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REVIEW 4 major objections 5 minor 124 references

Runaway O-type stars make up 17.5% of the local volume-complete population, versus 7.0% for B-type stars.

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2026-08-02 01:30 UTC pith:56CIZHZR

load-bearing objection Useful first volume-complete runaway fractions; the headline uncertainties understate the Poisson noise and the 3D check does not actually validate the 2D-selected fractions. the 4 major comments →

arxiv 2607.14633 v1 pith:56CIZHZR submitted 2026-07-16 astro-ph.SR astro-ph.GA

Runaway OB stars within 1 kpc of the Sun

Juan Martinez Garcia , Nicholas Wright , Alexis Quintana This is my paper
classification astro-ph.SR astro-ph.GA
keywords runaway starsOB starsstellar kinematicsGalactic rotationpeculiar velocitiesstellar ejectionssolar neighbourhoodvolume-complete sample
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.

This paper tries to establish how common runaway stars are among the OB stars nearest to the Sun, using a sample that is complete within 1 kpc rather than a magnitude- or spectroscopically-limited sample. By subtracting a fitted Galactic rotation model from astrometric proper motions, the authors identify runaways as stars whose two-dimensional peculiar velocity exceeds 23 km/s. They find that 17.5% of O-type stars and 7.0% of B-type stars in this volume are runaways. Because the O-type fraction far exceeds the roughly 2% ceiling predicted by binary-supernova simulations, the paper argues that dynamical ejection is the dominant production channel for O-type runaways.

Core claim

Using a volume-complete catalogue of 40 O-type stars and 24,488 B-type stars within 1 kpc of the Sun, the paper measures runaway fractions of 17.5% for O-type stars and 7.0% for B-type stars, applying a fixed two-dimensional peculiar-velocity threshold of 23 km/s. This is the first measurement of the runaway fraction from a spatially complete local sample, and it confirms that O-type stars are ejected more often than B-type stars. The O-type fraction substantially exceeds the at-most-2% prediction of binary-supernova-scenario simulations, leading the authors to conclude that most O-type runaways are produced by dynamical ejection in dense clusters. They also calibrate the two-dimensional ana

What carries the argument

The central machinery is a Galactic rotation model, expanded to first order in galactocentric radius and fit to proper motions using a likelihood that handles asymmetric velocity uncertainties. Residual peculiar velocities are then fit to a Maxwell-Boltzmann distribution, whose shape sets a 23 km/s runaway threshold where the observed excess over the model becomes clear. A Monte Carlo propagation over distance, proper-motion, and model-parameter uncertainties converts each star's peculiar velocity into a runaway probability and yields the reported fractions with asymmetric error bars.

Load-bearing premise

The volume-complete catalogue is over 95% complete for OB stars within 1 kpc and its astro-photometric distances are accurate, and because peculiar velocities are computed from those distances, any systematic distance error or hidden incompleteness would bias both the threshold and the runaway fractions.

What would settle it

A complete radial-velocity survey of the same 1-kpc OB sample, combined with a re-derivation of distances from Gaia parallaxes, would settle the claim: if the 3D runaway fraction for O-type stars drops toward or below the binary-supernova prediction, or if the distances shift enough to change spectral classifications, the measured 17.5% figure would not survive.

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

If this is right

  • If the O-type runaway fraction is truly 17.5%, then previous magnitude- or spectroscopically-selected samples were biased toward catching runaways, and volume-complete samples give lower, cleaner fractions.
  • The O-type fraction exceeding the binary-supernova ceiling implies that most O-type runaways were ejected dynamically, placing constraints on the density and binary content of their birth clusters.
  • The B-type runaway fraction of about 7% is consistent with a mix of binary-supernova and dynamical ejections, suggesting that the two channels contribute differently for O and B stars.
  • Runaway stars show a more diffuse vertical distribution than the general OB population, meaning stars found far from the Galactic plane are more likely to be runaways.
  • The 3D calibration supports the use of 2D proper-motion selections for statistical studies, though individual stars moving mostly along the line of sight may be missed.

Where Pith is reading between the lines

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

  • If the 17.5% O-type fraction holds, then the roughly seven O-type runaways within 1 kpc are promising targets for tracing back to their birth clusters, which would test predictions about ejection ages and cluster densities.
  • A direct test would be to repeat this analysis on the same volume-complete sample once full radial velocities are available for more stars; the authors' own examples (stars with high radial but low tangential peculiar velocity) suggest some runaways will only be found in 3D.
  • The threshold choice matters: because the runaway fraction depends steeply on the adopted velocity cut, inter-study comparisons should use identical thresholds or identical Maxwell-Boltzmann fitting procedures.
  • The assumption of axisymmetric Galactic rotation could be relaxed using a non-axisymmetric model; the small residual structure the authors note around l=80 degrees hints that local spiral structure may perturb peculiar velocities at the few-km/s level.

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

4 major / 5 minor

Summary. The paper identifies runaway OB stars in the volume-complete Quintana et al. (2025) catalogue within 1 kpc of the Sun. It converts Gaia proper motions to transverse velocities, fits a first-order Galactic rotation model with MCMC, and computes 2D peculiar velocities for 40 O-type and 24,488 B-type stars. Runaways are selected with a fixed 2D velocity threshold of 23 km/s (Method 1) and with a 3-sigma normalized-velocity criterion (Method 2). The authors report runaway fractions of 17.5+0.1−2.5% for O stars and 7.0±0.1% for B stars by Method 1, and lower values by Method 2. They calibrate the 2D threshold using a 3,884-star subsample with radial velocities, compare with literature, and interpret the O-type fraction as evidence that dynamical ejection dominates over the binary-supernova channel.

Significance. If the central estimates are correct, this is a valuable, volume-complete measurement of runaway fractions, and the comparison with BSS/DES predictions is potentially important. The paper has real strengths: use of a nearly complete local sample, explicit Monte Carlo propagation of proper-motion and model uncertainties, a 3D calibration subsample, and careful comparison with heterogeneous literature values. However, the headline numbers rest on a 2D projection assumption that is asserted rather than tested, a threshold calibrated on the same data that are classified, and uncertainty reporting that omits finite-sample Poisson uncertainty. These issues are fixable but need to be addressed before the conclusions can be taken as established.

major comments (4)
  1. [Table 5 and §4.2] The listed counts and fractions are internally inconsistent. Method 1 B-type: 1502/24488 = 6.1%, not 7.0%. Method 2 O-type: 5/40 = 12.5%, not 10.0%. Method 2 B-type: 861/24488 = 3.5%, not 2.5%. Either the N_runaways columns or the quoted fractions are wrong. Since §4.2, the abstract, and the discussion rely on these values, the table and text must be reconciled.
  2. [§4.3, §5.1] The 3D calibration validates only the threshold scaling (23 km/s × sqrt(3/2) ≈ 28 km/s), not the recovered runaway fraction. The 3,884-star RV subsample is not used to compare 2D and 3D classifications for the same stars. The statement in §5.1 that 'the overall statistics of the sample should be similar if we assume spatial isotropy' is an assumption, not a test. If ejection directions are anisotropic (e.g., preferentially in the plane), the 2D fraction can be biased. The authors should compute 3D fractions on the RV subsample or perform an injection/recovery simulation to quantify projection bias.
  3. [§3.3, §4.1, Eq. (14)] The 23 km/s threshold is circular: it is derived from the same residual-velocity distribution that includes the runaway stars being selected. The Maxwell-Boltzmann fit in §3.3 is made to all residual velocities, and the authors themselves note (N = 0.92 ± 0.02) that the distribution is not perfectly Maxwellian. Setting the threshold where observed density is twice the model prediction does not establish 'more likely than not to be a runaway' in a probabilistic sense. The sensitivity of the resulting fractions to the fitting range and to iterative removal of high-velocity stars should be quantified.
  4. [§4.2, Table 5, abstract] The reported uncertainties for the O-type fraction are misleading as headline values. The Monte Carlo interval (+0.1/−2.5%) reflects only velocity/model perturbations, while the finite-sample Poisson uncertainty is 6.6% (Table 5). The abstract should either report the combined uncertainty or explicitly state that the quoted interval excludes Poisson sampling noise. Without this, the comparison with literature values and with the 2% BSS upper limit in §5.4 is presented with a confidence that the data do not support.
minor comments (5)
  1. [Abstract] The abstract says 24,487 B-type stars, while the text and Table 5 say 24,488. Please make this consistent.
  2. [§2.2] The text says the final O list contains 48 sources, but the three subsets sum to 49 (36+9+4), and the final sample is 40 O-type stars. The path from 48/49 to 40 (Hipparcos-only proper motion exclusions) should be stated explicitly.
  3. [Table 5] For the reader's benefit, the 'Poisson noise' column should be labelled as sqrt(N_runaways)/N_stars, as in Eq. (17), and the Method-1 O row should show the combined asymmetric interval including the Poisson term, or explain why it is omitted.
  4. [Figure 4 caption] There are typographical errors in the caption: 'Ma)(ell-Boltzman' and 'Runa(ay selection threshold'. Please correct.
  5. [§5.3] The notation '17.5+0.1−2.5 ± 6.6%' mixes asymmetric and symmetric uncertainties ambiguously. Define the convention for combining MC and Poisson uncertainties.

Circularity Check

0 steps flagged

No significant circularity: the runaway fractions are empirical tail counts above a data-calibrated threshold, and the self-citations used are not load-bearing reductions.

full rationale

The central derivation is a measurement, not a prediction from fitted parameters. Residual velocities are constructed by subtracting a Galactic rotation model fitted to the sample; runaway stars are then selected by two empirical criteria. The reported fractions are the tail fractions above the chosen threshold, so there is no equation in which a fitted parameter is renamed as the target result. The Maxwell-Boltzmann fit in §3.3 is used to motivate the 23 km/s threshold, and the fit is performed on the same residual-velocity distribution that contains the runaway tail. This is a genuine methodological weakness: the threshold is not independent of the population it is applied to, and the paper itself notes the distribution is not perfectly Maxwellian because ejected stars are included. However, the fraction is not algebraically forced by the fit; it is the observed survival function at that threshold, so this is a calibration concern rather than a circular reduction under the required standard. The Q25 catalogue is authored by overlapping authors, but it is an external, published astro-photometric catalogue with its own SED-fitting methodology and is supplemented by GOSC cross-matching; the completeness claim is not derived from the present paper's results. The 3D calibration in §4.3 checks threshold consistency with the sqrt(3/2) scaling and does not recompute the runaway fraction in 3D, and the paper explicitly concedes that some 2D-selected runaways would fail a 3D threshold. This is an unvalidated isotropy assumption, not circularity. Overall, no load-bearing step reduces to its own inputs, so the circularity score is low.

Axiom & Free-Parameter Ledger

11 free parameters · 7 axioms · 0 invented entities

The analysis uses several fitted parameters for the Galactic rotation model and Maxwell-Boltzmann velocity distributions, plus a data-calibrated runaway threshold. The main external input is the Q25 catalogue, which is assumed complete and distance-accurate; this is the most important unverified premise. No new physical entities are introduced.

free parameters (11)
  • V_phi,0 (mean azimuthal Galactic rotation velocity) = 236.52 ± 0.11 km/s
    Fitted to the proper motions of the sample; sets the mean azimuthal rotation used to compute peculiar velocities (Table 2).
  • dV_phi/dR (rotation curve shear) = -0.73 ± 0.17 km/s/kpc
    First-order radial derivative of the rotation curve, fitted via MCMC (§3.2, Table 2).
  • V_R,0 (mean radial velocity component) = 0.44 ± 0.10 km/s
    Fitted radial component of the Galactic rotation model (§3.2, Table 2).
  • dV_R/dR (radial shear) = -3.70 ± 0.29 km/s/kpc
    Fitted first-order radial derivative of the radial velocity component (§3.2, Table 2).
  • sigma (residual velocity dispersion in l) = 11.11 ± 0.06 km/s
    Fitted Gaussian dispersion of the residual l-direction velocities (§3.1, Table 2).
  • Maxwell-Boltzmann 2D normalization a_tilde = 0.0153 ± 0.0002 (km/s)^-2
    Fitted normalization of the 2D residual-velocity distribution (§3.3).
  • Maxwell-Boltzmann 2D scale b = 10.99 ± 0.06 km/s
    Fitted scale parameter of the 2D residual-velocity distribution (§3.3).
  • Maxwell-Boltzmann 3D normalization a_3D = (7.1 ± 0.2) × 10^-4 (km/s)^-3
    Fitted normalization of the 3D residual-velocity distribution for stars with radial velocities (§4.3).
  • Maxwell-Boltzmann 3D scale b_3D = 13.9 ± 0.2 km/s
    Fitted scale parameter of the 3D residual-velocity distribution (§4.3).
  • Method 1 2D peculiar-velocity threshold = 23 km/s (2D); 28 km/s (3D)
    Chosen where the observed probability density is roughly twice the Maxwell-Boltzmann model density; the model is fit to the same data that include runaways, so the threshold is data-calibrated rather than independently predicted (§4.1, §4.3).
  • Method 2 sigma factor = 3
    The normalized-velocity criterion E>1 uses a 3σ threshold per velocity component; this is an arbitrary statistical cutoff (§4.1).
axioms (7)
  • domain assumption Q25 catalogue is >95% complete for OB stars within 1 kpc
    The entire sample and the claimed volume-completeness rest on this estimate from Q25 (§2.1). If completeness is lower, especially for late B-type or high-velocity stars, the runaway fractions are biased.
  • domain assumption SED-fitted effective temperatures from Q25 correctly classify B-type members
    The B-star sample is not spectroscopically verified; runaway fractions for B stars assume the SED classifications are reliable (§2.1, §2.2).
  • domain assumption Galactic rotation model truncation to first order and axisymmetry
    Eq. 3 assumes V_phi and V_R vary linearly with R and that non-axisymmetric terms are negligible; residual structure near l=80 deg in Fig. 3 hints this is imperfect (§3, §3.2).
  • domain assumption Velocity distribution of non-runaway stars is Maxwell-Boltzmann
    Used to justify the runaway threshold; the normalization test gives N=0.92±0.02, so the data are not perfectly Maxwellian (§3.3).
  • domain assumption Distances from Q25, Bailer-Jones et al., and Hipparcos are unbiased
    Peculiar velocities scale with distance; a systematic distance error directly shifts transverse velocities and hence the runaway classification (§3).
  • domain assumption 3D cross-match subset is representative and velocities are isotropic
    The 3D calibration assumes the APOGEE/LAMOST cross-match is representative and that isotropy holds so that the 3D threshold equals sqrt(3/2) times the 2D threshold (§4.3).
  • domain assumption GOSC and Garmany et al. catalogues contain all O-type stars within 1 kpc
    Completeness of the 40-star O-type sample depends on these external catalogues being complete in the volume (§2.2).

pith-pipeline@v1.3.0-alltime-deepseek · 21498 in / 16246 out tokens · 165356 ms · 2026-08-02T01:30:44.424456+00:00 · methodology

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read the original abstract

Runaway stars are high-velocity stars ejected from their birth environments that can provide insights into the kinematic history of the stellar cluster they were ejected from. We derived runaway star probabilities for 40 O-type stars and $24,487$ B-type stars taken from a recently published volume-complete sample of OB stars within 1 kpc of the Sun. We fit a Galactic rotation model to the observed proper motions of these stars and identify runaway stars using both a fixed 2D peculiar velocity threshold of $23\,km\,s^{-1}$ and by comparing individual peculiar velocities to the dispersion of the whole sample. We find runaway fractions of $17.5^{+0.1}_{-2.5}\%$ for O-type stars and $6.9\pm0.1\%$ for B-type stars; both using the fixed velocity threshold method. These values are consistent with previous studies, but with differences that are largely attributable to the underlying samples of OB stars used in various studies to identify runaway stars and to variations in the methods used to select them.

Figures

Figures reproduced from arXiv: 2607.14633 by Alexis Quintana, Juan Martinez Garcia, Nicholas Wright.

Figure 1
Figure 1. Figure 1: Diagram of the coordinate system used in the XY-plane of the Galaxy. The large purple circle represents the Galactic Centre, while the small yellow circle represents the Sun. The star represents any given star. The arrows show the direction of different velocity components in the Galactic plane. stars with high SED-fitted effective temperature (over 30, 463 K) but without a spectral type in the literature … view at source ↗
Figure 2
Figure 2. Figure 2: Observed galactocentric velocity in the 𝑙 direction (blue) and best fit model (red) for all the stars in our sample. − − −    − − [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Peculiar velocities in the 𝑏 (top) and ℓ (bottom) directions. The solid lines represent the medians, which are by definition 0 in the 𝑏 direction and −0.2 𝑘𝑚 𝑠−1 in the ℓ direction. The dashed, dash-dotted and dotted lines represent 1, 2 and 3 standard deviations from the median. The peculiar veloc￾ities in the ℓ direction are essentially the residuals from the Galactic rotation model. 3.3 Fitting a Maxwel… view at source ↗
Figure 4
Figure 4. Figure 4: Histogram showing the distribution of 2D residual velocities defined as 𝑉 = q (𝑉 𝑔𝑎𝑙 ℓ − 𝑉 𝑚𝑜𝑑𝑒𝑙 ℓ ) 2 + (𝑉𝑏 − 𝑉𝑏 ) 2 . Also shown are the Maxwell￾Boltzmann fit to this distribution, represented by the dark green line marked with circles, and the Survival Function (SF, defined as 1− Cumulative Distribution Function), represented by the blue line with square markers. Note that the figure uses two different … view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of runaway probabilities for methods 1 and 2 [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Histogram showing the distribution of 3D residual velocities de￾fined as 𝑉 = q (𝑉 𝑔𝑎𝑙 ℓ − 𝑉 𝑚𝑜𝑑𝑒𝑙 ℓ ) 2 + (𝑉𝑏 − 𝑉𝑏 ) 2 + (𝑉 𝑝𝑒𝑐 𝑟 ) 2 . Also shown are the Maxwell-Boltzmann fit to this distribution, represented by the dark green line marked with circles, and the Survival Function, represented by the blue line marked with circles. 5.1 Comments on individual O-type stars The low number of O-type stars within… view at source ↗
Figure 8
Figure 8. Figure 8: Panels (1)-(3): Distribution of the runaway stars selected with Method 1 in (X,Y,Z), plotted over the spatial density of OB stars from Q25. Panel (4) Gaussian Fit of the Z distribution of our runaway stars and the OB stars from Q25. Guo et al. (2024) estimate that around 3% of the stars of their sam￾ple have an effective temperature over 30, 000 K to be compared with the 0.2% O-type star fraction for our s… view at source ↗

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Reference graph

Works this paper leans on

124 extracted references · 9 canonical work pages · 5 internal anchors

  1. [1]

    The Villafranca catalog of Galactic OB groups. I. Systems with O2-O3.5 stars. , keywords =. doi:10.1051/0004-6361/202038228 , archivePrefix =. 2009.05773 , primaryClass =

    Pith/arXiv arXiv 2009

  2. [2]

    , keywords =

    Search for Galactic runaway stars using Gaia Data Release 1 and HIPPARCOS proper motions. , keywords =. doi:10.1051/0004-6361/201832787 , archivePrefix =. 1804.06915 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    , keywords =

    A Comprehensive Search for Stellar Bowshock Nebulae in the Milky Way: A Catalog of 709 Mid-infrared Selected Candidates. , keywords =. doi:10.3847/0067-0049/227/2/18 , archivePrefix =. 1609.02204 , primaryClass =

    Pith/arXiv arXiv

  4. [4]

    , keywords =

    On the kinematics of a runaway Be star population. , keywords =. doi:10.1093/mnras/sty980 , archivePrefix =. 1804.05849 , primaryClass =

    Pith/arXiv arXiv

  5. [5]

    , keywords =

    Galactic runaway O and Be stars found using Gaia DR3. , keywords =. doi:10.1051/0004-6361/202346613 , archivePrefix =. 2311.01827 , primaryClass =

    Pith/arXiv arXiv

  6. [7]

    The Origins and Evolutionary Status of B Stars Found Far from the Galactic Plane. II. Kinematics and Full Sample Analysis. , keywords =. doi:10.1086/504079 , archivePrefix =. astro-ph/0603238 , primaryClass =

    Pith/arXiv arXiv

  7. [8]

    E-BOSS: an Extensive stellar BOw Shock Survey. I. Methods and first catalogue. , keywords =. doi:10.1051/0004-6361/201118116 , archivePrefix =. 1109.3689 , primaryClass =

    Pith/arXiv arXiv

  8. [9]

    E-BOSS: An Extensive stellar BOw Shock Survey. II. Catalogue second release. , keywords =. doi:10.1051/0004-6361/201424676 , archivePrefix =. 1504.04264 , primaryClass =

    Pith/arXiv arXiv

  9. [10]

    , keywords =

    Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars. , keywords =. doi:10.3847/1538-3881/ac7f2b , archivePrefix =. 2206.09281 , primaryClass =

    Pith/arXiv arXiv

  10. [11]

    Boletin de los Observatorios Tonantzintla y Tacubaya , keywords =

    Run-away Stars as the Result of the Gravitational Collapse of Proto-stellar Clusters. Boletin de los Observatorios Tonantzintla y Tacubaya , keywords =

  11. [12]

    , keywords =

    On the Origin of the Runaway Stars. , keywords =

  12. [13]

    Runaway Stars from Young Star Clusters Containing Initial Binaries. II. A Mass Spectrum and a Binary Energy Spectrum. , keywords =. doi:10.1086/115354 , adsurl =

    doi:10.1086/115354

  13. [14]

    , year = 1961, month = may, volume =

    On the origin of the O- and B-type stars with high velocities (the ``run-away'' stars), and some related problems. , year = 1961, month = may, volume =

    1961

  14. [15]

    Field O stars as runaways

    The origin of massive O-type field stars: II. Field O stars as runaways. , keywords =. doi:10.1051/0004-6361:20042489 , archivePrefix =. astro-ph/0503337 , primaryClass =

    Pith/arXiv arXiv

  15. [16]

    , keywords =

    The Binary Frequency and Origin of the OB Runaway Stars. , keywords =. doi:10.1086/191118 , adsurl =

    doi:10.1086/191118

  16. [17]

    , keywords =

    The Properties of Dynamically Ejected Runaway and Hyper-runaway Stars. , keywords =. doi:10.1088/0004-637X/751/2/133 , archivePrefix =. 1202.2356 , primaryClass =

    Pith/arXiv arXiv

  17. [18]

    , keywords =

    Dynamical ejections of massive stars from young star clusters under diverse initial conditions. , keywords =. doi:10.1051/0004-6361/201628233 , archivePrefix =. 1604.00006 , primaryClass =

    Pith/arXiv arXiv

  18. [19]

    , keywords =

    Hyper-velocity and tidal stars from binaries disrupted by a massive Galactic black hole. , keywords =. doi:10.1038/331687a0 , adsurl =

    doi:10.1038/331687a0

  19. [20]

    , keywords =

    High-velocity stars from close interaction of a globular cluster and a supermassive black hole. , keywords =. doi:10.1093/mnras/stv2123 , archivePrefix =. 1509.03170 , primaryClass =

    Pith/arXiv arXiv

  20. [21]

    , keywords =

    High-velocity stars from the interaction of a globular cluster and a massive black hole binary. , keywords =. doi:10.1093/mnras/stw531 , archivePrefix =. 1510.08310 , primaryClass =

    Pith/arXiv arXiv

  21. [22]

    Morphological astronomy

  22. [23]

    , keywords =

    The Characteristics of High-Velocity O and B Stars Which Are Ejected from Supernovae in Binary Systems. , keywords =. doi:10.1086/317190 , archivePrefix =. astro-ph/0005021 , primaryClass =

    Pith/arXiv arXiv

  23. [24]

    , keywords =

    The two-step ejection of massive stars and the issue of their formation in isolation. , keywords =. doi:10.1111/j.1365-2966.2010.16376.x , archivePrefix =. 1001.3671 , primaryClass =

    arXiv 2010

  24. [25]

    Runaway OB Stars in the Small Magellanic Cloud. III. Updated Kinematics and Insights into Dynamical versus Supernova Ejections. , keywords =. doi:10.3847/1538-4357/ad3909 , archivePrefix =. 2403.17198 , primaryClass =

    Pith/arXiv arXiv

  25. [26]

    , keywords =

    Classical OBe Stars as Post-supernova Runaways: Confirming Binary Origins. , keywords =. doi:10.3847/1538-4357/ac8988 , archivePrefix =. 2208.10408 , primaryClass =

    Pith/arXiv arXiv

  26. [27]

    , keywords =

    Stringent upper limit on Be star fractions produced by binary interaction. , keywords =. doi:10.1051/0004-6361/202141269 , archivePrefix =. 2106.12263 , primaryClass =

    Pith/arXiv arXiv

  27. [28]

    Improving the open cluster census. II. An all-sky cluster catalogue with Gaia DR3. , keywords =. doi:10.1051/0004-6361/202346285 , archivePrefix =. 2303.13424 , primaryClass =

    Pith/arXiv arXiv

  28. [29]

    , keywords =

    What is a globular cluster? An observational perspective. , keywords =. doi:10.1007/s00159-019-0119-3 , archivePrefix =. 1911.02835 , primaryClass =

    Pith/arXiv arXiv 1911

  29. [30]

    , keywords =

    Characterisation of young stellar clusters. , keywords =. doi:10.1051/0004-6361/201219695 , archivePrefix =. 1209.1585 , primaryClass =

    Pith/arXiv arXiv

  30. [31]

    , keywords =

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

    Pith/arXiv arXiv

  31. [32]

    , keywords =

    The Gaia-ESO Survey: empirical estimates of stellar ages from lithium equivalent widths (EAGLES). , keywords =. doi:10.1093/mnras/stad1293 , archivePrefix =. 2304.12197 , primaryClass =

    Pith/arXiv arXiv

  32. [33]

    , keywords =

    Kinematics of OB-associations in Gaia epoch. , keywords =. doi:10.1093/mnras/stx2225 , archivePrefix =. 1708.08337 , primaryClass =

    Pith/arXiv arXiv

  33. [34]

    , keywords =

    The kinematics of the Scorpius-Centaurus OB association from Gaia DR1. , keywords =. doi:10.1093/mnras/sty207 , archivePrefix =. 1801.08540 , primaryClass =

    Pith/arXiv arXiv

  34. [35]

    , keywords =

    Massive stars in the hinterland of the young cluster, Westerlund 2. , keywords =. doi:10.1093/mnras/sty1905 , archivePrefix =. 1807.06486 , primaryClass =

    Pith/arXiv arXiv

  35. [36]

    , keywords =

    The O star hinterland of the Galactic starburst, NGC 3603. , keywords =. doi:10.1093/mnras/stz864 , archivePrefix =. 1903.09053 , primaryClass =

    Pith/arXiv arXiv 1903

  36. [37]

    , keywords =

    Proper motions of OB stars in the far Carina Arm. , keywords =. doi:10.1093/mnras/stab2905 , archivePrefix =. 2110.02081 , primaryClass =

    Pith/arXiv arXiv

  37. [38]

    The Galactic O-Star Spectroscopic Survey (GOSSS)

    The Galactic O-star spectroscopic survey (GOSSS). Highlights of Spanish Astrophysics VI , year = 2011, editor =. doi:10.48550/arXiv.1010.5680 , archivePrefix =. 1010.5680 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1010.5680 2011

  38. [39]

    , keywords =

    The Be Star Spectra (BeSS) Database. , keywords =. doi:10.1088/0004-6256/142/5/149 , adsurl =

    doi:10.1088/0004-6256/142/5/149

  39. [40]

    Massive Stars: From alpha to Omega , year = 2013, month = jun, eid =

    First whole-sky results from the Galactic O-Star Spectroscopic Survey. Massive Stars: From alpha to Omega , year = 2013, month = jun, eid =. doi:10.48550/arXiv.1306.6417 , archivePrefix =. 1306.6417 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1306.6417 2013

  40. [41]

    The Galactic O-Star Spectroscopic Survey. I. Classification System and Bright Northern Stars in the Blue-violet at R -0.5ex 2500. , keywords =. doi:10.1088/0067-0049/193/2/24 , archivePrefix =. 1101.4002 , primaryClass =

    Pith/arXiv arXiv

  41. [42]

    Spatially resolved spectroscopy of massive close visual binaries using the William Herschel Telescope

    Lucky Spectroscopy, an equivalent technique to Lucky Imaging. Spatially resolved spectroscopy of massive close visual binaries using the William Herschel Telescope. , keywords =. doi:10.1051/0004-6361/201832885 , archivePrefix =. 1804.03133 , primaryClass =

    Pith/arXiv arXiv

  42. [43]

    The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 Additional O-type Systems. , keywords =. doi:10.3847/0067-0049/224/1/4 , archivePrefix =. 1602.01336 , primaryClass =

    Pith/arXiv arXiv

  43. [44]

    The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars. , keywords =. doi:10.1088/0067-0049/211/1/10 , archivePrefix =. 1312.6222 , primaryClass =

    Pith/arXiv arXiv

  44. [45]

    MONOS: Multiplicity Of Northern O-type Spectroscopic systems. I. Project description and spectral classifications and visual multiplicity of previously known objects. , keywords =. doi:10.1051/0004-6361/201935359 , archivePrefix =. 1904.11385 , primaryClass =

    Pith/arXiv arXiv 1904

  45. [46]

    Spectral Classification and Multicolour Photometry , year = 1973, editor =

    Two-Dimensional Classificaiton of the HD Stars. Spectral Classification and Multicolour Photometry , year = 1973, editor =

    1973

  46. [47]

    , keywords =

    New and revised parameters for several southern OB binaries. , keywords =. doi:10.1051/0004-6361/201423455 , archivePrefix =. 1404.1686 , primaryClass =

    Pith/arXiv arXiv

  47. [48]

    The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure. , keywords =. doi:10.3847/1538-3881/aad1f1 , archivePrefix =. 1805.04649 , primaryClass =

    Pith/arXiv arXiv

  48. [49]

    , keywords =

    Not all stars form in clusters - measuring the kinematics of OB associations with Gaia. , keywords =. doi:10.1093/mnras/sty117 , archivePrefix =. 1801.03938 , primaryClass =

    Pith/arXiv arXiv

  49. [50]

    , keywords =

    Internal motions in OB associations with Gaia DR2. , keywords =. doi:10.1093/mnras/staa454 , archivePrefix =. 2002.05044 , primaryClass =

    Pith/arXiv arXiv 2002

  50. [51]

    , keywords =

    The dynamics of the Vel cluster and nearby Vela OB2 association. , keywords =. doi:10.1093/mnras/staa939 , archivePrefix =. 2003.14209 , primaryClass =

    Pith/arXiv arXiv 2003

  51. [52]

    , keywords =

    OB Associations and their origins. , keywords =. doi:10.1016/j.newar.2020.101549 , archivePrefix =. 2011.09483 , primaryClass =

    arXiv 2020

  52. [53]

    OB Associations

    OB Associations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2203.10007 , archivePrefix =. 2203.10007 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2203.10007

  53. [54]

    Runaway Stars as Fossils of Sub-Cluster Mergers

    Massive Star Cluster Formation II. Runaway Stars as Fossils of Sub-Cluster Mergers. arXiv e-prints , keywords =. doi:10.48550/arXiv.2405.12286 , archivePrefix =. 2405.12286 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2405.12286

  54. [55]

    The early evolution of young massive clusters. II. The kinematic history of NGC 6618/M 17. , keywords =. doi:10.1051/0004-6361/202347383 , archivePrefix =. 2311.04174 , primaryClass =

    Pith/arXiv arXiv

  55. [56]

    , keywords =

    Impacts of the Local arm on the local circular velocity inferred from the Gaia DR3 young stars in the Milky Way. , keywords =. doi:10.1093/mnras/stae158 , archivePrefix =. 2310.06831 , primaryClass =

    Pith/arXiv arXiv

  56. [57]

    , keywords =

    A new kinematic model of the Galaxy: analysis of the stellar velocity field from Gaia Data Release 3. , keywords =. doi:10.1093/mnras/stae772 , archivePrefix =. 2307.08527 , primaryClass =

    Pith/arXiv arXiv

  57. [58]

    10.1051/0004-6361/201935656

    A geometric distance measurement to the Galactic center black hole with 0.3 , DOI= "10.1051/0004-6361/201935656", url= "https://doi.org/10.1051/0004-6361/201935656", journal =

    doi:10.1051/0004-6361/201935656

  58. [59]

    , keywords =

    The Galaxy in Context: Structural, Kinematic, and Integrated Properties. , keywords =. doi:10.1146/annurev-astro-081915-023441 , archivePrefix =. 1602.07702 , primaryClass =

    Pith/arXiv arXiv

  59. [60]

    Gaia EDR3 documentation Chapter 4: Astrometric data

  60. [61]

    , keywords =

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

    Pith/arXiv arXiv

  61. [62]

    , keywords =

    A Runaway Yellow Supergiant Star in the Small Magellanic Cloud. , keywords =. doi:10.3847/1538-3881/aab964 , archivePrefix =. 1803.02859 , primaryClass =

    Pith/arXiv arXiv

  62. [63]

    doi:10.1088/978-0-7503-1329-2 , adsurl =

    Astrophysics of Red Supergiants. doi:10.1088/978-0-7503-1329-2 , adsurl =

    doi:10.1088/978-0-7503-1329-2

  63. [64]

    APS April Meeting Abstracts , year = 2023, series =

    Investigating Milky Way Red Supergiants. APS April Meeting Abstracts , year = 2023, series =

    2023

  64. [65]

    , keywords =

    A New Catalog of Asymptotic Giant Branch Stars in Our Galaxy. , keywords =. doi:10.3847/1538-4365/ac1274 , archivePrefix =. 2107.02350 , primaryClass =

    Pith/arXiv arXiv

  65. [66]

    , keywords =

    A WISE view on extreme AGB stars. , keywords =. doi:10.1051/0004-6361/202142648 , archivePrefix =. 2203.09875 , primaryClass =

    Pith/arXiv arXiv

  66. [67]

    , keywords =

    A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2. , keywords =. doi:10.3847/1538-3881/ab1cbd , archivePrefix =. 1905.03744 , primaryClass =

    Pith/arXiv arXiv 1905

  67. [68]

    Rotating massive main-sequence stars. I. Grids of evolutionary models and isochrones. , keywords =. doi:10.1051/0004-6361/201016113 , archivePrefix =. 1102.0530 , primaryClass =

    Pith/arXiv arXiv

  68. [69]

    Star cluster formation from turbulent clumps. II. Gradual star cluster formation. , keywords =. doi:10.1093/mnras/sty3470 , archivePrefix =. 1809.04607 , primaryClass =

    Pith/arXiv arXiv

  69. [70]

    Stellar Spectral Classification

  70. [71]

    Swiss Society for Astrophysics and Astronomy , author=

    Dynamics of Young Star Clusters and Associations: Saas-Fee Advanced Course 42. Swiss Society for Astrophysics and Astronomy , author=. 2015 , publisher=

    2015

  71. [72]

    Galactic Dynamics: Second Edition

  72. [73]

    , keywords =

    Revisiting the Cygnus OB associations. , keywords =. doi:10.1093/mnras/stab2663 , archivePrefix =. 2109.07499 , primaryClass =

    Pith/arXiv arXiv

  73. [74]

    , keywords =

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

    Pith/arXiv arXiv

  74. [75]

    , keywords =

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

    Pith/arXiv arXiv

  75. [76]

    A study of the kinematical imprints of the physical processes governing the evolution and explosion of their binary progenitors

    Massive runaway and walkaway stars. A study of the kinematical imprints of the physical processes governing the evolution and explosion of their binary progenitors. , keywords =. doi:10.1051/0004-6361/201833297 , archivePrefix =. 1804.09164 , primaryClass =

    Pith/arXiv arXiv

  76. [77]

    Active OB Stars: Structure, Evolution, Mass Loss, and Critical Limits , year = 2011, editor =

    The multiplicity of massive stars. Active OB Stars: Structure, Evolution, Mass Loss, and Critical Limits , year = 2011, editor =. doi:10.1017/S1743921311011124 , archivePrefix =. 1009.4197 , primaryClass =

    Pith/arXiv arXiv 2011

  77. [78]

    , keywords =

    Binary systems and stellar mergers in massive star formation. , keywords =. doi:10.1111/j.1365-2966.2005.09360.x , archivePrefix =. astro-ph/0506689 , primaryClass =

    arXiv 2005

  78. [79]

    , keywords =

    Toward Understanding Massive Star Formation. , keywords =. doi:10.1146/annurev.astro.44.051905.092549 , archivePrefix =. 0707.1279 , primaryClass =

    Pith/arXiv arXiv

  79. [80]

    , keywords =

    Colliding Winds from Early-Type Stars in Binary Systems. , keywords =. doi:10.1086/171013 , adsurl =

    work page doi:10.1086/171013

  80. [81]

    Rotational mixing in tidally locked massive main-sequence binaries

    Rotational mixing in tidally locked massive main sequence binaries. Communications in Asteroseismology , keywords =. doi:10.48550/arXiv.0811.3981 , archivePrefix =. 0811.3981 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.0811.3981

Showing first 80 references.