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arxiv: 2606.30390 · v1 · pith:BLMWZ64Anew · submitted 2026-06-29 · 🌌 astro-ph.SR · astro-ph.HE

SN 2019vxm: A luminous and long-lived Type IIn supernova with early flash-ionisation features

Y.-Z. Cai , A. Pastorello , T. J. Moriya , X.-F. Wang , A. Reguitti , A. V. Filippenko , L. Tomasella , K. \v{C}otar
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A. Siviero N. Elias-Rosa T. G. Brink G. Valerin S. Benetti J.-W. Zhao Z.-H. Peng Z.-Y. Wang I. Altunin R. Baer-Way E. Baron V. Chander M. Chu A. deGraw J. M. DerKacy J. Isern C. Jennings R. Kotak L.-P. Li P. Marziani M. May P. A. Mazzali A. Morales-Garoffolo S. Moran P. Ochner I. Salmaso L. Tartaglia M. Turatto H.-Y. Wu D.-F. Xiang S.-Y. Yan J.-J. Zhang W. Zheng
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Pith reviewed 2026-06-30 03:43 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords Type IIn supernovaSN 2019vxmflash ionizationmass-loss ratecircumstellar materialdust formationlight curveBalmer lines
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The pith

SN 2019vxm reaches a peak of MV = -20.01 mag and its early flash-ionization lines set a lower limit of 0.01 solar masses per year on the progenitor mass-loss rate.

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

The paper analyzes the light curves and spectra of SN 2019vxm, a Type IIn supernova that brightens to MV = -20.01 mag in 35 days and then declines slowly over hundreds of days. Early spectra show a blue continuum plus narrow Balmer lines and flash-ionization lines of C III, N III and He II; matching these to existing models yields the mass-loss lower limit. A mid-infrared excess appears after seven months, consistent with a few thousandths of a solar mass of newly formed dust. High-resolution spectra detect a weak P Cygni absorption indicating slow unshocked circumstellar gas, and the overall bolometric light curve before day 100 follows a power-law decline similar to SN 2010jl.

Core claim

SN 2019vxm is a luminous long-lived Type IIn event whose peak absolute magnitude is MV = -20.01 +/- 0.13 mag at 35 days post-explosion. Its spectra begin with narrow symmetric Balmer lines and flash-ionization features; comparison with interacting-supernova models gives a progenitor mass-loss rate lower limit of at least 0.01 solar masses per year. The light curve and spectral evolution remain slow for months, a mid-infrared excess signals dust formation starting at or after 210 days, and line profiles later become broader and blueshifted, indicating ongoing circumstellar interaction.

What carries the argument

Comparison of the observed early flash-ionized spectrum to existing early-interacting SN spectral models, used to infer the density and thus the mass-loss rate of the progenitor's circumstellar material.

If this is right

  • The progenitor expelled material at a rate of at least 0.01 solar masses per year in the years preceding explosion.
  • A few 10^-3 solar masses of dust formed at or after 210 days, possibly reaching 0.01 solar masses by +4.5 years.
  • The bolometric luminosity before 100 days follows L(t) proportional to t to the power -0.49, matching the interaction-powered phase seen in SN 2010jl.
  • The gradual broadening and blueshift of H-alpha and H-beta, with growing red-wing deficit after +102 days, record the changing velocity structure of the shocked and unshocked material.
  • The weak P Cygni absorption at +19.7 days reveals slow-moving (60 km/s) unshocked circumstellar gas from the pre-supernova wind.

Where Pith is reading between the lines

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

  • Events with comparable early flash-ionization signatures may share a common pattern of dense, recently ejected circumstellar shells.
  • Long-term infrared monitoring could test whether dust continues to form or is destroyed by the forward shock at later epochs.
  • If similar mass-loss rates recur across the Type IIn population, they would constrain the final evolutionary stages of massive stars that produce these events.
  • The power-law index of the early light curve offers a simple diagnostic that future surveys could apply to identify other interaction-dominated supernovae without full spectroscopic coverage.

Load-bearing premise

The mass-loss rate lower limit rests on the assumption that current early-interacting SN spectral models correctly capture the geometry, density profile and composition of the circumstellar material without large systematic offsets.

What would settle it

An independent radio or X-ray measurement showing a mass-loss rate below 0.01 solar masses per year, or pre-explosion imaging that rules out a progenitor capable of such sustained mass loss, would falsify the lower limit derived from the flash-ionization lines.

Figures

Figures reproduced from arXiv: 2606.30390 by A. deGraw, A. Morales-Garoffolo, A. Pastorello, A. Reguitti, A. Siviero, A. V. Filippenko, C. Jennings, D.-F. Xiang, E. Baron, G. Valerin, H.-Y. Wu, I. Altunin, I. Salmaso, J. Isern, J.-J. Zhang, J. M. DerKacy, J.-W. Zhao, K. \v{C}otar, L.-P. Li, L. Tartaglia, L. Tomasella, M. Chu, M. May, M. Turatto, N. Elias-Rosa, P. A. Mazzali, P. Marziani, P. Ochner, R. Baer-Way, R. Kotak, S. Benetti, S. Moran, S.-Y. Yan, T. G. Brink, T. J. Moriya, V. Chander, W. Zheng, X.-F. Wang, Y.-Z. Cai, Z.-H. Peng, Z.-Y. Wang.

Figure 1
Figure 1. Figure 1: SN 2019vxm in a Copernico + AFOSC image taken with Sloan r filter on 2019 December 5. The SN is marked at the crosshair, near the centre of the image. 5750 5800 5850 5900 Rest Wavelength [Å] F [erg s 1 c m 2 Å 1 ] Na I (M W) Na I (M W) He I 5876 N a I D (Host) [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Zoomed-in view of the Na i D spectral region in the Coper￾nico/Echelle spectrum taken on 2019 December 06 (+19.7 d). These values are calculated under the assumption of a standard ΛCDM cosmology with H0 = 73 km s−1 Mpc−1 , ΩM = 0.27, and ΩΛ = 0.73 (Spergel et al. 2007). The Milky Way (MW) extinction toward SN 2019vxm is E(B − V)MW = 0.087 ± 0.002 mag (Schlafly & Finkbeiner 2011), in agreement with the valu… view at source ↗
Figure 3
Figure 3. Figure 3: Multiband (UV, optical, and MIR) apparent light curves of SN 2019vxm. Error bars are included for all photometric points, but the uncertainty is usually smaller than the marker size. A dotted vertical line indicates the epoch of explosion epoch. SN 2019vxm within the first ∼ 400 d is broadly consistent with that of SN 2017hcc, although at later phases the r − i colour of SN 2019vxm becomes noticeably bluer… view at source ↗
Figure 6
Figure 6. Figure 6: Pseudobolometric light curves of SN 2019vxm and comparison bright SNe IIn and SLSN-II. The comparison objects have either similar luminosities to that of the “optical” luminosity of SN 2019vxm or with long evolution times. The luminosity is calculated by integrating from the B to the I/i bands. where Bλ is the Planck function for the temperature of the dust Td, κλ(a) is the dust opacity coefficient as a fu… view at source ↗
Figure 5
Figure 5. Figure 5: Colour evolution of SN 2019vxm, compared to a sample of SNe IIn. Upper panel: (B− V) colour evolution. Lower panel: (R − I) or (r − i) colour evolution. The colour curves are corrected for both Galac￾tic and host-galaxy extinction. 100 0 100 200 300 400 500 600 700 Phases from maximum luminosity [days] 40.5 41.0 41.5 42.0 42.5 43.0 43.5 44.0 lo g 1 0(L B ol / e r g s 1 ) SN 2003ma SN 2005ip SN 2006gy SN 20… view at source ↗
Figure 8
Figure 8. Figure 8: Light-curve modelling of SN 2019vxm, overplotted with the comparison SN 2010jl. The light curve is fitted with a single power￾law function, shown as a blue line. was adopted for the analysis of SN 2010jl (e.g., Fransson et al. 2014; Moriya et al. 2013b; Ofek et al. 2014). Our fit resulted in L(t) = 2 × 1044(t/day)−0.49 erg s−1 . The fitted power-law lu￾minosity evolution is similar to those obtained for SN… view at source ↗
Figure 7
Figure 7. Figure 7: SED evolution of SN 2019vxm. The dashed blue lines represent the best black-body fits to the optical bands, while the dashed red lines represent the best fits of the grey-body dust emission model for silicates of a = 0.1 µm. Each model is overplotted with the SED, and SEDs are shifted vertically by an arbitrary constant for clarity. 3.6. Light-curve modelling We estimate the CSM properties of SN 2019vxm th… view at source ↗
Figure 9
Figure 9. Figure 9: The spectral evolution of SN 2019vxm. Some significant spectral features are marked with vertical-coloured lines. The marked phases are with respect to the time of the V-band maximum light. The spectra are redshift-corrected and calibrated to match the photometric data; vertical shifts have been applied for clarity. Telluric lines are indicated with encircled “plus” symbols. Data from different telescopes … view at source ↗
Figure 11
Figure 11. Figure 11: Fits to the Hα , He i , and Na i profiles of SN 2019vxm taken with the medium-resolution GTC/R2500R spectrum at +166.2 d. Up￾per panel: multicomponent fitting of Hα. Lower panel: multicomponent fitting of Na i D and He i λ5876. The Na i D lines from the interstellar medium (ISM) of the Milky Way (MW) are marked. Different compo￾nents are marked with different colours. the Copernico 1.82 m telescope on 201… view at source ↗
Figure 10
Figure 10. Figure 10: Hα and Hβ profiles of SN 2019vxm (shown in blue and red colours, respectively) in velocity space, taken from the high-resolution Copernico/Echelle spectrum at +19.7 d. The inset in the upper-left cor￾ner provides a zoomed-in view of the P Cygni profiles. To constrain the velocity of the narrow component, a higher resolution spectrum is necessary. With this motivation, we ob￾tained a high-resolution (R ≈ 2… view at source ↗
Figure 13
Figure 13. Figure 13: Hα profiles of SN 2019vxm at selected epochs, redshifted to the line rest wavelength (blue) and mirrored with respect to the com￾puted centroids (magenta). Assuming solar abundances and accounting for the effects of the phase mismatch, we estimate the mass-loss rate of the pro￾genitor of M˙ ≳ 10−2 M⊙ yr−1 . We consider this result as a lower limit since the actual spectroscopic epoch is later than the mod… view at source ↗
Figure 14
Figure 14. Figure 14: Spectra of SN 2019vxm compared to similar Type IIn SNe and SLSNe-II at early (0–40 days), post-peak (40–400 days), and late phases (up to ∼ 600 days). Prominent spectral lines are indicated by colours. Phases are given relative to the estimated explosion epochs. All spectra are redshift-corrected, dereddened, normalised, and vertically offset for clarity. In the top-left panel, a model from Boian & Groh (… view at source ↗
read the original abstract

We present the photometric and spectroscopic analysis of the luminous and long-lasting Type IIn supernova (SN) 2019vxm. The SN reaches a peak V-band absolute magnitude of MV = -20.01 +/- 0.13 mag in 35.0 days, and displays slow evolution in both the light curves and spectra, resembling that of long-lived SNe IIn. A mid-infrared (MIR) excess is detected starting from seven months after maximum brightness, suggesting a few 10^-3 solar masses of dust are newly formed at >= 210 days (and up to 0.01 solar masses at +4.5 yr). The spectra are dominated by a blue continuum at early stages, with narrow, symmetric Balmer lines and flash-ionisation emission lines of C III, N III, and He II. Comparing our flash-ionised spectrum with early interacting SN spectral models, we estimate a lower limit for the mass-loss rate of the progenitor of >= 0.01 solar masses per year. A weak P Cygni absorption feature is detected in the H-beta profile of the high-resolution Echelle spectrum at +19.7 d, suggesting the presence of slow-moving (60 +/- 10 km/s), unshocked circumstellar material (CSM) arising from the pre-SN wind of the progenitor. The H-alpha and H-beta profiles gradually evolve and become broader and asymmetric, showing a progressively increasing blueshift, with a clear flux deficit in the red wings of the broad velocity component after +102 days. Our observed bolometric light curve before about 100 days can be well fitted by a power-law function (L(t) = 2 x 10^44 (t/day)^-0.49 erg/s), which is very similar to SN 2010jl.

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

1 major / 2 minor

Summary. The manuscript presents photometric and spectroscopic observations of the luminous, long-lived Type IIn supernova SN 2019vxm. It reports a peak V-band absolute magnitude of MV = -20.01 ± 0.13 mag reached at 35 days post-explosion, slow light-curve and spectral evolution resembling other long-lived SNe IIn, a mid-infrared excess starting at +7 months indicating newly formed dust (a few 10^{-3} M_⊙ at ≥210 days), early flash-ionization lines (C III, N III, He II) plus narrow symmetric Balmer lines, a lower limit on progenitor mass-loss rate of ≥0.01 M_⊙ yr^{-1} obtained by comparing the flash-ionized spectrum to published early-interacting SN models, a weak P Cygni absorption in Hβ at +19.7 d indicating slow (60 ± 10 km s^{-1}) unshocked CSM, gradual broadening and blueshift of Hα/Hβ profiles, and a pre-+100 d bolometric light curve well described by the empirical power-law L(t) = 2 × 10^{44} (t/day)^{-0.49} erg s^{-1}, similar to SN 2010jl.

Significance. If the observational results hold, the paper adds a well-observed example of a luminous long-lived SN IIn with early flash features and MIR dust signature, useful for building the sample of events with quantified progenitor mass-loss constraints. Direct measurements (peak magnitude, line profiles, MIR excess) are supported by the described data. The power-law fit is presented as an empirical description. The mass-loss-rate lower limit, however, rests on the applicability of existing spectral models whose assumed wind-like density profile, geometry, and ionization balance may not match the actual CSM around SN 2019vxm.

major comments (1)
  1. [flash-ionization spectrum comparison / mass-loss rate section] Section on flash-ionization spectrum and mass-loss-rate estimate: the lower limit ≥0.01 M_⊙ yr^{-1} is derived solely by matching the observed C III, N III, He II, and narrow Balmer features to published early-interacting SN spectral models. No quantitative test is provided of how deviations in CSM geometry (e.g., clumpy vs. smooth), density gradient, or covering fraction would shift the inferred rate while still reproducing the line ratios at the observed epoch. Because the abstract and text present this value as a key result without bounding such systematics, the robustness of the lower limit cannot be assessed from the manuscript alone.
minor comments (2)
  1. [abstract] Abstract: the power-law normalization is written as '2 x 10^44'; confirm whether this is the exact best-fit value or a rounded approximation, and state the fit range explicitly.
  2. [discussion of progenitor mass loss] The manuscript labels the mass-loss rate a 'lower limit' but does not discuss alternative models or parameter variations that could raise or lower the bound; adding a short paragraph on this would strengthen the claim.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback on our manuscript. We address the single major comment point by point below.

read point-by-point responses

  1. Referee: Section on flash-ionization spectrum and mass-loss-rate estimate: the lower limit ≥0.01 M_⊙ yr^{-1} is derived solely by matching the observed C III, N III, He II, and narrow Balmer features to published early-interacting SN spectral models. No quantitative test is provided of how deviations in CSM geometry (e.g., clumpy vs. smooth), density gradient, or covering fraction would shift the inferred rate while still reproducing the line ratios at the observed epoch. Because the abstract and text present this value as a key result without bounding such systematics, the robustness of the lower limit cannot be assessed from the manuscript alone.

    Authors: We thank the referee for raising this point on the robustness of the mass-loss-rate lower limit. The value is obtained by direct comparison of the observed flash-ionization features (C III, N III, He II, and narrow Balmer lines) to the published early-interacting SN spectral models that best reproduce the line ratios and strengths at the observed epoch. These models assume a wind-like density profile, which is consistent with the narrow, symmetric Balmer lines in our data. We acknowledge that a quantitative exploration of alternative geometries (clumpy vs. smooth), density gradients, or covering fractions would require new dedicated radiative-transfer calculations that lie beyond the scope of this observational paper. The estimate is presented explicitly as a lower limit to reflect such uncertainties. In the revised manuscript we will expand the relevant section and abstract to state the model assumptions more explicitly and to emphasize the conservative nature of the lower limit, allowing readers to better assess its robustness. revision: partial

Circularity Check

0 steps flagged

No significant circularity; all central quantities are direct observations or comparisons to external models

full rationale

The mass-loss rate lower limit is obtained by direct comparison of the observed flash-ionized spectrum (C III, N III, He II lines) to independently published early-interacting SN spectral models; the paper does not derive or fit those models itself. The bolometric light curve is empirically fitted to a power-law form using the observed photometry, presented as a description rather than a first-principles prediction. Peak magnitude, evolution timescales, and velocity measurements are all direct observational results. No self-citations, self-definitional steps, or fitted inputs renamed as predictions appear in the derivation chain. The analysis remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard domain assumptions required to convert observed fluxes to absolute magnitudes and luminosities, plus the applicability of published spectral models for mass-loss estimation; two explicit fitted parameters appear in the reported power-law description of the bolometric light curve.

free parameters (2)
  • power-law normalization = 2 x 10^44
    Value 2 x 10^44 erg/s chosen to match the observed bolometric luminosity scale before 100 days.
  • power-law index = -0.49
    Value -0.49 obtained by fitting the early bolometric light curve.
axioms (2)
  • domain assumption Standard assumptions on distance, Galactic and host extinction, and cosmology are used to derive absolute magnitudes and bolometric luminosities.
    Required to report MV = -20.01 and the bolometric light curve.
  • domain assumption Published early-interacting SN spectral models accurately represent the flash-ionization physics and circumstellar geometry for this event.
    Invoked to convert observed line strengths into the mass-loss rate lower limit.

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Reference graph

Works this paper leans on

167 extracted references · 153 canonical work pages · 71 internal anchors

  1. [1]

    The Expulsion of Stellar Envelopes in Core-Collapse Supernovae

    The Expulsion of Stellar Envelopes in Core-Collapse Supernovae. , keywords =. doi:10.1086/306571 , archivePrefix =. astro-ph/9807046 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/306571

  2. [2]

    Lick Obs. Tech. Rep. 66 , year = 1993, volume =

    1993

  3. [3]

    , keywords =

    The importance of atmospheric differential refraction in spectrophotometry. , keywords =. doi:10.1086/131052 , adsurl =

    work page doi:10.1086/131052

  4. [4]

    , year = 1983, month = sep, volume =

    The determination of cloud masses and dust characteristics from submillimetre thermal emission. , year = 1983, month = sep, volume =

    1983

  5. [5]

    , year = 1997, month = jan, volume =

    Optical Spectra of Supernovae. , year = 1997, volume = 35, pages =. doi:10.1146/annurev.astro.35.1.309 , adsurl =

    work page doi:10.1146/annurev.astro.35.1.309 1997

  6. [6]

    , keywords =

    Optical Properties of Interstellar Graphite and Silicate Grains. , keywords =. doi:10.1086/162480 , adsurl =

    work page doi:10.1086/162480

  7. [7]

    , keywords =

    Spectroscopic Constraints on the Properties of Dust in Active Galactic Nuclei. , keywords =. doi:10.1086/172149 , adsurl =

    work page doi:10.1086/172149

  8. [8]

    , keywords =

    Mass extinction coefficients of various submicron amorphous carbon grains: Tabulated values from 40 NM to 2 mm. , keywords =

  9. [9]

    , keywords =

    A new subclass of Type II supernovae?. , keywords =

  10. [10]

    , keywords =

    Emission from Circumstellar Interaction in Normal Type II Supernovae. , keywords =. doi:10.1086/173557 , adsurl =

    work page doi:10.1086/173557

  11. [11]

    , keywords =

    Supernovae in dense winds. , keywords =. doi:10.1023/A:1000847125928 , adsurl =

    work page doi:10.1023/a:1000847125928

  12. [12]

    , keywords =

    The type IIn supernova 1995G: interaction with the circumstellar medium. , keywords =. doi:10.1046/j.1365-8711.2002.05366.x , archivePrefix =. astro-ph/0201483 , primaryClass =

    work page doi:10.1046/j.1365-8711.2002.05366.x 2002

  13. [13]

    , keywords =

    A luminous stellar outburst during a long-lasting eruptive phase first, and then SN IIn 2018cnf. , keywords =. doi:10.1051/0004-6361/201935420 , archivePrefix =. 1906.00814 , primaryClass =

    work page doi:10.1051/0004-6361/201935420 1906

  14. [14]

    D., 2012, @doi [ ] 10.1111/j.1365-2966.2012.21871.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.426.3282M 426, 3282

    Berkeley Supernova Ia Program - I. Observations, data reduction and spectroscopic sample of 582 low-redshift Type Ia supernovae. , keywords =. doi:10.1111/j.1365-2966.2012.21270.x , archivePrefix =. 1202.2128 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21270.x 2012

  15. [15]

    Transient Name Server Classification Report , keywords =

    Transient Classification Report for 2019-12-02. Transient Name Server Classification Report , keywords =

    2019

  16. [16]

    Transient Name Server Discovery Report , keywords =

    ASAS-SN Transient Discovery Report for 2019-12-01. Transient Name Server Discovery Report , keywords =

    2019

  17. [17]

    SN 2019vxm: A Shocking Coincidence between Fermi and TESS

    SN 2019vxm: A Shocking Coincidence between Fermi and TESS. , keywords =. doi:10.3847/1538-4357/ae6245 , archivePrefix =. 2511.15975 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ae6245

  18. [18]

    Astronomische Nachrichten , keywords =

    SNe 2019vxm and 2020tlf: two luminous type II Supernovae with signatures of circumstellar interaction. Astronomische Nachrichten , keywords =. doi:10.1002/asna.20230166 , adsurl =

    work page doi:10.1002/asna.20230166

  19. [19]

    Astrophysical Bulletin , keywords =

    Progress in Supernovae Studies with the 2.5-m Telescope at the Caucasus Mountain Observatory of SAI MSU. Astrophysical Bulletin , keywords =. doi:10.1134/S1990341323700232 , adsurl =

    work page doi:10.1134/s1990341323700232

  20. [20]

    , keywords =

    High-cadence, early-time observations of core-collapse supernovae from the TESS prime mission. , keywords =. doi:10.1093/mnras/staa3675 , archivePrefix =. 2010.06596 , primaryClass =

    work page doi:10.1093/mnras/staa3675 2010

  21. [21]

    American Astronomical Society Meeting Abstracts \#223 , year = 2014, series =

    All Sky Automated Survey for SuperNovae (ASAS-SN or ``Assassin''). American Astronomical Society Meeting Abstracts \#223 , year = 2014, series =

    2014

  22. [22]

    The All-Sky Automated Survey for Supernovae (ASAS-SN) Light Curve Server v1.0

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/aa80d9

  23. [23]

    HEAsoft: Unified Release of FTOOLS and XANADU

  24. [24]

    , archivePrefix = "arXiv", eprint =

    AT 2017be - a new member of the class of intermediate-luminosity red transients. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/sty2070 , adsurl =

    work page doi:10.1093/mnras/sty2070

  25. [25]

    arXiv e-prints , keywords =

    The Pan-STARRS1 Surveys. arXiv e-prints , keywords =

  26. [26]

    , keywords =

    The Pan-STARRS1 Database and Data Products. , keywords =. doi:10.3847/1538-4365/abb82d , archivePrefix =. 1612.05243 , primaryClass =

    work page doi:10.3847/1538-4365/abb82d

  27. [27]

    , keywords =

    Pan-STARRS Pixel Processing: Detrending, Warping, Stacking. , keywords =. doi:10.3847/1538-4365/abb82b , archivePrefix =. 1612.05245 , primaryClass =

    work page doi:10.3847/1538-4365/abb82b

  28. [28]

    , keywords =

    The Pan-STARRS Data-processing System. , keywords =. doi:10.3847/1538-4365/abb829 , archivePrefix =. 1612.05240 , primaryClass =

    work page doi:10.3847/1538-4365/abb829

  29. [29]

    , keywords =

    Pan-STARRS Photometric and Astrometric Calibration. , keywords =. doi:10.3847/1538-4365/abb82a , archivePrefix =. 1612.05242 , primaryClass =

    work page doi:10.3847/1538-4365/abb82a

  30. [30]

    , keywords =

    Pan-STARRS Pixel Analysis: Source Detection and Characterization. , keywords =. doi:10.3847/1538-4365/abb82c , archivePrefix =. 1612.05244 , primaryClass =

    work page doi:10.3847/1538-4365/abb82c

  31. [31]

    ATLAS: A High-Cadence All-Sky Survey System

    ATLAS: A High-cadence All-sky Survey System. , keywords =. doi:10.1088/1538-3873/aabadf , archivePrefix =. 1802.00879 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/aabadf

  32. [32]

    , keywords =

    Design and Operation of the ATLAS Transient Science Server. , keywords =. doi:10.1088/1538-3873/ab936e , archivePrefix =. 2003.09052 , primaryClass =

    work page doi:10.1088/1538-3873/ab936e 2003

  33. [33]

    Transient Name Server AstroNote , keywords =

    Release of the ATLAS Forced Photometry server for public use. Transient Name Server AstroNote , keywords =

  34. [34]

    2018-2020

    The ASAS-SN bright supernova catalogue - V. 2018-2020. , keywords =. doi:10.1093/mnras/stad355 , archivePrefix =. 2210.06492 , primaryClass =

    work page doi:10.1093/mnras/stad355 2018

  35. [35]

    Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology

    Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology. , keywords =. doi:10.1086/513700 , archivePrefix =. astro-ph/0603449 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/513700

  36. [36]

    F., & Finkbeiner, D

    Measuring Reddening with Sloan Digital Sky Survey Stellar Spectra and Recalibrating SFD. , keywords =. doi:10.1088/0004-637X/737/2/103 , archivePrefix =. 1012.4804 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/737/2/103

  37. [37]

    WISeREP - An Interactive Supernova Data Repository

    WISeREP An Interactive Supernova Data Repository. , keywords =. doi:10.1086/666656 , archivePrefix =. 1204.1891 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/666656

  38. [38]

    Pushing the Boundaries of Conventional Core-Collapse Supernovae: The Extremely Energetic Supernova SN 2003ma

    Pushing the Boundaries of Conventional Core-collapse Supernovae: The Extremely Energetic Supernova SN 2003ma. , keywords =. doi:10.1088/0004-637X/729/2/88 , archivePrefix =. 0911.2002 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/729/2/88 2002

  39. [39]

    Multi-wavelength Observations of the Enduring Type IIn Supernovae 2005ip and 2006jd

    Multi-wavelength Observations of the Enduring Type IIn Supernovae 2005ip and 2006jd. , keywords =. doi:10.1088/0004-637X/756/2/173 , archivePrefix =. 1206.5575 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/756/2/173

  40. [40]

    Coronal lines and dust formation in SN 2005ip: Not the brightest, but the hottest Type IIn supernova

    Coronal Lines and Dust Formation in SN 2005ip: Not the Brightest, but the Hottest Type IIn Supernova. , keywords =. doi:10.1088/0004-637X/695/2/1334 , archivePrefix =. 0809.5079 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/695/2/1334

  41. [41]

    SN 2006gy: Discovery of the most luminous supernova ever recorded, powered by the death of an extremely massive star like Eta Carinae

    SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by the Death of an Extremely Massive Star like Carinae. , keywords =. doi:10.1086/519949 , archivePrefix =. astro-ph/0612617 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/519949

  42. [42]

    SN 2006gy: An extremely luminous supernova in the galaxy NGC 1260

    SN 2006gy: An Extremely Luminous Supernova in the Galaxy NGC 1260. , keywords =. doi:10.1086/516749 , archivePrefix =. astro-ph/0612408 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/516749

  43. [43]

    SN 2006tf: Precursor Eruptions and the Optically Thick Regime of Extremely Luminous Type IIn Supernovae

    SN 2006tf: Precursor Eruptions and the Optically Thick Regime of Extremely Luminous Type IIn Supernovae. , keywords =. doi:10.1086/591021 , archivePrefix =. 0804.0042 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591021

  44. [44]

    SN 2010jl: Optical to hard X-ray observations reveal an explosion embedded in a ten solar mass cocoon

    SN 2010jl: Optical to Hard X-Ray Observations Reveal an Explosion Embedded in a Ten Solar Mass Cocoon. , keywords =. doi:10.1088/0004-637X/781/1/42 , archivePrefix =. 1307.2247 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/781/1/42

  45. [45]

    SN2008am: A Super-Luminous Type IIn Supernova

    SN 2008am: A Super-luminous Type IIn Supernova. , keywords =. doi:10.1088/0004-637X/729/2/143 , archivePrefix =. 1101.3581 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/729/2/143

  46. [46]

    , keywords =

    The long-lived Type IIn SN 2015da: Infrared echoes and strong interaction within an extended massive shell. , keywords =. doi:10.1051/0004-6361/201936553 , archivePrefix =. 1908.08580 , primaryClass =

    work page doi:10.1051/0004-6361/201936553 1908

  47. [47]

    , keywords =

    SN 2015da: late-time observations of a persistent superluminous Type IIn supernova with post-shock dust formation. , keywords =. doi:10.1093/mnras/stae726 , archivePrefix =. 2312.00253 , primaryClass =

    work page doi:10.1093/mnras/stae726

  48. [48]

    , keywords =

    A long life of excess: The interacting transient SN 2017hcc. , keywords =. doi:10.1051/0004-6361/202244565 , archivePrefix =. 2210.14076 , primaryClass =

    work page doi:10.1051/0004-6361/202244565

  49. [49]

    Handbook of Supernovae , year = 2017, editor =

    Interacting Supernovae: Types IIn and Ibn. Handbook of Supernovae , year = 2017, editor =. doi:10.1007/978-3-319-21846-5_38 , adsurl =

    work page doi:10.1007/978-3-319-21846-5_38 2017

  50. [50]

    , keywords =

    SN 2016iog: A fast-declining Type II-L supernova with an ultra-faint tail persistently interacting with circumstellar material. , keywords =. doi:10.1051/0004-6361/202556330 , archivePrefix =. 2511.12929 , primaryClass =

    work page doi:10.1051/0004-6361/202556330

  51. [51]

    , keywords =

    SN 2018hfm: a low-energy Type II supernova with prominent signatures of circumstellar interaction and dust formation. , keywords =. doi:10.1093/mnras/stab3007 , archivePrefix =. 2110.10440 , primaryClass =

    work page doi:10.1093/mnras/stab3007

  52. [52]

    VizieR Online Data Catalog: WISE All-Sky Data Release (Cutri+ 2012)

    2012

  53. [53]

    Evidence for Asphericity in the Type IIn Supernova 1998S

    Evidence for Asphericity in the Type IIN Supernova SN 1998S. , keywords =. doi:10.1086/308910 , archivePrefix =. astro-ph/9908040 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308910

  54. [54]

    A Wolf-Rayet-like progenitor of supernova SN 2013cu from spectral observations of a wind

    A Wolf-Rayet-like progenitor of SN 2013cu from spectral observations of a stellar wind. , keywords =. doi:10.1038/nature13304 , archivePrefix =. 1406.7640 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature13304

  55. [55]

    Explosion of red-supergiant stars: influence of the atmospheric structure on shock breakout and the early-time supernova radiation

    Explosion of red-supergiant stars: Influence of the atmospheric structure on shock breakout and early-time supernova radiation. , keywords =. doi:10.1051/0004-6361/201730942 , archivePrefix =. 1704.01697 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730942

  56. [56]

    PTF11iqb: Cool supergiant mass loss that bridges the gap between Type IIn and normal supernovae

    PTF11iqb: cool supergiant mass-loss that bridges the gap between Type IIn and normal supernovae. , keywords =. doi:10.1093/mnras/stv354 , archivePrefix =. 1501.02820 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv354

  57. [57]

    Early Emission from the Type IIn Supernova 1998S at High Resolution

    Early Emission from the Type IIn Supernova 1998S at High Resolution. , keywords =. doi:10.1088/0004-637X/806/2/213 , archivePrefix =. 1408.1404 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/806/2/213

  58. [58]

    , keywords =

    SN 2024cld: unveiling the complex mass-loss histories of evolved supergiant progenitors to core collapse supernovae. , keywords =. doi:10.1093/mnras/staf2261 , archivePrefix =. 2510.27631 , primaryClass =

    work page doi:10.1093/mnras/staf2261

  59. [59]

    , keywords =

    The Prevalence and Influence of Circumstellar Material around Hydrogen-rich Supernova Progenitors. , keywords =. doi:10.3847/1538-4357/acd8be , archivePrefix =. 2212.03313 , primaryClass =

    work page doi:10.3847/1538-4357/acd8be

  60. [60]

    SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features

    Massive stars exploding in a He-rich circumstellar medium: XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features. , keywords =. doi:10.1051/0004-6361/202558014 , archivePrefix =. 2511.04337 , primaryClass =

    work page doi:10.1051/0004-6361/202558014

  61. [61]

    Caltech Core-Collapse Project (CCCP) observations of type IIn supernovae: typical properties and implications for their progenitor stars

    Caltech Core-Collapse Project (CCCP) Observations of Type IIn Supernovae: Typical Properties and Implications for Their Progenitor Stars. , keywords =. doi:10.1088/0004-637X/744/1/10 , archivePrefix =. 1010.2689 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/744/1/10

  62. [62]

    , keywords =

    Broad emission lines from the opaque electron-scattering environment of SN 1998S. , keywords =. doi:10.1111/j.1365-2966.2001.04717.x , archivePrefix =. astro-ph/0106234 , primaryClass =

    work page doi:10.1111/j.1365-2966.2001.04717.x 2001

  63. [63]

    High Density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The first 1100 days

    High-density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The First 1100 Days. , keywords =. doi:10.1088/0004-637X/797/2/118 , archivePrefix =. 1312.6617 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/797/2/118

  64. [64]

    Dust Formation and He II 4686 emission in the Dense Shell of the Peculiar Type Ib Supernova 2006jc

    Dust Formation and He II 4686 Emission in the Dense Shell of the Peculiar Type Ib Supernova 2006jc. , keywords =. doi:10.1086/587860 , archivePrefix =. 0704.2249 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/587860

  65. [65]

    Early Dust Formation and a Massive Progenitor for SN 2011ja?

    Early dust formation and a massive progenitor for SN 2011ja?. , keywords =. doi:10.1093/mnras/stw164 , archivePrefix =. 1509.06379 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw164

  66. [66]

    , keywords =

    Progenitors of early-time interacting supernovae. , keywords =. doi:10.1093/mnras/staa1540 , archivePrefix =. 2001.07651 , primaryClass =

    work page doi:10.1093/mnras/staa1540 2001

  67. [67]

    V., Poznanski D., Wang X., Ganeshalingam M., Mannucci F., 2011, @doi [ ] 10.1111/j.1365-2966.2011.18162.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.412.1473L 412, 1473

    Nearby supernova rates from the Lick Observatory Supernova Search - II. The observed luminosity functions and fractions of supernovae in a complete sample. , keywords =. doi:10.1111/j.1365-2966.2011.18160.x , archivePrefix =. 1006.4612 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18160.x 2011

  68. [68]

    Catalogues and fractions of supernovae in a complete sample

    Supernovae at distances <40 Mpc: I. Catalogues and fractions of supernovae in a complete sample. , keywords =. doi:10.1051/0004-6361/202452684 , archivePrefix =. 2504.04393 , primaryClass =

    work page doi:10.1051/0004-6361/202452684

  69. [69]

    Supernova rate in the local Universe

    Supernovae at distances <40 Mpc: II. Supernova rate in the local Universe. , keywords =. doi:10.1051/0004-6361/202452685 , archivePrefix =. 2504.04507 , primaryClass =

    work page doi:10.1051/0004-6361/202452685

  70. [70]

    Supernova rates from the SUDARE VST-OmegaCAM search. I. Rates per unit volume. , keywords =. doi:10.1051/0004-6361/201526712 , archivePrefix =. 1509.04496 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201526712

  71. [71]

    The death of massive stars - II. Observational constraints on the progenitors of type Ibc supernovae

    The death of massive stars - II. Observational constraints on the progenitors of Type Ibc supernovae. , keywords =. doi:10.1093/mnras/stt1612 , archivePrefix =. 1301.1975 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1612 1975

  72. [72]

    V., Poznanski D., Wang X., Ganeshalingam M., Mannucci F., 2011, @doi [ ] 10.1111/j.1365-2966.2011.18162.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.412.1473L 412, 1473

    Observed fractions of core-collapse supernova types and initial masses of their single and binary progenitor stars. , keywords =. doi:10.1111/j.1365-2966.2011.17229.x , archivePrefix =. 1006.3899 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.17229.x 2011

  73. [73]

    Progenitors of core-collapse supernovae

    Progenitors of Core-Collapse Supernovae. , keywords =. doi:10.1146/annurev-astro-082708-101737 , archivePrefix =. 0908.0700 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-082708-101737

  74. [74]

    , keywords =

    Type IIn supernova light-curve properties measured from an untargeted survey sample. , keywords =. doi:10.1051/0004-6361/201936097 , archivePrefix =. 1906.05812 , primaryClass =

    work page doi:10.1051/0004-6361/201936097 1906

  75. [75]

    Royal Society Open Science , year = 2020, month = jul, volume =

    Supernovae and transients with circumstellar interaction. Royal Society Open Science , year = 2020, month = jul, volume =. doi:10.1098/rsos.200467 , adsurl =

    work page doi:10.1098/rsos.200467 2020

  76. [76]

    Carnegie Supernova Project: Observations of Type IIn supernovae

    Carnegie Supernova Project: Observations of Type IIn supernovae. , keywords =. doi:10.1051/0004-6361/201321180 , archivePrefix =. 1304.3038 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321180

  77. [77]

    Metallicity at the explosion sites of interacting transients

    Metallicity at the explosion sites of interacting transients. , keywords =. doi:10.1051/0004-6361/201525989 , archivePrefix =. 1505.04719 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525989

  78. [78]

    D., 2012, @doi [ ] 10.1111/j.1365-2966.2012.21871.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.426.3282M 426, 3282

    SN 2009kn - the twin of the Type IIn supernova 1994W. , keywords =. doi:10.1111/j.1365-2966.2012.21224.x , archivePrefix =. 1205.0353 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21224.x 2012

  79. [79]

    , keywords =

    SN 2020pvb: A Type IIn-P supernova with a precursor outburst. , keywords =. doi:10.1051/0004-6361/202348790 , archivePrefix =. 2402.02924 , primaryClass =

    work page doi:10.1051/0004-6361/202348790

  80. [80]

    SN 2011ht: Confirming a Class of Interacting Supernovae with Plateau Light Curves (Type IIn-P)

    SN 2011ht: confirming a class of interacting supernovae with plateau light curves (Type IIn-P). , keywords =. doi:10.1093/mnras/stt360 , archivePrefix =. 1209.0821 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt360

Showing first 80 references.