Pith. sign in

REVIEW 3 major objections 4 minor 2 cited by

Nucleosynthesis and the chemical enrichment of galaxies

T0 review · 3 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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

Pith's one-line read A review of stellar nucleosynthesis argues that neutron star mergers alone cannot explain the Milky Way's europium; a prompt r-process from core-collapse supernovae, such as magneto-rotational supernovae, is required.

desk verdict A comprehensive, honest review, but the headline r-process claim ('MRSNe are required') is conditional on BPS merger rates that the paper itself concedes could be different. read the letter →

arxiv 2506.20436 v1 pith:2363DRTI submitted 2025-06-25 astro-ph.GA astro-ph.HEastro-ph.SR

Chiaki Kobayashi This is my paper
classification astro-ph.GAastro-ph.HEastro-ph.SR
keywords nucleosynthesisgalacticchemicalevolutionr-processneutronstarmergersmagneto-rotationalsupernovaearchaeologystellaryieldsTypeIa
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This review argues that the chemical makeup of galaxies is best read by treating stars as fossils, and that the most important inputs to that reading are nucleosynthesis yields and binary physics. It further claims that, with current yields, the observed europium abundances in the Milky Way cannot be explained by neutron star mergers alone: an r-process associated with core-collapse supernovae, such as magneto-rotational supernovae, must also contribute. By comparing one-zone galactic chemical evolution models and cosmological chemodynamical simulations with observations, the review aims to show which stellar sources produce which elements, and how abundance patterns can constrain galaxy formation histories.

What carries the argument

The machinery is the yield-to-rate pipeline of galactic chemical evolution: stellar nucleosynthesis yield tables for core-collapse supernovae, hypernovae, electron-capture supernovae, AGB stars, Type Ia supernovae, neutron star mergers, and magneto-rotational supernovae, convolved with the initial mass function and with delay-time distributions for binary systems. These inputs feed the one-zone chemical evolution equation and are also implemented on the fly in cosmological chemodynamical simulations. The decisive diagnostic is the europium-to-iron versus iron-abundance plane: switching the r-process source on and off shows that neutron-star-merger-only models give too little europium arriving too late, while adding magneto-rotational supernovae produces the observed low-metallicity plateau; the metallicity distribution function is used to pin down the star-formation history so that abundance tracks can then act as a clean test of the nuclear physics inputs.

What would settle it

Run a galactic chemical evolution calculation that uses independently determined binary population synthesis rates for neutron star mergers, without tuning them to the target abundances, and require it to match the observed europium-to-iron plateau at low iron abundance as well as the solar europium abundance; if it succeeds without any core-collapse r-process source, the paper's central claim fails.

Watch

Extended reading notes

Core claim

The central claim is that reproducing the elemental abundance patterns of the Milky Way, especially europium and other r-process elements, requires an r-process site associated with core-collapse supernovae, most plausibly magneto-rotational supernovae, in addition to neutron star mergers. The review uses the K20 galactic chemical evolution model and newer chemodynamical simulations to show that neutron star mergers alone produce too little europium too late, and that including magneto-rotational supernovae reproduces the observed low-metallicity europium-to-iron plateau. Along the way it also argues that about three quarters of Type Ia supernovae in the solar neighbourhood must come from near-Chandrasekhar-mass explosions, that no extra light-element primary process is needed beyond AGB stars and electron-capture supernovae for the first neutron-capture peak, and that the observed alpha-to-iron bimodality arises naturally from delayed Type Ia enrichment even without a major merger.

Load-bearing premise

The argument that magneto-rotational supernovae are required for europium assumes that the model's fixed hypernova fraction, half of stars above twenty solar masses, and its adopted binary merger timing are representative of the real Universe; if those inputs are wrong, the needed r-process source could instead be neutron star mergers or something else.

Editorial extensions

If this is right

  • Observed europium abundances in the Milky Way cannot be explained by neutron star mergers alone; a prompt r-process source from core-collapse supernovae must contribute.
  • The near-Chandrasekhar Type Ia supernova fraction in the solar neighbourhood should be about 75 percent, with sub-Chandrasekhar explosions becoming relatively more important in some dwarf spheroidal galaxies.
  • AGB stars plus electron-capture supernovae can reproduce the first neutron-capture peak elements such as strontium, yttrium, and zirconium without invoking an extra light-element primary process.
  • The observed alpha-to-iron bimodality in the Milky Way arises naturally in chemodynamical simulations from delayed Type Ia enrichment, without requiring a major merger.
  • When the metallicity distribution function is known, element abundance tracks can be used to constrain nuclear astrophysics; without it, the tracks remain degenerate with the assumed star-formation history.

Reading between the lines

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

  • Beyond the paper: if magneto-rotational supernovae are genuinely required, then the rotation and magnetic-field properties of the first stars become decisive for the early-universe r-process budget, and actinide-boosted extremely metal-poor stars could be used to distinguish MRSNe from collapsar enrichment.
  • Beyond the paper: the same framework implies that in low-mass dwarf galaxies with slow star formation, the stochastic appearance of r-process elements may measure the relative rates and delay distributions of neutron star mergers and MRSNe, not just their yields.
  • Beyond the paper: a direct testable extension would be to model the europium scatter in the very metal-poor halo as a function of the assumed MRSN fraction and compare with large spectroscopic samples, yielding an independent measurement of that fraction.
  • Beyond the paper: the central requirement would weaken if future binary population synthesis models raise neutron star merger rates or shorten their delays; the review itself notes that no current binary population synthesis model works, so this is the point to watch.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. This manuscript is an invited review of stellar nucleosynthesis and galactic chemical evolution (GCE). The author summarizes nucleosynthesis yields from massive stars, asymptotic giant branch stars, Type Ia supernovae, and candidate r-process sites; describes the one-zone K20 GCE model and its equations; compares model predictions with observed abundance trends in the solar neighborhood, dwarf galaxies, and high-redshift systems; and reviews chemodynamical simulations. The review concludes that neutron-star mergers alone cannot reproduce the observed europium abundances and that an r-process associated with core-collapse supernovae, specifically magneto-rotational supernovae (MRSNe), is required. It also discusses the use of the metallicity distribution function, alpha/Fe bimodality, and elemental abundances for Galactic and extra-galactic archaeology.

Significance. If its conclusions hold, this is a valuable and comprehensive review: it collects the K20 yield framework, the GCE equations (Eqs. 1-16), and comparisons to a wide range of observations in one place, and it is honest about known discrepancies such as Ti underproduction, Au underproduction, Ag overproduction, and Th/U mismatch. Its main value is pedagogical and as a status report on the field. The central scientific claim, however, goes beyond a pure review: the statement that MRSNe are 'required' is presented as a robust conclusion, whereas the evidence in the manuscript itself shows this is conditional on the adopted binary population synthesis (BPS) delay-time distributions and on tuned GCE parameters. The manuscript would be substantially improved by reframing this claim as model-dependent and by quantifying the sensitivity of the r-process inference to the assumed NSM rate, delay times, and ejecta masses.

major comments (3)
  1. [Section 3.4, Section 3.3, Section 5] The paragraph after Fig. 14 states that 'an r-process associated with core-collapse supernovae, such as MRSNe, is required,' and Section 5 repeats this as a conclusion. This is stronger than the evidence reported in Section 3.1, which notes that Kobayashi et al. (2023b) constructed analytic NSM delay-time distributions that reproduce the observed [Eu/(Fe,O)] relations with NSMs only, and that the failure of NSM-only models is specific to current BPS predictions (rate too low, timescale too long, with NS-BH mergers viable only for unexpectedly high BH spins). The manuscript should therefore qualify the claim: within the K20 yield set and current BPS DTDs, NSMs alone are insufficient, but the requirement of MRSNe is conditional on the adopted population-synthesis model and on the assumed NSM ejecta masses. If the true merger rate is higher or the delay times are shorter, NSM-only models can satisfy the same constraints. Please revise the conclusion and the corresponding bullet in Section 3.3 accordingly.
  2. [Sections 2.2, 3.2, 3.3] The r-process inference is model-dependent in a way that the manuscript does not state explicitly. The K20 model fixes the hypernova fraction epsilon_HN = 0.5 for M >= 20 Msun, the failed-supernova threshold, the near-Ch SN Ia fraction near 75%, and the star-formation/inflow/outflow timescales by matching the observed MDF and abundance trends (Sections 2.2 and 3.2). The claim in Section 3.3 that contributions from both NS-NS/NS-BH mergers and MRSNe are 'necessary' then uses this calibrated model as the reference. This is a legitimate consistency check, but it is not an independent determination of the r-process site. The review should explicitly identify the most sensitive parameters (such as the BPS NSM DTD, the NSM ejecta mass, and the hypernova fraction) and state how the conclusion would change if those parameters were varied within their current uncertainties. At present the wording implies a stronger, model-independent requirement than the evidence supports.
  3. [Section 3.3, Section 3.4] The list of 'remaining problems' in Section 3.3 includes the underproduction of Ti, the factor-of-5 underproduction of Au, the factor-of-6 overproduction of Ag, and a mismatch in Th/U; Section 3.4 similarly notes that Au is underproduced by more than an order of magnitude even with both MRSNe and NSMs. These are not unrelated blemishes: Au and Eu are both third-peak r-process elements, so a large deficit in Au indicates that the adopted r-process yield sets are incomplete or that the fission/nuclear-physics treatment is missing a channel. The manuscript should state explicitly whether this known incompleteness affects the robustness of the Eu-based MRSNe requirement, rather than leaving the reader to reconcile the good agreement for Eu with the large Au discrepancy. A short discussion connecting the missing-Au problem to the uncertainty budget of the r-process conclusion would resolve this.
minor comments (4)
  1. [Section 3.3 vs. Section 3.4] The Au underproduction is given as 'a factor of 5' in Section 3.3 and as 'more than ten times lower' in Section 3.4; these numbers should be harmonized with a clear statement of which model output and solar reference is used.
  2. [Section 4 (after Eq. 16)] The text 'The SNIa rate RSNIs is given by Eq. (8)' appears to contain a typo; it should read 'RSNIa'.
  3. [Section 3.1, IMF discussion] In the summary of the Kroupa IMF, the mass range for the third slope should presumably be 0.5 <~ m/Msun <~ 150, but the text reads '0.05 <~ m/Msun <~ 150'; please correct this.
  4. [Section 3.1, paragraph on DTDs] The sentence 'Currently, there is no BPS model that can explain the observation only with NSMs' could be made clearer by explicitly stating that this refers to NSM-only models with BPS-predicted DTDs, since the preceding sentence already notes that analytic NSM DTDs can reproduce the relation.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the review's abundance-ratio tests are calibrated against external observations, and the r-process conclusion is model-conditional rather than a fitted-parameter prediction.

full rationale

The paper does not present a prediction that reduces by construction to a fitted parameter. K20's star-formation timescales are explicitly fit to the observed metallicity distribution function (Section 3.2), but the text argues that abundance-ratio tracks are nearly independent of SFH once the MDF is fixed, so the subsequent [α/Fe]-[Fe/H], N/O-O/H, and neutron-capture comparisons are genuine yield tests. The hypernova fraction and SN Ia delay-time distribution parameters are acknowledged inputs calibrated to solar-neighbourhood abundance trends, and the review labels them as assumptions rather than as predictions. The strongest potential concern is the claim that MRSNe are required for the r-process (Sections 3.3-3.4). Section 3.1 explicitly states that Kobayashi et al. (2023b) constructed analytic NSM-only DTDs that reproduce the observed [Eu/(Fe,O)]-[Fe/H] relations and that only current binary population synthesis models fail, so the 'requirement' is conditional on the adopted BPS delay-time distributions. That is model sensitivity, not circularity: the BPS rates are external inputs, the paper discloses the alternative, and additional observational anchors (the Yong star's abundance pattern in Section 3.6, and Wallner et al. 2021 radioactive-nuclei constraints) provide independent support. The numerous citations to the author's own yield tables and simulations are routine references to model inputs rather than a load-bearing self-citation chain. No equation or fitted parameter is renamed as a prediction.

Assumptions & free parameters 8 free parameters · 5 assumptions · 0 invented entities

The central conclusions of the review rest on the K20 GCE model, which contains numerous fitted parameters (hypernova fraction, SN Ia DTD, star formation timescales) and adopts several domain assumptions (one-zone instantaneous mixing, 1D yield accuracy). The MRSNe requirement is not derived independently but emerges from a model calibrated to the same observations it then claims to explain.

free parameters (8)
  • Hypernova fraction ϵHN = 0.5 (Z=0,0.001), 0.4 (Z=0.004), 0.01 (Z=0.02)
    Fraction of massive stars >= 20 M⊙ that explode as hypernovae; chosen in K20 to reproduce Fe and Zn abundances (Section 2.2).
  • Failed supernova mass threshold = 30 M⊙
    Mass above which stars collapse to black holes without ejecting iron; set to match GCE and supernova observations (Section 2.2).
  • SN Ia near-Chandrasekhar fraction = 75% (with 25% sub-Ch) or 100% in K20 fiducial
    Relative contribution of near-Ch mass SNe Ia; constrained from Mn/Fe and Ni/Fe trends (Section 2.4).
  • Star formation timescale τs = 4.7 Gyr (solar neighborhood), 4 Gyr in Fig. 10
    Sets star formation efficiency; tuned to reproduce the observed MDF (Section 3.2).
  • Inflow timescale τi = Exponential form with free τi
    Sets gas accretion history; fitted to MDF in the solar neighborhood model (Section 3.2).
  • Outflow timescale τo = Proportional to SFR with a free constant
    Sets metal loss from supernova feedback; fitted to MDF and mass-metallicity relation (Section 3.2).
  • MRSN contribution rate = Not specified in review
    The rate at which magneto-rotational supernovae contribute to r-process enrichment is not derived; it is added to match the [Eu/Fe] plateau (Section 3.3).
  • AGB partial mixing zone mass = Optimized in K20
    Sets the 13C pocket size for s-process yields; tuned to reproduce observed s-process abundances (Section 2.3).
assumptions (5)
  • domain assumption Instantaneous mixing of gas within a single zone
    One-zone GCE model assumes the ISM is chemically homogeneous at any time (Section 3, Eq. 1).
  • domain assumption Nucleosynthesis yields from 1D stellar evolution and explosion models are accurate
    The review relies on yield tables from 1D models (K20, Limongi & Chieffi 2018) despite known multi-D effects (Section 2.2).
  • domain assumption The Kroupa IMF with massive-end slope x=1.3 is adopted
    The IMF is assumed constant in time and metallicity (Section 3.1, Eq. 2).
  • domain assumption The observed MDF uniquely constrains the SFH timescales
    The review argues that for a given MDF, elemental abundance tracks are nearly independent of SFH (Section 3.2), an assumption that underpins its use of GCE to constrain nuclear astrophysics.
  • ad hoc to paper Hypernova fraction is a free parameter that can be set to match observations
    The 50% hypernova fraction is recommended based on GCE fits, not first principles (Section 2.2).

how reviews work

0 comments
Cite this review

Pith. "Pith review of Nucleosynthesis and the chemical enrichment of galaxies." pith.science (2026). https://pith.science/paper/2363DRTI

@misc{pith2026250620436,
  author       = {Pith},
  title        = {Pith review of: Nucleosynthesis and the chemical enrichment of galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2363DRTI}},
  note         = {Machine review of arXiv:2506.20436}
}
read the original abstract

Stars are fossils that retain the history of their host galaxies. Carbon and heavier elements are created inside stars and are ejected when they die. From the spatial distribution of elements in galaxies, it is therefore possible to constrain the physical processes during galaxy formation and evolution. This approach, Galactic archaeology, has been popularly used for our Milky Way Galaxy thanks to a vast amount of data from the Gaia satellite and multi-object spectrographs, and now can also be applied to very distant galaxies with the James Webb Space Telescope (JWST) - extra-galactic archaeology. In these studies the most important factor is the input stellar physics, namely nucleosynthesis yields and binary physics, which predominantly determine the model predictions. In this review I give a summary of stellar nucleosynthesis, and how they are tested with the observations in the Milky Way. Then I show how chemical enrichment of galaxies can be calculated, and show some results with the latest nucleosynthesis yields.

Figures

Figures reproduced from arXiv: 2506.20436 by the authors.

Figure 19
Figure 19. Due to the limited resolution, star forming regions, supernova ejecta, and active galactic nuclei (AGN) cannot be resolved in [PITH_FULL_IMAGE:figures/full_fig_p022_19.png] view at source ↗

Discussion (0). Sign in to comment.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Gas-Phase Metallicity and Nitrogen Abundances in Low-Mass Galaxies Down to $M_\star\simeq10^{5.7}\,M_\odot$ at $z\simeq4.5$--$10.1$ from JWST Lensing Cluster Surveys

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    JWST lensing-cluster spectra push the z~6 mass–metallicity relation to M*~10^6.6 Msun and reveal a UV-vs-optical nitrogen discrepancy suggesting local nitrogen enhancement, possibly from Wolf-Rayet stars.

  2. The Synthetic Absorption Line Spectral Almanac (SALSA)

    astro-ph.GA 2025-10 conditional novelty 6.0 of 10

    A new public library generates millions of mock quasar absorption spectra from cosmological simulations, using a novel mesh-free Voronoi ray-tracing algorithm.

Reference graph

Works this paper leans on

267 extracted references · 42 canonical work pages · cited by 2 Pith papers

  1. [1]

    L., & Norman , M

    Abel , T., Bryan , G. L., & Norman , M. L. 2002, Science, 295, 93, 10.1126/science.295.5552.93

    doi:10.1126/science.295.5552.93 2002

  2. [2]

    S., Salvadori , S., Sk \'u lad \'o ttir , \'A ., et al

    Aguado , D. S., Salvadori , S., Sk \'u lad \'o ttir , \'A ., et al. 2023, , 520, 866, 10.1093/mnras/stad164

    doi:10.1093/mnras/stad164 2023

  3. [3]

    M., Nissen , P

    Amarsi , A. M., Nissen , P. E., & Sk \'u lad \'o ttir , \'A . 2019, , 630, A104, 10.1051/0004-6361/201936265

    doi:10.1051/0004-6361/201936265 2019

  4. [4]

    T., & Scheck , L

    Arcones , A., Janka , H. T., & Scheck , L. 2007, , 467, 1227, 10.1051/0004-6361:20066983

    doi:10.1051/0004-6361:20066983 2007

  5. [5]

    Z., Cullen , F., Carnall , A

    Arellano-C \'o rdova , K. Z., Cullen , F., Carnall , A. C., et al. 2024, arXiv e-prints, arXiv:2412.10557, 10.48550/arXiv.2412.10557

    arXiv doi:10.48550/arxiv.2412.10557 2024

  6. [6]

    2022, , 666, A109, 10.1051/0004-6361/202244258

    Arnaboldi , M., Bhattacharya , S., Gerhard , O., et al. 2022, , 666, A109, 10.1051/0004-6361/202244258

    doi:10.1051/0004-6361/202244258 2022

  7. [7]

    D., Meakin , C., Hirschi , R., et al

    Arnett , W. D., Meakin , C., Hirschi , R., et al. 2019, , 882, 18, 10.3847/1538-4357/ab21d9

    doi:10.3847/1538-4357/ab21d9 2019

  8. [8]

    J., & Scott , P

    Asplund , M., Grevesse , N., Sauval , A. J., & Scott , P. 2009, , 47, 481, 10.1146/annurev.astro.46.060407.145222

    arXiv 2009

Show all 267 references
  1. [9]

    1995, , 451, L49, 10.1086/309687

    Audouze , J., & Silk , J. 1995, , 451, L49, 10.1086/309687

    1995 doi

  2. [10]

    1967, , 18, 379, 10.1103/PhysRevLett.18.379

    Barkat , Z., Rakavy , G., & Sack , N. 1967, , 18, 379, 10.1103/PhysRevLett.18.379

    1967 doi

  3. [11]

    C., & Christlieb , N

    Beers , T. C., & Christlieb , N. 2005, , 43, 531, 10.1146/annurev.astro.42.053102.134057

    2005

  4. [12]

    2003, , 410, 527, 10.1051/0004-6361:20031213

    Bensby , T., Feltzing , S., & Lundstr \"o m , I. 2003, , 410, 527, 10.1051/0004-6361:20031213

    2003 doi

  5. [13]

    2004, , 415, 155, 10.1051/0004-6361:20031655

    ---. 2004, , 415, 155, 10.1051/0004-6361:20031655

    2004 doi

  6. [14]

    M., Crowther , P

    Bestenlehner , J. M., Crowther , P. A., Caballero-Nieves , S. M., et al. 2020, , 499, 1918, 10.1093/mnras/staa2801

    2020 doi

  7. [15]

    2015, , 449, 506, 10.1093/mnras/stv271

    Bisterzo , S., Gallino , R., K \"a ppeler , F., et al. 2015, , 449, 506, 10.1093/mnras/stv271

    2015 doi

  8. [16]

    X., Dessart , L., & Hillier , D

    Blondin , S., Bravo , E., Timmes , F. X., Dessart , L., & Hillier , D. J. 2022, , 660, A96, 10.1051/0004-6361/202142323

    2022 doi

  9. [17]

    Boesgaard , A. M. 1968, , 154, 185, 10.1086/149749

    1968 doi

  10. [18]

    A., de Koter , A., Bestenlehner , J

    Brands , S. A., de Koter , A., Bestenlehner , J. M., et al. 2022, , 663, A36, 10.1051/0004-6361/202142742

    2022 doi

  11. [19]

    Bromm , V., & Larson , R. B. 2004, , 42, 79, 10.1146/annurev.astro.42.053102.134034

    2004

  12. [21]

    E., Heger , A., Langer , N., et al

    Brown , G. E., Heger , A., Langer , N., et al. 2001, , 6, 457, 10.1016/S1384-1076(01)00077-X

    2001 doi

  13. [22]

    W., Mezzacappa , A., Hix , W

    Bruenn , S. W., Mezzacappa , A., Hix , W. R., et al. 2013, , 767, L6, 10.1088/2041-8205/767/1/L6

    2013 doi

  14. [23]

    V., et al

    Buck , T., Obreja , A., Macci \`o , A. V., et al. 2020, , 491, 3461, 10.1093/mnras/stz3241

    2020 doi

  15. [24]

    2018, , 478, 4513, 10.1093/mnras/sty1281

    Buder , S., Asplund , M., Duong , L., et al. 2018, , 478, 4513, 10.1093/mnras/sty1281

    2018 doi

  16. [25]

    J., Saxena , A., Cameron , A

    Bunker , A. J., Saxena , A., Cameron , A. J., et al. 2023, , 677, A88, 10.1051/0004-6361/202346159

    2023 doi

  17. [26]

    F., Doherty , C

    Buntain , J. F., Doherty , C. L., Lugaro , M., et al. 2017, , 471, 824, 10.1093/mnras/stx1502

    2017 doi

  18. [27]

    M., Burbidge , G

    Burbidge , E. M., Burbidge , G. R., Fowler , W. A., & Hoyle , F. 1957, Reviews of Modern Physics, 29, 547, 10.1103/RevModPhys.29.547

    1957 doi

  19. [28]

    1987, in Nuclear Astrophysics, ed

    Burkert , A., & Hensler , G. 1987, in Nuclear Astrophysics, ed. W. Hillebrandt , R. Kuhfuss , E. Mueller , & J. W. Truran , Vol. 287, 159, 10.1007/BFb0016576

    1987 doi

  20. [29]

    2021, , 589, 29, 10.1038/s41586-020-03059-w

    Burrows , A., & Vartanyan , D. 2021, , 589, 29, 10.1038/s41586-020-03059-w

    2021 doi

  21. [30]

    Busso , M., Gallino , R., & Wasserburg , G. J. 1999, , 37, 239, 10.1146/annurev.astro.37.1.239

    1999 doi

  22. [31]

    Cameron , A. G. W. 1973, , 15, 121, 10.1007/BF00172440

    1973 doi

  23. [32]

    J., Katz , H., Rey , M

    Cameron , A. J., Katz , H., Rey , M. P., & Saxena , A. 2023, , 523, 3516, 10.1093/mnras/stad1579

    2023 doi

  24. [33]

    M., Alatalo , K., et al

    Cappellari , M., McDermid , R. M., Alatalo , K., et al. 2013, , 432, 1862, 10.1093/mnras/stt644

    2013 doi

  25. [34]

    I., Cohen , J

    Carlos , M., Karakas , A. I., Cohen , J. G., Kobayashi , C., & Mel \'e ndez , J. 2018, , 856, 161, 10.3847/1538-4357/aab36c

    2018 doi

  26. [35]

    C., Cullen , F., McLure , R

    Carnall , A. C., Cullen , F., McLure , R. J., et al. 2024, , 534, 325, 10.1093/mnras/stae2092

    2024 doi

  27. [36]

    2004, , 416, 1117, 10.1051/0004-6361:20034074

    Cayrel , R., Depagne , E., Spite , M., et al. 2004, , 416, 1117, 10.1051/0004-6361:20034074

    2004 doi

  28. [37]

    Cen , R., & Ostriker , J. P. 1999, , 519, L109, 10.1086/312123

    1999 doi

  29. [38]

    2014, , 565, A51, 10.1051/0004-6361/201423432

    Cescutti , G., & Chiappini , C. 2014, , 565, A51, 10.1051/0004-6361/201423432

    2014 doi

  30. [39]

    2018, , 478, 4101, 10.1093/mnras/sty1185

    Cescutti , G., Hirschi , R., Nishimura , N., et al. 2018, , 478, 4101, 10.1093/mnras/sty1185

    2018 doi

  31. [40]

    2017, , 607, A23, 10.1051/0004-6361/201731398

    Cescutti , G., & Kobayashi , C. 2017, , 607, A23, 10.1051/0004-6361/201731398

    2017 doi

  32. [41]

    2003, , 115, 763, 10.1086/376392

    Chabrier , G. 2003, , 115, 763, 10.1086/376392

    2003 doi

  33. [42]

    2014, , 790, 162, 10.1088/0004-637X/790/2/162

    Chen , K.-J., Heger , A., Woosley , S., et al. 2014, , 790, 162, 10.1088/0004-637X/790/2/162

    2014 doi

  34. [43]

    2006, , 449, L27, 10.1051/0004-6361:20064866

    Chiappini , C., Hirschi , R., Meynet , G., et al. 2006, , 449, L27, 10.1051/0004-6361:20064866

    2006 doi

  35. [44]

    1997, , 477, 765, 10.1086/303726

    Chiappini , C., Matteucci , F., & Gratton , R. 1997, , 477, 765, 10.1086/303726

    1997 doi

  36. [45]

    2013, , 764, 21, 10.1088/0004-637X/764/1/21

    Chieffi , A., & Limongi , M. 2013, , 764, 21, 10.1088/0004-637X/764/1/21

    2013 doi

  37. [46]

    2018, , 618, A133, 10.1051/0004-6361/201833283

    Choplin , A., Hirschi , R., Meynet , G., et al. 2018, , 618, A133, 10.1051/0004-6361/201833283

    2018 doi

  38. [47]

    2012, , 744, 158, 10.1088/0004-637X/744/2/158

    Coc , A., Goriely , S., Xu , Y., Saimpert , M., & Vangioni , E. 2012, , 744, 158, 10.1088/0004-637X/744/2/158

    2012 doi

  39. [48]

    2013, , 51, 393, 10.1146/annurev-astro-082812-141017

    Conroy , C. 2013, , 51, 393, 10.1146/annurev-astro-082812-141017

    2013 doi

  40. [49]

    2019, , 875, 106, 10.3847/1538-4357/ab10db

    C \^o t \'e , B., Eichler , M., Arcones , A., et al. 2019, , 875, 106, 10.3847/1538-4357/ab10db

    2019 doi

  41. [50]

    2010, , 467, 811, 10.1038/nature09451

    Cresci , G., Mannucci , F., Maiolino , R., et al. 2010, , 467, 811, 10.1038/nature09451

    2010 doi

  42. [51]

    2011, , 197, 17, 10.1088/0067-0049/197/2/17

    Cristallo , S., Piersanti , L., Straniero , O., et al. 2011, , 197, 17, 10.1088/0067-0049/197/2/17

    2011 doi

  43. [53]

    A., Schnurr , O., Hirschi , R., et al

    Crowther , P. A., Schnurr , O., Hirschi , R., et al. 2010, , 408, 731, 10.1111/j.1365-2966.2010.17167.x

    2010

  44. [54]

    V., Lambert , D

    Cunha , K., Smith , V. V., Lambert , D. L., & Hinkle , K. H. 2003, , 126, 1305, 10.1086/377023

    2003 doi

  45. [55]

    2020, , 492, 821, 10.1093/mnras/stz3379

    Curti , M., Maiolino , R., Cirasuolo , M., et al. 2020, , 492, 821, 10.1093/mnras/stz3379

    2020 doi

  46. [56]

    2024, arXiv e-prints, arXiv:2407.02575, 10.48550/arXiv.2407.02575

    Curti , M., Witstok , J., Jakobsen , P., et al. 2024, arXiv e-prints, arXiv:2407.02575, 10.48550/arXiv.2407.02575

    2024 doi arXiv

  47. [57]

    2019, , 486, 2827, 10.1093/mnras/stz937

    Dav \'e , R., Angl \'e s-Alc \'a zar , D., Narayanan , D., et al. 2019, , 486, 2827, 10.1093/mnras/stz937

    2019 doi

  48. [58]

    2004, , 48, 861, 10.1016/j.newar.2004.07.001

    De Donder , E., & Vanbeveren , D. 2004, , 48, 861, 10.1016/j.newar.2004.07.001

    2004 doi

  49. [59]

    A., & Hartwick , F

    Denissenkov , P. A., & Hartwick , F. D. A. 2014, , 437, L21, 10.1093/mnrasl/slt133

    2014 doi

  50. [60]

    2024, , 689, A152, 10.1051/0004-6361/202348636

    D'Eugenio , F., Maiolino , R., Carniani , S., et al. 2024, , 689, A152, 10.1051/0004-6361/202348636

    2024 doi

  51. [61]

    L., Gil-Pons , P., Lau , H

    Doherty , C. L., Gil-Pons , P., Lau , H. H. B., Lattanzio , J. C., & Siess , L. 2014, , 437, 195, 10.1093/mnras/stt1877

    2014 doi

  52. [62]

    L., Gil-Pons , P., Siess , L., Lattanzio , J

    Doherty , C. L., Gil-Pons , P., Siess , L., Lattanzio , J. C., & Lau , H. H. B. 2015, , 446, 2599, 10.1093/mnras/stu2180

    2015 doi

  53. [63]

    2017, Galaxies, 5, 35, 10.3390/galaxies5030035

    Dolag , K., Mevius , E., & Remus , R.-S. 2017, Galaxies, 5, 35, 10.3390/galaxies5030035

    2017 doi

  54. [65]

    2016, , 463, 3948, 10.1093/mnras/stw2265

    Dubois , Y., Peirani , S., Pichon , C., et al. 2016, , 463, 3948, 10.1093/mnras/stw2265

    2016 doi

  55. [66]

    Federrath , C., Sur , S., Schleicher , D. R. G., Banerjee , R., & Klessen , R. S. 2011, , 731, 62, 10.1088/0004-637X/731/1/62

    2011 doi

  56. [67]

    G., Courty , S., Gibson , B

    Few , C. G., Courty , S., Gibson , B. K., Michel-Dansac , L., & Calura , F. 2014, , 444, 3845, 10.1093/mnras/stu1709

    2014 doi

  57. [68]

    S., McCarthy , I

    Font , A. S., McCarthy , I. G., Poole-Mckenzie , R., et al. 2020, , 498, 1765, 10.1093/mnras/staa2463

    2020 doi

  58. [69]

    Franco , M., Coppin , K. E. K., Geach , J. E., et al. 2021, Nature Astronomy, 5, 1240, 10.1038/s41550-021-01515-9

    2021 doi

  59. [70]

    J., Kavanagh , P

    Fransson , C., Barlow , M. J., Kavanagh , P. J., et al. 2024, Science, 383, 898, 10.1126/science.adj5796

    2024 doi

  60. [71]

    2016, , 456, 1803, 10.1093/mnras/stv2723

    Frischknecht , U., Hirschi , R., Pignatari , M., et al. 2016, , 456, 1803, 10.1093/mnras/stv2723

    2016 doi

  61. [72]

    1998, , 338, 161

    Fuhrmann , K. 1998, , 338, 161

    1998

  62. [73]

    M., Woosley , S

    Fuller , G. M., Woosley , S. E., & Weaver , T. A. 1986, , 307, 675, 10.1086/164452

    1986 doi

  63. [74]

    2023, , 674, A38, 10.1051/0004-6361/202243511

    Gaia Collaboration , Recio-Blanco , A., Kordopatis , G., et al. 2023, , 674, A38, 10.1051/0004-6361/202243511

    2023 doi

  64. [75]

    Grand , R. J. J., G \'o mez , F. A., Marinacci , F., et al. 2017, , 467, 179, 10.1093/mnras/stx071

    2017 doi

  65. [76]

    H., Springel , V., White , S

    Greif , T. H., Springel , V., White , S. D. M., et al. 2011, , 737, 75, 10.1088/0004-637X/737/2/75

    2011 doi

  66. [77]

    2022, , 926, L9, 10.3847/2041-8213/ac4f68

    Grichener , A., Kobayashi , C., & Soker , N. 2022, , 926, L9, 10.3847/2041-8213/ac4f68

    2022 doi

  67. [78]

    J., Heger , A., Karakas , A

    Grimmett , J. J., Heger , A., Karakas , A. I., & M \"u ller , B. 2018, , 479, 495, 10.1093/mnras/sty1417

    2018 doi

  68. [79]

    2019, , 489, 3539, 10.1093/mnras/stz2428

    Grisoni , V., Matteucci , F., Romano , D., & Fu , X. 2019, , 489, 3539, 10.1093/mnras/stz2428

    2019 doi

  69. [80]

    2017, , 472, 3637, 10.1093/mnras/stx2201

    Grisoni , V., Spitoni , E., Matteucci , F., et al. 2017, , 472, 3637, 10.1093/mnras/stx2201

    2017 doi

  70. [82]

    J., Montes , F., & Arcones , A

    Hansen , C. J., Montes , F., & Arcones , A. 2014, , 797, 123, 10.1088/0004-637X/797/2/123

    2014 doi

  71. [83]

    T., Andersen , J., Nordstr \"o m , B., et al

    Hansen , T. T., Andersen , J., Nordstr \"o m , B., et al. 2016, , 586, A160, 10.1051/0004-6361/201527235

    2016 doi

  72. [84]

    K., et al

    Harikane , Y., Ouchi , M., Inoue , A. K., et al. 2020, , 896, 93, 10.3847/1538-4357/ab94bd

    2020 doi

  73. [85]

    N., Kobayashi , C., Tominaga , N., & Nomoto , K

    Hartwig , T., Ishigaki , M. N., Kobayashi , C., Tominaga , N., & Nomoto , K. 2023, , 946, 20, 10.3847/1538-4357/acbcc6

    2023 doi

  74. [86]

    R., Bovy , J., Holtzman , J

    Hayden , M. R., Bovy , J., Holtzman , J. A., et al. 2015, , 808, 132, 10.1088/0004-637X/808/2/132

    2015 doi

  75. [87]

    2022, , 512, 2867, 10.1093/mnras/stac584

    Hayden-Pawson , C., Curti , M., Maiolino , R., et al. 2022, , 512, 2867, 10.1093/mnras/stac584

    2022 doi

  76. [88]

    J., & Kobayashi , C

    Haynes , C. J., & Kobayashi , C. 2019, , 483, 5123, 10.1093/mnras/sty3389

    2019 doi

  77. [89]

    Heger , A., & Woosley , S. E. 2002, , 567, 532, 10.1086/338487

    2002 doi

  78. [90]

    2010, , 724, 341, 10.1088/0004-637X/724/1/341

    ---. 2010, , 724, 341, 10.1088/0004-637X/724/1/341

    2010 doi

  79. [91]

    2005, , 43, 435, 10.1146/annurev.astro.43.072103.150600

    Herwig , F. 2005, , 43, 435, 10.1146/annurev.astro.43.072103.150600

    2005 arXiv

  80. [92]

    R., Vink , J

    Higgins , E. R., Vink , J. S., Hirschi , R., Laird , A. M., & Sabhahit , G. N. 2023, , 526, 534, 10.1093/mnras/stad2537

    2023 doi

  81. [93]

    2014, , 781, 60, 10.1088/0004-637X/781/2/60

    Hirano , S., Hosokawa , T., Yoshida , N., et al. 2014, , 781, 60, 10.1088/0004-637X/781/2/60

    2014 doi

  82. [94]

    2007, , 461, 571, 10.1051/0004-6361:20065356

    Hirschi , R. 2007, , 461, 571, 10.1051/0004-6361:20065356

    2007 doi

  83. [95]

    2017, , 551, 478, 10.1038/nature24301

    Hitomi Collaboration , Aharonian , F., Akamatsu , H., et al. 2017, , 551, 478, 10.1038/nature24301

    2017 doi

  84. [96]

    1996, , 457, 500, 10.1086/176748

    Hoeflich , P., & Khokhlov , A. 1996, , 457, 500, 10.1086/176748

    1996 doi

  85. [97]

    F., Hernquist , L., Cox , T

    Hopkins , P. F., Hernquist , L., Cox , T. J., et al. 2006, , 163, 1, 10.1086/499298

    2006 doi

  86. [98]

    F., Wetzel , A., Kere s , D., et al

    Hopkins , P. F., Wetzel , A., Kere s , D., et al. 2018, , 480, 800, 10.1093/mnras/sty1690

    2018 doi

  87. [99]

    1954, , 1, 121, 10.1086/190005

    Hoyle , F. 1954, , 1, 121, 10.1086/190005

    1954 doi

  88. [100]

    2024, , 527, 3276, 10.1093/mnras/stad3313

    Ibrahim , D., & Kobayashi , C. 2024, , 527, 3276, 10.1093/mnras/stad3313

    2024 doi

  89. [101]

    2025, arXiv e-prints, arXiv:2501.11209, 10.48550/arXiv.2501.11209

    ---. 2025, arXiv e-prints, arXiv:2501.11209, 10.48550/arXiv.2501.11209

    2025 doi

  90. [102]

    N., Tominaga , N., Kobayashi , C., & Nomoto , K

    Ishigaki , M. N., Tominaga , N., Kobayashi , C., & Nomoto , K. 2018, , 857, 46, 10.3847/1538-4357/aab3de

    2018 doi

  91. [103]

    J., & Rebolo , R

    Israelian , G., Garc \' a L \'o pez , R. J., & Rebolo , R. 1998, , 507, 805, 10.1086/306351

    1998 doi

  92. [104]

    1999, , 125, 439, 10.1086/313278

    Iwamoto , K., Brachwitz , F., Nomoto , K., et al. 1999, , 125, 439, 10.1086/313278

    1999 doi

  93. [105]

    A., Nomoto , K., et al

    Iwamoto , K., Mazzali , P. A., Nomoto , K., et al. 1998, , 395, 672, 10.1038/27155

    1998 doi

  94. [106]

    2012, Annual Review of Nuclear and Particle Science, 62, 407, 10.1146/annurev-nucl-102711-094901

    Janka , H.-T. 2012, Annual Review of Nuclear and Particle Science, 62, 407, 10.1146/annurev-nucl-102711-094901

    2012 doi

  95. [107]

    P., Frebel , A., Chiti , A., & Simon , J

    Ji , A. P., Frebel , A., Chiti , A., & Simon , J. D. 2016, , 531, 610, 10.1038/nature17425

    2016 doi

  96. [108]

    2010, , 725, L176, 10.1088/2041-8205/725/2/L176

    Jones , T., Ellis , R., Jullo , E., & Richard , J. 2010, , 725, L176, 10.1088/2041-8205/725/2/L176

    2010 doi

  97. [109]

    M., et al

    J \"o nsson , H., Ryde , N., Harper , G. M., et al. 2014, , 564, A122, 10.1051/0004-6361/201423597

    2014 doi

  98. [110]

    V., & Lambert , D

    Jorissen , A., Smith , V. V., & Lambert , D. L. 1992, , 261, 164

    1992

  99. [111]

    A., Obergaulinger , M., & Nagataki , S

    Just , O., Aloy , M. A., Obergaulinger , M., & Nagataki , S. 2022, , 934, L30, 10.3847/2041-8213/ac83a1

    2022 doi

  100. [112]

    Just , O., Bauswein , A., Ardevol Pulpillo , R., Goriely , S., & Janka , H. T. 2015, , 448, 541, 10.1093/mnras/stv009

    2015 doi

  101. [114]

    I., & Lattanzio , J

    Karakas , A. I., & Lattanzio , J. C. 2014, , 31, e030, 10.1017/pasa.2014.21

    2014 doi

  102. [115]

    I., & Lugaro , M

    Karakas , A. I., & Lugaro , M. 2016, , 825, 26, 10.3847/0004-637X/825/1/26

    2016 doi

  103. [116]

    1992, , 391, 502, 10.1086/171366

    Katz , N. 1992, , 391, 502, 10.1086/171366

    1992 doi

  104. [117]

    Kawata , D., & Gibson , B. K. 2003, , 340, 908, 10.1046/j.1365-8711.2003.06356.x

    2003

  105. [118]

    C., Bessell , M

    Keller , S. C., Bessell , M. S., Frebel , A., et al. 2014, , 506, 463, 10.1038/nature12990

    2014 doi

  106. [119]

    J., Karakas , A

    Kemp , A. J., Karakas , A. I., Casey , A. R., Kobayashi , C., & Izzard , R. G. 2022, , 509, 1175, 10.1093/mnras/stab3103

    2022 doi

  107. [120]

    C., & Evans , N

    Kennicutt , R. C., & Evans , N. J. 2012, , 50, 531, 10.1146/annurev-astro-081811-125610

    2012 doi

  108. [121]

    E., Schmidt , B

    Kerzendorf , W. E., Schmidt , B. P., Asplund , M., et al. 2009, , 701, 1665, 10.1088/0004-637X/701/2/1665

    2009 doi

  109. [122]

    J., Nicholls , D

    Kewley , L. J., Nicholls , D. C., & Sutherland , R. S. 2019, , 57, 511, 10.1146/annurev-astro-081817-051832

    2019 doi

  110. [123]

    N., Xie , J

    Kirby , E. N., Xie , J. L., Guo , R., et al. 2019, , 881, 45, 10.3847/1538-4357/ab2c02

    2019 doi

  111. [124]

    2004, , 347, 740, 10.1111/j.1365-2966.2004.07258.x

    Kobayashi , C. 2004, , 347, 740, 10.1111/j.1365-2966.2004.07258.x

    2004

  112. [125]

    2010, in American Institute of Physics Conference Series, Vol

    Kobayashi , C. 2010, in American Institute of Physics Conference Series, Vol. 1240, Hunting for the Dark: the Hidden Side of Galaxy Formation, ed. V. P. Debattista & C. C. Popescu , 123--126, 10.1063/1.3458465

    2010 doi

  113. [126]

    2014, in Setting the scene for Gaia and LAMOST, ed

    Kobayashi , C. 2014, in Setting the scene for Gaia and LAMOST, ed. S. Feltzing , G. Zhao , N. A. Walton , & P. Whitelock , Vol. 298, 167--178, 10.1017/S1743921313006339

    2014 doi

  114. [127]

    2016, in The General Assembly of Galaxy Halos: Structure, Origin and Evolution, ed

    Kobayashi , C. 2016, in The General Assembly of Galaxy Halos: Structure, Origin and Evolution, ed. A. Bragaglia , M. Arnaboldi , M. Rejkuba , & D. Romano , Vol. 317, 57--63, 10.1017/S1743921315009783

    2016 doi

  115. [128]

    2022, in The Origin of Outflows in Evolved Stars, ed

    Kobayashi , C. 2022, in The Origin of Outflows in Evolved Stars, ed. L. Decin , A. Zijlstra , & C. Gielen , Vol. 366, 63--82, 10.1017/S1743921322001132

    2022 doi

  116. [129]

    2023, Experimental Astronomy, 55, 75, 10.1007/s10686-022-09862-9

    ---. 2023, Experimental Astronomy, 55, 75, 10.1007/s10686-022-09862-9

    2023 doi

  117. [130]

    2023 a , , 956, L14, 10.3847/2041-8213/acf7c7

    Kobayashi , C., Bhattacharya , S., Arnaboldi , M., & Gerhard , O. 2023 a , , 956, L14, 10.3847/2041-8213/acf7c7

    2023 doi

  118. [131]

    2024, , 962, L6, 10.3847/2041-8213/ad1de1

    Kobayashi , C., & Ferrara , A. 2024, , 962, L6, 10.3847/2041-8213/ad1de1

    2024 doi

  119. [132]

    N., Tominaga , N., & Nomoto , K

    Kobayashi , C., Ishigaki , M. N., Tominaga , N., & Nomoto , K. 2014, , 785, L5, 10.1088/2041-8205/785/1/L5

    2014 doi

  120. [133]

    I., et al

    Kobayashi , C., Izutani , N., Karakas , A. I., et al. 2011 a , , 739, L57, 10.1088/2041-8205/739/2/L57

    2011 doi

  121. [134]

    I., & Lugaro , M

    Kobayashi , C., Karakas , A. I., & Lugaro , M. 2020 a , , 900, 179, 10.3847/1538-4357/abae65

    2020 doi

  122. [136]

    2020 b , , 895, 138, 10.3847/1538-4357/ab8e44

    Kobayashi , C., Leung , S.-C., & Nomoto , K. 2020 b , , 895, 138, 10.3847/1538-4357/ab8e44

    2020 doi

  123. [137]

    2011, , 729, 16, 10.1088/0004-637X/729/1/16

    Kobayashi , C., & Nakasato , N. 2011, , 729, 16, 10.1088/0004-637X/729/1/16

    2011 doi

  124. [138]

    2009, , 707, 1466, 10.1088/0004-637X/707/2/1466

    Kobayashi , C., & Nomoto , K. 2009, , 707, 1466, 10.1088/0004-637X/707/2/1466

    2009 doi

  125. [139]

    2015, , 804, L24, 10.1088/2041-8205/804/1/L24

    Kobayashi , C., Nomoto , K., & Hachisu , I. 2015, , 804, L24, 10.1088/2041-8205/804/1/L24

    2015 doi

  126. [140]

    Kobayashi , C., Springel , V., & White , S. D. M. 2007, , 376, 1465, 10.1111/j.1365-2966.2007.11555.x

    2007

  127. [141]

    2023, arXiv e-prints, arXiv:2302.07255, 10.48550/arXiv.2302.07255

    Kobayashi , C., & Taylor , P. 2023, arXiv e-prints, arXiv:2302.07255, 10.48550/arXiv.2302.07255

    2023 doi arXiv

  128. [142]

    2011 c , , 730, L14, 10.1088/2041-8205/730/2/L14

    Kobayashi , C., Tominaga , N., & Nomoto , K. 2011 c , , 730, L14, 10.1088/2041-8205/730/2/L14

    2011 doi

  129. [143]

    2000, , 539, 26, 10.1086/309195

    Kobayashi , C., Tsujimoto , T., & Nomoto , K. 2000, , 539, 26, 10.1086/309195

    2000 doi

  130. [144]

    1998, , 503, L155, 10.1086/311556

    Kobayashi , C., Tsujimoto , T., Nomoto , K., Hachisu , I., & Kato , M. 1998, , 503, L155, 10.1086/311556

    1998 doi

  131. [145]

    2006, , 653, 1145, 10.1086/508914

    Kobayashi , C., Umeda , H., Nomoto , K., Tominaga , N., & Ohkubo , T. 2006, , 653, 1145, 10.1086/508914

    2006 doi

  132. [146]

    2023 b , , 943, L12, 10.3847/2041-8213/acad82

    Kobayashi , C., Mandel , I., Belczynski , K., et al. 2023 b , , 943, L12, 10.3847/2041-8213/acad82

    2023 doi

  133. [147]

    Kormendy , J., & Ho , L. C. 2013, , 51, 511, 10.1146/annurev-astro-082708-101811

    2013 doi

  134. [148]

    2012, Progress of Theoretical and Experimental Physics, 2012, 01A301, 10.1093/ptep/pts009

    Kotake , K., Sumiyoshi , K., Yamada , S., et al. 2012, Progress of Theoretical and Experimental Physics, 2012, 01A301, 10.1093/ptep/pts009

    2012 doi

  135. [149]

    P., Sneden , C., Smith , G

    Kraft , R. P., Sneden , C., Smith , G. H., et al. 1997, , 113, 279, 10.1086/118251

    1997 doi

  136. [150]

    G., et al

    Kriek , M., Conroy , C., van Dokkum , P. G., et al. 2016, , 540, 248, 10.1038/nature20570

    2016 doi

  137. [151]

    A., Fink , M., et al

    Kromer , M., Sim , S. A., Fink , M., et al. 2010, , 719, 1067, 10.1088/0004-637X/719/2/1067

    2010 doi

  138. [152]

    2001, , 322, 231, 10.1046/j.1365-8711.2001.04022.x

    Kroupa , P. 2001, , 322, 231, 10.1046/j.1365-8711.2001.04022.x

    2001

  139. [153]

    2008, in Astronomical Society of the Pacific Conference Series, Vol

    Kroupa , P. 2008, in Astronomical Society of the Pacific Conference Series, Vol. 390, Pathways Through an Eclectic Universe, ed. J. H. Knapen , T. J. Mahoney , & A. Vazdekis , 3. 0708.1164

    2008 arXiv

  140. [154]

    A., & Gilmore , G

    Kroupa , P., Tout , C. A., & Gilmore , G. 1993, , 262, 545, 10.1093/mnras/262.3.545

    1993 doi

  141. [155]

    2018, , 861, 143, 10.3847/1538-4357/aac2df

    Leung , S.-C., & Nomoto , K. 2018, , 861, 143, 10.3847/1538-4357/aac2df

    2018 doi

  142. [156]

    2020, , 888, 80, 10.3847/1538-4357/ab5c1f

    ---. 2020, , 888, 80, 10.3847/1538-4357/ab5c1f

    2020 doi

  143. [157]

    2018, , 237, 13, 10.3847/1538-4365/aacb24

    Limongi , M., & Chieffi , A. 2018, , 237, 13, 10.3847/1538-4365/aacb24

    2018 doi

  144. [158]

    2003, , 594, L123, 10.1086/378734

    Limongi , M., Chieffi , A., & Bonifacio , P. 2003, , 594, L123, 10.1086/378734

    2003 doi

  145. [159]

    Lind , K., & Amarsi , A. M. 2024, , 62, 475, 10.1146/annurev-astro-052722-103557

    2024 doi

  146. [160]

    2022, , 665, A33, 10.1051/0004-6361/202142195

    Lind , K., Nordlander , T., Wehrhahn , A., et al. 2022, , 665, A33, 10.1051/0004-6361/202142195

    2022 doi

  147. [161]

    A., Pignatari , M., & Herwig , F

    Lucatello , S., Masseron , T., Johnson , J. A., Pignatari , M., & Herwig , F. 2011, , 729, 40, 10.1088/0004-637X/729/1/40

    2011 doi

  148. [162]

    2014, , 52, 415, 10.1146/annurev-astro-081811-125615

    Madau , P., & Dickinson , M. 2014, , 52, 415, 10.1146/annurev-astro-081811-125615

    2014 doi

  149. [163]

    2003, , 598, 1163, 10.1086/378948

    Maeda , K., & Nomoto , K. 2003, , 598, 1163, 10.1086/378948

    2003 doi

  150. [164]

    2000, , 38, 143, 10.1146/annurev.astro.38.1.143

    Maeder , A., & Meynet , G. 2000, , 38, 143, 10.1146/annurev.astro.38.1.143

    2000 doi

  151. [165]

    1998, , 115, 2285, 10.1086/300353

    Magorrian , J., Tremaine , S., Richstone , D., et al. 1998, , 115, 2285, 10.1086/300353

    1998 doi

  152. [166]

    2019, , 27, 3, 10.1007/s00159-018-0112-2

    Maiolino , R., & Mannucci , F. 2019, , 27, 3, 10.1007/s00159-018-0112-2

    2019 doi

  153. [167]

    2014, , 52, 107, 10.1146/annurev-astro-082812-141031

    Maoz , D., Mannucci , F., & Nelemans , G. 2014, , 52, 107, 10.1146/annurev-astro-082812-141031

    2014 doi

  154. [168]

    Marek , A., & Janka , H. T. 2009, , 694, 664, 10.1088/0004-637X/694/1/664

    2009 doi

  155. [169]

    2022, , 664, A181, 10.1051/0004-6361/202243474

    Martinet , S., Meynet , G., Nandal , D., et al. 2022, , 664, A181, 10.1051/0004-6361/202243474

    2022 doi

  156. [170]

    2001, The chemical evolution of the Galaxy , Vol

    Matteucci , F. 2001, The chemical evolution of the Galaxy , Vol. 253, 10.1007/978-94-010-0967-6

    2001 doi

  157. [171]

    2021, , 29, 5, 10.1007/s00159-021-00133-8

    ---. 2021, , 29, 5, 10.1007/s00159-021-00133-8

    2021 doi

  158. [172]

    1990, , 365, 539, 10.1086/169508

    Matteucci , F., & Brocato , E. 1990, , 365, 539, 10.1086/169508

    1990 doi

  159. [173]

    2014, , 438, 2177, 10.1093/mnras/stt2350

    Matteucci , F., Romano , D., Arcones , A., Korobkin , O., & Rosswog , S. 2014, , 438, 2177, 10.1093/mnras/stt2350

    2014 doi

  160. [174]

    2024, , 534, L35, 10.1093/mnrasl/slae077

    McKenzie , M., Monty , S., Yong , D., et al. 2024, , 534, L35, 10.1093/mnrasl/slae077

    2024 doi

  161. [175]

    2014, , 564, A134, 10.1051/0004-6361/201322198

    Mennekens , N., & Vanbeveren , D. 2014, , 564, A134, 10.1051/0004-6361/201322198

    2014 doi

  162. [176]

    2016, , 589, A64, 10.1051/0004-6361/201628193

    ---. 2016, , 589, A64, 10.1051/0004-6361/201628193

    2016 doi

  163. [177]

    2002, , 390, 561, 10.1051/0004-6361:20020755

    Meynet , G., & Maeder , A. 2002, , 390, 561, 10.1051/0004-6361:20020755

    2002 doi

  164. [178]

    C., & Hernquist , L

    Mihos , J. C., & Hernquist , L. 1996, , 464, 641, 10.1086/177353

    1996 doi

  165. [179]

    F., Halevi , G., et al

    M \"o sta , P., Roberts , L. F., Halevi , G., et al. 2018, , 864, 171, 10.3847/1538-4357/aad6ec

    2018 doi

  166. [180]

    2020, , 498, 3549, 10.1093/mnras/staa2610

    Mura-Guzm \'a n , A., Yong , D., Abate , C., et al. 2020, , 498, 3549, 10.1093/mnras/staa2610

    2020 doi

  167. [181]

    2023, , 949, L16, 10.3847/2041-8213/acd550

    Nagele , C., & Umeda , H. 2023, , 949, L16, 10.3847/2041-8213/acd550

    2023 doi

  168. [182]

    A., Woods , T

    Nandal , D., Regan , J. A., Woods , T. E., et al. 2024, , 683, A156, 10.1051/0004-6361/202348035

    2024 doi

  169. [183]

    F., & White , S

    Navarro , J. F., & White , S. D. M. 1994, , 267, 401, 10.1093/mnras/267.2.401

    1994 doi

  170. [184]

    2015, , 810, 109, 10.1088/0004-637X/810/2/109

    Nishimura , N., Takiwaki , T., & Thielemann , F.-K. 2015, , 810, 109, 10.1088/0004-637X/810/2/109

    2015 doi

  171. [185]

    1987, , 322, 206, 10.1086/165716

    Nomoto , K. 1987, , 322, 206, 10.1086/165716

    1987 doi

  172. [186]

    1997 a , , 616, 79, 10.1016/S0375-9474(97)00076-6

    Nomoto , K., Hashimoto , M., Tsujimoto , T., et al. 1997 a , , 616, 79, 10.1016/S0375-9474(97)00076-6

    1997 doi

  173. [187]

    1997 b , , 621, 467, 10.1016/S0375-9474(97)00291-1

    Nomoto , K., Iwamoto , K., Nakasato , N., et al. 1997 b , , 621, 467, 10.1016/S0375-9474(97)00291-1

    1997 doi

  174. [188]

    2013, , 51, 457, 10.1146/annurev-astro-082812-140956

    Nomoto , K., Kobayashi , C., & Tominaga , N. 2013, , 51, 457, 10.1146/annurev-astro-082812-140956

    2013 doi

  175. [189]

    1984, , 286, 644

    Nomoto, K., Thielemann, F.-K., & Yokoi, K. 1984, , 286, 644

    1984

  176. [190]

    M., Lind , K., et al

    Nordlander , T., Amarsi , A. M., Lind , K., et al. 2017, , 597, A6, 10.1051/0004-6361/201629202

    2017 doi

  177. [191]

    Nugent , P., Baron , E., Branch , D., Fisher , A., & Hauschildt , P. H. 1997, , 485, 812, 10.1086/304459

    1997 doi

  178. [192]

    A., Brammer , G., van Dokkum , P

    Oesch , P. A., Brammer , G., van Dokkum , P. G., et al. 2016, , 819, 129, 10.3847/0004-637X/819/2/129

    2016 doi

  179. [193]

    Pagel , B. E. J. 1997, Nucleosynthesis and Chemical Evolution of Galaxies

    1997

  180. [194]

    2004, in Cosmochemistry

    Pettini , M. 2004, in Cosmochemistry. The melting pot of the elements, ed. C. Esteban , R. Garc \' a L \'o pez , A. Herrero , & F. S \'a nchez , 257--298, 10.48550/arXiv.astro-ph/0303272

    2004 doi arXiv

  181. [195]

    2018, , 473, 4077, 10.1093/mnras/stx2656

    Pillepich , A., Springel , V., Nelson , D., et al. 2018, , 473, 4077, 10.1093/mnras/stx2656

    2018 doi

  182. [196]

    1998, , 334, 505

    Portinari , L., Chiosi , C., & Bressan , A. 1998, , 334, 505. astro-ph/9711337

    1998 arXiv

  183. [197]

    2018, , 476, 3432, 10.1093/mnras/sty316

    Prantzos , N., Abia , C., Limongi , M., Chieffi , A., & Cristallo , S. 2018, , 476, 3432, 10.1093/mnras/sty316

    2018 doi

  184. [198]

    1993, , 403, 630, 10.1086/172233

    Prantzos , N., Casse , M., & Vangioni-Flam , E. 1993, , 403, 630, 10.1086/172233

    1993 doi

  185. [199]

    Rees , M. J. 1984, , 22, 471, 10.1146/annurev.aa.22.090184.002351

    1984

  186. [200]

    \'A ., & Arcones , A

    Reichert , M., Obergaulinger , M., Eichler , M., Aloy , M. \'A ., & Arcones , A. 2021, , 501, 5733, 10.1093/mnras/stab029

    2021 doi

  187. [201]

    2025, , 536, L8, 10.1093/mnrasl/slae101

    Renzini , A. 2025, , 536, L8, 10.1093/mnrasl/slae101

    2025 doi

  188. [202]

    2018, , 480, 538, 10.1093/mnras/sty1729

    Ritter , C., Herwig , F., Jones , S., et al. 2018, , 480, 538, 10.1093/mnras/sty1729

    2018 doi

  189. [203]

    2024 a , , 272, 15, 10.3847/1538-4365/ad391d

    Roberti , L., Limongi , M., & Chieffi , A. 2024 a , , 272, 15, 10.3847/1538-4365/ad391d

    2024 doi

  190. [204]

    2024 b , , 270, 28, 10.3847/1538-4365/ad1686

    ---. 2024 b , , 270, 28, 10.3847/1538-4365/ad1686

    2024 doi

  191. [205]

    U., Preston , G

    Roederer , I. U., Preston , G. W., Thompson , I. B., et al. 2014, , 147, 136, 10.1088/0004-6256/147/6/136

    2014 doi

  192. [206]

    I., Tosi , M., & Matteucci , F

    Romano , D., Karakas , A. I., Tosi , M., & Matteucci , F. 2010, , 522, A32, 10.1051/0004-6361/201014483

    2010 doi

  193. [207]

    J., & Ventura , P

    Romano , D., Matteucci , F., Zhang , Z.-Y., Ivison , R. J., & Ventura , P. 2019, , 490, 2838, 10.1093/mnras/stz2741

    2019 doi

  194. [208]

    K., Kromer , M., Seitenzahl , I

    R \"o pke , F. K., Kromer , M., Seitenzahl , I. R., et al. 2012, , 750, L19, 10.1088/2041-8205/750/1/L19

    2012 doi

  195. [209]

    J., & Seitenzahl , I

    Ruiter , A. J., & Seitenzahl , I. R. 2024, arXiv e-prints, arXiv:2412.01766, 10.48550/arXiv.2412.01766

    2024 doi arXiv

  196. [210]

    2023, , 948, 35, 10.3847/1538-4357/acc39f

    Saccardi , A., Salvadori , S., D'Odorico , V., et al. 2023, , 948, 35, 10.3847/1538-4357/acc39f

    2023 doi

  197. [211]

    Salpeter , E. E. 1955, , 121, 161, 10.1086/145971

    1955 doi

  198. [212]

    H., et al

    Scannapieco , C., Wadepuhl , M., Parry , O. H., et al. 2012, , 423, 1726, 10.1111/j.1365-2966.2012.20993.x

    2012

  199. [213]

    A., Bower , R

    Schaye , J., Crain , R. A., Bower , R. G., et al. 2015, , 446, 521, 10.1093/mnras/stu2058

    2015 doi

  200. [214]

    Schneider , F. R. N., Sana , H., Evans , C. J., et al. 2018, Science, 359, 69, 10.1126/science.aan0106

    2018 doi

  201. [215]

    R., Cescutti , G., R \"o pke , F

    Seitenzahl , I. R., Cescutti , G., R \"o pke , F. K., Ruiter , A. J., & Pakmor , R. 2013, , 559, L5, 10.1051/0004-6361/201322599

    2013 doi

  202. [216]

    M., Barnes , J., & Metzger , B

    Siegel , D. M., Barnes , J., & Metzger , B. D. 2019, , 569, 241, 10.1038/s41586-019-1136-0

    2019 doi

  203. [217]

    2024, , 968, L23, 10.3847/2041-8213/ad4b1a

    Sk \'u lad \'o ttir , \'A ., Koutsouridou , I., Vanni , I., et al. 2024, , 968, L23, 10.3847/2041-8213/ad4b1a

    2024 doi

  204. [218]

    Smartt , S. J. 2009, , 47, 63, 10.1146/annurev-astro-082708-101737

    2009 doi

  205. [219]

    J., Kobayashi , C., et al

    Sneden , C., Cowan , J. J., Kobayashi , C., et al. 2016, , 817, 53, 10.3847/0004-637X/817/1/53

    2016 doi

  206. [220]

    2005, , 430, 655, 10.1051/0004-6361:20041274

    Spite , M., Cayrel , R., Plez , B., et al. 2005, , 430, 655, 10.1051/0004-6361:20041274

    2005 doi

  207. [221]

    2019, , 623, A60, 10.1051/0004-6361/201834188

    Spitoni , E., Silva Aguirre , V., Matteucci , F., Calura , F., & Grisoni , V. 2019, , 623, A60, 10.1051/0004-6361/201834188

    2019 doi

  208. [222]

    2010, , 401, 791, 10.1111/j.1365-2966.2009.15715.x

    Springel , V. 2010, , 401, 791, 10.1111/j.1365-2966.2009.15715.x

    2010

  209. [223]

    2005, , 361, 776, 10.1111/j.1365-2966.2005.09238.x

    Springel , V., Di Matteo , T., & Hernquist , L. 2005, , 361, 776, 10.1111/j.1365-2966.2005.09238.x

    2005

  210. [224]

    Springel , V., Yoshida , N., & White , S. D. M. 2001, , 6, 79, 10.1016/S1384-1076(01)00042-2

    2001 doi

  211. [225]

    2013, , 433, 1094, 10.1093/mnras/stt789

    Stacy , A., & Bromm , V. 2013, , 433, 1094, 10.1093/mnras/stt789

    2013 doi

  212. [226]

    1994, , 281, L97

    Steinmetz , M., & Mueller , E. 1994, , 281, L97. astro-ph/9312010

    1994 arXiv

  213. [227]

    2022, , 658, A125, 10.1051/0004-6361/202141536

    Sz \'e csi , D., Agrawal , P., W \"u nsch , R., & Langer , N. 2022, , 658, A125, 10.1051/0004-6361/202141536

    2022 doi

  214. [228]

    2018, , 857, 111, 10.3847/1538-4357/aab95f

    Takahashi , K., Yoshida , T., & Umeda , H. 2018, , 857, 111, 10.3847/1538-4357/aab95f

    2018 doi

  215. [229]

    2014, , 442, 2751, 10.1093/mnras/stu983

    Taylor , P., & Kobayashi , C. 2014, , 442, 2751, 10.1093/mnras/stu983

    2014 doi

  216. [230]

    2015 a , , 448, 1835, 10.1093/mnras/stv139

    ---. 2015 a , , 448, 1835, 10.1093/mnras/stv139

    2015 doi

  217. [231]

    2015 b , , 452, L59, 10.1093/mnrasl/slv087

    ---. 2015 b , , 452, L59, 10.1093/mnrasl/slv087

    2015 doi

  218. [232]

    2017, , 471, 3856, 10.1093/mnras/stx1860

    ---. 2017, , 471, 3856, 10.1093/mnras/stx1860

    2017 doi

  219. [233]

    Taylor , P., Kobayashi , C., & Kewley , L. J. 2020, , 496, 4433, 10.1093/mnras/staa1904

    2020 doi

  220. [234]

    2002, , 385, 337, 10.1051/0004-6361:20011817

    Teyssier , R. 2002, , 385, 337, 10.1051/0004-6361:20011817

    2002 doi

  221. [235]

    2003, , 401, 429, 10.1051/0004-6361:20030153

    Thomas , D., & Maraston , C. 2003, , 401, 429, 10.1051/0004-6361:20030153

    2003 doi

  222. [236]

    2005, , 621, 673, 10.1086/426932

    Thomas , D., Maraston , C., Bender , R., & Mendes de Oliveira , C. 2005, , 621, 673, 10.1086/426932

    2005 doi

  223. [237]

    X., Woosley , S

    Timmes , F. X., Woosley , S. E., & Weaver , T. A. 1995, , 98, 617, 10.1086/192172

    1995 doi

  224. [238]

    Tinsley , B. M. 1980, , 5, 287

    1980

  225. [239]

    2009, , 690, 526, 10.1088/0004-637X/690/1/526

    Tominaga , N. 2009, , 690, 526, 10.1088/0004-637X/690/1/526

    2009 doi

  226. [240]

    2007, , 660, 516, 10.1086/513063

    Tominaga , N., Umeda , H., & Nomoto , K. 2007, , 660, 516, 10.1086/513063

    2007 doi

  227. [241]

    Trujillo , I., Ferreras , I., & de La Rosa , I. G. 2011, , 415, 3903, 10.1111/j.1365-2966.2011.19017.x

    2011

  228. [242]

    2003, , 422, 871, 10.1038/nature01571

    Umeda , H., & Nomoto , K. 2003, , 422, 871, 10.1038/nature01571

    2003 doi

  229. [243]

    van de Voort , F., Pakmor , R., Bieri , R., & Grand , R. J. J. 2022, , 512, 5258, 10.1093/mnras/stac710

    2022 doi

  230. [244]

    van de Voort , F., Pakmor , R., Grand , R. J. J., et al. 2020, , 494, 4867, 10.1093/mnras/staa754

    2020 doi

  231. [245]

    G., & Conroy , C

    van Dokkum , P. G., & Conroy , C. 2010, , 468, 940, 10.1038/nature09578

    2010 doi

  232. [246]

    2023, , 526, 2620, 10.1093/mnras/stad2910

    Vanni , I., Salvadori , S., Sk \'u lad \'o ttir , \'A ., Rossi , M., & Koutsouridou , I. 2023, , 526, 2620, 10.1093/mnras/stad2910

    2023 doi

  233. [247]

    2023, , 678, A173, 10.1051/0004-6361/202346981

    Vanzella , E., Loiacono , F., Bergamini , P., et al. 2023, , 678, A173, 10.1051/0004-6361/202346981

    2023 doi

  234. [248]

    2009, , 499, 835, 10.1051/0004-6361/200811139

    Ventura , P., & D'Antona , F. 2009, , 499, 835, 10.1051/0004-6361/200811139

    2009 doi

  235. [249]

    2018 a , , 478, 155, 10.1093/mnras/sty1047

    Vincenzo , F., & Kobayashi , C. 2018 a , , 478, 155, 10.1093/mnras/sty1047

    2018 doi

  236. [250]

    2018 b , , 610, L16, 10.1051/0004-6361/201732395

    ---. 2018 b , , 610, L16, 10.1051/0004-6361/201732395

    2018 doi

  237. [251]

    2020, , 496, 80, 10.1093/mnras/staa1451

    ---. 2020, , 496, 80, 10.1093/mnras/staa1451

    2020 doi

  238. [252]

    2019, , 488, 4674, 10.1093/mnras/stz2065

    Vincenzo , F., Kobayashi , C., & Yuan , T. 2019, , 488, 4674, 10.1093/mnras/stz2065

    2019 doi

  239. [253]

    Vink , J. S. 2022, , 60, 203, 10.1146/annurev-astro-052920-094949

    2022 doi

  240. [254]

    S., Muijres , L

    Vink , J. S., Muijres , L. E., Anthonisse , B., et al. 2011, , 531, A132, 10.1051/0004-6361/201116614

    2011 doi

  241. [255]

    2023, , 944, 40, 10.3847/1538-4357/acac91

    Volpato , G., Marigo , P., Costa , G., et al. 2023, , 944, 40, 10.3847/1538-4357/acac91

    2023 doi

  242. [256]

    B., Hotchkis , M

    Wallner , A., Froehlich , M. B., Hotchkis , M. A. C., et al. 2021, Science, 372, 742, 10.1126/science.aax3972

    2021 doi

  243. [257]

    Wallstr \"o m , S. H. J., Muller , S., Roueff , E., et al. 2019, , 629, A128, 10.1051/0004-6361/201935860

    2019 doi

  244. [258]

    2013, , 770, L22, 10.1088/2041-8205/770/2/L22

    Wanajo , S. 2013, , 770, L22, 10.1088/2041-8205/770/2/L22

    2013 doi

  245. [259]

    2013, , 767, L26, 10.1088/2041-8205/767/2/L26

    Wanajo , S., Janka , H.-T., & M \"u ller , B. 2013, , 767, L26, 10.1088/2041-8205/767/2/L26

    2013 doi

  246. [260]

    T., Kitaura , F

    Wanajo , S., Nomoto , K., Janka , H. T., Kitaura , F. S., & M \"u ller , B. 2009, , 695, 208, 10.1088/0004-637X/695/1/208

    2009 doi

  247. [261]

    2014, , 789, L39, 10.1088/2041-8205/789/2/L39

    Wanajo , S., Sekiguchi , Y., Nishimura , N., et al. 2014, , 789, L39, 10.1088/2041-8205/789/2/L39

    2014 doi

  248. [262]

    Wehmeyer , B., Pignatari , M., & Thielemann , F. K. 2015, , 452, 1970, 10.1093/mnras/stv1352

    2015 doi

  249. [263]

    2012, , 750, L22, 10.1088/2041-8205/750/1/L22

    Winteler , C., K \"a ppeli , R., Perego , A., et al. 2012, , 750, L22, 10.1088/2041-8205/750/1/L22

    2012 doi

  250. [264]

    M., Gawiser , E., & Prochaska , J

    Wolfe , A. M., Gawiser , E., & Prochaska , J. X. 2005, , 43, 861, 10.1146/annurev.astro.42.053102.133950

    2005

  251. [265]

    E., Agarwal , B., Bromm , V., et al

    Woods , T. E., Agarwal , B., Bromm , V., et al. 2019, , 36, e027, 10.1017/pasa.2019.14

    2019 doi

  252. [266]

    E., & Weaver , T

    Woosley , S. E., & Weaver , T. A. 1995, , 101, 181, 10.1086/192237

    1995 doi

  253. [267]

    M., & Gonzalez , J

    Worthey , G., Faber , S. M., & Gonzalez , J. J. 1992, , 398, 69, 10.1086/171836

    1992 doi

  254. [268]

    L., & Ivans , I

    Yong , D., Lambert , D. L., & Ivans , I. I. 2003, , 599, 1357, 10.1086/379369

    2003 doi

  255. [269]

    S., et al

    Yong , D., Kobayashi , C., Da Costa , G. S., et al. 2021, , 595, 223, 10.1038/s41586-021-03611-2

    2021 doi

  256. [270]

    T., Kewley , L

    Yuan , T. T., Kewley , L. J., Swinbank , A. M., Richard , J., & Livermore , R. C. 2011, , 732, L14, 10.1088/2041-8205/732/1/L14

    2011 doi

  257. [271]

    2013, , 433, 1114, 10.1093/mnras/stt794

    Yusof , N., Hirschi , R., Meynet , G., et al. 2013, , 433, 1114, 10.1093/mnras/stt794

    2013 doi

  258. [272]

    J., Papadopoulos , P

    Zhang , Z.-Y., Romano , D., Ivison , R. J., Papadopoulos , P. P., & Matteucci , F. 2018, , 558, 260, 10.1038/s41586-018-0196-x

    2018 doi

  259. [273]

    L., et al

    Zhao , G., Mashonkina , L., Yan , H. L., et al. 2016, , 833, 225, 10.3847/1538-4357/833/2/225

    2016 doi

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.