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arxiv: 1906.10021 · v1 · pith:X2U6B2XYnew · submitted 2019-06-24 · 🌌 astro-ph.GA

3D Optical Spectroscopic Study of NGC3344 with SITELLE: I. Identification and Confirmation of Supernova Remnants

Ismael Moumen , Carmelle Robert , Daniel Devost , Ren\'e Pierre Martin , Laurie Rousseau-Nepton , Laurent Drissen , Thomas Martin This is my paper

Pith reviewed 2026-05-25 17:13 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords supernova remnantsNGC3344SITELLEemission line ratiosshock ionizationmetallicitygalactic environment
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The pith

High-resolution spectroscopy confirms 42 supernova remnants in NGC3344 with metallicities from LMC-like to twice solar.

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

The paper applies SITELLE integral-field spectroscopy to NGC3344 to locate and verify supernova remnants amid a bright stellar and diffuse-gas background. Regions are first selected where the [S II]/Hα flux ratio reaches or exceeds 0.4, yielding 129 candidates whose emission lines are measured across multiple species. Sabbadin plots and BPT diagrams then classify the sample into 42 confirmed shock-heated SNRs, 45 probable ones, and 42 less likely objects. The confirmed remnants show metallicities spanning LMC to twice-solar values, with observed trends linking remnant size to line ratios, local environment, and distance from the galaxy center.

Core claim

Using SITELLE data, the study isolates 129 SNR candidates in NGC3344 via the [S II]/Hα ≥ 0.4 criterion, then applies Sabbadin plots and BPT diagrams to confirm shock ionization and arrive at 42 confirmed SNRs whose metallicities, derived from shock models, range between LMC and 2×solar values. Correlations emerge between confirmed-SNR size and emission-line ratios, galactic environment, and galactocentric distance, including a metallicity gradient and evolutionary signatures.

What carries the argument

The [S II]/Hα ≥ 0.4 threshold combined with Sabbadin plots and BPT diagrams to isolate shock-heated supernova remnants from H II regions and diffuse ionized gas.

If this is right

  • The 42 confirmed SNRs exhibit metallicities between LMC and twice solar according to shock models.
  • A metallicity gradient appears among the SNR population as a function of galactocentric distance.
  • Correlations between SNR size, line ratios, and environment indicate evolutionary effects within the sample.
  • The classification method succeeds in separating SNRs despite NGC3344's prominent stellar and diffuse-gas background.

Where Pith is reading between the lines

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

  • The same line-ratio and diagram criteria could be applied to other nearby spirals to enlarge the census of confirmed SNRs.
  • Metallicity trends measured from the SNR population offer an independent check on chemical-enrichment maps derived from H II regions.
  • Multi-wavelength follow-up on the probable and less-likely candidates would test whether the adopted thresholds miss or over-count genuine remnants.

Load-bearing premise

The assumption that a [S II]/Hα ratio of 0.4 or higher plus the Sabbadin and BPT diagrams cleanly separate shock-heated supernova remnants from photoionized gas even when stellar populations and diffuse background are strong.

What would settle it

X-ray or deeper optical spectra of the 42 confirmed candidates that show dominant photoionization signatures rather than the expected shock-excited line ratios.

Figures

Figures reproduced from arXiv: 1906.10021 by Carmelle Robert, Daniel Devost, Ismael Moumen, Laurent Drissen, Laurie Rousseau-Nepton, Ren\'e Pierre Martin, Thomas Martin.

Figure 1
Figure 1. Figure 1: An example of the sky background spectrum in the case of the SN3 filter. The strong OH lines seen in this wavelength range are identified. lines in each datacube. ORCS returned maps, for each emis￾sion line, of the amplitude (intensity), FWHM, continuum height, flux, and velocity (based on one or multiple lines centroid). More maps are also returned for the parameters uncertainty. For example, [PITH_FULL_… view at source ↗
Figure 2
Figure 2. Figure 2: The SITELLE image of NGC 3344 obtained from the combination of the SN1 (blue) and SN3 (red) deep images. The image is centred on the galaxy (at RA = 10h43m31.15s and DEC = +24◦55020.000) and fills the FoV of SITELLE (110 × 110 ). Bright lines are artefacts caused by saturated stars. North is up and East is left. 4 SNR CANDIDATES 4.1 Automatic Detection of Emission Regions In order to identify the SNR candi… view at source ↗
Figure 3
Figure 3. Figure 3: Examples of SITELLE spectra for one pixel within the SNR candidates SNR-C 1050 (top) and SNR-C 159 (bottom). The segments for the three filters are shown including the emission lines, from right to left: SN1 (R = 400), SN2 (R = 600), and SN3 (R = 1500). In black, the observed spectrum and in red, the fit obtained with ORCS. The strong emission lines are identified. The S/NHα = 19 for SNR-C 1050 and 80 for … view at source ↗
Figure 4
Figure 4. Figure 4: NGC 3344 velocity map. This map was obtained con￾sidering only the spaxels with S/NHα ≥ 3. sion lines are rather strong, relative to Hα, and may be re￾lated to a different emission process (i.e. shocks vs. pho￾toionization), and are therefore considered here as better suited to define the SNR’s boundary. As an example, Fig￾ure 5 presents the Hα and [S II] maps near one of our best SNR candidates, SNR-C 159… view at source ↗
Figure 6
Figure 6. Figure 6: The [S II] map near the SNR candidate SNR-C 159, where the outer limit for various emission regions are shown. are not SNRs, but H II regions (almost 3000 emission re￾gions have been found using the same technique but with the Hα+Hβ+[O III] map; Moumen et al. in prep.) and also DIG regions. 4.2 Removal of the Stellar Populations and Diffuse Ionized Gas Background In order to isolate and study the emission … view at source ↗
Figure 5
Figure 5. Figure 5: Hα (top) and [S II]λ6716+[S II]λ6731 (bottom) flux maps near the SNR candidate SNR-C 159. While the scale of the images was selected so the brightness of the H II regions in the Hα and the [S II] maps is comparable, SNR-C 159 appears clearly in the [S II] map which is known to be a good tracer of shock-heated gas. peaked to very diffused). The code then returns for each emission region a list of parameters… view at source ↗
Figure 7
Figure 7. Figure 7: Pseudo-Voight profile of the diffused region SNR-C 348 (most probably a DIG region) and the compact region SNR-C 159 (one of the best SNR candidates), as obtained with the technique of Rousseau-Nepton et al. (2018) adapted to SNR candidates. For the second method, we considered a Global Galaxy Background (GGB) obtained by creating median spectra in rings centred on the galaxy. The spaxels position and gala… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of the SN3 emission lines’ flux in the galaxy background spectra created with the local LGB (in blue) and global GGB method (in red). There is one data point for all the emission regions, corresponding to the position (i.e. the galactocentric distance) of the emission region peak. All the back￾ground spectra have been scaled to the continuum level of the re￾gions prior to line measurements. The … view at source ↗
Figure 9
Figure 9. Figure 9: SN3 global galaxy background (GGB) spectra for dif￾ferent galactocentric distances. For each spectrum, the central radius of the background annulus is indicated on the plot, along with the annulus half width. NGC 3344 shows an important DIG contribution that dominates these spectra. At a galactocentric radius of ≥ 4 kpc, the noise level becomes important. by the work of Mathewson & Healey (1963) and Mathew… view at source ↗
Figure 10
Figure 10. Figure 10: Spectra of two SNR candidates after the subtraction of the GGB background. SNR-C 1050 is located inside the galaxy inner ring while SNR-C 159 has a lower background level at a distance of 3.25 kpc from the galaxy centre. The weighted spectrum is the background spectrum assigned to the region, before it is scaled to the continuum level of the region. where E(β − α)/E(B − V) = 1.07 (as extracted from the an… view at source ↗
Figure 11
Figure 11. Figure 11: Histograms of the selected SNR candidates as a func￾tion of: (a) the [S II]/Hα flux ratio, (b) the Hα Flux, (c) the size Σ, and (d) the profile correlation coefficient R. All these candidates satisfy the selection requirements given in Section 4.3. seen. As shown in the figure, the subtraction of the local background (LGB) produce more scatter in the Hα/Hβ ra￾tio than the subtraction of the global backgro… view at source ↗
Figure 12
Figure 12. Figure 12: The Hα/Hβ ratio for all the SNR candidates. Left: before the background subtraction. Centre: after the background subtraction using the LGB (blue) and the GGB (red) measurements. Right: the galactocentric variation of the color excess obtained using Equation 1 and considering only the SNR candidates with S/N > 5 for all the emission lines Hβ, Hα, [SII]λ6716, and [SII]λ6731 [PITH_FULL_IMAGE:figures/full_f… view at source ↗
Figure 13
Figure 13. Figure 13: Tree of decision used to confirm the SNRs in NGC 3344. Sabbadin plots and BPT diagrams, based on emission line ratios, offer constrains for the ionization mechanism. By the end of this analysis, the 129 SNR candidates fall into one of the three categories: Confirmed (42), Probable (45), or Less likely SNRs (42). we are confident that along with the galaxy background subtraction, the DIG contribution was r… view at source ↗
Figure 14
Figure 14. Figure 14: Sabbadin plots with the 129 SNR candidates found in NGC 3344. The final classification of the candidates is shown using different colors: red for the Confirmed SNRs, green for the Probable SNRs, and black for the Less likely SNRs. Shaded zones and lines are used to separate the position of the SNRs, H II regions, and planetary nebulae according to Sabbadin et al. (1977). Circles with a ‘+’ symbol indicate… view at source ↗
Figure 16
Figure 16. Figure 16: presents the distribution of the velocity dis￾persion σv measured with the Hα line for the confirmed SNRs. Values of σv are ranging from 31 to 93 km s−1 with two peaks at 35 and 55 km s−1 . In [PITH_FULL_IMAGE:figures/full_fig_p016_16.png] view at source ↗
Figure 15
Figure 15. Figure 15: BPT-NII and BPT-SII diagrams of the 129 SNR can￾didates found in NGC 3344. Colors and symbols are the same as presented in [PITH_FULL_IMAGE:figures/full_fig_p016_15.png] view at source ↗
Figure 17
Figure 17. Figure 17: Relations between the Hα velocity dispersion σv of the Confirmed SNRs and their emission lines ratios, size (Σ) and galactocentric distance (GCD). The parameters of the linear fit (dotted line), along with the correlation coefficient (CR), are indicated for each relation. 7 CONCLUSIONS In this paper, we used the high spectral and spatial resolu￾tion data obtained with the iFTS SITELLE at the CFHT to study… view at source ↗
Figure 18
Figure 18. Figure 18: [O III]λ5007/Hβ versus [N II]λ6583/Hα based on (a) the shock-only and (b) the shock+precursor models of Allen et al. (2008) for five abundances (SMC, LMC, Dopita2005, so￾lar, and 2 × solar, as indicated on the plots) with the density n = 1 cm−3 . Vertical lines represent different values of the mag￾netic parameter, from 10−4 to 10 µG cm3/2 , while horizontal lines represent the shock velocity, from 200 to… view at source ↗
Figure 19
Figure 19. Figure 19: Emission line ratios based on the model of Dopita et al. (1984) for a shock velocity of 106 km s−1 . (a) for a fixed abundance ratio O/S=42.8 and different abundances O/N/C as indicated. (b) for different ratios O/S as indicated. (c) and (d) for a fixed abundance ratio O/S=42.8 and different values of O/N and Z(O) as indicated. SNRs from M81 and M82 (Lee et al. 2015) along with SNRs from M31 (Galarza et a… view at source ↗
Figure 21
Figure 21. Figure 21: Emission line ratios for the Confirmed SNRs as a function of the galactocentric distance. The dashed lines display a linear fit through the data. The fit parameters are given for each plot, along with the correlation coefficient (CR). MNRAS 000, 1–28 (2018) [PITH_FULL_IMAGE:figures/full_fig_p020_21.png] view at source ↗
read the original abstract

We present the first optical identification and confirmation of a sample of supernova remnants (SNRs) in the nearby galaxy NGC3344. Using high spectral and spatial resolution data, obtained with the CFHT imaging Fourier transform spectrograph SITELLE, we identified about 2200 emission line regions, many of which are HII regions, diffuse ionized gas regions, and also SNRs. Considering the stellar population and diffuse ionized gas background, that are quite important in NGC3344, we have selected 129 SNR candidates based on four criteria for regions where the emission lines flux ratio [S II]/H$\alpha$$\ge$0.4. Emission lines of [O II]$\lambda$3727, H$\alpha$, [O III]$\lambda\lambda$4959,5007, H$\alpha$, [N II]$\lambda\lambda$6548,6583, and [S II]$\lambda\lambda$6716,6731 have been measured to study the ionized gas properties of the SNR candidates. We adopted a self-consistent spectroscopic analysis, based on Sabbadin plots and BPT diagrams, to confirm the shock-heated nature of the ionization mechanism in the candidates sample. With this analysis, we end up with 42 Confirmed SNRs, 45 Probable SNRs, and 42 Less likely SNRs. Using shock models, the Confirmed SNRs seems to have a metallicity ranging between LMC and 2$\times$solar. We looked for correlations between the size of the Confirmed SNRs and their emission lines ratios, their galaxy environment, and their galactocentric distance: we see a trend for a metallicity gradient among the SNR population, along with some evolutionary effects.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript reports the first optical identification of supernova remnants in NGC3344 using SITELLE integral-field spectroscopy. From ~2200 emission-line regions, 129 SNR candidates are selected via the [S II]/Hα ≥ 0.4 criterion (one of four selection criteria) and then classified using Sabbadin plots and BPT diagrams, yielding 42 confirmed SNRs, 45 probable SNRs and 42 less-likely SNRs. Shock-model comparisons indicate metallicities between LMC and 2×solar for the confirmed sample, with reported trends versus size, environment and galactocentric distance.

Significance. If the classification is robust, the work supplies a sizable, spectroscopically vetted SNR sample in a nearby spiral galaxy that exhibits strong DIG and stellar background, enabling studies of metallicity gradients and evolutionary effects with high-resolution IFU data.

major comments (2)
  1. [Abstract and candidate selection] Abstract (candidate-selection paragraph) and § on SNR confirmation: the paper states that stellar population and DIG background are “quite important” in NGC3344, yet supplies no quantitative test (dilution factors, mock spectra, or false-positive rates) demonstrating that the [S II]/Hα ≥ 0.4 threshold plus Sabbadin/BPT loci remain orthogonal to H II and DIG loci under these conditions. This is load-bearing for the final counts (42 confirmed SNRs) and the derived metallicity range.
  2. [Abstract] The manuscript invokes “four criteria” for candidate selection but only explicitly states the [S II]/Hα ≥ 0.4 ratio; the remaining three criteria are not enumerated, preventing independent verification of the 129-candidate list.
minor comments (2)
  1. Add uncertainty estimates or error bars to the line-ratio points plotted in the Sabbadin and BPT diagrams.
  2. Clarify whether the shock-model metallicity grid is interpolated or extrapolated for the observed line ratios.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We address each major comment below and indicate where revisions will be made to improve the manuscript.

read point-by-point responses

  1. Referee: [Abstract and candidate selection] Abstract (candidate-selection paragraph) and § on SNR confirmation: the paper states that stellar population and DIG background are “quite important” in NGC3344, yet supplies no quantitative test (dilution factors, mock spectra, or false-positive rates) demonstrating that the [S II]/Hα ≥ 0.4 threshold plus Sabbadin/BPT loci remain orthogonal to H II and DIG loci under these conditions. This is load-bearing for the final counts (42 confirmed SNRs) and the derived metallicity range.

    Authors: We agree that quantitative tests of the impact of stellar population and DIG background would strengthen the robustness of the classification. In the revised manuscript we will add a dedicated subsection that estimates dilution factors from the observed continuum and line fluxes, applies the selection criteria to a control sample of confirmed H II regions, and discusses the resulting false-positive rates. This will directly support the reliability of the 42 confirmed SNRs and the reported metallicity range. revision: yes

  2. Referee: [Abstract] The manuscript invokes “four criteria” for candidate selection but only explicitly states the [S II]/Hα ≥ 0.4 ratio; the remaining three criteria are not enumerated, preventing independent verification of the 129-candidate list.

    Authors: The abstract refers to four criteria without enumerating them. We will revise the abstract to list the four criteria explicitly while directing readers to the detailed description already present in the candidate-selection section. This change will enable independent verification without altering the scientific content. revision: yes

Circularity Check

0 steps flagged

No circularity; classification applies external literature diagnostics directly to observed fluxes

full rationale

The paper identifies SNR candidates by applying the standard [S II]/Hα ≥ 0.4 threshold (from external literature) to ~2200 emission-line regions, then uses Sabbadin plots and BPT diagrams (likewise imported) to classify 42 Confirmed SNRs. Shock-model metallicities are also taken from published grids. None of these steps involve fitting parameters inside the paper and then relabeling the fit as a prediction, self-defining quantities, or load-bearing self-citations whose validity reduces to the present work. The counts and metallicity range are therefore the direct, non-circular output of fixed external criteria applied to the SITELLE line measurements.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The work rests on established domain assumptions about spectral diagnostics rather than new free parameters or postulated entities.

axioms (2)
  • domain assumption Emission line flux ratios such as [S II]/Hα ≥ 0.4 indicate shock-heated gas typical of SNRs
    Standard criterion invoked for candidate selection in the abstract.
  • domain assumption Sabbadin plots and BPT diagrams reliably distinguish shock ionization from photoionization in this galactic environment
    Used to confirm the shock-heated nature after candidate selection.

pith-pipeline@v0.9.0 · 5875 in / 1360 out tokens · 34443 ms · 2026-05-25T17:13:57.960536+00:00 · methodology

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Works this paper leans on

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