HCO$^+$ and the Effect of Mixing in SN 1987A

A. M. S. Richards (Manchester); Cardiff; C. Fransson (Stockholm University); F. D. Priestley (Cardiff); H. L. Gomez (Cardiff); H. M. Davies; J. Larsson (KTH Royal Institute of Technology); Maynooth University); M. J. Barlow (UCL); M. Matsuura

REVIEW 3 major objections 5 minor 166 references

HCO$^+$ and the Effect of Mixing in SN 1987A

T0 review · 3 major / 5 minor · reviewed 2026-08-01 · deepseek-v4-flash

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

Pith's one-line read SN 1987A's HCO+ emission shows hydrogen was mixed into the remnant's carbon–oxygen core.

desk verdict First resolved HCO+ map in SN 1987A is a real advance, but the mass and mixing conclusions lean on a J=4-3 detection that the paper's own error budget makes marginal. read the letter →

arxiv 2607.26189 v1 pith:5AEYO4YH submitted 2026-07-28 astro-ph.SR

H. M. Davies , M. Matsuura , H. L. Gomez (Cardiff) , A. M. S. Richards (Manchester) , P. Cigan (George Mason University , United States Naval Observatory) , R. Indebetouw (University of Virginia , National Radio Astronomy Observatory)

show 7 more authors

F. D. Priestley (Cardiff) R. Wesson (UCL Cardiff Maynooth University) M. J. Barlow (UCL) J. Larsson (KTH Royal Institute of Technology) C. Fransson (Stockholm University)

This is my paper · ORCID

classification astro-ph.SR

keywords HCO+SN1987AsupernovaremnantsmolecularejectachemicalmixingastrochemistryALMAradiativetransfer

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

SN 1987A is a rare supernova remnant where HCO+ is detected in the ejecta itself, and this paper uses that fact to read the explosion's mixing history. The authors establish that the HCO+ J=3–2 emission is co-spatial with CO, quantify the HCO+ mass at 3–9 × 10^-6 solar masses from two rotational transitions, and argue that the abundance ratio to CO can only be reached if hydrogen from the star's envelope was transported inward to the carbon- and oxygen-rich nuclear zones. This makes HCO+ a tracer of mixing that other remnant observations do not provide. A simple formation-rate estimate falls short of the observed mass unless the ionisation rate is higher than the canonical interstellar value or additional hydrogen sits with the CO — either way, hydrogen must be co-located with CO.

What carries the argument

The load-bearing object is HCO+ itself, a molecular ion that requires carbon, oxygen, and hydrogen to meet: the proposed formation route CO + H3+ → HCO+ + H2. Two ALMA lines (J=3–2 and J=4–3) feed a non-local-thermodynamic-equilibrium radiative-transfer calculation that turns observed intensities into column density and kinetic temperature, with the H2 collision-partner density fixed at 10^6 or 10^5 cm^-3. Spatial comparison with CO, SiO, Hα, and H2 isolates where the ion forms, and a timescale-integrated formation-rate estimate tests whether the reaction can account for the observed mass. The electron destruction channel (dissociative recombination) sets the condition that HCO+ survives onl

What would settle it

High-spatial-resolution maps of H2 emission in the same velocity channels as the HCO+ clumps: if the H2 there is far below 10^5 cm^-3, or absent, the adopted collision densities collapse and the inferred HCO+ mass and mixing conclusion no longer hold. A cleaner test would be detection of the HCO+ J=1–0 line: its intensity, combined with J=3–2 and J=4–3, would break the column-density/temperature degeneracy and settle the mass without fixing the collision density.

Watch

Extended reading notes

Core claim

The central claim is that HCO+ in SN 1987A exists because the ejecta are not radially stratified: hydrogen reached the CO-rich nuclear zones before and during the explosion. High-resolution ALMA maps show the J=3–2 HCO+ emitting region overlaps the CO J=2–1 emission (Spearman correlation 0.72), while the brighter HCO+ peaks sit apart from Hα and H2, placing HCO+ in compact, mildly ionised gas inside the ejecta. Using the J=3–2 and J=4–3 line intensities with a non-LTE radiative-transfer calculation, the paper derives column density and kinetic temperature for two assumed H2 collision densities, giving an HCO+ mass of 3–9 × 10^-6 solar masses and a fractional abundance relative to CO of 3×10^

Load-bearing premise

The HCO+ mass rests on an assumed H2 collisional-partner density that is obtained by spreading the star's entire 6-solar-mass hydrogen envelope uniformly through the ejecta volume — effectively assuming hydrogen is already everywhere, which is exactly the mixing the paper sets out to infer.

Editorial extensions

If this is right

HCO+ becomes a quantitative tracer of hydrogen transport into metal-rich ejecta, giving models of Rayleigh–Taylor and smaller-scale mixing a new observable to match.
The HCO+/CO ratio of 3×10^-6 to 3×10^-4 sets a floor on how much hydrogen must be mixed into the C/O zones; reproducing it requires either an elevated H2 ionisation rate (about 3×10^-16 s^-1) or additional co-located H2.
Because HCO+ tracks CO spatially and forms from CO, CO maps can be used to predict where HCO+ emission should appear in other remnants.
The non-coincidence of HCO+ with Hα and H2 implies HCO+ marks shielded, low-ionisation gas and supports UV irradiation, not electron collisions, as the H2 excitation mechanism in SN 1987A's ejecta.

Reading between the lines

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

If the true H2 distribution is clumpy rather than uniform, the density used in the radiative-transfer calculation could be locally higher or lower; high-resolution H2 maps would test whether the assumed 10^5–10^6 cm^-3 densities coincide with the HCO+ clumps.
The same technique applied to other young core-collapse remnants with detectable molecular ejecta could show whether deep hydrogen mixing is a generic feature of the explosion mechanism or peculiar to SN 1987A's blue supergiant progenitor.
A full chemical network including CH+, OH+, H2O, and CO+ would likely change the inferred required hydrogen fraction; the paper's single-reaction estimate is deliberately minimal, so the mixing conclusion is more robust than the specific mass of hydrogen inferred.

Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

Colleague — worth a look, but with eyes open. The paper gives the first resolved HCO+ J=3-2 map of SN 1987A's ejecta, plus a J=4-3 measurement, and argues that HCO+ requires hydrogen mixed into the C/O zones. The qualitative case is solid: the J=3-2 emission is clearly detected, clumpy, co-spatial with CO (Spearman 0.72), and sits where H-alpha is fainter. That is a genuine new observational result, and it does imply some hydrogen transport into the metal-rich layers, given HCO+ needs H, C and O in the same gas.

The quantitative anchor is the problem. The RADEX mass of 3–9e-6 M_sun rests on the J=4-3 line, but that line's significance collapses under the paper's own uncertainties. Table 2 gives continuum error 2.54e-20 for J=4-3, calibration 0.40, RMS 0.24; combining them gives ~2.6e-20, so the 5.69e-20 line is ~2 sigma. The text quotes ±1.0e-20, inconsistent with the table. The MC SED fit gives an even larger continuum uncertainty (0.92e-19). So the two-line RADEX constraint on T_kin and column is not secure; the mass range is likely much broader and not robust.

Also note the H2 collisional density in RADEX is derived by spreading the whole 6 M_sun hydrogen envelope uniformly through the ejecta. That assumes hydrogen is everywhere, which is the conclusion. Switching 1e6 vs 1e5 cm^-3 changes the mass by only a factor ~3, but the deeper problem is unquantified: if hydrogen is only in clumps, the local density and excitation change. The chemistry feasibility test is order-of-magnitude and needs a factor-ten boost in ionization rate to match observations, so the 'moderate mixing' language overreaches.

None of this kills the main point. The data show HCO+ exists where CO is, and that demands some hydrogen mixing. But the specific mass and mixing fraction should be treated as illustrative, not measured. The paper needs a corrected error budget and a clearer statement of assumptions before the numbers go into the literature.

Who's it for? SN remnant and astrochemistry people. The resolved map and the CO-HCO+ correlation will be useful benchmarks. I'd send it to a referee, but the referee should insist on fixing the error propagation and softening the quantitative claims.

Referee Report

3 major / 5 minor

Summary. The paper reports ALMA observations of HCO+ J=3-2 and J=4-3 emission from the ejecta of SN 1987A. It finds the J=3-2 emission to be clumpy and co-spatial with CO, with a Spearman correlation of 0.72, and less similar to SiO and Hα. Using RADEX non-LTE radiative transfer on the two line intensities, the authors derive an HCO+ column density and mass of 3–9×10^-6 M_sun (depending on the adopted H2 collisional density, 1e5 or 1e6 cm^-3). They compare this to the CO mass and conclude that the fractional abundance M_HCO+/M_CO = 3×10^-6–3×10^-4 implies that a moderate amount of hydrogen was mixed into the carbon- and oxygen-rich zones. A chemical feasibility estimate for formation via CO + H3+ yields ~1e-7 M_sun, an order of magnitude below the claimed mass unless the H2 ionization rate is raised by an order of magnitude.

Significance. If the quantitative result were robust, this would be an important observational constraint: HCO+ is a direct tracer of hydrogen transport into the metal-rich core of an SN remnant, and no other remnant currently offers a comparable measurement. The paper's qualitative contributions are solid and should be credited: the spatially resolved ALMA detection of HCO+, the morphological comparison with CO/SiO/Hα/H2, and the explicit attempt to connect the observed molecular gas to hydrodynamic mixing scenarios. However, the quantitative anchor for the central claim—the HCO+ mass and the inferred 'moderate' hydrogen mixing—is currently too fragile. The J=4-3 detection is marginal under the paper's own error budget, and the formation-rate estimate does not independently validate the mass. The paper is worth pursuing, but the load-bearing quantitative steps need substantial revision.

major comments (3)

[§3.4 / Table 2] The J=4-3 line, which anchors the RADEX mass, is not a secure detection under the paper's own error budget. Table 2 lists σ_cal=0.40, σ_RMS=0.24, and σ_cont=2.54 (10^-20 W/m^2). Propagating in quadrature gives σ≈2.58, so the continuum-subtracted line (5.69×10^-20) is only ≈2.2σ, not the ±1.0 quoted in the text. Moreover, §3.1 gives the MC SED continuum uncertainty at 356 GHz as ±0.92×10^-19, roughly 90% of the continuum; if that uncertainty is used, the line is sub-significant. Since the J=3-2 line alone cannot break the T_kin–N_HCO+ degeneracy, the derived N_HCO+ and mass (3–9×10^-6 M_sun) are not robust. The error budget and the quoted line intensities must be reconciled before the central quantitative claim can be accepted.
[§5.1] The formation-rate 'feasibility test' yields ~1×10^-7 M_sun, an order of magnitude below the adopted 3–9×10^-6 M_sun, and the gap is closed by assuming ζ=3×10^-16 s^-1. Because ζ is not independently constrained for SN ejecta, this does not demonstrate that the observed HCO+ can be formed; it simply adjusts a free parameter. The calculation also assumes spatially uniform CO and H3+, which §5.2 later concedes is unrealistic. Consequently, the abstract's statement that the fractional abundance 'suggests a moderate amount of hydrogen was mixed' is not quantitatively supported by this section. Either an independent constraint on ζ must be provided, or the chemistry should be presented as a qualitative plausibility argument only.
[§4.1] The H2 collisional density input to RADEX is derived by spreading the full 6 M_sun hydrogen envelope uniformly through the ejecta volume. This presumes the very H–C/O co-location the paper aims to infer. The two tested densities (1e5 and 1e6 cm^-3) change the derived mass by only a factor ~3, but they do not sample the possibility that H2 is absent or clumpy in the HCO+ region; if the local n_H2 differs, the excitation solution and N_HCO+ shift. The paper should state explicitly that the mass is conditional on H2 being co-located with HCO+ and should quantify how an H2 filling factor changes the allowed mass. As written, the RADEX mass cannot independently support the 'moderate mixing' conclusion.

minor comments (5)

[Table 2] Errorc for J=4-3 is listed as 2.54×10^-20, but 30% of Cdust=10.17×10^-20 is 3.05×10^-20. Reconcile the table, the text, and the quoted total uncertainty ±1.0×10^-20.
[Fig. 1 / §3.1] The continuum contour levels are inconsistent: the figure caption lists 4.5e-5, 6e-5, 8e-5 Jy/beam, while the text quotes 7e-5 and 9e-4 Jy/beam. Please check and unify.
[§3.4] The J=4-3 Gaussian fit fixes the FWHM to the J=3-2 value (1906 km/s). Given the limited spectral coverage of the J=4-3 data, state explicitly how this assumption affects the integrated intensity and the subsequent RADEX fit.
[§5.1 / §5.2] The paper first assumes a uniform distribution of CO and H3+ for the formation estimate and then argues that uniform mixing is unrealistic. This tension should be acknowledged earlier and the quantitative conclusions adjusted accordingly.
[Abstract / §4.2] The mass range 3–9×10^-6 M_sun and the fractional abundance range spanning two orders of magnitude are conditional on two fixed H2 densities and f=1. The abstract should present these as conditional estimates, not as a measured range.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the HCO+ mass is a RADEX fit to observed line intensities, and the mixing inference is a plausibility argument with acknowledged assumptions.

full rationale

The derivation chain for the central mass estimate is a standard RADEX fit: two observed continuum-subtracted line intensities (Table 2) are compared to RADEX models varying T_kin and N_HCO+, and the mass follows from the fitted column density via M = f Ω N d^2 m (Sects 4.1-4.2). The J=4-3 line is an independent second observable; no equation defines the output mass from the assumed inputs by construction. The H2 collisional density is assumed (Sect. 4.1: 'We estimate an approximate H2 density by calculating it from the mass of the hydrogen envelope... 6 M_sun... and the volume of the ejecta'), but the paper explicitly brackets the assumption with two densities (1e6 and 1e5 cm^-3) and the resulting mass changes by only a factor ~3. The conclusion that hydrogen was mixed is anchored by the detection of HCO+ itself and its co-spatiality with CO, not solely by the assumed density. Section 5.1's formation-rate estimate is presented as a feasibility test, not a prediction; the ionization rate is adjusted to match the observed mass, and the paper flags this ('we suspect this is predominantly due to the assumption that the rate of ionisation of H2 is ζ = 3e-17 s^-1'). The paper also states the uniform-mixing assumption is 'unrealistic' (Sect. 5.2) and that a filling factor of 1 may overestimate the mass (Sect. 5.1), so the limitations are on the table. Self-citations (Matsuura et al. 2017, Larsson et al. 2023, Matsuura et al. 2024) provide prior observational/context data, but are not invoked as an unverified uniqueness theorem and are not load-bearing for the mass fit. The apparent J=4-3 continuum-uncertainty inconsistency (Table 2 vs Sect. 3.1) is a robustness concern, not circularity.

Assumptions & free parameters 5 free parameters · 7 assumptions · 0 invented entities

The central mass/mixing claim rests on several hand-chosen inputs. The H2 collisional density is derived by diluting the whole 6 M_sun hydrogen envelope uniformly over the ejecta volume — an assumption of the very mixing under test. The chemical feasibility estimate agrees with the observed mass only after a post-hoc tenfold boost of the ionisation rate ζ. The dust-continuum subtraction, which removes 64% of the raw J=4-3 flux, depends on a fitted modified-blackbody SED with β, T, M_d free. Filling factor f=1 and a Gaussian line profile with fixed FWHM=1906 km/s close the chain. No invented entities are introduced.

free parameters (5)

H2 collisional partner density n_H2 = 1e6 and 1e5 cm^-3 (two fixed cases)
Input to RADEX (Sect. 4.1); drives the T_kin/N_HCO+ fit and hence the mass. Derived from diluting the 6 M_sun hydrogen envelope uniformly over the ejecta volume, i.e., it presumes the mixing conclusion.
Ionisation rate ζ of H2 = 3e-17 s^-1 (canonical ISM); 3e-16 s^-1 to match observed mass
The formation estimate (Sect. 5.1) gives ~1e-7 M_sun; agreement with 3-9e-6 M_sun requires the order-of-magnitude boost. Post-hoc tuning of the chemistry.
Filling factor f for HCO+ mass = 1
Assumed uniform (Sect. 4.2). Directly multiplies the mass; with clumpy emission (Fig. 3) the mass could be overestimated, as the paper concedes.
Dust SED parameters β, T, M_d = β=2.1, T=17.8 K, M_d=1.4 M_sun
Fitted modified blackbody (MC, 5000 draws) setting the continuum subtracted from both HCO+ lines. The J=4-3 line is only 5.69e-20 vs 10.17e-20 W/m2 continuum, so the mass depends on this fit.
Gaussian FWHM of HCO+ lines = 1906 km/s (fit to J=3-2; fixed for J=4-3)
Used to extrapolate flux beyond the observed ±1650 km/s coverage and as the RADEX line width; a non-Gaussian profile would shift the integrated intensity and mass.

assumptions (7)

domain assumption HCO+ forms predominantly via CO + H3+ → HCO+ + H2 with UMIST rate coefficients; destruction is dominated by dissociative recombination with electrons.
Central chemistry in Sect. 5.1 and 5.3; alternative routes (CH+ + H2O, CO+ + HCO) are set aside.
domain assumption Steady-state H3+ in the SN ejecta follows the ISM relation n_H3+ = ζ n_H2 / k_H3+, with k_H3+ set equal to the HCO+ formation rate k(T).
Sect. 5.1, citing Oka (2006) for dense clouds; applied to SN ejecta without in-situ validation.
ad hoc to paper Ejecta is chemically well-mixed and uniform (uniform CO and H3+ distributions) for the formation estimate; density evolves as t^-3 (homologous expansion).
Stated in Sect. 5.1 and later conceded as 'unrealistic given the partial retention of the progenitor structure' (Sect. 5.2). Load-bearing for the 1e-7 M_sun estimate and the mixing inference.
domain assumption H2 is the dominant collisional partner, and the LAMDA HCO+-H2 collisional rate data apply.
Sect. 4.1; in partially ionised ejecta, electrons could be a significant collider, changing the RADEX excitation solution and derived column/mass.
domain assumption Dust continuum is a single-temperature modified blackbody with κ ∝ λ^-β, and the FIR/sub-mm SED from ~7 years earlier (Herschel) is representative of the HCO+ epoch to within ~3%.
Sect. 3.1; the J=4-3 continuum (10.17e-20 W/m2) is 64% of the raw flux, so the mass depends on this SED assumption. A 44Ti-decay heating correction is applied.
standard math Free expansion at 1300 km/s (from FWHM 1900 km/s via the McCray 1993 relation) gives the ejecta volume; SN distance is 51.2 kpc.
Sect. 4.1 mass/volume/density conversions.
domain assumption Macroscopic mixing from Rayleigh-Taylor instabilities occurs as in 3D CCSN models (Wongwathanarat et al. 2015; Utrobin et al. 2019).
Background for the interpretation (Sects. 1 and 5.2); not derived here.

how reviews work

0 comments

Cite this review

Pith. "Pith review of HCO$^+$ and the Effect of Mixing in SN 1987A." pith.science (2026). https://pith.science/paper/5AEYO4YH

@misc{pith2026260726189,
  author       = {Pith},
  title        = {Pith review of: HCO$^+$ and the Effect of Mixing in SN 1987A},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5AEYO4YH}},
  note         = {Machine review of arXiv:2607.26189}
}

abstract

We present high angular resolution observations of the HCO$^+$ emission in the central ejecta of the supernova remnant SN 1987A using the Atacama Large Millimeter Array (ALMA). We use this to infer the degree and type of mixing required within the ejecta in order to form HCO$^+$. The distribution of the $J=3-2$ HCO$^+$ emission is co-spatial with that of the $J=2-1$ CO emission, with an overlap between their brightest peaks. The correlation between the two molecules is strong and suggests that HCO$^+$ could form from reactions involving CO. We obtain additional observations of the $J=4-3$ HCO$^+$ emission to calculate the mass of HCO$^+$. The estimated HCO$^+$ mass is $3\text{--}9 \times 10^{-6}\,M_{\odot}$. The relatively large fractional abundance of HCO$^+$ with respect to CO ($M_{\mathrm{HCO}^+}/M_{\mathrm{CO}} = 3 \times 10^{-6}\text{--}3 \times 10^{-4}$) suggests that a moderate amount of hydrogen was mixed into the carbon- and oxygen-rich nuclear zones of the ejecta prior to and during the supernova explosion, in addition to large-scale macroscopic mixing.

Figures

Figures reproduced from arXiv: 2607.26189 by the authors.

**Figure 1.** (a) An image of the brightness distribution of the continuum-included J = 3 − 2 HCO+ emission, integrated across its velocity space. Overlain are contours of the 315 GHz continuum emission from Matsuura et al. (2024), which is displayed in panel (b). The continuum consists of dust emission from the ejecta and synchrotron emission from the equatorial ring. The continuum contour levels correspond to 4.5×10−5 , 6×10−… view at source ↗

**Figure 2.** A modified blackbody fit to sub-millimeter and farinfrared observations of thermal dust emission using a Monte-Carlo simulation. Circles show ALMA dust observations in the sub-mm where the temporal span of observations is averaged to SN day 10402 (Cigan et al. 2019). Diamonds show Herschel dust observations in the far-infrared taken on SN days 9090 and 9122 (Matsuura et al. 2015). The blue error bar on the ALMA da… view at source ↗

**Figure 3.** Velocity channel map of the J = 3 − 2 transition of HCO+ emission from velocities beginning at −1950 km s−1 to 1650 km s−1 , binned in 300 km s−1 increments. Each image channel is labelled with the central velocity of the 300 km s−1 bin. Velocities are in LSRK. Continuum is included in this figure which, if uniformly spread out over the region, is ∼ 0.02 mJy beam−1 , i.e. very low level. The typical RMS noise on the… view at source ↗

Figures from the paper (3 more)

**Figure 4.** Figure 4: Comparison of (a) ALMA J = 3–2 HCO+, (b) HST Hα, and (c) JWST H2 emission. (a) Continuum-included J = 3– 2 HCO+ image, obtained by integrating over velocity space. The white contours indicate HCO+ emission levels of 0.3, 0.5 and 0.85 Jy beam−1 km s−1 in all three panel…

**Figure 5.** Figure 5: Upper: Flux density profile for the J = 3 − 2 HCO+ with continuum included in the flux density. This profile was fitted with a gaussian curve to retrieve the FWHM of the line which was calculated to be +1906 km s−1 shown as a black line. Lower: Flux density profile fo…

**Figure 6.** Figure 6: χ 2 distribution for comparisons of RADEX line intensities with observed line fluxes with respect to the RADEX input parameters of kinetic temperature, Tkin, and column density, NHCO+ , of HCO+. (a) and (b) show the results using the continuumsubtracted HCO+ line inte…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

166 extracted references · 18 canonical work pages

[1]

ALMA Partnership et al., 2017, ALMA Cycle 5 Technical Handbook

2017
[6]

Astropy Collaboration et al., 2013, @doi [ ] 10.1051/0004-6361/201322068 , http://adsabs.harvard.edu/abs/2013A

doi:10.1051/0004-6361/201322068 2013
[7]

Astropy Collaboration et al., 2022, @doi [ ] 10.3847/1538-4357/ac7c74 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935..167A 935, 167

doi:10.3847/1538-4357/ac7c74 2022
[10]

L., Safi-Harb S., Jones S., Pignatari M., 2026, arXiv

Boccioli L., Roberti L., Fryer C. L., Safi-Harb S., Jones S., Pignatari M., 2026, arXiv

2026
[11]

Bouchet P., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2770 , https://ui.adsabs.harvard.edu/abs/2024ApJ...965...51B 965, 51

doi:10.3847/1538-4357/ad2770 2024
[12]

CASA Team et al., 2022, @doi [ ] 10.1088/1538-3873/ac9642 , https://ui.adsabs.harvard.edu/abs/2022PASP..134k4501C 134, 114501

doi:10.1088/1538-3873/ac9642 2022
[13]

Cherchneff I., Dwek E., 2009, @doi [ ] 10.1088/0004-637X/703/1/642 , https://ui.adsabs.harvard.edu/abs/2009ApJ...703..642C 703, 642

doi:10.1088/0004-637x/703/1/642 2009
[16]

H., Hirschi R., Murphy L., Kaiser E., Ekstr \"o m S., Georgy C., Meynet G., 2021, @doi [ ] 10.1093/mnrasl/slaa196 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.502L..40F 502, L40

Farrell E., Groh J. H., Hirschi R., Murphy L., Kaiser E., Ekstr \"o m S., Georgy C., Meynet G., 2021, @doi [ ] 10.1093/mnrasl/slaa196 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.502L..40F 502, L40

doi:10.1093/mnrasl/slaa196 2021

Show all 166 references

[17]

Fransson C., et al., 2013, @doi [ ] 10.1088/0004-637X/768/1/88 , https://ui.adsabs.harvard.edu/abs/2013ApJ...768...88F 768, 88

2013 doi
[18]

Fransson C., et al., 2015, @doi [ ] 10.1088/2041-8205/806/1/l19 , 806, L19

2015 doi
[19]

Fransson C., Larsson J., Spyromilio J., Leibundgut B., McCray R., Jerkstrand A., 2016, @doi [ ] 10.3847/2041-8205/821/1/L5 , https://ui.adsabs.harvard.edu/abs/2016ApJ...821L...5F 821, L5

2016 doi
[20]

Gabler M., Wongwathanarat A., Janka H.-T., 2021, @doi [ ] 10.1093/mnras/stab116 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.502.3264G 502, 3264

2021 doi
[21]

H., et al., 2019, @doi [ ] 10.1051/0004-6361/201833720 , https://ui.adsabs.harvard.edu/abs/2019A&A...627A..24G 627, A24

Groh J. H., et al., 2019, @doi [ ] 10.1051/0004-6361/201833720 , https://ui.adsabs.harvard.edu/abs/2019A&A...627A..24G 627, A24

2019 doi
[22]

A., Spyromilio J., 2008, @doi [ ] 10.1051/0004-6361:200810551 , https://ui.adsabs.harvard.edu/abs/2008A&A...492..481G 492, 481

Gr \"o ningsson P., Fransson C., Leibundgut B., Lundqvist P., Challis P., Chevalier R. A., Spyromilio J., 2008, @doi [ ] 10.1051/0004-6361:200810551 , https://ui.adsabs.harvard.edu/abs/2008A&A...492..481G 492, 481

2008 doi
[23]

J., Janka H

Hammer N. J., Janka H. T., M \"u ller E., 2010, @doi [ ] 10.1088/0004-637X/714/2/1371 , https://ui.adsabs.harvard.edu/abs/2010ApJ...714.1371H 714, 1371

2010 doi
[25]

D., 2007, Computing in Science Engineering, 9, 90

Hunter J. D., 2007, Computing in Science Engineering, 9, 90

2007
[27]

Jerkstrand A., Fransson C., Kozma C., 2011, @doi [ ] 10.1051/0004-6361/201015937 , https://ui.adsabs.harvard.edu/abs/2011A&A...530A..45J 530, A45

2011 doi
[28]

C., et al., 2023, @doi [ ] 10.3847/1538-4357/ad0036 , https://ui.adsabs.harvard.edu/abs/2023ApJ...958...95J 958, 95

Jones O. C., et al., 2023, @doi [ ] 10.3847/1538-4357/ad0036 , https://ui.adsabs.harvard.edu/abs/2023ApJ...958...95J 958, 95

2023 doi
[29]

Kifonidis K., Plewa T., Scheck L., Janka H.-T., M \"u ller E., 2006, @doi [ ] 10.1051/0004-6361:20054512 , https://ui.adsabs.harvard.edu/abs/2006A&A...453..661K 453, 661

2006 doi
[30]

Kunkel W., et al., 1987, , https://ui.adsabs.harvard.edu/abs/1987IAUC.4316....1K 4316, 1

1987
[31]

Larsson J., et al., 2011, @doi [ ] 10.1038/nature10090 , https://ui.adsabs.harvard.edu/abs/2011Natur.474..484L 474, 484

2011 doi
[32]

Larsson J., et al., 2013, @doi [ ] 10.1088/0004-637X/768/1/89 , https://ui.adsabs.harvard.edu/abs/2013ApJ...768...89L 768, 89

2013 doi
[33]

Larsson J., et al., 2016, @doi [ ] 10.3847/1538-4357/833/2/147 , https://ui.adsabs.harvard.edu/abs/2016ApJ...833..147L 833, 147

2016 doi
[34]

Larsson J., et al., 2019a, @doi [ ] 10.3847/1538-4357/ab03d1 , https://ui.adsabs.harvard.edu/abs/2019ApJ...873...15L 873, 15

doi
[35]

Larsson J., et al., 2019b, @doi [ ] 10.3847/1538-4357/ab4ff2 , https://ui.adsabs.harvard.edu/abs/2019ApJ...886..147L 886, 147

doi
[36]

Larsson J., et al., 2023, @doi [ ] 10.3847/2041-8213/acd555 , https://ui.adsabs.harvard.edu/abs/2023ApJ...949L..27L 949, L27

2023 doi
[42]

Matsuura M., et al., 2011, @doi [Science] 10.1126/science.1205983 , https://ui.adsabs.harvard.edu/abs/2011Sci...333.1258M 333, 1258

2011 doi
[43]

Matsuura M., et al., 2015, @doi [ ] 10.1088/0004-637X/800/1/50 , https://ui.adsabs.harvard.edu/abs/2015ApJ...800...50M 800, 50

2015 doi
[45]

Matsuura M., et al., 2024, @doi [ ] 10.1093/mnras/stae1032 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.532.3625M 532, 3625

2024 doi
[46]

N., Wyrowski F., Menten K

Mazumdar P., Tram L. N., Wyrowski F., Menten K. M., Tang X., 2022, @doi [ ] 10.1051/0004-6361/202037564 , https://ui.adsabs.harvard.edu/abs/2022A&A...668A.180M 668, A180

2022 doi
[49]

J., Cordiner M

McElroy D., Walsh C., Markwick A. J., Cordiner M. A., Smith K., Millar T. J., 2013, @doi [ ] 10.1051/0004-6361/201220465 , https://ui.adsabs.harvard.edu/abs/2013A&A...550A..36M 550, A36

2013 doi
[50]

P., Waters B., Schiebel D., Young W., Golap K., 2007, in Shaw R

McMullin J. P., Waters B., Schiebel D., Young W., Golap K., 2007, in Shaw R. A., Hill F., Bell D. J., eds, Vol. 376, Astronomical Data Analysis Software and Systems XVI. p. 127

2007
[51]

J., Bennett A., Rawlings J

Millar T. J., Bennett A., Rawlings J. M. C., Brown P. D., Charnley S. B., 1991, , https://ui.adsabs.harvard.edu/abs/1991A&AS...87..585M 87, 585

1991
[53]

J., Walsh C., Van de Sande M., Markwick A

Millar T. J., Walsh C., Van de Sande M., Markwick A. J., 2024, @doi [ ] 10.1051/0004-6361/202346908 , https://ui.adsabs.harvard.edu/abs/2024A&A...682A.109M 682, A109

2024 doi
[54]

Nozawa T., Kozasa T., Umeda H., Maeda K., Nomoto K., 2003, @doi [ ] 10.1086/379011 , https://ui.adsabs.harvard.edu/abs/2003ApJ...598..785N 598, 785

2003 doi
[56]

Ono M., Nozawa T., Nagataki S., Kozyreva A., Orlando S., Miceli M., Chen K.-J., 2024, @doi [ ] 10.3847/1538-4365/ad1a08 , https://ui.adsabs.harvard.edu/abs/2024ApJS..271...33O 271, 33

2024 doi
[58]

T., Bigiel F., Neumann L., 2023, @doi [ ] 10.1093/mnras/stad1741 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.6138P 523, 6138

Panessa M., Seifried D., Walch S., Gaches B., Barnes A. T., Bigiel F., Neumann L., 2023, @doi [ ] 10.1093/mnras/stad1741 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.6138P 523, 6138

2023 doi
[62]

P., Park S., Zhekov S

Ravi A. P., Park S., Zhekov S. A., Orlando S., Miceli M., Frank K. A., Broos P. S., Burrows D. N., 2024, @doi [ ] 10.3847/1538-4357/ad3800 , https://ui.adsabs.harvard.edu/abs/2024ApJ...966..147R 966, 147

2024 doi
[63]

Rawlings J., Williams D., 1990, , 246, 208

1990
[66]

Sarangi A., Cherchneff I., 2013, @doi [ ] 10.1088/0004-637X/776/2/107 , https://ui.adsabs.harvard.edu/abs/2013ApJ...776..107S 776, 107

2013 doi
[67]

L., van der Tak F

Sch \"o ier F. L., van der Tak F. F. S., van Dishoeck E. F., Black J. H., 2005, @doi [ ] 10.1051/0004-6361:20041729 , https://ui.adsabs.harvard.edu/abs/2005A&A...432..369S 432, 369

2005 doi
[69]

H., 2018, @doi [ ] 10.1093/mnras/sty2060 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.480.5580S 480, 5580

Sluder A., Milosavljevi \'c M., Montgomery M. H., 2018, @doi [ ] 10.1093/mnras/sty2060 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.480.5580S 480, 5580

2018 doi
[71]

Spyromilio J., Meikle W. P. S., Learner R. C. M., Allen D. A., 1988, Letters to Nature, 334, 327

1988
[72]

P., Chugai N

Utrobin V. P., Chugai N. N., 2005, @doi [ ] 10.1051/0004-6361:20042599 , https://ui.adsabs.harvard.edu/abs/2005A&A...441..271U 441, 271

2005 doi
[73]

P., Chugai N

Utrobin V. P., Chugai N. N., Andronova A. A., 1995, , https://ui.adsabs.harvard.edu/abs/1995A&A...295..129U 295, 129

1995
[74]

P., Wongwathanarat A., Janka H

Utrobin V. P., Wongwathanarat A., Janka H. T., M \"u ller E., 2015, @doi [ ] 10.1051/0004-6361/201425513 , https://ui.adsabs.harvard.edu/abs/2015A&A...581A..40U 581, A40

2015 doi
[75]

P., Wongwathanarat A., Janka H

Utrobin V. P., Wongwathanarat A., Janka H. T., M \"u ller E., Ertl T., Woosley S. E., 2019, @doi [ ] 10.1051/0004-6361/201834976 , https://ui.adsabs.harvard.edu/abs/2019A&A...624A.116U 624, A116

2019 doi
[76]

P., Wongwathanarat A., Janka H

Utrobin V. P., Wongwathanarat A., Janka H. T., M \"u ller E., Ertl T., Menon A., Heger A., 2021, @doi [ ] 10.3847/1538-4357/abf4c5 , https://ui.adsabs.harvard.edu/abs/2021ApJ...914....4U 914, 4

2021 doi
[77]

Virtanen P., et al., 2020, @doi [Nature Methods] https://doi.org/10.1038/s41592-019-0686-2 , https://rdcu.be/b08Wh 17, 261

2020 doi
[78]

Wesson R., et al., 2026, @doi [ ] 10.1093/mnras/stag325 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.tmp..301W

2026 doi
[79]

T., 2015, @doi [ ] 10.1051/0004-6361/201425025 , 577, 1371–1385

Wongwathanarat A., M \"u ller E., Janka H. T., 2015, @doi [ ] 10.1051/0004-6361/201425025 , 577, 1371–1385

2015 doi
[83]

Wootten A., et al., 2022, @doi [ ] 10.3847/1538-4357/ac391a , https://ui.adsabs.harvard.edu/abs/2022ApJ...925...59W 925, 59

2022 doi
[84]

Zhou P., et al., 2022, @doi [ ] 10.3847/1538-4357/ac63b5 , https://ui.adsabs.harvard.edu/abs/2022ApJ...931..144Z 931, 144

2022 doi
[85]

van der Tak F. F. S., Black J. H., Sch \"o ier F. L., Jansen D. J., van Dishoeck E. F., 2007, @doi [ ] 10.1051/0004-6361:20066820 , https://ui.adsabs.harvard.edu/abs/2007A&A...468..627V 468, 627

2007 doi
[86]

C., Varoquaux G., 2011, Computing in Science Engineering, 13, 22

van der Walt S., Colbert S. C., Varoquaux G., 2011, Computing in Science Engineering, 13, 22

2011
[87]

, year = 1987, month = feb, volume =

Supernova 1987A in the Large Magellanic Cloud. , year = 1987, month = feb, volume =

1987
[88]

2017 , month=

ALMA spectral survey of Supernova 1987A – molecular inventory, chemistry, dynamics and explosive nucleosynthesis , volume=. 2017 , month=. doi:doi:10.1093/mnras/stx830 , journal=

2017 doi
[89]

arXiv , Author =:1307.6212 , Journal =

doi:10.1051/0004-6361/201322068 , Eid =. arXiv , Author =:1307.6212 , Journal =

arXiv
[90]

doi:10.3847/1538-3881/aabc4f , Eid =

, Keywords =. doi:10.3847/1538-3881/aabc4f , Eid =

doi
[91]

, keywords =

The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

arXiv
[92]

Nature Methods , year = "2020", volume=

SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python. Nature Methods , year = "2020", volume=

2020
[93]

Computing in Science Engineering , title=

S. Computing in Science Engineering , title=. 2011 , volume=

2011
[94]

J. D. Computing in Science Engineering , title=. 2007 , volume=

2007
[95]

doi:10.3847/1538-4357/ab4b46 , year =

High Angular Resolution. doi:10.3847/1538-4357/ab4b46 , year =

doi
[96]

2017 , issn =

Very Deep inside the SN 1987A Core Ejecta: Molecular Structures Seen in 3D , journal =. 2017 , issn =. doi:10.3847/2041-8213/aa784c , author =

2017 doi
[97]

, keywords =

Supernova 1987A. , keywords =. doi:10.1146/annurev.aa.27.090189.003213 , adsurl =
[98]

, keywords =

The Oxygen Temperature of SN 1987A. , keywords =. doi:10.1086/176498 , adsurl =

doi
[99]

, keywords =

Carbon Monoxide in SN 1987A. , keywords =. doi:10.1086/171749 , adsurl =

doi
[100]

, keywords =

CO Formation in the Metal-rich Ejecta of SN 1987A. , keywords =. doi:10.1086/167601 , adsurl =

doi
[101]

, keywords =

Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout. , keywords =
[102]

, keywords =

Three-dimensional Simulations of Mixing Instabilities in Supernova Explosions. , keywords =. doi:10.1088/0004-637X/714/2/1371 , archivePrefix =. 0908.3474 , primaryClass =

arXiv
[103]

Chemistry in Supernova 1987A , volume=

J.M.C Rawlings and D.A Williams , year=. Chemistry in Supernova 1987A , volume=
[104]

, keywords =

Dense Molecular Clouds in the Crab Supernova Remnant. , keywords =. doi:10.3847/1538-4357/ac391a , archivePrefix =. 2111.06033 , primaryClass =

arXiv
[105]

, keywords =

Submillimeter observations of molecular gas interacting with the supernova remnant W28. , keywords =. doi:10.1051/0004-6361/202037564 , archivePrefix =. 2211.06100 , primaryClass =

arXiv
[106]

, keywords =

Unusually High HCO ^ + /CO Ratios in and outside Supernova Remnant W49B. , keywords =. doi:10.3847/1538-4357/ac63b5 , archivePrefix =. 2203.13111 , primaryClass =

arXiv
[107]

, keywords =

Detection of Water in the Shocked Gas Associated with IC 443: Constraints on Shock Models. , keywords =. doi:10.1086/427231 , adsurl =

doi
[108]

, keywords =

Submillimeter obseravtions of the shocked molecular gas associated with the supernova remnant IC 443. , keywords =
[109]

Spyromilio and W

J. Spyromilio and W. P. S. Meikle and R. C. M. Learner and D. A. Allen , year=. Carbon monoxide in supernova 1987A , volume=. Letters to Nature , publisher=
[110]

, keywords =

Carbon Monoxide in the Cold Debris of Supernova 1987A. , keywords =. doi:10.1088/2041-8205/773/2/L34 , archivePrefix =. 1307.6561 , primaryClass =

arXiv
[111]

Arnett, W. D. and Bahcall, J. N. and Kirshner, R. P. and Woosley, S. E. , title =. , volume =. 1989 , doi =

1989
[112]

, keywords =

The ^ 44 Ti-powered spectrum of SN 1987A. , keywords =. doi:10.1051/0004-6361/201015937 , archivePrefix =. 1103.3653 , primaryClass =

arXiv
[113]

, keywords =

Observation of a neutrino burst from the supernova SN1987A. , keywords =. doi:10.1103/PhysRevLett.58.1490 , adsurl =

doi
[114]

, keywords =

Properties of the SN 1987A Circumstellar Ring and the Distance to the Large Magellanic Cloud. , keywords =. doi:10.1086/186164 , adsurl =

doi
[115]

New Views of the Magellanic Clouds , year = 1999, journal =

Distance to SN 1987 A and the LMC. New Views of the Magellanic Clouds , year = 1999, journal =

1987
[116]

With diagnostic plots to interpret observed line intensity ratios

A computer program for fast non-LTE analysis of interstellar line spectra. With diagnostic plots to interpret observed line intensity ratios. , keywords =. doi:10.1051/0004-6361:20066820 , archivePrefix =. 0704.0155 , primaryClass =

arXiv
[117]

, keywords =

An atomic and molecular database for analysis of submillimetre line observations. , keywords =. doi:10.1051/0004-6361:20041729 , archivePrefix =. astro-ph/0411110 , primaryClass =

arXiv
[118]

, year = 2016, month = sep, volume =

The Remnant of Supernova 1987A. , year = 2016, month = sep, volume =. doi:10.1146/annurev-astro-082615-105405 , adsurl =

2016 doi
[119]

, year = 1973, month = oct, volume =

The Formation and Depletion of Molecules in Dense Interstellar Clouds. , year = 1973, month = oct, volume =. doi:10.1086/152436 , adsurl =

1973 doi
[120]

and Viti, Serena , year=

Williams, David A. and Viti, Serena , year=. Observational Molecular Astronomy: Exploring the Universe Using Molecular Line Emissions , DOI=
[121]

Simulation of clustering by a modified continuous distribution of ellipsoids

Optical constants of cosmic carbon analogue grains - I. Simulation of clustering by a modified continuous distribution of ellipsoids. , keywords =. doi:10.1093/mnras/282.4.1321 , adsurl =

doi
[122]

, keywords =

Dust Grain-Size Distributions and Extinction in the Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud. , keywords =. doi:10.1086/318651 , archivePrefix =. astro-ph/0008146 , primaryClass =

arXiv
[123]

Steps toward interstellar silicate mineralogy. I. Laboratory results of a silicate glass of mean cosmic composition. , keywords =
[124]

, keywords =

Supernova 1987A revisited. , keywords =. doi:10.1146/annurev.aa.31.090193.001135 , adsurl =
[125]

, keywords =

Supernova 1987A: a Template to Link Supernovae to Their Remnants. , keywords =. doi:10.1088/0004-637X/810/2/168 , archivePrefix =. 1508.02275 , primaryClass =

arXiv
[126]

, keywords =

Chandra Observes the End of an Era in SN 1987A. , keywords =. doi:10.3847/0004-637X/829/1/40 , archivePrefix =. 1608.02160 , primaryClass =

arXiv
[127]

, keywords =

^ 44 Ti gamma-ray emission lines from SN1987A reveal an asymmetric explosion. , keywords =. doi:10.1126/science.aaa2259 , adsurl =

doi
[128]

ALMA Cycle 5 Technical Handbook
[129]

, keywords =

10 mu.m spectral observations of SN 1987A : the first year. , keywords =. doi:10.1093/mnras/235.1.19P , adsurl =

doi
[130]

, keywords =

Nickel, argon and cobalt in the infrared spectrum of SN1987A: the core becomes visible. , keywords =. doi:10.1038/331505a0 , adsurl =

doi
[131]

, keywords =

Silicon monoxide in supernova 1987A. , keywords =. doi:10.1093/mnras/252.1.39P , adsurl =

doi
[132]

, keywords =

The Chemically Controlled Synthesis of Dust in Type II-P Supernovae. , keywords =. doi:10.1088/0004-637X/776/2/107 , archivePrefix =. 1309.5887 , primaryClass =

arXiv
[133]

, keywords =

Cosmic-ray ionization of molecular clouds. , keywords =. doi:10.1051/0004-6361/200911794 , archivePrefix =. 0904.4149 , primaryClass =

arXiv
[134]

, keywords =

X-ray illumination of the ejecta of supernova 1987A. , keywords =. doi:10.1038/nature10090 , archivePrefix =. 1106.2300 , primaryClass =

arXiv
[135]

Chevalier and Kevin France and Robert P

Claes Fransson and Josefin Larsson and Katia Migotto and Dominic Pesce and Peter Challis and Roger A. Chevalier and Kevin France and Robert P. Kirshner and Bruno Leibundgut and Peter Lundqvist and Richard McCray and Jason Spyromilio and Francesco Taddia and Anders Jerkstrand a...
[136]

, keywords =

JWST NIRSpec Observations of Supernova 1987A-From the Inner Ejecta to the Reverse Shock. , keywords =. doi:10.3847/2041-8213/acd555 , archivePrefix =. 2302.03576 , primaryClass =

arXiv
[137]

, keywords =

Time evolution of the line emission from the inner circumstellar ring of SN 1987A and its hot spots. , keywords =. doi:10.1051/0004-6361:200810551 , archivePrefix =. 0810.2661 , primaryClass =

arXiv
[138]

, keywords =

Deep JWST/NIRCam imaging of Supernova 1987A. , keywords =. doi:10.1093/mnras/stae1032 , archivePrefix =. 2404.10042 , primaryClass =

arXiv
[139]

Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

CASA Architecture and Applications. Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

2007
[140]

, year = 1989, month = jan, volume =

Abundances of the elements: Meteoritic and solar. , year = 1989, month = jan, volume =. doi:10.1016/0016-7037(89)90286-X , adsurl =

1989 doi
[141]

Explosive Nucleosynthesis in SN 1987A. II. Composition, Radioactivities, and the Neutron Star Mass. , year = 1990, month = jan, volume =. doi:10.1086/168308 , adsurl =

1990 doi
[142]

, year = 1988, month = jan, volume =

Recent results on SN 1987A. , year = 1988, month = jan, volume =. doi:10.1017/S1323358000022475 , adsurl =

1988 doi
[143]

, keywords =

Supernova 1987A: Six Weeks Later. , keywords =. doi:10.1086/165908 , adsurl =

doi
[144]

, keywords =

SN 1987A: After the Peak. , keywords =. doi:10.1086/166468 , adsurl =

doi
[145]

, keywords =

The Chemical Composition of the Sun. , keywords =. doi:10.1146/annurev.astro.46.060407.145222 , archivePrefix =. 0909.0948 , primaryClass =
[146]

Abundances of the Heavy Elements in the Magellanic Clouds. III. Interpretation of Results. , year = 1992, month = jan, volume =. doi:10.1086/170893 , adsurl =

1992 doi
[147]

Tielens, A. G. G. M. , year=. The Physics and Chemistry of the Interstellar Medium , DOI=
[148]

, keywords =

Three-dimensional Distribution of Ejecta in Supernova 1987A at 10,000 Days. , keywords =. doi:10.3847/1538-4357/833/2/147 , archivePrefix =. 1609.04413 , primaryClass =

arXiv
[149]

, keywords =

Strong effects of time-dependent ionization in early SN 1987A. , keywords =. doi:10.1051/0004-6361:20042599 , archivePrefix =. astro-ph/0501036 , primaryClass =

arXiv
[150]

, keywords =

A Stubbornly Large Mass of Cold Dust in the Ejecta of Supernova 1987A. , keywords =. doi:10.1088/0004-637X/800/1/50 , archivePrefix =. 1411.7381 , primaryClass =

arXiv
[151]

, keywords =

CASA, the Common Astronomy Software Applications for Radio Astronomy. , keywords =. doi:10.1088/1538-3873/ac9642 , archivePrefix =. 2210.02276 , primaryClass =

arXiv
[152]

, keywords =

Improved measurement of the Ti44 half-life from a 14-year long study. , keywords =. doi:10.1103/PhysRevC.74.065803 , adsurl =

doi
[153]

, keywords =

The Morphology of the Ejecta in Supernova 1987A: A Study over Time and Wavelength. , keywords =. doi:10.1088/0004-637X/768/1/89 , archivePrefix =. 1212.5051 , primaryClass =

arXiv
[154]

, keywords =

Energy spectra of X-ray clusters of galaxies. , keywords =. doi:10.1086/154870 , adsurl =

doi
[155]

, keywords =

Late Spectral Evolution of the Ejecta and Reverse Shock in SN 1987A. , keywords =. doi:10.1088/0004-637X/768/1/88 , archivePrefix =. 1212.5052 , primaryClass =

arXiv
[156]

and Dunne, L

James, A. and Dunne, L. and Eales, S. and Edmunds, M. G. , title = ". , volume =. 2002 , month =. doi:10.1046/j.1365-8711.2002.05660.x , url =

2002
[157]

, keywords =

The evolution of HCO ^ + in molecular clouds using a novel chemical post-processing algorithm. , keywords =. doi:10.1093/mnras/stad1741 , archivePrefix =. 2210.06251 , primaryClass =

arXiv
[158]

, keywords =

A Three-dimensional View of Molecular Hydrogen in SN 1987A. , keywords =. doi:10.3847/1538-4357/ab03d1 , archivePrefix =. 1901.11235 , primaryClass =

1901 arXiv
[159]

, keywords =

Discovery of Molecular Hydrogen in SN 1987A. , keywords =. doi:10.3847/2041-8205/821/1/L5 , archivePrefix =. 1603.05560 , primaryClass =

arXiv
[160]

Science , keywords =

Herschel Detects a Massive Dust Reservoir in Supernova 1987A. Science , keywords =. doi:10.1126/science.1205983 , archivePrefix =. 1107.1477 , primaryClass =

arXiv
[161]

, keywords =

Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS. , keywords =. doi:10.3847/1538-4357/ad0036 , archivePrefix =. 2307.06692 , primaryClass =

arXiv
[162]

, keywords =

Molecules in the Ejecta of SN 1987A. , keywords =. doi:10.1086/168981 , adsurl =

doi
[164]

, year = 2013, month = feb, volume =

The UMIST database for astrochemistry 2012. , year = 2013, month = feb, volume =. doi:10.1051/0004-6361/201220465 , archivePrefix =. 1212.6362 , primaryClass =

2012 arXiv
[165]

, keywords =

The UMIST database for astrochemistry 2006. , keywords =. doi:10.1051/0004-6361:20064981 , adsurl =

2006 doi
[166]

, keywords =

The UMIST database for astrochemistry 1999. , keywords =. doi:10.1051/aas:2000265 , adsurl =

1999 doi
[167]

, keywords =

The UMIST Database for Astrochemistry 1995. , keywords =. doi:10.1051/aas:1997118 , adsurl =

1995 doi
[168]

, keywords =

Gas phase reactions and rate coefficients for use in astrochemistry - The UMIST ratefile. , keywords =
[169]

, keywords =

Dust in the Early Universe: Dust Formation in the Ejecta of Population III Supernovae. , keywords =. doi:10.1086/379011 , archivePrefix =. astro-ph/0307108 , primaryClass =

arXiv
[170]

, keywords =

Gamma Rays, X-Rays, and Optical Light from the Cobalt and the Neutron Star in SN 1987A. , keywords =. doi:10.1086/167915 , adsurl =

doi
[171]

, keywords =

The Gamma-Ray Light Curves of SN 1987A. , keywords =. doi:10.1086/168952 , adsurl =

doi
[172]

, keywords =

The infancy of core-collapse supernova remnants. , keywords =. doi:10.1093/mnras/stab116 , archivePrefix =. 2008.01763 , primaryClass =

2008 arXiv
[173]

, keywords =

Supernova 1987A: neutrino-driven explosions in three dimensions and light curves. , keywords =. doi:10.1051/0004-6361/201425513 , archivePrefix =. 1412.4122 , primaryClass =

arXiv
[174]

, keywords =

Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A. , keywords =. doi:10.1051/0004-6361/201834976 , archivePrefix =. 1812.11083 , primaryClass =

arXiv
[175]

, keywords =

Supernova 1987A: 3D Mixing and Light Curves for Explosion Models Based on Binary-merger Progenitors. , keywords =. doi:10.3847/1538-4357/abf4c5 , archivePrefix =. 2102.09686 , primaryClass =
[176]

, keywords =

Theoretical Light Curve of SN 1987A and Mixing of Hydrogen and Nickel in the Ejecta. , keywords =. doi:10.1086/169114 , adsurl =

doi
[177]

, keywords =

Asymmetry of SN 1987A: fast \^56\^Ni clump. , keywords =
[178]

The Chemistry of Population III Supernova Ejecta. I. Formation of Molecules in the Early Universe. , keywords =. doi:10.1088/0004-637X/703/1/642 , archivePrefix =. 0907.3621 , primaryClass =

arXiv
[179]

, keywords =

The theory of gamma-ray emergence in supernova 1987A. , keywords =. doi:10.1038/333534a0 , adsurl =

doi
[180]

Proceedings of the National Academy of Sciences , keywords =

Interstellar Chemistry Special Feature: Interstellar H3+. Proceedings of the National Academy of Sciences , keywords =. doi:10.1073/pnas.0601242103 , adsurl =

doi
[181]

, keywords =

Latest Evolution of the X-Ray Remnant of SN 1987A: Beyond the Inner Ring. , keywords =. doi:10.3847/1538-4357/ad3800 , archivePrefix =. 2403.07990 , primaryClass =

arXiv
[182]

, keywords =

The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A. , keywords =. doi:10.3847/1538-4365/ad1a08 , archivePrefix =. 2305.02550 , primaryClass =

arXiv
[183]

, keywords =

Hydrogen Molecules in SN 1987A. , keywords =. doi:10.1086/176580 , adsurl =

doi
[184]

Grids of stellar models with rotation. IV. Models from 1.7 to 120 M _ at a metallicity Z = 0.0004. , keywords =. doi:10.1051/0004-6361/201833720 , archivePrefix =. 1904.04009 , primaryClass =

1904 arXiv
[185]

, keywords =

Is GW190521 the merger of black holes from the first stellar generations?. , keywords =. doi:10.1093/mnrasl/slaa196 , archivePrefix =. 2009.06585 , primaryClass =

2009 arXiv
[186]

, keywords =

Can Stellar Mixing Explain the Lack of Type Ib Supernovae in Long-duration Gamma-Ray Bursts?. , keywords =. doi:10.1088/2041-8205/773/1/L7 , archivePrefix =. 1305.0515 , primaryClass =

arXiv
[187]

Late Spectral Evolution of SN 1987A. II. Line Emission. , keywords =. doi:10.1086/305452 , archivePrefix =. astro-ph/9712224 , primaryClass =

arXiv
[188]

, keywords =

3D insights into SN 1987A: ALMA observations compared to hydrodynamical explosion simulations. , keywords =. doi:10.1093/mnras/stag325 , archivePrefix =. 2602.11259 , primaryClass =
[189]

, keywords =

JWST MIRI Imager Observations of Supernova SN 1987A. , keywords =. doi:10.3847/1538-4357/ad2770 , archivePrefix =. 2402.14014 , primaryClass =

arXiv
[190]

2026 , title =

Boccioli, Luca and Roberti, Lorenzo and Fryer, Chris L and Safi-Harb, Samar and Jones, Samuel and Pignatari, Marco , journal =. 2026 , title =

2026
[191]

, keywords =

Molecular nucleation theory of dust formation in core-collapse supernovae applied to SN 1987A. , keywords =. doi:10.1093/mnras/sty2060 , archivePrefix =. 1612.09013 , primaryClass =

arXiv
[192]

, keywords =

Ns 1987A in SN 1987A. , keywords =. doi:10.3847/1538-4357/ab93c2 , archivePrefix =. 2004.06078 , primaryClass =

2004 arXiv
[193]

, keywords =

The UMIST Database for Astrochemistry 2022. , keywords =. doi:10.1051/0004-6361/202346908 , archivePrefix =. 2311.03936 , primaryClass =

2022 arXiv
[194]

, keywords =

Modelling the ArH ^ + emission from the Crab nebula. , keywords =. doi:10.1093/mnras/stx2327 , archivePrefix =. 1709.01373 , primaryClass =

arXiv
[195]

, keywords =

The nature of the H _ 2 -emitting gas in the Crab nebula. , keywords =. doi:10.1093/mnras/sts695 , archivePrefix =. 1212.5642 , primaryClass =

arXiv
[196]

Contemporary Physics , keywords =

The supernova 1987A system and its recent evolution ─ a review. Contemporary Physics , keywords =. doi:10.1080/00107514.2025.2562755 , archivePrefix =. 2510.13629 , primaryClass =

2025
[197]

, keywords =

The Matter Beyond the Ring: The Recent Evolution of SN 1987A Observed by the Hubble Space Telescope. , keywords =. doi:10.3847/1538-4357/ab4ff2 , archivePrefix =. 1910.09582 , primaryClass =

1910 arXiv
[198]

Non-spherical core collapse supernovae. II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A. , keywords =. doi:10.1051/0004-6361:20054512 , archivePrefix =. astro-ph/0511369 , primaryClass =

1987 arXiv

Pith tools

Reviewed August 1, 2026 · model on record in the stance chip above.

[1] [1]

ALMA Partnership et al., 2017, ALMA Cycle 5 Technical Handbook

2017

[2] [6]

Astropy Collaboration et al., 2013, @doi [ ] 10.1051/0004-6361/201322068 , http://adsabs.harvard.edu/abs/2013A

doi:10.1051/0004-6361/201322068 2013

[3] [7]

Astropy Collaboration et al., 2022, @doi [ ] 10.3847/1538-4357/ac7c74 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935..167A 935, 167

doi:10.3847/1538-4357/ac7c74 2022

[4] [10]

L., Safi-Harb S., Jones S., Pignatari M., 2026, arXiv

Boccioli L., Roberti L., Fryer C. L., Safi-Harb S., Jones S., Pignatari M., 2026, arXiv

2026

[5] [11]

Bouchet P., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2770 , https://ui.adsabs.harvard.edu/abs/2024ApJ...965...51B 965, 51

doi:10.3847/1538-4357/ad2770 2024

[6] [12]

CASA Team et al., 2022, @doi [ ] 10.1088/1538-3873/ac9642 , https://ui.adsabs.harvard.edu/abs/2022PASP..134k4501C 134, 114501

doi:10.1088/1538-3873/ac9642 2022

[7] [13]

Cherchneff I., Dwek E., 2009, @doi [ ] 10.1088/0004-637X/703/1/642 , https://ui.adsabs.harvard.edu/abs/2009ApJ...703..642C 703, 642

doi:10.1088/0004-637x/703/1/642 2009

[8] [16]

H., Hirschi R., Murphy L., Kaiser E., Ekstr \"o m S., Georgy C., Meynet G., 2021, @doi [ ] 10.1093/mnrasl/slaa196 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.502L..40F 502, L40

Farrell E., Groh J. H., Hirschi R., Murphy L., Kaiser E., Ekstr \"o m S., Georgy C., Meynet G., 2021, @doi [ ] 10.1093/mnrasl/slaa196 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.502L..40F 502, L40

doi:10.1093/mnrasl/slaa196 2021