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105,971 OB stars mapped within 2 kpc reveal local spiral arms and future supernova progenitors

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-07-09 20:36 UTC pith:6EWZAD3X

load-bearing objection Solid OB star catalog extending to 2 kpc; the BH-vs-ccSN excess claim is the soft spot the 2 major comments →

arxiv 2607.07068 v1 pith:6EWZAD3X submitted 2026-07-08 astro-ph.GA astro-ph.SR

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

Alexis L. Quintana , Kiril Maltsev , Eloisa Poggio , Emily L. Hunt , Nicholas J. Wright , Sara R. Berlanas , Laia Casamiquela , Abel de Burgos
show 5 more authors
Hanna Parul Misha Haywood Paola Di Matteo Chervin Laporte Juan Mart\'inez Garc\'ia
This is my paper
classification astro-ph.GA astro-ph.SR
keywords OB starsGaia DR3Milky Way spiral armscore-collapse supernova progenitorsblack hole formationstar formation ratestellar cataloguesSED fitting
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper constructs the largest and most carefully validated catalogue of OB-type stars (effective temperature above 10,000 K) within 2 kiloparsecs of the Sun, using Gaia DR3 astrometry and photometry combined with multi-band survey data fed into a Bayesian spectral-energy-distribution fitter. From the derived stellar parameters—initial mass, age, distance, and extinction—the authors produce a three-dimensional map of young stellar populations across the local Galactic thin disk, showing where star formation is clustered, how it traces spiral arm segments (notably the Sagittarius-Carina arm), and where large underdensities such as the Perseus Gap / Giant Oval Cavity sit. They then apply a statistical supernova model to classify over 4,200 of these stars as core-collapse supernova or direct-collapse black hole progenitor candidates, estimate waiting times to explosion or collapse, and find that more black hole progenitors are expected to collapse within the next 1 million years than supernovae are expected to explode—despite black hole progenitors being far rarer overall. This excess of imminent collapses is interpreted as evidence for a recent, localized burst of massive star formation in the solar neighbourhood.

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.

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.

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.

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.

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

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.

Where Pith is reading between the lines

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

  • 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.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 10 minor

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)
  1. 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
  2. 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)
  1. 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.
  2. 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.
  3. 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.
  4. 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.
  5. 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.
  6. 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.
  7. 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.
  8. 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.
  9. Typo in Section 6.3: 'pens within less than 100 years' should be 'happens within less than 100 years'.
  10. 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

0 steps flagged

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.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

The paper does not invent new physical entities. It relies on established stellar evolution models, a recent supernova model, and standard astronomical data products. The free parameters are standard data analysis choices (thresholds, bandwidths) rather than physically fitted constants.

free parameters (3)
  • CMD selection thresholds = M_G < 1.5 mag, (BP-RP)_0 < 0.5 mag
    Chosen by hand in Section 2.1 to be more liberal than A0V star values to account for uncertainties.
  • Overdensity bandwidths = h_local = 100 pc, h_mean = 500 pc
    Chosen in Appendix D to reflect the scale of OB associations and star-forming complexes.
  • SED fitter additional uncertainty ln(f)
    Free parameter in the emcee fit indicating quality of fit (Section 2.2).
axioms (4)
  • domain assumption Single-star evolution models (Ekström et al. 2012) accurately represent the life cycles of the observed OB stars.
    Used throughout Section 6 to derive ages, ZAMS masses, and waiting times. Acknowledged as a limitation in Section 6.3.3.
  • 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.
    Used in Section 6.1 to classify progenitors. The model is recent and favored by some gravitational wave observations but not independently verified.
  • domain assumption The 3D extinction map from Edenhofer et al. (2024), including its reconstructed version beyond 1.25 kpc, provides accurate A_V values.
    Used in Section 2.2 to correct photometry. Validated in Appendix A for Cyg OB2.
  • domain assumption The Gaia DR3 astrometric and photometric data, after the applied corrections, are sufficiently complete and accurate for this census.
    Foundational to the entire sample selection in Section 2.1.

pith-pipeline@v1.1.0-glm · 39704 in / 2819 out tokens · 285161 ms · 2026-07-09T20:36:47.508713+00:00 · methodology

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read the original 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.

Figures

Figures reproduced from arXiv: 2607.07068 by Abel de Burgos, Alexis L. Quintana, Chervin Laporte, Eloisa Poggio, Emily L. Hunt, Hanna Parul, Juan Mart\'inez Garc\'ia, Kiril Maltsev, Laia Casamiquela, Misha Haywood, Nicholas J. Wright, Paola Di Matteo, Sara R. Berlanas.

Figure 1
Figure 1. Figure 1: Left panel: HR diagram of the 1,049,399 candidate OB stars from their median SED-fitted effective temperatures and luminosities. Right panel: median 𝐷XY = √ 𝑋2 + 𝑌2 values as a function of the median A𝑉 for these same stars. Each point has been colour-coded by gaussian KDE density. The vertical dashed lines correspond to the threshold of log(𝑇eff ) = 4 and 𝐷XY = 2000 pc adopted to create our final catalogu… view at source ↗
Figure 2
Figure 2. Figure 2: Observed (in blue) and completeness-corrected (in orange) num￾bers of SED-fitted OB stars within 2 kpc (right-hand Y axis). Each top line represents the fraction of sources that passed the different cuts (based on astrometric data quality) from Section 2.1 and discussed in Section 3.1, with the total obtained through the convolution of each curve (left-hand Y axis). including 𝑇eff up to 20,000 K. From this… view at source ↗
Figure 3
Figure 3. Figure 3: Far left and middle right panels: Comparison of our SED-fitted effective temperatures (ordinate) with the spectroscopic temperatures (abscissa) from the Gaia DR3 ESP-HS (top left), APOGE DR17 (top right), LAMOST DR6 (bottom left) and SHBoost 2024 (bottom right) catalogues, with each star colour-coded by its Gaussian KDE density (in units of stars per log(𝑇eff ) 2 ), and including a black 1:1 line. Middle l… view at source ↗
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Left panel: normalised surface density of the 147,639 OB stars across the X-Y plane (X is positive towards the direction of Galactic Centre and Y towards the direction of Galactic rotation). The small annotations correspond to OB associations and/or massive star-forming regions, whilst the larger ones correspond to broader features, as described in Section 4.1. The inner circle encompasses a radius of √ 𝑋2… view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: Gaussian KDE (adopting a bandwith of 100 pc) of the median 𝑍-height for the 130,441 SED-fitted OB stars situated in the mid-Galactic plane (|𝑍| < 150 pc), across the X-Y plane. Right panel: Sech2 fit of the distribution of 𝑍 values of the 105,971 SED-fitted OB stars within 2 kpc. the OB stars sit closer to the Galactic mid-Plane, and our value is slightly smaller than the value of 76 ± 1 pc fro… view at source ↗
Figure 7
Figure 7. Figure 7: Left panel: Same as the left panel from [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Same as the left panel from [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Top-down view (across the X-Y plane) of our clustered population of stars, colour-coded by the number of OB stars found as member of HR24 across bins of 50 pc size. On the left panel are displayed all 12,352 clustered OB stars, and on the right panel the 611 clustered OB stars with log(𝑇eff ) > 4.3 [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Fraction of clustered OB stars (i.e., that are members of the OCs from HR24) in our catalogue for each bin of 100 pc size of Galactocentric radius RGC, where we have adopted R0 = 8.23 kpc from Leung et al. (2023) for the distance of the Sun to the Galactic Centre. Every subset is defined by the effective temperature threshold as written on the different panels. 6.1 The final fates of massive OB-type stars… view at source ↗
Figure 11
Figure 11. Figure 11: Far left panel: observed, median SED-fitted ZAMS mass distribution of the ccSN explosion progenitor candidates from our catalogue of OB-type stars. Middle right panel: waiting time before the next SN explosion for this subset, estimated from the solar-metallicity, rotating single-star evolutionary models from Ekström et al. (2012), as outlined in Section 6.3. Middle left and far right panels: same but for… view at source ↗
Figure 12
Figure 12. Figure 12: Same as [PITH_FULL_IMAGE:figures/full_fig_p014_12.png] view at source ↗

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Reference graph

Works this paper leans on

235 extracted references · 235 canonical work pages · 168 internal anchors

  1. [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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202243940

  2. [2]

    Stellar Structure and Evolution

    work page

  3. [3]

    An introduction to modern astrophysics, Second Edition

    work page

  4. [4]

    , year = 1966, month = mar, volume =

    The Hydrodynamic Behavior of Supernovae Explosions. , year = 1966, month = mar, volume =. doi:10.1086/148549 , adsurl =

    work page doi:10.1086/148549 1966

  5. [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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-023-01977-z

  6. [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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/749/1/91

  7. [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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty699

  8. [8]

    arXiv e-prints , keywords =

    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 =

    work page doi:10.48550/arxiv.2603.17011

  9. [9]

    GWTC-5.0: Population Properties of Merging Compact Binaries

    GWTC-5.0: Population Properties of Merging Compact Binaries. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.27226 , archivePrefix =. 2605.27226 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.27226

  10. [10]

    The search for failed supernovae with the Large Binocular Telescope: a new candidate and the failed SN fraction with 11 yr of data

    The search for failed supernovae with the Large Binocular Telescope: a new candidate and the failed SN fraction with 11 yr of data. , keywords =. doi:10.1093/mnras/stab2605 , archivePrefix =. 2104.03318 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab2605

  11. [11]

    Multiplicity of Galactic Luminous Blue Variable stars

    Multiplicity of Galactic luminous blue variable stars. , keywords =. doi:10.1051/0004-6361/202040062 , archivePrefix =. 2105.12380 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202040062

  12. [12]

    The Pair-Instability Mass Gap for Black Holes

    The Pair-instability Mass Gap for Black Holes. , keywords =. doi:10.3847/2041-8213/abf2c4 , archivePrefix =. 2103.07933 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/abf2c4 2041

  13. [13]

    , keywords =

    White dwarf models for type I supernovae and quiet supernovae, and presupernova evolution. , keywords =. doi:10.1007/BF00168350 , adsurl =

    work page doi:10.1007/bf00168350

  14. [14]

    Ultra-stripped supernovae: progenitors and fate

    Ultra-stripped supernovae: progenitors and fate. , keywords =. doi:10.1093/mnras/stv990 , archivePrefix =. 1505.00270 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv990

  15. [15]

    The Neutron Star and Black Hole Initial Mass Function

    The Neutron Star and Black Hole Initial Mass Function. , keywords =. doi:10.1086/176778 , archivePrefix =. astro-ph/9510136 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/176778

  16. [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 =

    work page doi:10.1086/150760 1971

  17. [17]

    astroquery: An Astronomical Web-Querying Package in Python

    astroquery: An Astronomical Web-querying Package in Python. , keywords =. doi:10.3847/1538-3881/aafc33 , archivePrefix =. 1901.04520 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aafc33 1901

  18. [18]

    Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3. , keywords =. doi:10.3847/1538-3881/abd806 , archivePrefix =. 2012.05220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/abd806 2012

  19. [19]

    Validation of the accuracy and precision of Gaia EDR3 parallaxes with globular clusters

    Validation of the accuracy and precision of Gaia EDR3 parallaxes with globular clusters. , keywords =. doi:10.1051/0004-6361/202140418 , archivePrefix =. 2101.10206 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202140418

  20. [20]

    An estimation of the Gaia EDR3 parallax bias from stellar clusters and Magellanic Clouds data

    An estimation of the Gaia EDR3 parallax bias from stellar clusters and Magellanic Clouds data. , keywords =. doi:10.1051/0004-6361/202142365 , archivePrefix =. 2110.01475 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202142365

  21. [21]

    A census of OB stars within 1 kpc and the star formation and core collapse supernova rates of the Milky Way

    A census of OB stars within 1 kpc and the star formation and core collapse supernova rates of the Milky Way. , keywords =. doi:10.1093/mnras/staf083 , archivePrefix =. 2503.08286 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staf083

  22. [22]

    A reanalysis of the Gaia Data Release 2 photometric sensitivity curves using HST/STIS spectrophotometry

    Reanalysis of the Gaia Data Release 2 photometric sensitivity curves using HST/STIS spectrophotometry. , keywords =. doi:10.1051/0004-6361/201834051 , archivePrefix =. 1808.02820 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201834051

  23. [23]

    Stellar variability in Gaia DR3. I. Three-band photometric dispersions for 145 million sources. , keywords =. doi:10.1051/0004-6361/202346759 , archivePrefix =. 2304.14249 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202346759

  24. [24]

    Gaia Early Data Release 3: Photometric content and validation

    Gaia Early Data Release 3. Photometric content and validation. , keywords =. doi:10.1051/0004-6361/202039587 , archivePrefix =. 2012.01916 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039587 2012

  25. [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 =

    work page 2005

  26. [26]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  27. [27]

    A parsec-scale Galactic 3D dust map out to 1.25 kpc from the Sun

    A parsec-scale Galactic 3D dust map out to 1.25 kpc from the Sun. , keywords =. doi:10.1051/0004-6361/202347628 , archivePrefix =. 2308.01295 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202347628

  28. [28]

    Parameters of 220 million stars from Gaia BP/RP spectra

    Parameters of 220 million stars from Gaia BP/RP spectra. , keywords =. doi:10.1093/mnras/stad1941 , archivePrefix =. 2303.03420 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad1941

  29. [29]

    The flare and spiral structure of the Milky Way's disc as traced by young giant stars

    The flare and spiral structure of the Milky Way's disc as traced by young giant stars. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.12603 , archivePrefix =. 2605.12603 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.12603

  30. [30]

    Gaia Data Release 3. Apsis. II. Stellar parameters. , keywords =. doi:10.1051/0004-6361/202243919 , archivePrefix =. 2206.05992 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202243919

  31. [31]

    Intrinsic Colors, Temperatures, and Bolometric Corrections of Pre-Main Sequence Stars

    Intrinsic Colors, Temperatures, and Bolometric Corrections of Pre-main-sequence Stars. , keywords =. 2013. doi:10.1088/0067-0049/208/1/9 , archivePrefix =. 1307.2657 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/208/1/9 2013

  32. [32]

    The Optical to Mid-Infrared Extinction Law Based on the APOGEE, Gaia DR2, Pan-STARRS1, SDSS, APASS, 2MASS and WISE Surveys

    The Optical to Mid-infrared Extinction Law Based on the APOGEE, Gaia DR2, Pan-STARRS1, SDSS, APASS, 2MASS, and WISE Surveys. , keywords =. doi:10.3847/1538-4357/ab1c61 , archivePrefix =. 1904.04575 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1c61 1904

  33. [33]

    emcee: The MCMC Hammer

    emcee: The MCMC Hammer. , keywords =. 2013. doi:10.1086/670067 , archivePrefix =. 1202.3665 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/670067 2013

  34. [34]

    The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

    The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation. , keywords =. doi:10.1093/mnras/stad557 , archivePrefix =. 2212.03981 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad557

  35. [35]

    2MASS All Sky Catalog of point sources

    work page

  36. [36]

    Gaia Data Release 1. Cross-match with external catalogues - Algorithm and results

    Gaia Data Release 1. Cross-match with external catalogues. Algorithm and results. , keywords =. doi:10.1051/0004-6361/201730965 , archivePrefix =. 1710.06739 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730965

  37. [37]

    Gaia Data Release 2. Cross-match with external catalogues - Algorithms and results

    Gaia Data Release 2. Cross-match with external catalogues: algorithms and results. , keywords =. doi:10.1051/0004-6361/201834142 , archivePrefix =. 1808.09151 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201834142

  38. [38]

    and Piedipalumbo, E

    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 =

    work page doi:10.1111/j.1365-2966.2005.09330.x 2005

  39. [39]

    IGAPS: the merged IPHAS and UVEX optical surveys of theNorthern Galactic Plane

    IGAPS: the merged IPHAS and UVEX optical surveys of the northern Galactic plane. , keywords =. doi:10.1051/0004-6361/201937333 , archivePrefix =. 2002.05157 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201937333 2002

  40. [40]

    The VST Photometric Halpha Survey of the Southern Galactic Plane and Bulge (VPHAS+)

    The VST Photometric H Survey of the Southern Galactic Plane and Bulge (VPHAS+). , keywords =. doi:10.1093/mnras/stu394 , archivePrefix =. 1402.7024 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu394

  41. [41]

    Grids of stellar models with rotation. I. Models from 0.8 to 120 M _ ☉ at solar metallicity (Z = 0.014). , keywords =. 2012. doi:10.1051/0004-6361/201117751 , archivePrefix =. 1110.5049 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201117751 2012

  42. [42]

    A new library of theoretical stellar spectra with scaled-solar and alpha-enhanced mixtures

    A new library of theoretical stellar spectra with scaled-solar and -enhanced mixtures. , keywords =. 2014. doi:10.1093/mnras/stu365 , archivePrefix =. 1404.3243 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu365 2014

  43. [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 =

    work page 2003

  44. [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 Society of the Pacific, ISBN: 1-58381-131-1, 2003, p.31 , year = "2003", volume =

    work page 2002

  45. [45]

    Journal of Computational and Applied Mathematics , keywords =

    The classical stellar atmosphere problem. Journal of Computational and Applied Mathematics , keywords =

    work page

  46. [46]

    , keywords =

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

    work page doi:10.1146/annurev.astro.46.060407.145222

  47. [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 =

    work page doi:10.1098/rsta.2011.0269 2011

  48. [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 =

    work page doi:10.1093/mnras/staf1409

  49. [49]

    , keywords =

    Catalog of Galactic OB Stars. , keywords =. doi:10.1086/374771 , adsurl =

    work page doi:10.1086/374771

  50. [50]

    A Galactic O-Star Catalog

    A Galactic O Star Catalog. , keywords =. doi:10.1086/381380 , archivePrefix =. astro-ph/0311196 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/381380

  51. [51]

    Mapping Luminous Hot Stars in the Galaxy

    Mapping luminous hot stars in the Galaxy. , keywords =. doi:10.1051/0004-6361/202039726 , archivePrefix =. 2102.08684 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039726

  52. [52]

    Gaia Data Release 3: A Golden Sample of Astrophysical Parameters

    Gaia Data Release 3. A golden sample of astrophysical parameters. , keywords =. doi:10.1051/0004-6361/202243800 , archivePrefix =. 2206.05870 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202243800

  53. [53]

    The Galactic spiral structure as revealed by O- and early B-type stars

    The Galactic spiral structure as revealed by O- and early B-type stars. , keywords =. doi:10.1093/mnras/stz1357 , archivePrefix =. 1905.05542 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1357 1905

  54. [54]

    Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost

    Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost. , keywords =. doi:10.1051/0004-6361/202451427 , archivePrefix =. 2407.06963 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202451427

  55. [55]

    Galactic spiral structure revealed by Gaia EDR3

    Galactic spiral structure revealed by Gaia EDR3. , keywords =. doi:10.1051/0004-6361/202140687 , archivePrefix =. 2103.01970 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202140687

  56. [56]

    The Galactic warp revealed by Gaia DR2 kinematics

    The Galactic warp revealed by Gaia DR2 kinematics. , keywords =. doi:10.1093/mnrasl/sly148 , archivePrefix =. 1805.03171 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/sly148

  57. [57]

    ASPCAP: The Apogee Stellar Parameter and Chemical Abundances Pipeline

    ASPCAP: The APOGEE Stellar Parameter and Chemical Abundances Pipeline. , keywords =. doi:10.3847/0004-6256/151/6/144 , archivePrefix =. 1510.07635 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-6256/151/6/144

  58. [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 =

    work page doi:10.3847/1538-4365/ac4414

  59. [59]

    Gaia Data Release 3: Astrophysical parameters inference system (Apsis) I -- methods and content overview

    Gaia Data Release 3. Astrophysical parameters inference system (Apsis). I. Methods and content overview. , keywords =. doi:10.1051/0004-6361/202243688 , archivePrefix =. 2206.05864 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202243688

  60. [60]

    Stellar labels for hot stars from low-resolution spectra. I. The HotPayne method and results for 330 000 stars from LAMOST DR6. , keywords =. doi:10.1051/0004-6361/202141570 , archivePrefix =. 2108.02878 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202141570

  61. [61]

    A Catalogue of OB Stars from LAMOST Spectroscopic Survey

    A Catalog of OB Stars from LAMOST Spectroscopic Survey. , keywords =. doi:10.3847/1538-4365/ab0a0d , archivePrefix =. 1902.07607 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab0a0d 1902

  62. [62]

    A new Gaia census of OB associations within 1 kpc

    A new Gaia census of OB associations within 1 kpc. , keywords =. doi:10.1093/mnras/stag853 , archivePrefix =. 2512.05854 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stag853

  63. [63]

    Disentangling the spatial substructure of Cygnus OB2 from Gaia DR2

    Disentangling the spatial substructure of Cygnus OB2 from Gaia DR2. , keywords =. doi:10.1093/mnras/stz117 , archivePrefix =. 1901.02959 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz117 1901

  64. [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 =

    work page doi:10.1086/145754 1953

  65. [65]

    The Alma catalog of OB stars. II. A cross-match with Gaia DR2 and an updated map of the solar neighbourhood

    The Alma catalogue of OB stars - II. A cross-match with Gaia DR2 and an updated map of the solar neighbourhood. , keywords =. doi:10.1093/mnras/stab688 , archivePrefix =. 2103.02748 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab688

  66. [66]

    The observed spiral structure of the Milky Way

    The observed spiral structure of the Milky Way. , keywords =. doi:10.1051/0004-6361/201424039 , archivePrefix =. 1407.7331 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424039

  67. [67]

    A three-dimensional map of the Milky Way using classical Cepheid variable stars

    A three-dimensional map of the Milky Way using classical Cepheid variable stars. Science , keywords =. doi:10.1126/science.aau3181 , archivePrefix =. 1806.10653 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.aau3181

  68. [68]

    Trigonometric Parallaxes Of High-Mass Star Forming Regions: Our View Of The Milky Way

    Trigonometric Parallaxes of High-mass Star-forming Regions: Our View of the Milky Way. , keywords =. doi:10.3847/1538-4357/ab4a11 , archivePrefix =. 1910.03357 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab4a11 1910

  69. [69]

    Galaxies in the universe : an introduction

    work page

  70. [70]

    , keywords =

    Star-forming complexes and the spiral structure of our Galaxy. , keywords =. doi:10.1051/0004-6361:20021504 , adsurl =

    work page doi:10.1051/0004-6361:20021504

  71. [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 =

    work page doi:10.1086/597811 2009

  72. [72]

    Open clusters in AurOB2

    Open clusters in Auriga OB2. , keywords =. doi:10.1093/mnras/stw640 , archivePrefix =. 1604.03881 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw640

  73. [73]

    Quantifying the scale of star formation across the Perseus spiral arm using young clusters around Cas OB5

    Quantifying the scale of star formation across the Perseus spiral arm using young clusters around Cas OB5. , keywords =. doi:10.1051/0004-6361/202452615 , archivePrefix =. 2504.01748 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202452615

  74. [74]

    Mapping the distribution of OB stars and associations in Auriga

    Mapping the distribution of OB stars and associations in Auriga. , keywords =. doi:10.1093/mnras/stad1160 , archivePrefix =. 2304.08370 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad1160

  75. [75]

    Trigonometric Parallaxes of Star Forming Regions in the Perseus Spiral Arm

    Trigonometric Parallaxes of Star Forming Regions in the Perseus Spiral Arm. , keywords =. doi:10.1088/0004-637X/790/2/99 , archivePrefix =. 1407.1609 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/790/2/99

  76. [76]

    Spiral Structure in the Outer Galactic Disk. I. The Third Galactic Quadrant. , keywords =. doi:10.1086/524003 , archivePrefix =. 0709.3973 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/524003

  77. [77]

    , keywords =

    Evolution of the Local Spiral Structure Revealed by OB-type Stars in Gaia DR3. , keywords =. doi:10.3847/1538-3881/ad5201 , adsurl =

    work page doi:10.3847/1538-3881/ad5201

  78. [78]

    SPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc. , keywords =. doi:10.3847/1538-4357/ace5b3 , archivePrefix =. 2306.08150 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ace5b3

  79. [79]

    , keywords =

    The Cygnus superbubble revisited. , keywords =. doi:10.1051/0004-6361:20010387 , adsurl =

    work page doi:10.1051/0004-6361:20010387

  80. [80]

    The Massive Star Population of Cygnus OB2

    The massive star population of Cygnus OB2. , keywords =. doi:10.1093/mnras/stv323 , archivePrefix =. 1502.05718 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv323

Showing first 80 references.