Pith. sign in

REVIEW 2 major objections 6 minor 159 references

The supernova remnant population of the Small Magellanic Cloud

T0 review · 2 major / 6 minor · reviewed 2026-08-14 · deepseek-v4-flash

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

Pith's one-line read The Small Magellanic Cloud hosts about 4.7 core-collapse supernova remnants for every type Ia remnant, a ratio three times higher than in the Large Magellanic Cloud, implying that the galaxies' recent star formation histories set their…

desk verdict A careful SMC SNR census whose headline CC/Ia ratio depends on two environment-only classifications; the catalog and abundance results are worth engaging with despite that fragility. read the letter →

arxiv 1908.11234 v1 pith:JGVJYHWH submitted 2019-08-29 astro-ph.HE astro-ph.GA

P. Maggi , M. D. Filipovic , B. Vukotic , J. Ballet , F. Haberl , C. Maitra , P. Kavanagh , M. Sasaki
show 1 more author
M. Stupar
This is my paper · ORCID
classification astro-ph.HEastro-ph.GA
keywords supernovaremnantsSmallMagellanicCloudcore-collapsesupernovaetypeIaX-rayspectroscopystarformationhistoryinterstellarmediumabundances
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper builds a complete, multiwavelength census of the Small Magellanic Cloud's supernova remnants, then uses each remnant's X-ray spectrum and local stellar environment to assign it to a core-collapse or type Ia explosion. The central result is a measured ratio of $N_{\mathrm{CC}}/N_{\mathrm{Ia}} = 4.7$, with limits 2.8 to 5.3, about three times higher than the same method finds in the Large Magellanic Cloud. The difference would mean the type Ia rate tracks intermediate-age star formation: the LMC had a burst 0.5–1.5 billion years ago that seeded a large population of Ia progenitors, while the SMC did not. The same data also yield hot-gas abundances for O, Ne, Mg, and Fe at 0.1–0.2 solar and show that SMC remnants expand into a thinner, less disturbed medium than LMC remnants. A sympathetic reader would care because a nearby galaxy's SNR population is the cleanest available record of recent supernova physics and metal production.

What carries the argument

The argument rests on a two-part hint system. A spectral hint on a 1–5 scale is assigned from X-ray ejecta abundance flags (high or low X/Fe ratios for O, Ne, Mg, Si) or from the presence of a pulsar or pulsar wind nebula; an environmental hint is assigned from $N_{\mathrm{OB}}$, the number of massive blue stars within 100 pc, combined with $r = \Psi_1 M_1/(\Psi_2 M_2 + \Psi_3 M_3)$, the expected core-collapse to type Ia ratio from the local star formation history and SN Ia delay-time distribution. The two hints are combined with a weight of 2 on the spectral hint, and final scores below 2.5 are labelled likely type Ia, above 3.5 likely core-collapse; the two undecided remnants provide the lower and upper limits on the ratio. The X-ray analysis is done by simultaneously fitting source and background spectra with the background explicitly modelled rather than subtracted, which is what allows faint extended remnants to be typed.

What would settle it

A deep X-ray survey of the SMC outskirts beyond about 1.5 degrees that finds several iron-rich type Ia remnants in old stellar fields would push the 14/3 count down toward the LMC ratio; the paper itself flags these outskirts as the main unknown.

Watch

Extended reading notes

Core claim

After removing six objects previously misclassified as SNRs and adding two newly confirmed remnants, the paper presents a final list of 21 confirmed and 2 candidate SNRs in the SMC. From a homogeneous X-ray spectral analysis of all 19 remnants with available data, it detects SN ejecta in 11 objects, finds no Fe K line even in the brightest and youngest remnant, and measures the hot ISM abundances of O, Ne, Mg, and Fe to lie between 0.1 and 0.2 solar. Combining spectral typing (ejecta abundance flags, pulsar/PWN detections) with a star-formation-based typing from the local massive-star count and reconstructed star formation history, it estimates $N_{\mathrm{CC}}/N_{\mathrm{Ia}} = 4.7$ (14/3), with range 2.8 (14/5) to 5.3 (16/3). This is about three times the LMC ratio of 1.35 from the same method, which the paper attributes to an enhanced star formation episode 0.5–1.5 Gyr ago in the LMC but not the SMC. It further reports that SMC remnants on average expand into a less dense and less disturbed medium, consistent with the galaxies' different morphologies.

Load-bearing premise

The headline number assumes that the typing rules for core-collapse versus type Ia remnants, calibrated on LMC remnants, transfer to the SMC, and that the survey has not missed type Ia remnants, especially in the poorly observed outer regions.

Editorial extensions

If this is right

  • If the ratio is correct, the SMC's supernova type mix is set by its recent star formation history: the absence of a 0.5–1.5 Gyr burst suppresses type Ia production even though the SMC has old stars.
  • Galactic SN Ia rates should not be inferred from stellar mass alone; the delay-time distribution plus recent star formation history matters, so galaxies with similar masses can differ in their core-collapse to type Ia ratio by a factor of about three.
  • The 0.1–0.2 solar hot-gas abundances of O, Ne, Mg, and Fe, combined with ratios to stellar abundances, imply that SNR shocks partially destroy dust and return depleted elements to the gas phase.
  • The lower ambient densities in the SMC explain why its remnants are larger, more circular, and fainter in X-rays at a given radio flux than LMC remnants, a trend that should hold for other low-density dwarf galaxies.
  • The cleaned sample means future population studies of SMC SNRs should use the 21 confirmed objects rather than older compilations that include the six rejected sources.

Reading between the lines

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

  • If the central ratio holds, similarly low-mass, low-metallicity dwarf galaxies may be even more dominated by core-collapse supernovae than their stellar populations suggest; integrated type Ia rates in such galaxies would provide a direct test.
  • The line-of-sight depth of the SMC means some core-collapse classifications based on projected massive-star counts could be wrong; using the X-ray absorption column as a depth proxy before typing could sharpen the ratio.
  • The absence of Fe K emission in the youngest and brightest remnant supports models in which most iron is still unshocked; repeated X-ray observations over decades could catch the reverse shock reaching the iron and test ejecta stratification.
  • The same two-hint typing method could be applied to SNR samples in other Local Group galaxies; if the SMC's low type Ia fraction is real, galaxies with intermediate-age star formation episodes should show higher type Ia fractions.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 6 minor

Summary. The paper presents a multiwavelength census of the Small Magellanic Cloud supernova remnant population. Combining XMM-Newton spectral analysis, radio continuum data, MCELS imaging, and new WiFeS optical spectroscopy, the authors assemble a clean sample of 21 confirmed SNRs and 2 candidates, rejecting six previously catalogued objects. The homogeneous X-ray analysis searches for ejecta, detects no Fe K lines, and measures ISM abundances in eight SNRs. The headline result is NCC/NIa = 4.7 (14/3), with limits 2.8–5.3, about three times the LMC value of 1.35 obtained with the same method; the authors interpret this as evidence that the SMC lacks the intermediate-age star formation episode of the LMC. The paper also compares radio properties, sizes, morphologies, and line-of-sight depths of SMC and LMC SNRs.

Significance. If correct, the measured CC/Ia ratio is an important constraint on the SMC star formation history and on delay-time distributions, and the catalog itself will be a reference. The paper's strengths are the careful, homogeneous X-ray spectral reduction with explicit background modelling, the systematic checks on plasma models and abundance tables, the multiwavelength confirmation of new remnants, and the direct comparison with the LMC using the same pipeline. The main caveats are the small number statistics (14 CC vs 3 Ia) and the sensitivity of the headline ratio to environment-based typing, which the authors partly acknowledge but do not quantify.

major comments (2)
  1. [Sect. 4.7, Table A.1] The headline NCC/NIa = 4.7 (14/3) counts MCSNR J0052−7236 and J0103−7247 as core-collapse solely on the basis of the 'hint-SF' environment metric (NOB = 130 and 117, r = 1.60 and 1.76), while their X-ray spectra are fitted with ISM-like abundances (hint-spec = 3). The text itself warns that the SMC's large line-of-sight depth means NOB and r 'might not reflect the correct environment' and that classifying high-NOB–r SNRs as CC 'should be done with caution.' The quoted range 2.8–5.3 only reassigns the two undecided SNRs and does not cover the uncertainty in these two classifications; reclassifying them as Ia or unclassified changes the ratio to about 4.0 or 2.4 and weakens the LMC contrast. Please add an explicit robustness test that recomputes NCC/NIa under alternative assignments for all SNRs with hint-spec = 3 or with environment-only typing, and report the resulting range.
  2. [Sect. 4.7, Tables 4 and 5] The typing thresholds (NOB bin boundaries 80 and 115; r boundaries 0.6 and 1.5; final combined-hint cutoffs 2.5 and 3.5) are introduced as fixed, hand-set values transferred from the LMC analysis. The SMC SFH is acknowledged to be noisier, and the discriminatory power in the SMC is weaker (the average NOB of secure CC SNRs, 160±63, overlaps substantially with that of likely Ia, 92±22). Because the final counts are only 14 CC versus 3 Ia, small shifts in these thresholds could move one or two objects across the 'undecided' boundaries and materially change the headline ratio. Please provide a sensitivity analysis of the ratio to, e.g., ±20% variations in the thresholds, or otherwise quantify the robustness of the 4.7 value to the choice of cutoffs.
minor comments (6)
  1. [Sect. 3.2] The object name 'MCSNR J0040−7336' appears to be a typo for 'MCSNR J0041−7336' in the discussion of the diffuse emission background.
  2. [Sect. 4.6] The name 'MCSNR J0052−7237' is used in the first paragraph and in Table 1; the correct identifier is 'MCSNR J0052−7236'.
  3. [Sect. 4.7] In the third paragraph, 'dagnostic' should be 'diagnostic'.
  4. [Fig. B.1 caption] The caption refers to 'MCSNR J048−7319'; this should be 'MCSNR J0048−7319'.
  5. [Abstract and Sect. 5] The initial count of '19 confirmed and 4 candidate SNRs' versus the final '21 confirmed SNRs and 2 candidates' is explained in the text, but a brief sentence in the abstract would avoid apparent inconsistency for the casual reader.
  6. [Table A.3] The column header 'NH LMC' may confuse readers; it appears to denote the fitted SMC absorption column density in units of 10^21 cm^-2, not a quantity specific to the LMC.

Circularity Check

1 steps flagged · score 2.0 of 10

No material circularity: the SMC CC/Ia ratio and SNR classifications are a new application of a published method to independent multiwavelength data; the authors' self-citation of MHK16 is minor and not load-bearing.

  1. other [Sect. 4.7 (Tables 4 and 5); method adopted from MHK16]
    "We covered the various methods of SNR typing in MHK16. We mostly use our X-ray spectral results ... or the detection of an associated (NS) or PWN. We then add secondary evidence based on the local stellar environment of SMC SNRs to tentatively type the rest of the sample, a method we explain in detail in MHK16."

    The typing rubric and the LMC comparison ratio (1.35, 'measured by a similar method') are imported from the authors' own MHK16, so the SMC-versus-LMC contrast is not fully independent of the same group's earlier calibration. This is only a minor self-citation, however: the SMC spectral fits, NOB counts, and SFH-based r values are computed anew for this sample, the three Ia and the majority of CC classifications rest on X-ray ejecta or compact-object associations rather than on the MHK16 calibration, and no fitted parameter from this paper is recycled into the headline ratio.

full rationale

The derivation chain for the headline NCC/NIa = 4.7 (14/3) is a count of individually typed SNRs, not a fitted quantity. The spectral typing uses X-ray ejecta abundance flags and Fe K non-detections; the environment metric combines an external photometric catalogue (Zaritsky et al. 2002), an external SFH (Harris & Zaritsky 2004), and literature delay-time distributions (Maoz & Badenes 2010). Two SNRs (J0052-7236 and J0103-7247) are classed as CC through the NOB-r hint alone, and the paper explicitly cautions that 'classifying the high NOB–r SNRs as CC should be done with caution' because of SMC line-of-sight depth; this is a robustness/sensitivity concern about those two classifications, not a circular reuse of the measured ratio. The secure subsample (ejecta, PWN, BeXRB, Fe-rich Ia) already gives 12 CC and 3 Ia, so the central claim retains independent content. The main self-reference is the adoption of MHK16's method and the LMC benchmark value of 1.35, which is normal methodological continuity rather than load-bearing circularity.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central CC/Ia ratio is a counting experiment over typed SNRs. The counts inherit uncertainties from the spectral fitting (abundances, temperatures) and from the typing scheme: the hint-spec and hint-SF grids in Tables 4-5 use hand-set thresholds, and the spectral models are standard but rely on atomic data. The most consequential assumptions are that the projected stellar environment traces the true progenitor type despite line-of-sight depth, and that the detected sample is not type-biased in incompleteness.

free parameters (3)
  • NOB bin boundaries in Table 5 = 80 and 115
    Hand-chosen thresholds for the number of blue stars used to assign the 'hint-SF' type; no optimization or sensitivity analysis is given, and the final count (14 CC vs 3 Ia) depends on them.
  • r bin boundaries in Table 5 = 0.6 and 1.5
    Hand-chosen thresholds for the SFH-derived CC/Ia ratio used in the typing grid; no sensitivity analysis is provided.
  • hint-spec vs hint-SF weighting = 2:1
    The final hint is a weighted mean with a coefficient of two for hint-spec (Sect. 4.7); this arbitrary weight affects the classification of borderline objects such as J0048-7319 and J0100-7133.
assumptions (5)
  • domain assumption The X-ray spectra of SNRs are adequately described by collisional ionization equilibrium or non-equilibrium thermal plasma models (vpshock, vnei, vsedov) with abundances tied to a chosen solar abundance table.
    Invoked throughout Sect. 3.2 and 4.3; the derived abundances and the ejecta flags, which feed the CC/Ia typing, depend on these models.
  • domain assumption The SMC distance is 60 kpc for all sources, with no line-of-sight depth applied to individual objects.
    Stated in Sect. 4.1; used to convert sizes, luminosities, and densities. The paper notes the SMC depth is 3-7.5 kpc, so this is an approximation.
  • domain assumption The delay-time distribution parameters for type Ia supernovae from Maoz & Badenes (2010) apply to the SMC and are used in Eq. 3 to compute r.
    Used in Sect. 4.7 to estimate the expected CC/Ia ratio r from the local star formation history.
  • ad hoc to paper The typing hints in Tables 4 and 5, calibrated on the LMC and projected stellar counts, track the true progenitor type of each SMC SNR.
    This is the load-bearing classification assumption; the authors themselves note in Sect. 4.7 that the SMC's line-of-sight depth weakens the star-formation-based hint.
  • ad hoc to paper The detected and typed SMC SNR sample is representative of the true population, with no strong type-dependent incompleteness.
    The headline ratio counts typed SNRs; the authors concede in Sect. 4.7 that the poorly known outskirts might host more type Ia SNRs, which would change the ratio.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The supernova remnant population of the Small Magellanic Cloud." pith.science (2026). https://pith.science/paper/JGVJYHWH

@misc{pith2026190811234,
  author       = {Pith},
  title        = {Pith review of: The supernova remnant population of the Small Magellanic Cloud},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JGVJYHWH}},
  note         = {Machine review of arXiv:1908.11234}
}
abstract

Aims: We present a comprehensive study of the supernova remnant (SNR) population of the Small Magellanic Cloud (SMC). We measure multiwavelength properties of the SMC SNRs and compare them to those of the Large Magellanic Cloud (LMC) population. Methods: This study combines the large dataset of XMM-Newton observations of the SMC, archival and recent radio continuum observations, an optical line emission survey, and new optical spectroscopic observations. We can thus build a complete and clean sample of 19 confirmed and 4 candidate SNRs. The homogeneous X-ray spectral analysis allows to search for SN ejecta and Fe K line emission, and to measure interstellar medium (ISM) abundances. We estimate the ratio of core-collapse to type Ia supernova rates of the SMC based on the X-ray properties and the local stellar environment of each SNR. Results : After the removal of unconfirmed or misclassified objects, and the addition of two newly confirmed SNRs based on multi-wavelength features, we present a final list of 21 confirmed SNRs and 2 candidates. While no Fe K line is detected even for the brightest and youngest SNR, we find X-ray evidence of SN ejecta in 11 SNRs. We estimate a ratio of 4.7$_{-1.9} ^{+0.6}$ core-collapse supernova to every type Ia SN, three times higher than in the LMC. The difference can be ascribed to the absence of the enhanced star formation episode in the SMC, which occurred in the LMC 0.5-1.5 Gyr ago. The hot-gas abundances of O, Ne, Mg, and Fe are 0.1-0.2 times solar. Their ratios with respect to SMC stellar abundances reflect the effects of dust depletion and partial dust destruction in SNR shocks. We find evidence that the ambient medium probed by SMC SNRs is less disturbed and less dense on average than in the LMC, consistent with the different morphologies of the two galaxies.

Figures

Figures reproduced from arXiv: 1908.11234 by the authors.

Figure 1
Figure 1. Left : MCSNR candidate J0056−7209 on a composite MCELS image (R, G, B = [S ii], Hα, and [O iii], respectively). On the east and west side of the ellipse, fragmented filaments typical of older supernova remnants are clearly seen. The white bar shows the position of the WiFeS spectrograph slit. The spectrograph slit is actually a combination of 25 × 1 00 wide adjacent slits each, repeated 36 times to yield an effectiv… view at source ↗
Figure 2
Figure 2. P×V 1/2 of SNRs in SMC (orange triangles, this work) and LMC (grey plus signs, MHK16) as a function of their size. Lines of constant SN energy (times filling factor f , see text in Sect. 4.3.1) are overplotted in units of 1051 erg ≡1 foe. P × √ V ≡ f −1 √ EM × kT as a function of average diameter in pc. For multiple-component spectra, we used the sum of all EM, and the EM-averaged temperature. Lines of constant ener… view at source ↗
Figure 3
Figure 3. Red part of optical spectra of SNR candidates J0056–7209 (left) and J0109–7318 (right) as seen by the WiFeS spectrograph. All main lines characteristics of old SNRs are seen: [N ii]λλ6548, 6583Å, Hα and [S ii]λλ6717, 6731Å [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Comparison of the effect of type of spectral models (left) and input abundance tables (right) on abundance derived with X-ray spectra of SNRs. Left : O, Ne, Mg, and Fe abundances (by group of three, from left to right, respectively) relative to the reference value of W…
Figure 5
Figure 5. Figure 5: Distribution of parameters of 19 confirmed SMC SNRs using kernel smoothing. The colour of symbols indicate progenitor type for a particular SNR. Data points that fall in the same bin on the x-axis are plotted within a vertical column with equidistant spacing. The upper…
Figure 6
Figure 6. Figure 6: Histogram of ambient density around LMC and SMC SNRs, estimated from the X-ray spectrum as n ∝ √ EM/V (see Sect. 4.3.1). SNRs of the LMC population are slightly smaller (median of 33 pc vs. 43 pc in the SMC7 ). The observed difference might be due to the lower complete…
Figure 7
Figure 7. Figure 7: The broad-band X-ray flux vs. 1 GHz flux density for the sample of SMC and LMC SNRs with available data for age and explosion type (Table A.1, B17). The position of the colour-coded symbols along the axis with no measured radio flux is offset by -0.2 dex from the faint…
Figure 8
Figure 8. Figure 8: Left : Comparison of the distribution of NH fraction for LMC and SMC SNRs. Right : Spatial distribution of SMC SNRs, with NH fraction used as a proxy for the line-of-sight depth within the neutral gas. total H i column density through a galaxy, e.g. for the SMC. Theref…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

159 extracted references · 64 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    Alsaberi , R. Z. E., Maitra , C., Filipovi \'c , M. D., et al. 2019, , 486, 2507

    2019

  4. [4]

    Alsabti , A. W. & Murdin , P. 2017, Handbook of Supernovae

    2017

  5. [5]

    & Grevesse , N

    Anders , E. & Grevesse , N. 1989, , 53, 197

    1989

  6. [6]

    Arnaud , K. A. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes , 17

    1996

  7. [7]

    J., & Scott , P

    Asplund , M., Grevesse , N., Sauval , A. J., & Scott , P. 2009, , 47, 481

    2009

  8. [8]

    A., Badenes , C., et al

    Auchettl , K., Lopez , L. A., Badenes , C., et al. 2019, , 871, 64

    2019

Show all 159 references
  1. [9]

    Badenes , C., Maoz , D., & Draine , B. T. 2010, , 407, 1301

    2010

  2. [10]

    & McCammon , D

    Balucinska-Church , M. & McCammon , D. 1992, , 400, 699

    1992

  3. [11]

    Baumgardt , H., Parmentier , G., Anders , P., & Grebel , E. K. 2013, , 430, 676

    2013

  4. [12]

    J., Rossa , J., Weis , K., & Dennerl , K

    Bomans , D. J., Rossa , J., Weis , K., & Dennerl , K. 2003, in IAU Symposium, Vol. 212, A Massive Star Odyssey: From Main Sequence to Supernova, ed. K. van der Hucht , A. Herrero , & C. Esteban , 637

    2003

  5. [13]

    J., Hendrick , S

    Borkowski , K. J., Hendrick , S. P., & Reynolds , S. P. 2006 a , , 652, 1259

    2006

  6. [14]

    J., Williams , B

    Borkowski , K. J., Williams , B. J., Reynolds , S. P., et al. 2006 b , , 642, L141

    2006

  7. [15]

    2013, , 555, A1

    Bouret , J.-C., Lanz , T., Martins , F., et al. 2013, , 555, A1

    2013

  8. [16]

    M., Filipovi \'c , M

    Bozzetto , L. M., Filipovi \'c , M. D., Vukoti \'c , B., et al. 2017, , 230, 2

    2017

  9. [17]

    M., Kavanagh , P

    Bozzetto , L. M., Kavanagh , P. J., Maggi , P., et al. 2014, , 439, 1110

    2014

  10. [18]

    E., Reyes Navarro , F

    Carlos Reyes , R. E., Reyes Navarro , F. A., Mel \'e ndez , J., Steiner , J., & Elizalde , F. 2015, , 51, 135

    2015

  11. [19]

    & Limongi , M

    Chieffi , A. & Limongi , M. 2017, , 836, 79

    2017

  12. [20]

    & Wilcots , E

    Chomiuk , L. & Wilcots , E. M. 2009, , 703, 370

    2009

  13. [21]

    A., Tosi , M., et al

    Cignoni , M., Cole , A. A., Tosi , M., et al. 2012, , 754, 130

    2012

  14. [22]

    Cox , D. P. & Daltabuit , E. 1971, , 167, 113

    1971

  15. [23]

    J., Filipovic , M

    Crawford , E. J., Filipovic , M. D., de Horta , A. Y., et al. 2011, Serbian Astronomical Journal, 183, 95

    2011

  16. [24]

    J., Filipovi \'c , M

    Crawford , E. J., Filipovi \'c , M. D., McEntaffer , R. L., et al. 2014, , 148, 99

    2014

  17. [25]

    & Molendi , S

    De Luca , A. & Molendi , S. 2004, , 419, 837

    2004

  18. [26]

    Dickey , J. M. & Lockman , F. J. 1990, , 28, 215

    1990

  19. [27]

    2007, , 310, 255

    Dopita , M., Hart , J., McGregor , P., et al. 2007, , 310, 255

    2007

  20. [28]

    Dopita , M. A. 1979, Australian Journal of Physics, 32, 123

    1979

  21. [29]

    A., Seitenzahl , I

    Dopita , M. A., Seitenzahl , I. R., Sutherland , R. S., et al. 2019, , 157, 50

    2019

  22. [30]

    A., Seitenzahl , I

    Dopita , M. A., Seitenzahl , I. R., Sutherland , R. S., et al. 2016, , 826, 150

    2016

  23. [31]

    A., Vogt , F

    Dopita , M. A., Vogt , F. P. A., Sutherland , R. S., et al. 2018, , 237, 10

    2018

  24. [32]

    Duin, R. P. W. 1976, IEEE Transactions on Computers, 1175

    1976

  25. [33]

    & Tibshirani, R

    Efron, B. & Tibshirani, R. J. 1994, An introduction to the bootstrap (CRC press)

    1994

  26. [34]

    D., Bohlsen , T., Reid , W., et al

    Filipovi \'c , M. D., Bohlsen , T., Reid , W., et al. 2002, , 335, 1085

    2002

  27. [35]

    D., Haberl , F., Winkler , P

    Filipovi \'c , M. D., Haberl , F., Winkler , P. F., et al. 2008, , 485, 63

    2008

  28. [36]

    D., Haynes , R

    Filipovic , M. D., Haynes , R. F., White , G. L., & Jones , P. A. 1998, , 130, 421

    1998

  29. [37]

    D., Jones , P

    Filipovic , M. D., Jones , P. A., White , G. L., et al. 1997, , 121, 321

    1997

  30. [38]

    D., Payne , J

    Filipovi \'c , M. D., Payne , J. L., Reid , W., et al. 2005, , 364, 217

    2005

  31. [39]

    L., Morse , J

    Finkelstein , S. L., Morse , J. A., Green , J. C., et al. 2006, , 641, 919

    2006

  32. [40]

    2018, , 480, 2743

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

    2018

  33. [41]

    Galvin , T. J. & Filipovic , M. D. 2014, Serbian Astronomical Journal, 189, 15

    2014

  34. [42]

    J., Filipovi \'c , M

    Galvin , T. J., Filipovi \'c , M. D., Tothill , N. F. H., et al. 2014, , 353, 603

    2014

  35. [43]

    F., Plucinsky , P

    Garofali , K., Williams , B. F., Plucinsky , P. P., et al. 2017, , 472, 308

    2017

  36. [44]

    C., & Hartigan , P

    Ghavamian , P., Raymond , J., Smith , R. C., & Hartigan , P. 2001, , 547, 995

    2001

  37. [45]

    B., et al

    Graczyk , D., Pietrzy \'n ski , G., Thompson , I. B., et al. 2014, , 780, 59

    2014

  38. [46]

    Green , D. A. 2019, arXiv e-prints, arXiv:1907.02638

    2019 arXiv

  39. [47]

    V., Kniazev , A

    Gvaramadze , V. V., Kniazev , A. Y., & Oskinova , L. M. 2019, , 485, L6

    2019

  40. [48]

    D., Bozzetto , L

    Haberl , F., Filipovi \'c , M. D., Bozzetto , L. M., et al. 2012 a , , 543, A154

    2012

  41. [49]

    D., Pietsch , W., & Kahabka , P

    Haberl , F., Filipovi \'c , M. D., Pietsch , W., & Kahabka , P. 2000, , 142, 41

    2000

  42. [50]

    & Pietsch , W

    Haberl , F. & Pietsch , W. 2004, , 414, 667

    2004

  43. [51]

    2012 b , , 545, A128

    Haberl , F., Sturm , R., Ballet , J., et al. 2012 b , , 545, A128

    2012

  44. [52]

    D., Pietsch , W., & Crawford , E

    Haberl , F., Sturm , R., Filipovi \'c , M. D., Pietsch , W., & Crawford , E. J. 2012 c , , 537, L1

    2012

  45. [53]

    & Zaritsky , D

    Harris , J. & Zaritsky , D. 2004, , 127, 1531

    2004

  46. [54]

    & Zaritsky , D

    Harris , J. & Zaritsky , D. 2009, , 138, 1243

    2009

  47. [55]

    K., & Duffau , S

    Haschke , R., Grebel , E. K., & Duffau , S. 2012, , 144, 107

    2012

  48. [56]

    R., Lanz , T., & Hubeny , I

    Heap , S. R., Lanz , T., & Hubeny , I. 2006, , 638, 409

    2006

  49. [57]

    M., Guerrero , M

    H \'e nault-Brunet , V., Oskinova , L. M., Guerrero , M. A., et al. 2012, , 420, L13

    2012

  50. [58]

    P., Reynolds , S

    Hendrick , S. P., Reynolds , S. P., & Borkowski , K. J. 2005, , 622, L117

    2005

  51. [59]

    W., Howarth , I

    Hilditch , R. W., Howarth , I. D., & Harries , T. J. 2005, , 357, 304

    2005

  52. [60]

    P., Hayashi , I., & Koyama , K

    Hughes , J. P., Hayashi , I., & Koyama , K. 1998, , 505, 732

    1998

  53. [61]

    Hughes , J. P. & Smith , R. C. 1994, , 107, 1363

    1994

  54. [62]

    2009, , 496, 841

    Hunter , I., Brott , I., Langer , N., et al. 2009, , 496, 841

    2009

  55. [63]

    1983, in IAU Symposium, Vol

    Inoue , H., Koyama , K., & Tanaka , Y. 1983, in IAU Symposium, Vol. 101, Supernova Remnants and their X-ray Emission, ed. J. Danziger & P. Gorenstein , 535--540

    1983

  56. [64]

    L., Campana , S., Covino , S., et al

    Israel , G. L., Campana , S., Covino , S., et al. 2000, , 531, L131

    2000

  57. [65]

    2011, , 415, 1366

    Kapakos , E., Hatzidimitriou , D., & Soszy \'n ski , I. 2011, , 415, 1366

    2011

  58. [66]

    J., Sasaki , M., Bozzetto , L

    Kavanagh , P. J., Sasaki , M., Bozzetto , L. M., et al. 2016, , 586, A4

    2016

  59. [67]

    A., Staveley-Smith , L., & Bessell , M

    Kim , S., Dopita , M. A., Staveley-Smith , L., & Bessell , M. S. 1999, , 118, 2797

    1999

  60. [68]

    Y., & Kim , H.-J

    Koo , B.-C., Lee , J.-J., Jeong , I.-G., Seok , J. Y., & Kim , H.-J. 2016, , 821, 20

    2016

  61. [69]

    V., et al

    Koyama , K., Petre , R., Gotthelf , E. V., et al. 1995, , 378, 255

    1995

  62. [70]

    Kuntz , K. D. & Snowden , S. L. 2008, , 478, 575

    2008

  63. [71]

    M., Dufour , R

    Kurt , C. M., Dufour , R. J., Garnett , D. R., et al. 1999, , 518, 246

    1999

  64. [72]

    P., Slane , P

    Lee , J.-J., Park , S., Hughes , J. P., Slane , P. O., & Burrows , D. N. 2011, , 731, L8

    2011

  65. [73]

    & Schaerer , D

    Lejeune , T. & Schaerer , D. 2001, , 366, 538

    2001

  66. [74]

    2010, , 725, 842

    Leonidaki , I., Zezas , A., & Boumis , P. 2010, , 725, 842

    2010

  67. [75]

    2007, The Astrophysical Journal, 658, 1027

    Leroy , A., Bolatto , A., Stanimirovic , S., et al. 2007, The Astrophysical Journal, 658, 1027

    2007

  68. [76]

    & Nomoto , K

    Leung , S.-C. & Nomoto , K. 2018, , 861, 143

    2018

  69. [77]

    2003, , 591, 1220

    Lodders , K. 2003, , 591, 1220

    2003

  70. [78]

    S., Blair , W

    Long , K. S., Blair , W. P., Winkler , P. F., et al. 2010, , 187, 495

    2010

  71. [79]

    S., Kuntz , K

    Long , K. S., Kuntz , K. D., Blair , W. P., et al. 2014, , 212, 21

    2014

  72. [80]

    Lopez , L. A. 2014, in IAU Symposium, Vol. 296, Supernova Environmental Impacts, ed. A. Ray & R. A. McCray , 239--244

    2014

  73. [81]

    A., Castro , D., Slane , P

    Lopez , L. A., Castro , D., Slane , P. O., Ramirez-Ruiz , E., & Badenes , C. 2014, , 788, 5

    2014

  74. [82]

    & Klessen , R

    Mac Low , M.-M. & Klessen , R. S. 2004, Reviews of Modern Physics, 76, 125

    2004

  75. [83]

    & Acero , F

    Maggi , P. & Acero , F. 2017, , 597, A65

    2017

  76. [84]

    J., et al

    Maggi , P., Haberl , F., Kavanagh , P. J., et al. 2014, , 561, A76

    2014

  77. [85]

    J., et al

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

    2016

  78. [86]

    D., et al

    Maitra , C., Ballet , J., Filipovi \'c , M. D., et al. 2015, , 584, A41

    2015

  79. [87]

    & Badenes , C

    Maoz , D. & Badenes , C. 2010, , 407, 1314

    2010

  80. [88]

    & Mannucci , F

    Maoz , D. & Mannucci , F. 2012, , 29, 447

    2012

  81. [89]

    & Kroupa , P

    Maschberger , T. & Kroupa , P. 2011, , 411, 1495

    2011

  82. [90]

    S., Ford , V

    Mathewson , D. S., Ford , V. L., Dopita , M. A., et al. 1984, , 55, 189

    1984

  83. [91]

    2012, ArXiv e-prints [ [arXiv] 1209.3114 ]

    Merloni , A., Predehl , P., Becker , W., et al. 2012, ArXiv e-prints [ [arXiv] 1209.3114 ]

    2012 arXiv

  84. [92]

    2014, , 438, 1067

    Meschin , I., Gallart , C., Aparicio , A., et al. 2014, , 438, 1067

    2014

  85. [93]

    C., White , G

    Millar , W. C., White , G. L., & Filipovic , M. D. 2012, Serbian Astronomical Journal, 184, 19

    2012

  86. [94]

    C., White , G

    Millar , W. C., White , G. L., Filipovi \'c , M. D., et al. 2011, , 332, 221

    2011

  87. [95]

    2006, , 448, 1247

    Misanovic , Z., Pietsch , W., Haberl , F., et al. 2006, , 448, 1247

    2006

  88. [96]

    2001, Publications of the Astronomical Society of Japan, 53, L45

    Mizuno , N., Rubio , M., Mizuno , A., et al. 2001, Publications of the Astronomical Society of Japan, 53, L45

    2001

  89. [97]

    2010, , 712, 1248

    Muller , E., Ott , J., Hughes , A., et al. 2010, , 712, 1248

    2010

  90. [98]

    No \"e l , N. E. D., Aparicio , A., Gallart , C., et al. 2009, , 705, 1260

    2009

  91. [99]

    2013, , 51, 457

    Nomoto , K., Kobayashi , C., & Tominaga , N. 2013, , 51, 457

    2013

  92. [100]

    2010, , 520, A74

    North , P., Gauderon , R., Barblan , F., & Royer , F. 2010, , 520, A74

    2010

  93. [101]

    N., Filipovi \'c , M

    O'Brien , A. N., Filipovi \'c , M. D., Crawford , E. J., et al. 2013, , 347, 159

    2013

  94. [102]

    A., Filipovi \'c , M

    Owen , R. A., Filipovi \'c , M. D., Ballet , J., et al. 2011, , 530, A132

    2011

  95. [103]

    G., Schlegel , E

    Pannuti , T. G., Schlegel , E. M., Filipovi \'c , M. D., et al. 2011, , 142, 20

    2011

  96. [104]

    G., Swartz , D

    Pannuti , T. G., Swartz , D. A., Laine , S., et al. 2015, , 150, 91

    2015

  97. [105]

    P., Burrows , D

    Park , S., Hughes , J. P., Burrows , D. N., et al. 2003, , 598, L95

    2003

  98. [106]

    L., Filipovi \'c , M

    Payne , J. L., Filipovi \'c , M. D., Pannuti , T. G., et al. 2004 a , , 425, 443

    2004

  99. [107]

    L., Filipovi \'c , M

    Payne , J. L., Filipovi \'c , M. D., Reid , W., et al. 2004 b , , 355, 44

    2004

  100. [108]

    L., White , G

    Payne , J. L., White , G. L., Filipovi \'c , M. D., & Pannuti , T. G. 2007, , 376, 1793

    2007

  101. [109]

    A., Peimbert , A., Peimbert , M., & Ruiz , M

    Pe \ n a-Guerrero , M. A., Peimbert , A., Peimbert , M., & Ruiz , M. T. 2012, , 746, 115

    2012

  102. [110]

    Peimbert , M., Peimbert , A., & Ruiz , M. T. 2000, , 541, 688

    2000

  103. [111]

    W., Oey , M

    Pellegrini , E. W., Oey , M. S., Winkler , P. F., et al. 2012, , 755, 40

    2012

  104. [112]

    2019, , 567, 200

    Pietrzy \'n ski , G., Graczyk , D., Gallenne , A., et al. 2019, , 567, 200

    2019

  105. [113]

    2005, , 434, 483

    Pietsch , W., Freyberg , M., & Haberl , F. 2005, , 434, 483

    2005

  106. [114]

    2004, , 426, 11

    Pietsch , W., Misanovic , Z., Haberl , F., et al. 2004, , 426, 11

    2004

  107. [115]

    P., Beardmore , A

    Plucinsky , P. P., Beardmore , A. P., Foster , A., et al. 2017, , 597, A35

    2017

  108. [116]

    A., Payne , J

    Reid , W. A., Payne , J. L., Filipovi \'c , M. D., et al. 2006, , 367, 1379

    2006

  109. [117]

    2002, , 564, 704

    Rela \ n o , M., Peimbert , M., & Beckman , J. 2002, , 564, 704

    2002

  110. [118]

    L., DeRoo , C., et al

    Roper , Q., McEntaffer , R. L., DeRoo , C., et al. 2015, , 803, 106

    2015

  111. [119]

    2015, , 449, 639

    Rubele , S., Girardi , L., Kerber , L., et al. 2015, , 449, 639

    2015

  112. [120]

    2012, , 537, A106

    Rubele , S., Kerber , L., Girardi , L., et al. 2012, , 537, A106

    2012

  113. [121]

    Russell , S. C. & Dopita , M. A. 1990, , 74, 93

    1990

  114. [122]

    Russell , S. C. & Dopita , M. A. 1992, , 384, 508

    1992

  115. [123]

    2019, The Astrophysical Journal, 881, 85

    Sano , H., Matsumura , H., Yamane , Y., et al. 2019, The Astrophysical Journal, 881, 85

    2019

  116. [124]

    2012, , 544, A144

    Sasaki , M., Pietsch , W., Haberl , F., et al. 2012, , 544, A144

    2012

  117. [125]

    N., et al

    Schenck , A., Park , S., Burrows , D. N., et al. 2014, , 791, 50

    2014

  118. [126]

    2016, , 151, 161

    Schenck , A., Park , S., & Post , S. 2016, , 151, 161

    2016

  119. [127]

    L., Madore , B

    Scowcroft , V., Freedman , W. L., Madore , B. F., et al. 2016, , 816, 49

    2016

  120. [128]

    1986, Density estimation for statistics and data analysis

    Silverman, B. 1986, Density estimation for statistics and data analysis

    1986

  121. [129]

    D., Dwek , E., & Jones , A

    Slavin , J. D., Dwek , E., & Jones , A. P. 2015, , 803, 7

    2015

  122. [130]

    M., Sault , R

    Stanimirovic , S., Staveley-Smith , L., Dickey , J. M., Sault , R. J., & Snowden , S. L. 1999, , 302, 417

    1999

  123. [131]

    Stanimirovi \'c , S., Staveley-Smith , L., & Jones , P. A. 2004, , 604, 176

    2004

  124. [132]

    2011, , 534, A55

    Stiele , H., Pietsch , W., Haberl , F., et al. 2011, , 534, A55

    2011

  125. [133]

    A., & Filipovi \'c , M

    Stupar , M., Parker , Q. A., & Filipovi \'c , M. D. 2008, , 390, 1037

    2008

  126. [134]

    D., et al

    Sturm , R., Dra s kovi \'c , D., Filipovi \'c , M. D., et al. 2013 a , , 558, A101

    2013

  127. [135]

    M., et al

    Sturm , R., Haberl , F., Oskinova , L. M., et al. 2013 b , , 556, A139

    2013

  128. [136]

    at f\"ur Physik, Technische Universit\

    Sturm , R. K. N. 2012, PhD thesis, Fakult\"at f\"ur Physik, Technische Universit\"at M\"unchen, Germany

    2012

  129. [137]

    & Subramaniam , A

    Subramanian , S. & Subramaniam , A. 2009, , 496, 399

    2009

  130. [138]

    & Subramaniam , A

    Subramanian , S. & Subramaniam , A. 2012, , 744, 128

    2012

  131. [139]

    2010, , 62, 1239

    Takeda , Y., Kambe , E., Sadakane , K., & Masada , S. 2010, , 62, 1239

    2010

  132. [140]

    2016, , 68, S9

    Takeuchi , Y., Yamaguchi , H., & Tamagawa , T. 2016, , 68, S9

    2016

  133. [141]

    2001, , 372, 667

    Testor , G. 2001, , 372, 667

    2001

  134. [142]

    K., Eichler , M., Panov , I

    Thielemann , F. K., Eichler , M., Panov , I. V., & Wehmeyer , B. 2017, Annual Review of Nuclear and Particle Science, 67, 253

    2017

  135. [143]

    J., Bleeker , J

    van der Heyden , K. J., Bleeker , J. A. M., & Kaastra , J. S. 2004, , 421, 1031

    2004

  136. [144]

    2012, , 20, 49

    Vink , J. 2012, , 20, 49

    2012

  137. [145]

    R., Dolphin , A

    Weisz , D. R., Dolphin , A. E., Skillman , E. D., et al. 2013, , 431, 364

    2013

  138. [146]

    J., Borkowski , K

    Williams , B. J., Borkowski , K. J., Reynolds , S. P., et al. 2006, , 652, L33

    2006

  139. [147]

    2000, , 542, 914

    Wilms , J., Allen , A., & McCray , R. 2000, , 542, 914

    2000

  140. [148]

    F., Crawford , E

    Wong , G. F., Crawford , E. J., Filipovic , M. D., et al. 2012 a , Serbian Astronomical Journal, 184, 93

    2012

  141. [149]

    F., Filipovic , M

    Wong , G. F., Filipovic , M. D., Crawford , E. J., et al. 2011 a , Serbian Astronomical Journal, 182, 43

    2011

  142. [150]

    F., Filipovic , M

    Wong , G. F., Filipovic , M. D., Crawford , E. J., et al. 2011 b , Serbian Astronomical Journal, 183, 103

    2011

  143. [151]

    F., Filipovic , M

    Wong , G. F., Filipovic , M. D., Crawford , E. J., et al. 2012 b , Serbian Astronomical Journal, 185, 53

    2012

  144. [152]

    T., & M \"u ller , E

    Wongwathanarat , A., Janka , H. T., & M \"u ller , E. 2013, , 552, A126

    2013

  145. [153]

    J., Plucinsky , P

    Xi , L., Gaetz , T. J., Plucinsky , P. P., Hughes , J. P., & Patnaude , D. J. 2019, , 874, 14

    2019

  146. [154]

    2014, , 785, L27

    Yamaguchi , H., Badenes , C., Petre , R., et al. 2014, , 785, L27

    2014

  147. [155]

    2010, , 715, 412

    Yamaguchi , H., Sawada , M., & Bamba , A. 2010, , 715, 412

    2010

  148. [156]

    J., & Kennicutt , Jr., R

    Ye , T., Turtle , A. J., & Kennicutt , Jr., R. C. 1991, , 249, 722

    1991

  149. [157]

    S., Amy , S

    Ye , T. S., Amy , S. W., Wang , Q. D., Ball , L., & Dickel , J. 1995, , 275, 1218

    1995

  150. [158]

    D., Roper , Q., et al

    Yew , M., Filipovi \'c , M. D., Roper , Q., et al. 2018, , 35, e015

    2018

  151. [159]

    B., Grebel , E

    Zaritsky , D., Harris , J., Thompson , I. B., Grebel , E. K., & Massey , P. 2002, , 123, 855

    2002

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.