest energies. The required proton energy ($W_{\rm p} \gtrsim 10^{51}$ erg) can be substantially reduced if the remnant interacts with a dense ambient medium. A magnetar wind nebula scenario can reproduce the broadband spectrum but is strongly disfavored by the observed source morphology. Simulated Cherenkov Telescope Array Observatory (CTAO) observations indicate that exposures of $\sim 50$ h will constrain the proton cut-off energy, enabling a decisive test of hadronic emission in this region.

Figures

Figures reproduced from arXiv: 2607.15955 by Manoel F. Sousa, Rita. C. Anjos.

Figure 1
Figure 1. Figure 1: H.E.S.S. VHE 𝛾-ray significance map of the region surrounding SNR CTB 37B / CXOU J1714–3810 (H. E. S. S. Collaboration et al. 2018a), smoothed with a Gaussian kernel of width 0.05◦ . The red star marks the position of the magnetar CXOU J1714–3810 (Olausen & Kaspi 2014). The green circle indicates the radio extent of CTB 37B, with a radius of 5.1 ′ (Green 2025; Xin et al. 2016). The cyan ellipse represents … view at source ↗
Figure 2
Figure 2. Figure 2: Multi-band SED of the region around the magnetar CXOU J1714-3810 in the SNR model for leptonic models. Observational data across radio, X-ray, GeV, and TeV bands are taken from Kassim et al. (1991) (radio), Aharonian et al. (2008a); Blumer et al. (2019) (X-ray), Ajello et al. (2017); Abdollahi et al. (2022) (GeV), and H. E. S. S. Collaboration et al. (2018a) (TeV). The right panel presents the SED modeled … view at source ↗
Figure 3
Figure 3. Figure 3: Multi-band SED of the magnetar CXOU J1714-3810 region modeled within the SNR lepto-hadronic scenario. The relativistic electron and proton populations are described by an exponential cutoff power-law distribution (ecpl; left panel) and a log-parabolic distribution (lp; right panel). In both cases, a fixed electron-to-proton ratio of 𝐾ep = 10−2 is assumed. component, both models yield a non-thermal X-ray fl… view at source ↗
Figure 4
Figure 4. Figure 4: Multi-wavelength SED of the magnetar CXOU J1714-3810 region within the MWN model. The left panel shows the SED modeled with an electron spectrum following an ecpl, while the right panel uses a lp distribution. Observational data are from Kassim et al. (1991) (radio), Gotthelf et al. (2019) (X-ray), Ajello et al. (2017); Abdollahi et al. (2022) (GeV), and H. E. S. S. Collaboration et al. (2018a) (TeV). can … view at source ↗
Figure 5
Figure 5. Figure 5: illustrates the impact of adopting effective gas densities of 𝑛 = 5 cm−3 and 𝑛 = 10 cm−3 on the SED of the SNR region within the lepto-hadronic-ecpl model (𝐾ep = 10−2 ). At these higher densities, gamma-ray emission becomes predominantly hadronic, as the increased target gas density enhances pion production. Conse￾quently, the total energy of relativistic protons required to reproduce the observed spectrum… view at source ↗
Figure 6
Figure 6. Figure 6: Simulated observations of CTAO for CTB 37B/CXOU J1714-3810 region assuming an exposure time of 𝑡obs = 50 h, employing the full southern-array IRFs at a zenith angle of 𝑧 = 20◦ . Upper panels: Simulated VHE gamma-ray excess maps for the leptonic (left) and lepto-hadronic (right) emission scenarios. The maps are generated with a spatial binning of 0.02◦ and smoothed using a Gaussian kernel with width 0.05◦ .… view at source ↗
Figure 7
Figure 7. Figure 7: SED of the region associated with CTB 37B/CXOU J1714-3810, including simulated flux points for the CTAO assuming an observation time of 𝑡obs = 50 h. The emission is modeled using a leptonic-ecpl scenario (left panel) and a lepto-hadronic-ecpl scenario with 𝐾ep = 10−2 (right panel), both of which provide statistically favored representations of the observational data. do Universo” of Fundação de Apoio à Ciê… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

169 extracted references · 12 canonical work pages

  1. [1]

    2024 , eprint=

    A gamma ray study of Galactic PeVatron candidates LHAASO J1825-1236 and J1839-0545 , author=. 2024 , eprint=

    2024

  2. [3]

    Survey of the Inner Galaxy in Very High Energy Gamma Rays

    The H.E.S.S. Survey of the Inner Galaxy in Very High Energy Gamma Rays. , keywords =. doi:10.1086/498013 , archivePrefix =. astro-ph/0510397 , primaryClass =

    Pith/arXiv arXiv

  3. [4]

    , keywords =

    Chandra and HESS observations of the supernova remnant CTB 37B. , keywords =. doi:10.1051/0004-6361:200809655 , archivePrefix =. 0803.0682 , primaryClass =

    Pith/arXiv arXiv

  4. [5]

    , keywords =

    3FHL: The Third Catalog of Hard Fermi-LAT Sources. , keywords =. doi:10.3847/1538-4365/aa8221 , archivePrefix =. 1702.00664 , primaryClass =

    Pith/arXiv arXiv

  5. [6]

    , keywords =

    2FHL: The Second Catalog of Hard Fermi-LAT Sources. , keywords =. doi:10.3847/0067-0049/222/1/5 , archivePrefix =. 1508.04449 , primaryClass =

    Pith/arXiv arXiv

  6. [7]

    , keywords =

    Incremental Fermi Large Area Telescope Fourth Source Catalog. , keywords =. doi:10.3847/1538-4365/ac6751 , archivePrefix =. 2201.11184 , primaryClass =

    Pith/arXiv arXiv

  7. [8]

    arXiv e-prints , keywords =

    Fermi Large Area Telescope Fourth Source Catalog Data Release 4 (4FGL-DR4). arXiv e-prints , keywords =. doi:10.48550/arXiv.2307.12546 , archivePrefix =. 2307.12546 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2307.12546

  8. [9]

    , keywords =

    Fermi Large Area Telescope Third Source Catalog. , keywords =. doi:10.1088/0067-0049/218/2/23 , archivePrefix =. 1501.02003 , primaryClass =

    Pith/arXiv arXiv

  9. [10]

    , keywords =

    Extended VHE -ray emission towards SGR1806-20, LBV 1806-20, and stellar cluster Cl* 1806-20. , keywords =. doi:10.1051/0004-6361/201628695 , archivePrefix =. 1606.05404 , primaryClass =

    Pith/arXiv arXiv

  10. [11]

    Galactic plane survey

    The H.E.S.S. Galactic plane survey. , keywords =. doi:10.1051/0004-6361/201732098 , archivePrefix =. 1804.02432 , primaryClass =

    Pith/arXiv arXiv

  11. [12]

    IEEE Transactions on Automatic Control , keywords =

    A New Look at the Statistical Model Identification. IEEE Transactions on Automatic Control , keywords =

  12. [13]

    , keywords =

    Gammapy: A Python package for gamma-ray astronomy. , keywords =. doi:10.1051/0004-6361/202346488 , archivePrefix =. 2308.13584 , primaryClass =

    Pith/arXiv arXiv

  13. [14]

    doi:10.5281/zenodo.17814297 , url =

    Acero, Fabio and Aguasca-Cabot, Arnau and Barrios-Jiménez, Luis and Arnesen, Tora Therese Høiland and Batt, Anushka and Bernete, Juan and Biederbeck, Noah and Buchner, Johannes and Bylund, Tomas and Djuvsland, Julia and Donath, Axel and Emery, Gabriel and Egg, Katharina and Feijen, Kirsty and Fröse, Stefan and Galelli, Claudio and Gréaux, Lucas and Khélif...

  14. [15]

    , keywords =

    Background modelling in very-high-energy -ray astronomy. , keywords =. doi:10.1051/0004-6361:20066674 , archivePrefix =. astro-ph/0610959 , primaryClass =

    Pith/arXiv arXiv

  15. [16]

    , keywords =

    Analysis methods for results in gamma-ray astronomy. , keywords =. doi:10.1086/161295 , adsurl =

    doi:10.1086/161295

  16. [17]

    doi:10.5281/zenodo.5499840 , url =

    CTAO Instrument Response Functions - prod5 version v0.1 , month = sep, year = 2021, publisher =. doi:10.5281/zenodo.5499840 , url =

    doi:10.5281/zenodo.5499840 2021

  17. [18]

    Nuovo Cimento C Geophysics Space Physics C , year = 2017, month = may, volume =

    GRBs as multimessenger sources. Nuovo Cimento C Geophysics Space Physics C , year = 2017, month = may, volume =. doi:10.1393/ncc/i2017-17126-2 , adsurl =

    doi:10.1393/ncc/i2017-17126-2 2017

  18. [19]

    Frontiers in Astronomy and Space Sciences , keywords =

    Multimessenger Search for the Sources of Cosmic Rays using Cosmic Neutrinos. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2019.00032 , adsurl =

    arXiv 2019

  19. [20]

    , keywords =

    Cosmic rays from pulsars and magnetars. , keywords =. doi:10.1111/j.1745-3933.2010.00874.x , archivePrefix =. 1005.1003 , primaryClass =

    arXiv 2010

  20. [21]

    , keywords =

    The First LHAASO Catalog of Gamma-Ray Sources. , keywords =. doi:10.3847/1538-4365/acfd29 , archivePrefix =. 2305.17030 , primaryClass =

    arXiv

  21. [22]

    , keywords =

    A Catalog of the Highest-energy Cosmic Rays Recorded during Phase I of Operation of the Pierre Auger Observatory. , keywords =. doi:10.3847/1538-4365/aca537 , adsurl =

    doi:10.3847/1538-4365/aca537

  22. [23]

    , keywords =

    Constraining models for the origin of ultra-high-energy cosmic rays with a novel combined analysis of arrival directions, spectrum, and composition data measured at the Pierre Auger Observatory. , keywords =. doi:10.1088/1475-7516/2024/01/022 , archivePrefix =. 2305.16693 , primaryClass =

    Pith/arXiv arXiv 2024

  23. [24]

    Nature Astronomy , keywords =

    Massive stars as major factories of Galactic cosmic rays. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0724-0 , archivePrefix =. 1804.02331 , primaryClass =

    Pith/arXiv arXiv

  24. [25]

    , keywords =

    Massive star cluster origin for the galactic cosmic ray population at very-high energies. , keywords =. doi:10.1093/mnras/stac3469 , archivePrefix =. 2211.11625 , primaryClass =

    Pith/arXiv arXiv

  25. [26]

    , keywords =

    The origin of galactic cosmic rays. , keywords =. doi:10.1007/s00159-013-0070-7 , archivePrefix =. 1311.7346 , primaryClass =

    Pith/arXiv arXiv

  26. [27]

    , keywords =

    Magnetars as powering sources of gamma-ray burst associated supernovae, and unsupervized clustering of cosmic explosions. , keywords =. doi:10.1093/mnras/stae901 , archivePrefix =. 2403.18076 , primaryClass =

    Pith/arXiv arXiv

  27. [28]

    European Physical Journal Web of Conferences , year = 2023, series =

    UHECR results of combined analyses of TA and Auger experiments. European Physical Journal Web of Conferences , year = 2023, series =. doi:10.1051/epjconf/202328004001 , adsurl =

    arXiv 2023

  28. [29]

    Annual Review of Nuclear and Particle Science , keywords =

    Ultra-High-Energy Gamma-Ray Astronomy. Annual Review of Nuclear and Particle Science , keywords =. doi:10.1146/annurev-nucl-112822-025357 , archivePrefix =. 2310.01744 , primaryClass =

    Pith/arXiv arXiv

  29. [30]

    , keywords =

    Formation of Very Strongly Magnetized Neutron Stars: Implications for Gamma-Ray Bursts. , keywords =. doi:10.1086/186413 , adsurl =

    doi:10.1086/186413

  30. [31]

    Radiative mechanism for outbursts

    The soft gamma repeaters as very strongly magnetized neutron stars - I. Radiative mechanism for outbursts. , keywords =. doi:10.1093/mnras/275.2.255 , adsurl =

    doi:10.1093/mnras/275.2.255

  31. [32]

    , keywords =

    Binary Coalescences as Sources of Ultrahigh-Energy Cosmic Rays. , keywords =. doi:10.1103/PhysRevLett.132.091401 , archivePrefix =. 2307.06200 , primaryClass =

    Pith/arXiv arXiv

  32. [33]

    doi:10.1142/10986 , adsurl =

    Science with the Cherenkov Telescope Array. doi:10.1142/10986 , adsurl =

    doi:10.1142/10986

  33. [34]

    W. B. Atwood and A. A. Abdo and M. Ackermann and W. Althouse and B. Anderson and M. Axelsson and L. Baldini and J. Ballet and D. L. Band and G. Barbiellini and J. Bartelt and D. Bastieri and B. M. Baughman and K. Bechtol and D. Bédérède and F. Bellardi and R. Bellazzini and B. Berenji and G. F. Bignami and D. Bisello and E. Bissaldi and R. D. Blandford an...

    2009

  34. [35]

    Publications of the Astronomical Society of Japan , keywords =

    Identification of CXOU J171405.7-381031 as a New Magnetar with XMM-Newton. Publications of the Astronomical Society of Japan , keywords =. doi:10.1093/pasj/62.5.L33 , archivePrefix =. 1008.0234 , primaryClass =

    Pith/arXiv arXiv

  35. [36]

    The Astrophysical Journal , keywords =

    Two Magnetar Candidates in HESS Supernova Remnants. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/710/2/941 , archivePrefix =. 0912.4985 , primaryClass =

    Pith/arXiv arXiv

  36. [37]

    Astronomy and Astrophysics , keywords =

    Discovery of a VHE gamma-ray source coincident with the supernova remnant CTB 37A. Astronomy and Astrophysics , keywords =. doi:10.1051/0004-6361:200809722 , archivePrefix =. 0803.0702 , primaryClass =

    Pith/arXiv arXiv

  37. [38]

    The Astrophysical Journal , keywords =

    An Energetic Magnetar in HESS J1713-381/CTB 37B. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/725/1/1384 , archivePrefix =. 1008.2558 , primaryClass =

    Pith/arXiv arXiv

  38. [39]

    The Astrophysical Journal , keywords =

    The Prelude to and Aftermath of the Giant Flare of 2004 December 27: Persistent and Pulsed X-Ray Properties of SGR 1806-20 from 1993 to 2005. The Astrophysical Journal , keywords =. doi:10.1086/507459 , archivePrefix =. astro-ph/0602402 , primaryClass =

    Pith/arXiv arXiv 2004

  39. [40]

    Monthly Notices of the Royal Astronomical Society , keywords =

    A downward revision to the distance of the 1806-20 cluster and associated magnetar from Gemini Near-Infrared Spectroscopy. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1745-3933.2008.00453.x , archivePrefix =. 0802.0815 , primaryClass =

    arXiv 2008

  40. [41]

    dos Anjos and Jaziel G

    Rita C. dos Anjos and Jaziel G. Coelho and Jonas P. Pereira and Fernando Catalani , title =. Journal of Cosmology and Astroparticle Physics , abstract =. 2021 , month =. doi:10.1088/1475-7516/2021/10/023 , url =

    doi:10.1088/1475-7516/2021/10/023 2021

  41. [42]

    Coelho and Luana N

    Jaziel G. Coelho and Luana N. Padilha and Rita C. dos Anjos and Cynthia V. Ventura and Geanderson A. Carvalho , title =. 2022 , month =. doi:10.1088/1475-7516/2022/10/041 , url =

    doi:10.1088/1475-7516/2022/10/041 2022

  42. [43]

    , keywords =

    A GeV Source in the Direction of Supernova Remnant CTB 37B. , keywords =. doi:10.3847/0004-637X/817/1/64 , archivePrefix =. 1509.08548 , primaryClass =

    Pith/arXiv arXiv

  43. [44]

    , keywords =

    Suzaku Observations of SGR1900+14 and SGR1806-20. , keywords =. doi:10.1093/pasj/61.sp1.S387 , archivePrefix =. 0808.3846 , primaryClass =

    Pith/arXiv arXiv

  44. [45]

    , keywords =

    The McGill Magnetar Catalog. , keywords =. doi:10.1088/0067-0049/212/1/6 , archivePrefix =. 1309.4167 , primaryClass =

    Pith/arXiv arXiv

  45. [46]

    Reports on Progress in Physics , keywords =

    Physics of strongly magnetized neutron stars. Reports on Progress in Physics , keywords =. doi:10.1088/0034-4885/69/9/R03 , archivePrefix =. astro-ph/0606674 , primaryClass =

    Pith/arXiv arXiv

  46. [47]

    Advances in Space Research , year = 2011, month = apr, volume =

    The multi-wavelength properties of Anomalous X-ray Pulsars and Soft Gamma-ray Repeaters. Advances in Space Research , year = 2011, month = apr, volume =. doi:10.1016/j.asr.2010.08.031 , adsurl =

    doi:10.1016/j.asr.2010.08.031 2011

  47. [48]

    , keywords =

    Proper Motions and Origins of SGR 1806-20 and SGR 1900+14. , keywords =. doi:10.1088/0004-637X/761/1/76 , archivePrefix =. 1210.8151 , primaryClass =

    Pith/arXiv arXiv 1900

  48. [49]

    , keywords =

    An exceptionally bright flare from SGR 1806-20 and the origins of short-duration -ray bursts. , keywords =. doi:10.1038/nature03519 , archivePrefix =. astro-ph/0502329 , primaryClass =

    Pith/arXiv arXiv

  49. [50]

    , keywords =

    The Nature of a Cosmic-Ray Accelerator, CTB37B, Observed with Suzaku and Chandra. , keywords =. doi:10.1093/pasj/61.sp1.S197 , archivePrefix =. 0808.2339 , primaryClass =

    Pith/arXiv arXiv

  50. [51]

    Science , keywords =

    A New Population of Very High Energy Gamma-Ray Sources in the Milky Way. Science , keywords =. doi:10.1126/science.1108643 , archivePrefix =. astro-ph/0504380 , primaryClass =

    Pith/arXiv arXiv

  51. [53]

    , keywords =

    Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field. , keywords =. doi:10.1086/507770 , archivePrefix =. astro-ph/0607344 , primaryClass =

    Pith/arXiv arXiv

  52. [54]

    , keywords =

    A New Look at the ``Jet'' in the CTB 37A/B Supernova Remnant Complex. , keywords =. doi:10.1086/170110 , adsurl =

    work page doi:10.1086/170110

  53. [55]

    1509.03319 , adsurl =

    naima: a Python package for inference of relativistic particle energy distributions from observed nonthermal spectra , year = 2015, journal =. 1509.03319 , adsurl =

    Pith/arXiv arXiv 2015

  54. [56]

    Galaxies , year = 2023, month = mar, volume =

    Challenges of This Century in High-Density Compact Objects, High-Energy Astrophysics, and Multi-Messenger Observations: Quo Vadis?. Galaxies , year = 2023, month = mar, volume =. doi:10.3390/galaxies11020048 , adsurl =

    work page doi:10.3390/galaxies11020048 2023

  55. [57]

    , keywords =

    Fermi Large Area Telescope observations of the supernova remnant HESS J1731-347. , keywords =. doi:10.1051/0004-6361/201322737 , archivePrefix =. 1405.4888 , primaryClass =

    Pith/arXiv arXiv

  56. [58]

    , keywords =

    Evolution of High-energy Particle Distribution in Mature Shell-type Supernova Remnants. , keywords =. doi:10.3847/1538-4357/834/2/153 , archivePrefix =. 1611.07564 , primaryClass =

    Pith/arXiv arXiv

  57. [59]

    , keywords =

    Modeling the Multi-Wavelength Emission of the Shell-type Supernova Remnant RX J1713.7-3946. , keywords =. doi:10.1088/0004-637X/735/2/120 , archivePrefix =. 1011.0145 , primaryClass =

    Pith/arXiv arXiv

  58. [60]

    , keywords =

    Gamma-Ray Observations of the Supernova Remnant RX J0852.0-4622 with the Fermi Large Area Telescope. , keywords =. doi:10.1088/2041-8205/740/2/L51 , archivePrefix =. 1109.4658 , primaryClass =

    Pith/arXiv arXiv 2041

  59. [61]

    , keywords =

    The acceleration of cosmic rays in shock fronts - I. , keywords =. doi:10.1093/mnras/182.2.147 , adsurl =

    doi:10.1093/mnras/182.2.147

  60. [62]

    10 ^ 14 to 10 ^ 18 eV

    Cosmic Rays from the Knee to the Second Knee:. 10 ^ 14 to 10 ^ 18 eV. Modern Physics Letters A , keywords =. doi:10.1142/S0217732307024139 , archivePrefix =. astro-ph/0611387 , primaryClass =

    Pith/arXiv arXiv

  61. [63]

    , keywords =

    An unusual supernova in the error box of the -ray burst of 25 April 1998. , keywords =. doi:10.1038/27150 , archivePrefix =. astro-ph/9806175 , primaryClass =

    Pith/arXiv arXiv 1998

  62. [64]

    , keywords =

    Energy Spectrum and Chemical Composition of Ultrahigh Energy Cosmic Rays from Semi-relativistic Hypernovae. , keywords =. doi:10.1088/0004-637X/746/1/40 , archivePrefix =. 1111.6256 , primaryClass =

    Pith/arXiv arXiv

  63. [65]

    IAU General Assembly , year = 2015, volume =

    Mopra CO-line observation towards SNR CTB37B. IAU General Assembly , year = 2015, volume =

    2015

  64. [66]

    Cosmic Rays and Particle Physics

  65. [67]

    , keywords =

    Gamma rays from cosmic rays in supernova remnants. , keywords =. doi:10.1051/0004-6361/201220394 , archivePrefix =. 1210.8071 , primaryClass =

    Pith/arXiv arXiv

  66. [68]

    Planets, Stars and Stellar Systems

    Gamma-Ray Emission of Supernova Remnants and the Origin of Galactic Cosmic Rays , author=. Planets, Stars and Stellar Systems. Volume 5: Galactic Structure and Stellar Populations , volume=

  67. [69]

    , keywords =

    Energy Partition between Energetic Electrons and Turbulent Magnetic Field in Supernova Remnant RX J1713.7-3946. , keywords =. doi:10.1088/0004-637X/773/2/138 , archivePrefix =. 1306.4399 , primaryClass =

    Pith/arXiv arXiv

  68. [70]

    , keywords =

    On the Foundation of Equipartition in Supernova Remnants. , keywords =. doi:10.3847/1538-4357/aaac2d , archivePrefix =. 1801.10422 , primaryClass =

    Pith/arXiv arXiv

  69. [71]

    , keywords =

    MAGPIS: A Multi-Array Galactic Plane Imaging Survey. , keywords =. doi:10.1086/503253 , adsurl =

    doi:10.1086/503253

  70. [72]

    , keywords =

    The Bolocam Galactic Plane Survey: Survey Description and Data Reduction. , keywords =. doi:10.1088/0067-0049/192/1/4 , archivePrefix =. 1011.0691 , primaryClass =

    Pith/arXiv arXiv

  71. [73]

    , keywords =

    Magnetars in the Metagalaxy: An Origin for Ultra-High-Energy Cosmic Rays in the Nearby Universe. , keywords =. doi:10.1086/374776 , archivePrefix =. astro-ph/0208444 , primaryClass =

    Pith/arXiv arXiv

  72. [74]

    Ultrahigh energy cosmic ray acceleration in newly born magnetars and their associated gravitational wave signatures , author =. Phys. Rev. D , volume =. 2011 , month =. doi:10.1103/PhysRevD.84.023002 , url =

    work page doi:10.1103/physrevd.84.023002 2011

  73. [75]

    Kinematics and Physics of Celestial Bodies , keywords =

    Magnetar SGR 1900+14 as a Potential Source of Galactic Cosmic Rays with Energies Above 10 ^ 20 eV. Kinematics and Physics of Celestial Bodies , keywords =. doi:10.3103/S0884591318040037 , adsurl =

    work page doi:10.3103/s0884591318040037 1900

  74. [76]

    A review

    Magnetars: the physics behind observations. A review. Reports on Progress in Physics , keywords =. doi:10.1088/0034-4885/78/11/116901 , archivePrefix =. 1507.02924 , primaryClass =

    Pith/arXiv arXiv

  75. [77]

    , keywords =

    Prospects for Gamma-Ray Emission from Magnetar Regions in CTAO Observations. , keywords =. doi:10.3847/1538-4357/ad9b23 , archivePrefix =. 2412.02860 , primaryClass =

    Pith/arXiv arXiv

  76. [78]

    , keywords =

    A giant -ray flare from the magnetar SGR 1806 - 20. , keywords =. doi:10.1038/nature03525 , archivePrefix =. astro-ph/0503030 , primaryClass =

    Pith/arXiv arXiv

  77. [79]

    , keywords =

    TeV gamma-rays from accreting magnetars in massive binaries. , keywords =. doi:10.1111/j.1365-2966.2009.14893.x , archivePrefix =. 0901.0392 , primaryClass =

    arXiv 2009

  78. [80]

    , keywords =

    Spatially resolved X-ray study of supernova remnants that host magnetars: Implication of their fossil field origin. , keywords =. doi:10.1051/0004-6361/201936002 , archivePrefix =. 1909.01922 , primaryClass =

    Pith/arXiv arXiv 1909

  79. [81]

    , keywords =

    Magnetars. , keywords =. doi:10.1146/annurev-astro-081915-023329 , archivePrefix =. 1703.00068 , primaryClass =

    Pith/arXiv arXiv

  80. [82]

    , keywords =

    Comparing supernova remnants around strongly magnetized and canonical pulsars. , keywords =. doi:10.1093/mnras/stu1594 , archivePrefix =. 1409.1027 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.