REVIEW 2 major objections 10 minor 235 references
Unveiling the Milky Way with a Gaia DR3 census of OB-type stars within 2 kpc. I. Tracing local Galactic structure, massive star-forming regions and core-collapse supernova progenitors
T0 review · 2 major / 10 minor · reviewed 2026-07-09 · glm-5.2
Pith's one-line read 105,971 OB stars mapped within 2 kpc reveal local spiral arms and future supernova progenitors
desk verdict Solid OB star catalog extending to 2 kpc; the BH-vs-ccSN excess claim is the soft spot read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The central machinery is an astro-photometric Bayesian SED fitter that combines Gaia DR3 parallax and photometry with ground-based optical and near-infrared surveys (2MASS, IGAPS, VPHAS+), constrains extinction using a 3D dust map, and fits stellar atmosphere and evolutionary models to derive initial mass, fractional age, distance, and effective temperature for each star. A statistical core-collapse supernova model (M25) then maps the derived zero-age main-sequence masses onto final fates—successful neutrino-driven supernova with neutron star remnant, failed supernova with black hole remnant, or electron-capture supernova—using metallicity-dependent carbon-oxygen core mass thresholds.
What would settle it
If spectroscopic follow-up of the 4,200+ progenitor candidates reveals that a substantial fraction have ZAMS masses or ages inconsistent with the SED-fitted values—particularly if binary companions are detected that shift stars across the supernova / direct-collapse boundary—then the reported excess of imminent BH collapses over supernovae could be an artefact of the single-star assumption rather than a real signature of recent star formation.
Extended reading notes
Core claim
By fitting physical parameters for 105,971 OB-type stars within 2 kpc and applying a bimodal supernova model, the paper finds that the local Milky Way currently harbours more massive stars on the verge of direct black hole collapse than on the verge of supernova explosion, an imbalance attributed to a recent burst of massive star formation (likely associated with Cyg OB2) rather than to a steady-state rate. The paper also establishes that no OB-type supernova progenitor is expected to explode within 100 parsecs of Earth in the next 1 million years.
Load-bearing premise
The SED fitting and supernova classification assume every star is a single, non-interacting system. A large fraction of massive OB stars are known to exist in binaries, and binary mass transfer can change a star's final mass, lifetime, and whether it explodes as a supernova or collapses directly into a black hole. The authors acknowledge this limitation explicitly through the case of P Cyg, whose classification flips when binary effects are considered.
Editorial extensions
If this is right
- The catalogue of 4,200+ ccSN and BH progenitor candidates provides a prioritized target list for spectroscopic follow-up surveys such as WEAVE-SCIP and 4MOST, which can test the SED-fitted masses and ages against direct spectroscopic measurements.
- The finding that more BH collapses than supernovae are expected within 1 Myr, if confirmed, implies that the local core-collapse event rate is time-variable rather than constant, complicating estimates of the Galactic supernova rate that assume steady-state star formation.
- The spatial correlation between OB star overdensities and young open clusters, combined with the ~10% membership fraction of OB stars in clusters, constrains the fraction of massive stars born in clustered environments versus the field.
- Future Gaia DR4 astrometry (expected to be ~2.25 times more precise) and a potential near-infrared successor (GaiaNIR) would push the catalogue deeper into high-extinction regions toward the Galactic Centre, where current optical surveys are incomplete.
Reading between the lines
- If the single-star assumption were relaxed, binary mass transfer could strip envelopes and shift progenitors between the supernova and direct-collapse BH channels, potentially altering the reported excess of BH collapses over supernovae. The direction of the effect is not obvious: stripping could push some stars that would have collapsed silently into the explosive channel, or vice versa, dependin
- The reported mean waiting time of ~7,800 years between supernova explosions on the 2 kpc scale, combined with the much longer ~15,000-year average inferred from extrapolating the 1 kpc rate over ~400 Myr, suggests that the local Milky Way is currently in a star-formation overdensity phase. If so, the next few thousand years should see a local supernova rate elevated above the long-term Galactic av
- The offset between OB star overdensities and young open cluster positions in highly extinguished regions like Cyg OB2 implies that OB star catalogues can probe star formation sites that cluster catalogues miss, making the two tracers complementary rather than redundant for mapping embedded massive star formation.
Signed reviews
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. This paper presents a catalogue of 105,971 OB-type stars (T_eff > 10,000 K) within 2 kpc of the Sun, identified via astro-photometric SED fitting of Gaia DR3 data combined with 2MASS, IGAPS, and VPHAS+ photometry. The authors validate their catalogue against spectroscopic surveys (APOGEE, LAMOST, Gaia ESP-HS, SHBoost), demonstrate high completeness (>95% across magnitudes), and map the spatial distribution of young stellar populations across the Galactic thin disk. They identify large-scale structures (Sagittarius-Carina arm, Cepheus Spur, Giant Oval Cavity), compare OB star overdensities with young open clusters from Hunt & Reffert (2024), and use a statistical supernova model (Maltsev et al. 2025) to classify 3,998 ccSN progenitor and 233 direct-collapse BH progenitor candidates. The most novel claim is that more BH progenitors are expected to collapse within 1 Myr than ccSNe to explode, interpreted as evidence for a recent massive star formation burst.
Significance. The catalogue represents a substantial expansion over the authors' previous 1 kpc census (Q25), covering four times the area and providing a valuable community resource for spectroscopic follow-up (WEAVE, 4MOST). The cross-validation against four independent spectroscopic surveys is commendable and lends credibility to the derived effective temperatures. The spatial mapping of OB stars and their correlation with young open clusters provides a useful complementary view to existing structure tracers. The application of a recently developed, observationally-constrained supernova model (M25) to a large stellar census is a genuine attempt to move beyond simple mass-threshold progenitor classifications. The identification of specific ccSN/BH progenitor candidates, while subject to the uncertainties discussed below, provides a concrete target list for follow-up. The authors are transparent about limitations in Appendix F and Section 6.3.3.
major comments (2)
- Section 6.3.1 and the abstract claim that 'more BH progenitors to collapse within the next 1 Myr than ccSN to explode' is indicative of a recent massive star formation burst. This claim is load-bearing for the paper's most novel conclusion, but it rests on classifying stars into fate categories (Table 2) whose thresholds are separated by as little as 1.12 M_sun (between 22.20 and 23.32 M_sun). The SED-fitted log(M/M_sun) has a 1-sigma of ~0.14 dex (Section 2.3), corresponding to ~32% uncertainty in linear mass (~7 M_sun at 22 M_sun). This uncertainty far exceeds the spacing between adjacent fate thresholds. The classification in Section 6.2 uses median SED-fitted ZAMS masses, collapsing the full posterior to a point estimate. If the mass posteriors were propagated through the Table 2 thresholds, the apparent excess of BH progenitors could be an artifact of classification noise near the 8
- Section 6.3.3 acknowledges that *P Cyg is a likely binary donor whose classification changes when binary effects are considered, and the SED fitter assumes all stars are single (Section 3.2.2). Given that a large fraction of massive OB stars are in binary systems, this assumption systematically affects derived ZAMS masses, ages, and therefore both the individual progenitor classifications and the statistical distribution of waiting times. The paper should quantify or at least bound the impact of binarity on the relative BH/ccSN numbers. Without this, the central claim in Section 6.3.1 remains uncertain. A Monte Carlo test injecting a realistic binary fraction and mass-ratio distribution into the SED fitting pipeline, then re-classifying fates, would suffice to demonstrate robustness.
minor comments (10)
- Section 2.1, Eq. (1): the threshold M_G < 1.5 mag is described as 'more liberal' than the A0V value of 1 mag from Pecaut & Mamajek (2013). It would help to state explicitly what contamination fraction this liberal threshold introduces, or reference the contamination analysis already performed in Q25.
- Section 3.2.1: the comparison with APOGEE shows a tendency to overestimate temperatures, opposite to the other surveys. The authors attribute this to APOGEE's 20,000 K model grid limit. It would strengthen the paper to show a histogram or subsample restricted to T_eff < 20,000 K to confirm that the offset vanishes there.
- Section 4.1, right panel of Fig. 5: the overdensity parameter Delta_Sigma is defined in Appendix D, but the bandwidth choices (h_local = 100 pc, h_mean = 500 pc) are stated only in the appendix. These should be mentioned in the main text caption or Section 4.1 for self-contained reading.
- Table 3: several entries have extremely asymmetric error bars on distance (e.g., chi Oph: 705 +1975/-351 pc). These large upper bounds suggest the SED-fitted distance posterior is poorly constrained for some sources. A note flagging which entries have distance uncertainties exceeding the median would help readers assess the reliability of individual progenitor candidates.
- Section 5: the claim that ~10% of OB stars are found in clustered environments is compared to the ~38% of OB association members that are also cluster members within 1 kpc. The jump from 1 to 2 kpc changes the surface area by a factor of 4, so a direct comparison of these fractions without accounting for volume-dependent completeness may be misleading. A brief clarification would help.
- Figure 12 caption: the text mentions '10 ccSN progenitor candidates we expect to explode within less than 1 Myr (as blue stars)' but Table 3 lists 10 entries above the dashed line, some with tau_cc > 0.8 Myr. The caption should clarify that these are the 10 with the shortest median waiting times, not all with tau_cc < 1 Myr.
- Appendix E: the comparison with alternative spiral arm models is useful but somewhat cursory. A quantitative metric (e.g., cross-correlation between OB star density and model arm positions) would strengthen the comparison beyond visual inspection.
- Section 6.1.2: the minimum M_ZAMS thresholds of 8.55 and 8.85 M_sun for electron-capture and neutrino-driven SNe are derived from specific stellar evolution models (Temaj et al. 2024). A brief note on how sensitive these thresholds are to the choice of model would provide context for the reader.
- Typo in Section 6.3: 'pens within less than 100 years' should be 'happens within less than 100 years'.
- Section 3.2.2: the median offset of 0.06 dex in log(M/M_sun) relative to HR24 is attributed to methodological differences. Given that this offset is comparable to the 1-sigma scatter (~0.14 dex), a brief discussion of whether a simple additive correction would improve agreement would be useful.
Circularity Check
No significant circularity found; derivation chain is self-contained against external benchmarks
full rationale
The paper's main derivation chain is: (1) select OB star candidates from Gaia DR3 photometry/astrometry using standard quality cuts (Section 2.1); (2) fit stellar parameters (Teff, log(M/M_sun), fractional age, distance) via SED fitting using external stellar atmosphere models (BT-NextGen, Kurucz, Tübingen NLTE) and external evolutionary models (Ekström et al. 2012), with extinction from the external Edenhofer et al. (2024) 3D map (Section 2.2); (3) classify final fates using the Maltsev et al. (2025) SN model, which maps M_ZAMS thresholds to outcomes (Table 2). The SED fitter itself is described in Q25 (Quintana et al. 2025a), a self-citation, but it is validated against four independent spectroscopic surveys (Gaia ESP-HS, APOGEE DR17, LAMOST DR6, SHBoost 2024) in Section 3.2.1, and initial masses are cross-checked against the independent Hunt & Reffert (2024) cluster catalogue in Section 3.2.2. The M25 SN model (Maltsev et al. 2025, co-authored by present author Maltsev) is an external model validated against gravitational wave observations (Willcox et al. 2025). The key novel claim — more BH progenitors collapsing within 1 Myr than ccSNe exploding — is an output of combining fitted masses/ages with the M25 fate thresholds, not a quantity that was fitted to or defined in terms of the output. The stellar evolution models (Ekström et al. 2012) and the M_CO-to-M_ZAMS relation (Schneider et al. 2021; Temaj et al. 2024) are fully external. While the single-star assumption and mass uncertainties (noted by the skeptic) are legitimate correctness concerns, they do not constitute circularity: the prediction is not forced by construction or by a self-citation chain. The authors transparently acknowledge in Appendix F that individual error bars are too large for faithful individual predictions, and in Section 6.3.3 that binarity changes classifications. These are honest limitations, not circular reasoning. The self-citations (Q25 for the SED fitter, M25 for the SN model) are not load-bearing in a circular sense because both are independently validated against external data. Score 1 reflects the minor self-citation of the SED fitter, which is not circular but warrants noting.
Assumptions & free parameters
free parameters (3)
- CMD selection thresholds =
M_G < 1.5 mag, (BP-RP)_0 < 0.5 mag
- Overdensity bandwidths =
h_local = 100 pc, h_mean = 500 pc
- SED fitter additional uncertainty ln(f)
assumptions (4)
- domain assumption Single-star evolution models (Ekström et al. 2012) accurately represent the life cycles of the observed OB stars.
- domain assumption The M25 supernova model (Maltsev et al. 2025) correctly predicts the final fate (SN vs. BH) of massive stars based on M_CO and metallicity.
- domain assumption The 3D extinction map from Edenhofer et al. (2024), including its reconstructed version beyond 1.25 kpc, provides accurate A_V values.
- domain assumption The Gaia DR3 astrometric and photometric data, after the applied corrections, are sufficiently complete and accurate for this census.
Cite this review
Pith. "Pith review of Unveiling the Milky Way with a Gaia DR3 census of OB-type stars within 2 kpc. I. Tracing local Galactic structure, massive star-forming regions and core-collapse supernova progenitors." pith.science (2026). https://pith.science/paper/6EWZAD3X
@misc{pith2026260707068,
author = {Pith},
title = {Pith review of: Unveiling the Milky Way with a Gaia DR3 census of OB-type stars within 2 kpc. I. Tracing local Galactic structure, massive star-forming regions and core-collapse supernova progenitors},
year = {2026},
howpublished = {\url{https://pith.science/paper/6EWZAD3X}},
note = {Machine review of arXiv:2607.07068}
}
abstract
O- and B-type stars are young and hot, thereby serving as vital tracers of the star formation and spiral arm structure of the Milky Way. At the dusk of the \textit{Gaia} DR3 era, a high-confidence and accurate catalogue appears timely. Here we have characterized a population of 105,971 OB-type stars (T$_{\rm eff} >$ 10,000 K; hereafter OB stars) within 2 kpc from the Sun, using an astro-photometric Bayesian inference tool. Our resulting map unveils a complex view of the young stellar populations across the thin disk, with prominent large-scale features such as the Cepheus Spur, the Giant Oval Cavity, and a segment of the Sagittarius-Carina spiral arm all visible. Their inhomogeneous spatial distribution implies that massive star formation has taken place clustered across a few highly concentrated regions. We find a correlation between the overdensities of OB stars and young open clusters ($<$20 Myr), although OB stars can be better detected in high-extinction regions. We identify over 4200 OB stars as core-collapse supernova (ccSN) or direct-collapse black hole (BH) progenitor candidates, and therefore targets of interest for spectroscopic follow-up. Furthermore, we find no OB-type star ccSN progenitor to explode within the next 1 Myr within 100 pc, at which such an event could be harmful to Earth's biosphere. Finally, we identify more BH progenitors to collapse within the next 1 Myr than ccSN to explode, despite the former's much scarcer number - which could be indicative of a recent massive star formation burst in the local Milky Way.
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Reference graph
Works this paper leans on
-
[1]
Gaia Data Release 3: Summary of the content and survey properties
Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =
-
[2]
Stellar Structure and Evolution
-
[3]
An introduction to modern astrophysics, Second Edition
-
[4]
, year = 1966, month = mar, volume = 143, pages =
The Hydrodynamic Behavior of Supernovae Explosions. , year = 1966, month = mar, volume =. doi:10.1086/148549 , adsurl =
-
[5]
Unusual integrated metallicity profile of our Milky Way
The integrated metallicity profile of the Milky Way. Nature Astronomy , keywords =. doi:10.1038/s41550-023-01977-z , archivePrefix =. 2306.14100 , primaryClass =
-
[6]
Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity
Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity. , keywords =. doi:10.1088/0004-637X/749/1/91 , archivePrefix =. 1110.1726 , primaryClass =
-
[7]
X-ray Detectability of Accreting Isolated Black Holes in Our Galaxy
X-ray detectability of accreting isolated black holes in our Galaxy. , keywords =. doi:10.1093/mnras/sty699 , archivePrefix =. 1801.04667 , primaryClass =
-
[8]
Confirming Nunki as the closest core collapse progenitor candidate to the Sun. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.17011 , archivePrefix =. 2603.17011 , primaryClass =
Show all 235 references
- [9]
- [10]
- [11]
- [12]
-
[13]
, keywords =
White dwarf models for type I supernovae and quiet supernovae, and presupernova evolution. , keywords =. doi:10.1007/BF00168350 , adsurl =
- [14]
- [15]
-
[16]
, year = 1971, month = jan, volume =
Neutron-Star Formation, Thermonuclear Supernovae, and Heavy-Element Reimplosion. , year = 1971, month = jan, volume =. doi:10.1086/150760 , adsurl =
1971 doi
- [17]
- [18]
- [19]
- [20]
- [21]
- [22]
- [23]
- [24]
-
[25]
Astronomical Data Analysis Software and Systems XIV , year = 2005, editor =
TOPCAT & STIL: Starlink Table/VOTable Processing Software. Astronomical Data Analysis Software and Systems XIV , year = 2005, editor =
2005
- [26]
- [27]
- [28]
- [29]
- [30]
- [31]
- [32]
- [33]
- [34]
-
[35]
2MASS All Sky Catalog of point sources
- [36]
- [37]
-
[38]
, keywords =
The INT Photometric H Survey of the Northern Galactic Plane (IPHAS). , keywords =. 2005. doi:10.1111/j.1365-2966.2005.09330.x , archivePrefix =. astro-ph/0506726 , primaryClass =
2005 doi
- [39]
- [40]
- [41]
- [42]
-
[43]
Stellar Atmosphere Modeling, ASP Conference Proceedings, Vol
Handling of Atomic Data. Stellar Atmosphere Modeling, ASP Conference Proceedings, Vol. 288. Editors: Ivan Hubeny, Dimitri Mihalas, and Klaus Werner. San Francisco: Astronomical Society of the Pacific, ISBN: 1-58381-131-1, 2003, p.103 , year = "2003", volume =
2003
-
[44]
Stellar Atmosphere Modeling, ASP Conference Proceedings, Vol
Model Photospheres with Accelerated Lambda Iteration. Stellar Atmosphere Modeling, ASP Conference Proceedings, Vol. 288. Abstracts from a conference held 8-12 April 2002 in Tuebingen, Germany. Editors: Ivan Hubeny, Dimitri Mihalas, and Klaus Werner. San Francisco: Astronomical...
2002
-
[45]
Journal of Computational and Applied Mathematics , keywords =
The classical stellar atmosphere problem. Journal of Computational and Applied Mathematics , keywords =
-
[46]
, keywords =
The Chemical Composition of the Sun. , keywords =. doi:10.1146/annurev.astro.46.060407.145222 , archivePrefix =. 0909.0948 , primaryClass =
-
[47]
Philosophical Transactions of the Royal Society of London Series A , keywords =
Models of very-low-mass stars, brown dwarfs and exoplanets. Philosophical Transactions of the Royal Society of London Series A , keywords =. doi:10.1098/rsta.2011.0269 , archivePrefix =. 1112.3591 , primaryClass =
2011 doi
-
[48]
A cross-match with Gaia DR3 and an extension based on new spectral classifications
The Alma catalogue of OB stars ─ III. A cross-match with Gaia DR3 and an extension based on new spectral classifications. , keywords =. doi:10.1093/mnras/staf1409 , archivePrefix =. 2508.14875 , primaryClass =
- [49]
- [50]
- [51]
- [52]
- [53]
- [54]
- [55]
- [56]
- [57]
-
[58]
, keywords =
The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data. , keywords =. doi:10.3847/1538-4365/ac4414 , archivePrefix =. 2112.02026 , primaryClass =
- [59]
- [60]
- [61]
- [62]
- [63]
-
[64]
Studies in Galactic Structure. I. a Preliminary Determination of the Space Distribution of the Blue Giants. , year = 1953, month = sep, volume =. doi:10.1086/145754 , adsurl =
1953 doi
- [65]
- [66]
- [67]
- [68]
-
[69]
Galaxies in the universe : an introduction
-
[70]
, keywords =
Star-forming complexes and the spiral structure of our Galaxy. , keywords =. doi:10.1051/0004-6361:20021504 , adsurl =
-
[71]
, year = 2009, month = mar, volume =
The Spitzer/GLIMPSE Surveys: A New View of the Milky Way. , year = 2009, month = mar, volume =. doi:10.1086/597811 , adsurl =
2009 doi
- [72]
- [73]
- [74]
- [75]
- [76]
-
[77]
, keywords =
Evolution of the Local Spiral Structure Revealed by OB-type Stars in Gaia DR3. , keywords =. doi:10.3847/1538-3881/ad5201 , adsurl =
- [78]
-
[79]
, keywords =
The Cygnus superbubble revisited. , keywords =. doi:10.1051/0004-6361:20010387 , adsurl =
- [80]
- [81]
- [82]
-
[83]
Nature Communications , keywords =
A large, long-lived, slowly-expanding superbubble across the Perseus arm. Nature Communications , keywords =. doi:10.1038/s41467-025-65591-5 , archivePrefix =. 2512.21927 , primaryClass =
- [84]
- [85]
- [86]
- [87]
-
[88]
, keywords =
The selection function of the Gaia DR3 open cluster census. , keywords =. doi:10.1051/0004-6361/202557781 , archivePrefix =. 2510.18343 , primaryClass =
- [89]
- [90]
- [91]
-
[92]
, keywords =
OB Associations and their origins. , keywords =. doi:10.1016/j.newar.2020.101549 , archivePrefix =. 2011.09483 , primaryClass =
2020 doi
- [93]
- [94]
- [95]
- [96]
- [97]
- [98]
- [99]
- [100]
-
[101]
Highlights of Spanish Astrophysics XII , year = 2025, editor =
Differences Between Gaia DR2 and Gaia EDR3 Photometry: Demonstration, Consequences, and Applications. Highlights of Spanish Astrophysics XII , year = 2025, editor =. doi:10.48550/arXiv.2407.21388 , archivePrefix =. 2407.21388 , primaryClass =
-
[102]
Catalogue of Bright Stars
- [103]
-
[104]
The Bright star catalogue
-
[105]
arXiv e-prints , keywords =
Gaia and massive stars in 2025. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.21385 , archivePrefix =. 2510.21385 , primaryClass =
2025 doi
-
[106]
EES2023: Proceedings of the Evry Schatzman School , year = 2024, editor =
Astrophysical Parameters associated to 'Hot' stars in Gaia DR3. EES2023: Proceedings of the Evry Schatzman School , year = 2024, editor =. doi:10.48550/arXiv.2411.04887 , archivePrefix =. 2411.04887 , primaryClass =
- [107]
- [108]
- [109]
- [110]
- [111]
- [112]
- [113]
- [114]
- [115]
- [116]
- [117]
- [118]
- [119]
- [120]
- [121]
- [122]
- [123]
- [124]
- [125]
- [126]
- [127]
- [128]
-
[129]
EAS Publications Series , year = 2011, editor =
Star Formation in Spiral Arms. EAS Publications Series , year = 2011, editor =. doi:10.1051/eas/1151002 , archivePrefix =. 1101.3109 , primaryClass =
2011 doi
- [130]
- [131]
-
[132]
, keywords =
The Gaia mission. , keywords =. doi:10.1051/0004-6361/20162927210.48550/arXiv.1609.04153 , archivePrefix =. 1609.04153 , primaryClass =
- [133]
-
[134]
, keywords =
The superclouds of the local Milky Way. , keywords =. doi:10.1051/0004-6361/202556469 , adsurl =
- [135]
-
[136]
The Gaia Universe , year = 2019, month = apr, eid =
The Future of the Gaia Universe. The Gaia Universe , year = 2019, month = apr, eid =. doi:10.5281/zenodo.2637972 , adsurl =
2019 doi
-
[137]
Astronomy and Geophysics , year = 2012, month = aug, volume =
Birth, life and death of massive stars. Astronomy and Geophysics , year = 2012, month = aug, volume =. doi:10.1111/j.1468-4004.2012.53430.x , adsurl =
2012 doi
-
[138]
Stellar Atmospheres; a Contribution to the Observational Study of High Temperature in the Reversing Layers of Stars
-
[139]
, keywords =
A comprehensive set of simulations studying the influence of gas expulsion on star cluster evolution. , keywords =. doi:10.1111/j.1365-2966.2007.12209.x , archivePrefix =. 0707.1944 , primaryClass =
2007 doi
- [140]
- [141]
- [142]
-
[143]
The evolution of stars and astrophysics
-
[144]
, keywords =
The Luminosity Function of OB Associations in the Galaxy. , keywords =. 1997. doi:10.1086/303587 , adsurl =
1997 doi
- [145]
- [146]
- [147]
- [148]
-
[149]
Publications of Michigan Observatory , year = 1951, month = jan, volume =
Application of the principle of natural groups to the classification of stellar spectra. Publications of Michigan Observatory , year = 1951, month = jan, volume =
1951
-
[150]
, keywords =
The large-scale kinematics of young stars in the Milky Way disc: First results from SDSS-V. , keywords =. doi:10.1051/0004-6361/202556444 , archivePrefix =. 2509.10387 , primaryClass =
- [151]
- [152]
- [153]
- [154]
- [155]
-
[156]
arXiv e-prints , keywords =
Good things always come in 3s: trimodality in the binary black-hole chirp-mass distribution supports bimodal black-hole formation. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.07573 , archivePrefix =. 2510.07573 , primaryClass =
- [157]
- [158]
-
[159]
Evolution of 8--10 M _ sun Stars toward Electron Capture Supernovae. II. Collapse of an O + NE + MG Core. , keywords =. doi:10.1086/165716 , adsurl =
- [160]
- [161]
- [162]
- [163]
- [164]
-
[165]
, keywords =
Observation of 23 Supernovae That Exploded <300 pc from Earth during the past 300 kyr. , keywords =. doi:10.1088/0004-637X/789/1/29 , adsurl =
- [166]
- [167]
- [168]
- [169]
- [170]
-
[171]
Supernovae and Gamma-Ray Bursters , year = 2003, editor =
Historical Supernovae. Supernovae and Gamma-Ray Bursters , year = 2003, editor =. doi:10.1007/3-540-45863-8_2 , adsurl =
2003 doi
- [172]
-
[173]
, keywords =
On the rate of core collapse supernovae in the milky way. , keywords =. doi:10.1016/j.newast.2020.101498 , archivePrefix =. 2009.03438 , primaryClass =
2020 doi
- [174]
-
[175]
Palaeogeography Palaeoclimatology Palaeoecology , year = 2017, month = jul, volume =
On the causes of mass extinctions. Palaeogeography Palaeoclimatology Palaeoecology , year = 2017, month = jul, volume =. doi:10.1016/j.palaeo.2016.11.005 , adsurl =
2017 doi
-
[176]
Proceedings of the National Academy of Science , year = 1984, month = feb, volume =
Periodicity of Extinctions in the Geologic Past. Proceedings of the National Academy of Science , year = 1984, month = feb, volume =. doi:10.1073/pnas.81.3.801 , adsurl =
1984 doi
-
[177]
, keywords =
Bayesian time series analysis of terrestrial impact cratering. , keywords =. doi:10.1111/j.1365-2966.2011.19112.x , archivePrefix =. 1105.4100 , primaryClass =
2011 doi
-
[178]
, keywords =
Orbital stability of the unseen solar companion linked to periodic extinction events. , keywords =. doi:10.1038/311641a0 , adsurl =
-
[179]
, keywords =
The effect of the solar motion on the flux of long-period comets. , keywords =. doi:10.1111/j.1365-2966.2010.17729.x , archivePrefix =. 1009.4190 , primaryClass =
2010 doi
- [180]
- [181]
- [182]
-
[183]
, keywords =
The star formation rate in disc galaxies: thresholds and dependence on gas amount. , keywords =. doi:10.1111/j.1365-2966.2003.07170.x , archivePrefix =. astro-ph/0309372 , primaryClass =
2003 doi
- [184]
- [185]
-
[186]
, keywords =
The late Miocene ^ 10 Be anomaly and the possibility of a supernova. , keywords =. doi:10.1051/0004-6361/202556253 , archivePrefix =. 2507.03685 , primaryClass =
- [187]
- [188]
- [189]
- [190]
-
[191]
, year = 2016, month = apr, volume =
Interstellar <mml:mmultiscripts>Fe 60 </mml:mmultiscripts> on the Surface of the Moon. , year = 2016, month = apr, volume =. doi:10.1103/PhysRevLett.116.151104 , adsurl =
2016 doi
-
[192]
, year = 2019, month = aug, volume =
Interstellar ^ 60 Fe in Antarctica. , year = 2019, month = aug, volume =. doi:10.1103/PhysRevLett.123.072701 , adsurl =
2019 doi
-
[193]
Science , keywords =
^ 60 Fe and ^ 244 Pu deposited on Earth constrain the r-process yields of recent nearby supernovae. Science , keywords =. doi:10.1126/science.aax3972 , adsurl =
- [194]
- [195]
- [196]
- [197]
-
[198]
, keywords =
A statistical study of 233 pulsar proper motions. , keywords =. doi:10.1111/j.1365-2966.2005.09087.x , archivePrefix =. astro-ph/0504584 , primaryClass =
2005 doi
- [199]
- [200]
- [201]
- [202]
- [203]
-
[204]
, keywords =
On the variation of the initial mass function. , keywords =. doi:10.1046/j.1365-8711.2001.04022.x , archivePrefix =. astro-ph/0009005 , primaryClass =
2001 doi
- [205]
- [206]
-
[207]
Science , keywords =
Time Scales of Critical Events Around the Cretaceous-Paleogene Boundary. Science , keywords =. doi:10.1126/science.1230492 , adsurl =
-
[208]
Nature Reviews Earth and Environment , year = 2022, month = may, volume =
The Chicxulub impact and its environmental consequences. Nature Reviews Earth and Environment , year = 2022, month = may, volume =. doi:10.1038/s43017-022-00283-y , adsurl =
2022 doi
- [209]
-
[210]
arXiv e-prints , keywords =
SpiralMap: A Python library of the Milky Way's spiral arms. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.11383 , archivePrefix =. 2506.11383 , primaryClass =
- [211]
-
[212]
, keywords =
Pulsar Distances and the Galactic Distribution of Free Electrons. , keywords =. doi:10.1086/172870 , adsurl =
-
[213]
, keywords =
The Milky Way's Spiral Arms Traced by Magnetic Fields, Dust, Gas, and Stars. , keywords =. doi:10.1086/176470 , adsurl =
- [214]
- [215]
- [216]
- [217]
- [218]
- [219]
-
[220]
Highlights of Spanish Astrophysics XII , year = 2025, editor =
An Up-Scaled Endeavor for Exploring OB Stars in the Milky Way Within the WEAVE-SCIP Survey. Highlights of Spanish Astrophysics XII , year = 2025, editor =
2025
-
[221]
EAS2024 , year = 2024, month = jul, eid =
The GaiaNIR mission: Future Space Astrometry in the Near Infrared. EAS2024 , year = 2024, month = jul, eid =
2024
-
[222]
Astrometry and Astrophysics in the Gaia Sky , year = 2018, editor =
GaiaNIR - A future all-sky astrometry mission. Astrometry and Astrophysics in the Gaia Sky , year = 2018, editor =. doi:10.1017/S1743921317005348 , adsurl =
2018 doi
-
[223]
doi:10.1007/978-94-010-0967-6 , adsurl =
The chemical evolution of the Galaxy. doi:10.1007/978-94-010-0967-6 , adsurl =
- [224]
- [225]
- [226]
- [227]
- [228]
- [229]
- [230]
-
[231]
, keywords =
The evolution of velocity dispersion in the Sco-Cen OB association. , keywords =. doi:10.1051/0004-6361/202555519 , adsurl =
- [232]
- [233]
- [234]
- [235]
Reviewed July 9, 2026 · model on record in the stance chip above.
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