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REVIEW 4 major objections 8 minor 182 references

LMC novae sit on heavier white dwarfs than M31 novae, which is why the Cloud shows a much higher share of recurrent eruptions.

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 →

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2026-07-30 10:35 UTC pith:E5G3XLMV

load-bearing objection Solid LMC compilation and first Yaron inversion for the Cloud; the RN P_rec mismatch is real but does not sink the M_WD comparison. the 4 major comments →

arxiv 2607.23849 v1 pith:E5G3XLMV submitted 2026-07-26 astro-ph.SR astro-ph.GA

A Century of Novae in the Large Magellanic Cloud

Allen W. Shafter This is my paper
classification astro-ph.SR astro-ph.GA
keywords Large Magellanic Cloudcataclysmic variable starsnovaerecurrent novaetime domain astronomywhite dwarf massMMRD relation
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 gathers a century of Large Magellanic Cloud nova candidates and isolates 39 systems with usable peak brightness and decline times. Those light curves confirm that LMC novae are, on average, a bit brighter and faster than novae in M31 or the Milky Way. For the first time the author inverts standard thermonuclear-runaway models against those light curves to estimate white-dwarf mass, accretion rate, ejecta speed, and recurrence time for each system. The models return systematically higher white-dwarf masses and faster ejecta than the same method gives for M31, and that mass difference accounts for the Cloud’s much larger fraction of recurrent-nova eruptions (~21% versus ~6%). A sympathetic reader cares because the result ties a simple observable (how bright and how fast a nova fades) to the underlying binary population and to the star-formation history of the host galaxy.

Core claim

When the Yaron et al. (2005) nova grids are inverted on the calibrated peak luminosities and t2 decline times of 39 LMC progenitors, the resulting white-dwarf masses average higher than those of M31 novae (observed mean ~1.23 solar masses, recurrence-time-debiased mean ~1.13 solar masses). Higher masses produce higher predicted ejecta velocities and a recurrent-nova eruption fraction of roughly 20.6% in the LMC versus 6.4% in M31.

What carries the argument

Inversion of the interpolated Yaron et al. (2005) model grid: observed bolometric peak luminosity L4 and mass-loss timescale t_ml (taken as t2) are mapped onto white-dwarf mass and accretion rate, which then predict maximum ejecta velocity and recurrence time.

Load-bearing premise

The method treats the observed two-magnitude fade time as the physical mass-loss timescale and assumes a coarse, interpolated cool-white-dwarf model grid correctly converts that pair of light-curve numbers into white-dwarf mass and accretion rate for every system.

What would settle it

A homogeneous spectroscopic campaign that measures true ejecta velocities and recurrence intervals for the same LMC sample, then checks whether the systems the models assign M_WD greater than or equal to about 1.3 solar masses are the ones that actually recur on decade timescales and show the broadest lines.

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

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If this is right

  • LMC nova populations should continue to show a higher He/N and hybrid fraction than M31 or the Galaxy because high-mass white dwarfs evolve faster and drive broader lines.
  • The luminosity-specific nova rate of the LMC should remain higher than that of M31 once discovery completeness improves.
  • At least one additional LMC system with a multi-day orbital period (for example 2016-04a) is a plausible unrecognized recurrent nova.
  • Vera Rubin deep, high-cadence imaging should drive LMC nova completeness near 100% and allow the same model inversion to be repeated on a far larger, less biased sample.

Where Pith is reading between the lines

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

  • If higher mean white-dwarf mass is the signature of a younger stellar population, the same light-curve-to-mass inversion applied to other star-forming dwarfs should recover elevated recurrent-nova fractions relative to massive spirals.
  • The tension between model-predicted recurrence times for the known LMC recurrent novae and their observed short intervals may be telling us that the adopted cool-grid accretion rates are systematically too low for those systems.
  • Once Rubin delivers near-complete light curves, a direct comparison of model-predicted versus spectroscopically measured velocities will be the cleanest external test of whether t2 really tracks mass-loss time across the full speed range.

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 / 8 minor

Summary. The manuscript compiles a century (1926–2025) of LMC nova candidates (66 eruptions), of which 48 eruptions from 39 unique progenitors have photometry sufficient to determine peak magnitudes and decline times. The author constructs an updated LMC MMRD relation, shows that LMC novae are on average faster (K-S: ~3.3σ vs M31) and slightly more luminous than M31/Galactic novae, and then inverts the Yaron et al. (2005) model grid — using L_bol from the peak magnitude and t_ml ≡ t2 — to derive WD masses, accretion rates, ejecta velocities, and recurrence times for the 39 systems. The derived mean WD mass is higher in the LMC (⟨M_WD⟩ = 1.23 M⊙ observed; 1.13 M⊙ after recurrence-time debiasing) than in M31 (1.15/1.08 M⊙), with the M_WD and V_max distributions differing at ~2.7–2.9σ. The higher masses are argued to explain the significantly larger fraction of RN eruptions in the LMC (13/63 = 20.6%) than in M31 (87/1360 = 6.4%; χ² = 16.6, ~4σ). The observational compilation is careful and object-by-object documented; the model-dependent conclusions are newer and more exposed.

Significance. If the model-dependent results hold, this is the first estimate of the fundamental parameters (M_WD, Ṁ, V_max, P_rec) of the LMC nova population and a meaningful constraint on how nova populations track recent star formation. Strengths worth naming: the sample size of well-characterized LMC novae is nearly doubled; the compilation is reproducible in the sense that every adopted light-curve parameter is documented object-by-object with uncertainties and provenance; filter and extinction corrections are explicit; the statistical comparisons report p-values; and the model outputs include checkable predictions (P_rec, V_max) that make the analysis falsifiable — indeed, Table 5 supplies exactly such a check. The Rubin-era outlook is timely. The principal weakness is that the load-bearing model inversion currently fails its own internal calibration test (see major comment 1), and the headline RN-fraction contrast rests on completeness assumptions the paper's own Figure 1 undercuts.

major comments (4)
  1. [§5.2, §5.5, §6.2, Table 5] The Yaron-model inversion fails its only internal ground-truth check, and the failure is not propagated. For 3 of 4 known RNe, predicted P_rec exceeds the observed value by 10^2–10^4x (1937-11a: 1.04e5 vs 66.9 yr; 1971-08a: 4.03e4 vs 37.7; 1996-11a: 2.98e3 vs 21.3), because the inversion assigns log dotM ~ -9.1 to -9.9 to systems that the paper itself notes (P_orb > 1 d) must have high dotM. In the bright/fast corner the (L4, t2) -> (M_WD, dotM) inversion is degenerate: high M_WD plus low dotM reproduces the inputs. Three consequences need addressing: (i) the §5.5 debiasing weights w_rec,i ∝ P_rec,i are demonstrably wrong where checkable — recompute <M_WD>_int using observed P_rec for the RNe (or excluding them); (ii) the quoted M_WD uncertainties (±0.02–0.03, Table 5) are incompatible with P_rec errors of 10^3x, so the error-box/RMS method (Eqs. 2–4) underestimates the degeneracy direct
  2. [§5.4 vs Figure 14 vs §7 items (3)–(4)] The reported LMC–M31 K-S statistics are internally inconsistent. The text gives p = 0.005 and 0.0009 (~2.8σ and ~3.3σ) for the M_WD and V_max distributions and p = 0.97 for P_rec; Figure 14 labels give p = 0.0032, 0.0069, and 0.18; the conclusions quote p = 3.21e-3 (2.9σ) for M_WD and 2.7σ for V_max. The discrepancies do not change the qualitative conclusion, but the significance levels of two headline results are quoted differently in three places. Please reconcile (presumably §5.4 is stale) and state explicitly whether censored (grid-edge) points were included in these tests.
  3. [§5.1–5.2, Tables 4–5] At least four novae return M_WD ≳ 1.40 M_sun (1987-09a, 2012-03a, 2024-03a, 2024-04a) and two return log dotM ≳ -7.0 (1999-09a, 2025-03a), i.e., solutions on the boundary of the coarse 4x6 interpolated grid. It is not stated how these censored values enter <M_WD> = 1.23, the Figures 12–13 histograms, and the K-S tests; face-value inclusion biases the mean. The edge artifact is visible: LMCRN 1968-12a at the (1.40, -7.18) corner yields V_max = 1146 km/s, implausibly low for a near-Chandrasekhar RN. Please provide a sensitivity check (e.g., means/K-S with censored objects excluded or treated via survival methods). Relatedly, the §5.2 procedure of inflating observational uncertainties 'by multiples of their original values until a solution was found' should be documented per object — which novae required it and by what factor — since it directly alters the derived parameter errors.
  4. [§6.2; Abstract; §7 item (6)] The RN eruption fraction (13/63 = 20.6% vs 87/1360 = 6.4%; chi^2 = 16.57, ~4σ) assumes binomial sampling from completely surveyed populations, which Figure 1 itself contradicts for the LMC (discovery completeness exceeded ~50% only in the past decade) and which ignores the very different monitoring histories of the two galaxies. The caveat is properly stated in §6.2 and conclusion (6), but the abstract presents the 20.6%/6.4% contrast unqualified, and the χ² test overstates the significance. Please temper the abstract, and ideally demonstrate robustness, e.g., by restricting the comparison to the well-monitored modern era or by a simple completeness simulation.
minor comments (8)
  1. [§4] Cross-reference errors: 'Figure 6' should be Figure 7 (twice), and 'the absolute magnitude distributions shown in Figure 8' should be Figure 9.
  2. [Tables 2–3; Figure 3] t2 for LMCN 1971-03a is given as 20±2 d in Table 2 but 22.0±3.0 d in Table 3 (the text and Fig. 3 caption say ~22±2–3). Also Figure 3 caption (c) gives t2 = 51±9 d while the panel label, §2.1.43, and Table 2 give 51±19 d.
  3. [throughout] Typos/style: 'suupernova' (§2.1.2); 'hace' (§2.1.3); 'was was' (§2.1.13); 'Taable' (§2.1.12); 'LMCN 1848-12a' should be 1948-12a (§2.1.5); '2010-10a' should be 2010-11a (§2, third paragraph); 'bandpassess', 'wavelenghth' (§3.2.1); 'amd' (Fig. 9 caption); 'P rce' (§6); 't2 ≃= 4±1' (§2.1.53); §2.1.66 heading reads 'LMCN 2024-09a' but the object is 2025-09a; 'AA VSO' spacing in §2.1.56 and references.
  4. [Table 1, note c] The reference list for Table 1 contains duplicate numbers: (30) is assigned twice, as are (52) and (58).
  5. [§6.2] The RN fraction uses 63 LMC eruptions while the abstract and §2 state 66; please state the accounting explicitly (exclusion of 1935-09a/SN 1935C, 1998-12a, 2001-06a).
  6. [§3.2, §5] Differential internal extinction within the LMC is neglected; only 1951-01a is excluded on this basis. A sentence on the expected impact for the remaining sample (e.g., novae behind the bar) would be useful. Relatedly, BC = −0.02±0.05 is taken from main-sequence stars with B−V = 0.17; nova photospheres at maximum are not main-sequence atmospheres, so either justify the choice or adopt a larger σ_BC.
  7. [Table 2] Several t2/t3 entries carry no stated uncertainties (e.g., 1988-10a: 5, 10; 2010-11a: 3.5, 5.0; 2012-03a t3 = 2.1); §3.1 says 10–20% is assumed in such cases, but please confirm these defaults are what propagate into Table 4 via Eq. (2).
  8. [§5.1–5.2] The interpolation residual errors δ_L4 and δ_tml entering Eq. (2) are never quantified; typical values per parameter should be reported, since they determine the relative weight of model vs observational uncertainty in the inversion.

Circularity Check

1 steps flagged

No meaningful circularity: LMC light-curve inputs and Yaron-model inversion are independent; mild self-citation supplies method and M31 benchmark only.

specific steps
  1. self citation load bearing [§5 opening; §5.1; Fig. 10–11; comparison in §5.4 / Fig. 13–14]
    "The analysis closely follows the procedure employed by A. W. Shafter & K. Hornoch (2026a) in their study of the nova population in M31, where the nova models presented by O. Yaron et al. (2005) were inverted... The interpolated grids, which are identical to those computed for the A. W. Shafter & K. Hornoch (2026a) study, are reproduced in Figure 10 and 11."

    The inversion recipe, grid interpolation, and the entire M31 comparison sample/distributions are imported from the author’s concurrent M31 papers rather than re-derived here. This is real self-dependence for method and benchmark, but it is not load-bearing for the LMC result itself: the LMC (L4, t2) inputs are independent photometry, and the underlying model grid is external (Yaron et al. 2005). No uniqueness theorem or fitted LMC parameter is smuggled in to force the higher-M_WD claim.

full rationale

The paper’s central chain is: (1) compile independent LMC photometry (m_max, t2) for 39 systems; (2) convert to (L4, t_ml≡t2); (3) invert the external Yaron et al. (2005) grid (T_WD=10^7 K, polynomial-interpolated) for M_WD, Ṁ, then read off model V_max and P_rec; (4) compare distributions to an M31 sample and to the observed RN eruption counts. None of these steps defines the output in terms of itself. Peak magnitudes and decline times are not fitted to force the claimed higher ⟨M_WD⟩; the RN fractions (~20.6% vs ~6.4%) are pure observational tallies (13/63 and 87/1360), not model outputs re-labeled as data. The only self-dependence is methodological and comparative: the inversion pipeline, t2–t3 transforms, interpolated grids, and M31 reference distributions are taken from the author’s concurrent papers (Shafter 2026b; Shafter & Hornoch 2026a,c). That is ordinary reuse of method and benchmark, not a load-bearing uniqueness claim or a fit renamed as prediction. Failures of model P_rec against the four known LMC RNe (Table 5) are a correctness/calibration problem, not circularity—the inversion is not constructed from the observed recurrence times. Score 1 reflects minor non-load-bearing self-citation only.

Axiom & Free-Parameter Ledger

5 free parameters · 6 axioms · 0 invented entities

The central claim rests on standard extragalactic-nova assumptions (known LMC distance, foreground reddening, MMRD-style light-curve parameters), on adopting the Yaron et al. 2005 model grid at fixed T_WD with t_ml≡t2, and on several photometric zero-point and color transforms. No new physical entities are postulated. Free parameters are mostly adopted constants and interpolation choices rather than global fits to the science claim.

free parameters (5)
  • T_WD (model grid choice) = 10^7 K
    Fixed at 10^7 K for all systems following Townsley & Bildsten (2004) reasoning; other Yaron grids (30 and 50 MK) are discarded. Choice shifts inferred M_WD and Ṁ.
  • Bolometric correction BC = −0.02 ± 0.05
    Adopted BC=−0.02±0.05 from main-sequence stars at B−V≈0.17 to convert M_V to L4; not measured per nova.
  • Nova colors at maximum for filter transforms = B−V=0.20, V−R=0.20, R−I=0.13
    B−V=0.20, V−R=0.20, R−I=0.13 from Craig et al. (2025) Silver sample applied uniformly to convert pg/g/R/I/o/G to V.
  • Second-order polynomial surface interpolation of Yaron grid
    Coarse 4 M_WD × 6 logṀ grid is replaced by continuous polynomial surfaces; residual grid error is propagated but functional form is a modeling choice.
  • E(B−V) foreground and R_V = E(B−V)=0.06±0.02, R=3.1
    Line-of-sight reddening fixed at 0.06±0.02 and R=3.1; internal LMC extinction variations largely ignored except case-by-case notes.
axioms (6)
  • domain assumption Mass-loss timescale in the Yaron models equals the observed t2 decline time (t_ml ≡ t2).
    Invoked in §5 following Shara et al. (2018) and Shafter & Hornoch (2026a); load-bearing for every inverted M_WD and Ṁ.
  • domain assumption Yaron et al. (2005) TNR model grid correctly predicts peak bolometric luminosity and mass-loss timescale as functions of M_WD and Ṁ.
    Entire §5 analysis inverts this grid; no alternative model suite is cross-checked.
  • domain assumption LMC distance modulus (m−M)_0 = 18.477 ± 0.026 (Pietrzyński et al. 2019).
    §3.2; converts all apparent peaks to M_V and L4.
  • domain assumption Empirical t3↔t2 transformations of Shafter (2026b) recover unbiased t2 when only t3 is published.
    §3.1; used for older novae whose only published decline parameter is t3.
  • standard math Standard arithmetic and statistical machinery (polynomial interpolation, Euclidean χ, K-S and χ² tests, binomial variance).
    Used throughout §§4–6 for fits and population comparisons.
  • domain assumption Spectroscopic FeII vs He/N classes (Williams 1992), possibly as evolutionary phases (Aydi et al. 2024a), still segregate fast/broad-lined from slow/narrow-lined systems when spectra are taken ~1–2 weeks post-max.
    §6.1; underpins the claim that the high He/N fraction tracks high M_WD.

pith-pipeline@v1.2.0-grok45-kimik3 · 53539 in / 4028 out tokens · 71729 ms · 2026-07-30T10:35:57.859450+00:00 · methodology

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Cite this review

Pith. "Pith review of A Century of Novae in the Large Magellanic Cloud." pith.science (2026). https://pith.science/paper/E5G3XLMV

@misc{pith2026260723849,
  author       = {Pith},
  title        = {Pith review of: A Century of Novae in the Large Magellanic Cloud},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/E5G3XLMV}},
  note         = {Machine review of arXiv:2607.23849}
}
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read the original abstract

A comprehensive study of novae in the Large Magellanic Cloud (LMC) is presented. A total of 66 nova eruptions have been reported in the LMC over the past century (1926-2025). Of these, a total of 48 eruptions from 39 unique progenitor systems (9 eruptions are recurrences of 4 known recurrent novae) have sufficient photometric data to permit the maximum magnitudes and rates of decline to be reliably estimated. These data confirm earlier studies showing that LMC novae are, on average, slightly more luminous and faster evolving compared with novae in the Andromeda galaxy (M31) or the Milky Way. For the first time, the nova models of Yaron et al. (2005) have been used in conjunction with the light curve data to estimate the fundamental properties of the LMC nova population. The models suggest that LMC novae are characterized by generally higher WD masses and higher expansion velocities compared with M31 novae. The higher average WD masses has resulted in a higher percentage of RN eruptions in the LMC ($\sim20.6$%) compared with that seen in M31 ($\sim6.40$%). Future observations made possible by the Vera Rubin Observatory promise to revolutionize our understanding of nova populations in the LMC, and in galaxies beyond the local group.

Figures

Figures reproduced from arXiv: 2607.23849 by Allen W. Shafter.

Figure 1
Figure 1. Figure 1: The history of nova candidate discoveries in the LMC plotted in decade wide bins from 1926 to 2025. The dashed red line shows the number of novae expected to erupt each decade (and its 1σ lower limit: dotted line) based on an estimated annual nova rate of 2.4 ± 0.8 yr−1 (P. Mr´oz et al. 2016a). It hasn’t been until the past decade when the number of novae observed has exceeded ∼ > 50% of the expected total… view at source ↗
Figure 2
Figure 2. Figure 2: The positions of the LMC nova candidates. The offsets were computed assuming the center of the LMC lies at R.A. = 5h 26m 41.19s; Decl. = −69◦ 11′ 9.15′′. The blue circled points represent known novae, the red circled points represent the 4 known RNe, and the two orange X symbols represent doubtful novae (LMCN 1998-12a and 2001-06a). Two additional novae, LMCN 2013-10a and 2015-03a, were observed in the out… view at source ↗
Figure 3
Figure 3. Figure 3: Light curves for selected novae used for the de￾termination of t2 times. (a) LMCN 1971-03a: V -band light curve from Table II of J. A. Graham & G. Araya (1971a). From these data we estimate a decline rate of 0.091 mag d−1 , or t2 = 22 ± 2 d. (b) LMCN 1987-09a: R-band data from R. H. McNaught & G. J. Garradd (1987) yields an initial decline rate of 1 mag d−1 giving t2 = 2.0 ± 0.2 d. (c) LMCN 2009-05a: V -ba… view at source ↗
Figure 5
Figure 5. Figure 5: Light curves for selected novae used for the de￾termination of t2 times. (a) LMCN 2024-03a: g-band pho￾tometry from ASAS-SN show a very rapidly decline (1.3 mag d−1 ) characterized by t2 = 1.5 ± 0.2. (b) LMCN 2024-04a: ASAS-SN g-band photometry showing a decline rate of 0.51 mag d−1 , corresponding to t2 = 3.9 ± 0.3 d. (c) LMCN 2025-03a: o-band light curve based on ATLAS data. The light declines at a rate … view at source ↗
Figure 6
Figure 6. Figure 6: The Julian Dates of the observed eruptions of LMCRN 1968-12a plotted as a function of the expected out￾burst number. The best fitting slope gives the mean recur￾rence period: ⟨Prec⟩ = 2098.42 ± 66.45 d, or 5.75 ± 0.18 yr. Expected outbursts Nos. 2, 3, 4, and 6 that most likely occurred near 1974, 1980, 1985, and 1996 were apparently missed. the eruption was observed by ATLAS survey. The re￾sulting light cu… view at source ↗
Figure 7
Figure 7. Figure 7: Left panel: The MMRD plot for the LMC (blue points: He/N novae; red points: Fe II novae). Right panel: The MMRD plot for M31 (on the same scale) based on data from J. G. Clark et al. (2024). The large blue squares in both plots indicate known RNe. The dashed lines show the best linear fits with MV = −8.77(±0.26) + 1.10(±0.22) log t2 and MV = −8.62(±0.21) + 0.93(±0.15) log t2 for the LMC and M31, respective… view at source ↗
Figure 8
Figure 8. Figure 8: The cumulative fractions of the t2 times for the LMC nova sample compared with those of M31 and the Galaxy (MW). The LMC and Galactic samples yield a K-S probability p = 0.159 and thus differ at only ∼ 1.4σ. On the other hand, both the LMC and Galactic samples differ from the M31 sample by 3.3σ (K-S p = 9.8×10−4 ) and 2.9σ (K-S p = 3.9 × 10−3 ), respectively. -6-5 -7 -11-10-9-8 MV 0 10 20 30 40 50 60 Numbe… view at source ↗
Figure 9
Figure 9. Figure 9: The absolute visual magnitude distribution for the LMC nova sample compared with the corresponding dis￾tributions for M31 and the Galaxy (MW). The relatively small LMC sample does not differ significantly from either the M31 or Galactic samples (∼ 1.2σ and ∼ 1.3σ, respec￾tively), but the larger Galactic amd M31 samples differ at > 3σ. sistent with the difference in stellar population between the two galaxi… view at source ↗
Figure 10
Figure 10. Figure 10: The interpolated model grids from A. W. Shafter & K. Hornoch (2026a) for our key input parame￾ters, the bolometric luminosity at the peak of the eruption, L4, (top panel), and the mass-loss timescale, tml (bottom panel) as functions of log M˙ (M⊙ yr−1 ) and MWD (M⊙). The interpolations were performed by fitting second-order polynomials to the nova models of O. Yaron et al. (2005) as described in section 5… view at source ↗
Figure 12
Figure 12. Figure 12: The distributions of the WD mass (upper left panel), the mass accretion rate (upper right panel) the maximum expansion velocity, Vmax, (lower left panel), and predicted recurrence time, Prec, (lower right panel), for the 39 LMC novae analyzed with the O. Yaron et al. (2005) models. The top panels in each figure show the distributions of Fe II novae (red), while the bottom panels show the He/N novae (blue)… view at source ↗
Figure 13
Figure 13. Figure 13: The derived distributions for MWD, log M˙ , Vmax and Prec for the LMC novae (blue histograms) compared with the distributions for M31 novae (grey histograms) from A. W. Shafter & K. Hornoch (2026a). troscopic classes, which are available for the majority of the novae, have also been included. 5.3. Observed Distributions of Nova Parameters [PITH_FULL_IMAGE:figures/full_fig_p019_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: The cumulative distributions of the four properties (M31: red; LMC: blue). No significant differences were found between the log M˙ and Prec distributions, but K-S tests show that the WD mass and Vmax distributions differ by ∼ 2.95σ and ∼ 2.69σ, respectively. sample. Finally, a comparison of the recurrence time dis￾tributions for the two galaxies suggest a possible dearth of LMC novae with predicted recur… view at source ↗
Figure 15
Figure 15. Figure 15: The intrinsic distributions for MWD and log M˙ (bottom left and bottom right, respectively, compared with the observed distributions which have been reproduced in the top panels of each figure. cation of Equation 6 from A. W. Shafter & K. Hornoch (2026a) to the observed MWD and log M˙ distributions of our LMC nova sample results in the intrinsic distri￾butions shown in [PITH_FULL_IMAGE:figures/full_fig_p… view at source ↗

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Reference graph

Works this paper leans on

182 extracted references · 26 canonical work pages · 2 internal anchors

  1. [1]

    , keywords =

    Shortest Recurrence Periods of Novae. , keywords =. doi:10.1088/0004-637X/793/2/136 , archivePrefix =. 1404.0582 , primaryClass =

    Pith/arXiv arXiv

  2. [2]

    , keywords =

    Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-nova Supersoft Phase. , keywords =. doi:10.1088/0004-637X/777/2/136 , archivePrefix =. 1309.3375 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    , keywords =

    Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O - M stars. , keywords =

  4. [4]

    , keywords =

    The morphological distribution of bright galaxies in the UVK color plane. , keywords =. doi:10.1086/182674 , adsurl =

    work page doi:10.1086/182674

  5. [5]

    Third Reference Catalogue of Bright Galaxies

  6. [6]

    Research Notes of the American Astronomical Society , keywords =

    Recent Extragalactic Nova Rate Determinations and their Implications. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/acc937 , adsurl =

    work page doi:10.3847/2515-5172/acc937

  7. [7]

    , keywords =

    The Absolute Magnitude of the Sun in Several Filters. , keywords =. doi:10.3847/1538-4365/aabfdf , archivePrefix =. 1804.07788 , primaryClass =

    Pith/arXiv arXiv

  8. [8]

    , keywords =

    The Spectroscopic Differences between Disk and Thick-Disk/Bulge Novae. , keywords =. doi:10.1086/306275 , adsurl =

    work page doi:10.1086/306275

  9. [9]

    The Golden Age of Cataclysmic Variables and Related Objects V , year = 2021, volume =

    Galactic and Extragalactic Novae - A Multiwavelenght Review. The Golden Age of Cataclysmic Variables and Related Objects V , year = 2021, volume =. doi:10.22323/1.368.0026 , adsurl =

    work page doi:10.22323/1.368.0026 2021

  10. [10]

    , keywords =

    Observations of galactic and extragalactic novae. , keywords =. doi:10.1007/s00159-020-0124-6 , archivePrefix =. 2004.06540 , primaryClass =

    Pith/arXiv arXiv 2004

  11. [11]

    , keywords =

    LSST: From Science Drivers to Reference Design and Anticipated Data Products. , keywords =. doi:10.3847/1538-4357/ab042c , archivePrefix =. 0805.2366 , primaryClass =

    Pith/arXiv arXiv

  12. [12]

    , keywords =

    Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class. , keywords =. doi:10.3847/1538-4357/ae0616 , adsurl =

    doi:10.3847/1538-4357/ae0616

  13. [13]

    , keywords =

    Constraining the evolution of cataclysmic variables via the masses and accretion rates of their underlying white dwarfs. , keywords =. doi:10.1093/mnras/stab3449 , archivePrefix =. 2111.13706 , primaryClass =

    Pith/arXiv arXiv

  14. [14]

    , volume =

    Dust distributions in the Magellanic Clouds. , volume =. 2022 , month = mar, doi =

    2022

  15. [15]

    , volume =

    The spatial distribution of the LMC foreground stars. , volume =. 1995 , adsurl =

    1995

  16. [16]

    Massive luminous early type stars in the LMC. I. The reddening of individual stars and the LMC reddening law. , volume =. 2002 , month = aug, doi =

    2002

  17. [17]

    arXiv e-prints , keywords =

    The Recurrent Nova Population in M31. arXiv e-prints , keywords =. 2026c , month = apr, eid =

  18. [18]

    2004 , volume =

    Thermal Evolution of Accreting White Dwarfs: Effects of Convective Overshoot and Mixing , journal =. 2004 , volume =. doi:10.1086/379701 , adsurl =

    doi:10.1086/379701 2004

  19. [19]

    , keywords =

    Intrinsic Colors, Temperatures, and Bolometric Corrections of Pre-main-sequence Stars. , keywords =. doi:10.1088/0067-0049/208/1/9 , archivePrefix =. 1307.2657 , primaryClass =

    Pith/arXiv arXiv

  20. [20]

    , keywords =

    On the Use of Empirical Bolometric Corrections for Stars. , keywords =. doi:10.1088/0004-6256/140/5/1158 , archivePrefix =. 1008.3913 , primaryClass =

    Pith/arXiv arXiv

  21. [21]

    The Astronomer's Telegram , keywords =

    SALT spectroscopic observations of the LMC nova PNV J05145365-7009486. The Astronomer's Telegram , keywords =. 2019c , month = nov, volume =

  22. [22]

    , keywords =

    Revisiting the classics: on the optical colours of novae as standard crayons. , keywords =. doi:10.1093/mnras/staf385 , archivePrefix =. 2412.15108 , primaryClass =

    Pith/arXiv arXiv

  23. [23]

    , keywords =

    A far red spectrum of Nova LMC 1981. , keywords =

    1981

  24. [24]

    , keywords =

    On The Rate of Novae in Galaxies of Different Types. , keywords =. doi:10.1086/304020 , adsurl =

    work page doi:10.1086/304020

  25. [25]

    , year = 1961, month = may, volume =

    U - B and B - V Colors of Black Bodies. , year = 1961, month = may, volume =. doi:10.1086/147090 , adsurl =

    work page doi:10.1086/147090 1961

  26. [26]

    , keywords =

    The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae. , keywords =. doi:10.3847/1538-4357/aabfbd , archivePrefix =. 1804.06880 , primaryClass =

    Pith/arXiv arXiv

  27. [27]

    , keywords =

    Challenging Classical Paradigms: Recurrent Nova M31N 2017-01e, a BeWD System in M31?. , keywords =. doi:10.3847/1538-4357/adf843 , archivePrefix =. 2508.02227 , primaryClass =

    Pith/arXiv arXiv 2017

  28. [28]

    , keywords =

    LMC 1995, the third supersoft X-ray nova. , keywords =

    1995

  29. [29]

    , keywords =

    Modelling nova populations in galaxies. , keywords =. doi:10.1093/mnras/stw458 , archivePrefix =. 1602.07849 , primaryClass =

    Pith/arXiv arXiv

  30. [30]

    , keywords =

    The Star Formation History of the Large Magellanic Cloud. , keywords =. doi:10.1088/0004-6256/138/5/1243 , archivePrefix =. 0908.1422 , primaryClass =

    Pith/arXiv arXiv

  31. [31]

    , keywords =

    The All-Sky Automated Survey for Supernovae (ASAS-SN) Light Curve Server v1.0. , keywords =. doi:10.1088/1538-3873/aa80d9 , archivePrefix =. 1706.07060 , primaryClass =

    Pith/arXiv arXiv

  32. [32]

    , keywords =

    The Formation of Novae Spectra. , keywords =. doi:10.1086/116268 , adsurl =

    work page doi:10.1086/116268

  33. [33]

    , keywords =

    Exploring the Maximum Magnitude versus Rate of Decline Relation for Novae in M31. , keywords =. doi:10.3847/1538-4365/ad3c39 , adsurl =

    work page doi:10.3847/1538-4365/ad3c39

  34. [34]

    , keywords =

    The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey. , keywords =. doi:10.3847/1538-4357/ac87ad , archivePrefix =. 2207.05689 , primaryClass =

    Pith/arXiv arXiv

  35. [35]

    , keywords =

    Exploring the Role of Globular Cluster Specific Frequency on the Nova Rates in Three Virgo Elliptical Galaxies. , keywords =. doi:10.1088/0004-637X/811/1/34 , archivePrefix =. 1508.03319 , primaryClass =

    Pith/arXiv arXiv

  36. [36]

    , keywords =

    A Spectroscopic and Photometric Survey of Novae in M31. , keywords =. doi:10.1088/0004-637X/734/1/12 , archivePrefix =. 1104.0222 , primaryClass =

    Pith/arXiv arXiv

  37. [37]

    Rate and statistical characteristics of the nova population

    Classical novae from the POINT-AGAPE microlensing survey of M31 - II. Rate and statistical characteristics of the nova population. , keywords =. doi:10.1111/j.1365-2966.2006.10297.x , archivePrefix =. astro-ph/0509493 , primaryClass =

    arXiv 2006

  38. [38]

    , keywords =

    On the Spatial Distribution, Stellar Population, and Rate of Novae in M31. , keywords =. doi:10.1086/324044 , adsurl =

    work page doi:10.1086/324044

  39. [39]

    , keywords =

    Fifty-Two Novae in M31 Discovered and Observed at Asiago from 1971 to 1986. , keywords =. doi:10.1086/114959 , adsurl =

    work page doi:10.1086/114959 1971

  40. [40]

    , keywords =

    The Spatial Distribution and Population of Novae in M31. , keywords =. doi:10.1086/165388 , adsurl =

    work page doi:10.1086/165388

  41. [41]

    , year = 1973, month = mar, volume =

    Novae in M 31 discovered and observed at Asiago from 1963 to 1970. , year = 1973, month = mar, volume =

    1963

  42. [42]

    , year = 1956, month = feb, volume =

    Novae in the Andromeda nebula. , year = 1956, month = feb, volume =. doi:10.1086/107284 , adsurl =

    work page doi:10.1086/107284 1956

  43. [43]

    , year = 1929, month = mar, volume =

    A spiral nebula as a stellar system, Messier 31. , year = 1929, month = mar, volume =. doi:10.1086/143167 , adsurl =

    doi:10.1086/143167 1929

  44. [44]

    Harvard College Observatory Bulletin , year = 1951, month = sep, volume =

    Three Notes on Variable Stars in the Small Magellanic Cloud. Harvard College Observatory Bulletin , year = 1951, month = sep, volume =

    1951

  45. [45]

    Annals of Harvard College Observatory , year = 1908, month = jan, volume =

    1777 variables in the Magellanic Clouds. Annals of Harvard College Observatory , year = 1908, month = jan, volume =

    1908

  46. [46]

    , year = 1926, month = may, volume =

    A spiral nebula as a stellar system: Messier 33. , year = 1926, month = may, volume =. doi:10.1086/142976 , adsurl =

    doi:10.1086/142976 1926

  47. [47]

    Nature , keywords =

    A distance to the Large Magellanic Cloud that is precise to one per cent. Nature , keywords =. doi:10.1038/s41586-019-0999-4 , archivePrefix =. 1903.08096 , primaryClass =

    Pith/arXiv arXiv 1903

  48. [48]

    A Hubble Space Telescope Survey for Novae in M87. I. Light and Color Curves, Spatial Distributions, and the Nova Rate. , keywords =. doi:10.3847/0067-0049/227/1/1 , archivePrefix =. 1602.00758 , primaryClass =

    Pith/arXiv arXiv

  49. [49]

    , keywords =

    Discovery of a New Photometric Sub-class of Faint and Fast Classical Novae. , keywords =. doi:10.1088/0004-637X/735/2/94 , archivePrefix =. 1003.1720 , primaryClass =

    Pith/arXiv arXiv

  50. [50]

    Research Notes of the American Astronomical Society , keywords =

    Concerning the Verity of the MMRD Relation for Novae. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/acf5e8 , archivePrefix =. 2309.00739 , primaryClass =

    Pith/arXiv arXiv

  51. [51]

    , keywords =

    Classical Novae in Andromeda: Light Curves from the Palomar Transient Factory and GALEX. , keywords =. doi:10.1088/0004-637X/752/2/133 , archivePrefix =. 1201.2393 , primaryClass =

    Pith/arXiv arXiv

  52. [52]

    , year = 1945, month = apr, volume =

    The Relation between Light-Curves and Luminosities of Novae. , year = 1945, month = apr, volume =. doi:10.1086/125689 , adsurl =

    work page doi:10.1086/125689 1945

  53. [53]

    The Astronomer's Telegram , keywords =

    Spectroscopic classification of TCP J05293666-7009566 as a likely classical nova in the LMC. The Astronomer's Telegram , keywords =. 2019b , month = jul, volume =

  54. [54]

    Transient Name Server AstroNote , keywords =

    Photometric follow-up of extragalactic nova candidate AT2025ggn with BHTOM.space global telescope network. Transient Name Server AstroNote , keywords =

  55. [55]

    The Astronomer's Telegram , keywords =

    SALT spectroscopic classification of ASASSN-20oh as a classical nova in the LMC. The Astronomer's Telegram , keywords =

  56. [56]

    , year = 1973, month = jan, volume =

    Nova in Large Magellanic Cloud. , year = 1973, month = jan, volume =

    1973

  57. [57]

    , year = 1972, month = feb, volume =

    Nova Mensae 1970b in the Large Magellanic Cloud. , year = 1972, month = feb, volume =

    1972

  58. [58]

    , year = 1999, month = jan, volume =

    Variable in the Large Magellanic Cloud. , year = 1999, month = jan, volume =

    1999

  59. [59]

    and Prialnik, D

    Yaron, O. and Prialnik, D. and Shara, M. M. and Kovetz, A. , title =. The Astrophysical Journal , volume =. 2005 , doi =

    2005

  60. [60]

    , year = 1991, month = apr, volume =

    Nova in the Large Magellanic Cloud 1991. , year = 1991, month = apr, volume =

    1991

  61. [61]

    The Astronomer's Telegram , keywords =

    Spectroscopic observations of the latest outburst of Nova LMC 1968. The Astronomer's Telegram , keywords =. 2024b , month = aug, volume =

    1968

  62. [62]

    Bessell, M. S. , title =. Publications of the Astronomical Society of the Pacific , volume =. 1990 , month = oct, doi =

    1990

  63. [63]

    , keywords =

    The Sloan Digital Sky Survey View of the Palomar-Green Bright Quasar Survey. , keywords =. doi:10.1086/432466 , archivePrefix =. astro-ph/0506022 , primaryClass =

    Pith/arXiv arXiv

  64. [64]

    , keywords =

    Catalog of 93 Nova Light Curves: Classification and Properties. , keywords =. doi:10.1088/0004-6256/140/1/34 , archivePrefix =. 1004.3698 , primaryClass =

    Pith/arXiv arXiv

  65. [65]

    The Astronomer's Telegram , keywords =

    OGLE-IV Pre-discovery Observations of MASTER OT J051032.58-692130.4. The Astronomer's Telegram , keywords =. 2016c , month = may, volume =

  66. [66]

    Advances in Astronomy , keywords =

    Master Robotic Net. Advances in Astronomy , keywords =. doi:10.1155/2010/349171 , archivePrefix =. 0907.0827 , primaryClass =

    Pith/arXiv arXiv 2010

  67. [67]

    The Astronomer's Telegram , keywords =

    ASASSN-15fd = Nova LMC 2015. The Astronomer's Telegram , keywords =

    2015

  68. [68]

    , keywords =

    A Light Curve Analysis of Recurrent and Very Fast Novae in Our Galaxy, Magellanic Clouds, and M31. , keywords =. doi:10.3847/1538-4365/aac833 , archivePrefix =. 1805.09932 , primaryClass =

    Pith/arXiv arXiv

  69. [69]

    The Astronomer's Telegram , keywords =

    Optical Spectroscopy of LMC Nova candidate 2012-03a. The Astronomer's Telegram , keywords =

    2012

  70. [70]

    , keywords =

    A Light Curve Analysis of Classical Novae: Free-free Emission versus Photospheric Emission. , keywords =. doi:10.1088/0004-637X/798/2/76 , archivePrefix =. 1410.7888 , primaryClass =

    Pith/arXiv arXiv

  71. [71]

    , year = 2004, month = oct, volume =

    Nova in the Large Magellanic Cloud 2004. , year = 2004, month = oct, volume =

    2004

  72. [72]

    , year = 2000, month = jul, volume =

    Nova in the Large Magellanic Cloud 2000. , year = 2000, month = jul, volume =

    2000

  73. [73]

    , year = 1995, month = mar, volume =

    Nova in the Large Magellanic Cloud 1995. , year = 1995, month = mar, volume =

    1995

  74. [74]

    , year = 1992, month = nov, volume =

    Nova in the Large Magellanic Cloud 1992. , year = 1992, month = nov, volume =

    1992

  75. [75]

    , keywords =

    Multiwavelength Observations of Nova LMC 1990 Number 2: The First Extragalactic Recurrent Nova. , keywords =. doi:10.1086/169804 , adsurl =

    work page doi:10.1086/169804 1990

  76. [76]

    , keywords =

    Nova LMC 1991 : evidence for a super-bright nova population. , keywords =

    1991

  77. [77]

    , keywords =

    The Evolution and Classification of Postoutburst Novae Spectra. , keywords =. doi:10.1086/170319 , adsurl =

    doi:10.1086/170319

  78. [78]

    Nova in the Large Magellanic Cloud 1990 No. 1. , year = 1990, month = feb, volume =

    1990

  79. [79]

    , year = 1988, month = mar, volume =

    Nova in the Large Magellanic Cloud. , year = 1988, month = mar, volume =

    1988

  80. [80]

    , keywords =

    The 2016 January eruption of recurrent Nova LMC 1968. , keywords =. doi:10.1093/mnras/stz2960 , archivePrefix =. 1909.03281 , primaryClass =

    Pith/arXiv arXiv 2016

Showing first 80 references.