adsabs/AstroCLIMB huggingface dataset:
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: The pair of left panels compares the normalized profiles of the light curves of different stars with that of R Cen; the leftmost panel includes curves of similar shapes; the second panel includes curves of different shapes (see text). The following panels display superimposed profiles of cycles taken from the light curves of stars discussed in the text: the four well-established HBB candidates, R Cen, R Nor, RU Cyg, and SV Cas, the possible additional HBB candidate, DH Cyg, the particular case of RU Tau, and the archetypal RV Tau star, AC Her.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Schematic evolution of the light curves in parameter space (W vs. A projection in the left panel and W vs. P projection in the right panel). Crosses show mean and rms values of the samples listed in the inserts. Colored ellipses approximate the regions covered by these samples. Arrows show the suggested evolution as described in the text: green for carbon stars, black for Mno stars of the Table 1 sample that will never experience a strong TDU event, blue and red for stars experiencing strong TDU events; the former are expected to have lower initial masses than the latter and to possibly transit from oxygen rich to carbon rich via a chaotic pulsation regime (dotted arrows).
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Distributions of the curve parameters in projections on planes for which a significant correlation is observed. The lines are the results of the linear fits listed in Table 8.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: Spatial distribution of HV-RRL candidates in the Galactic coordinates using a Mollweide projection. In the upper panel, colors of the dots indicate the [Fe/H] of the HV-RRL candidates, with black circles indicating they are neighbors of the LMC and SMC. Gray dots represent the rest of RRLs in the total sample, with the depth of gray indicating logarithm of density. Magenta and blue stars and lines denote the current position and previous orbit of the LMC and SMC, respectively. The lower panel displays the density of RRLs with velocity exceeding the Milky Way’s escape velocity, including the unbound member stars of the LMC and SMC.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: Galactocentric distance vs. metallicity distribution of the selected HV-RRL candidates. Cyan points with black outlines and error bars represent candidates located near the Magellanic Clouds, while orange points with error bars denote other candidates. The right subpanel of each main panel shows the corresponding [Fe/H] histogram, with horizontal lines marking the mean metallicity. Panels (a) through (d) illustrate the effects of varying selection criteria and gravitational potential models introduced in Section 3.1.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: Velocity distribution of selected hypervelocity RRL candidates in the Galactic rest frame. Left panel shows RRLs with radial velocity; right panel shows RRLs without radial velocity. Red dots represent the HV-RRL candidates in the gold sample; green dots represent those in the silver sample; and orange dots represent those in the bronze sample. Error bars are computed by Monte Carlo sampling. Gray dots depict the rest of the RRLs in the total sample. Black, blue, orange, green, and red lines denote the escape velocity computed from J. Bovy (2015), M. Cautun et al. (2020), G. Monari et al. (2018), P. J. McMillan (2017), and A. Irrgang et al. (2013), respectively.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: Spatial distribution of RRL samples from W22 (upper panels) and L23 (bottom panels) in the Galactic Cartesian coordinates. Left panels show XGC–ZGC distribution; right panels show YGC–ZGC distribution. Color bar on the right side stands for number density in logarithmic scale. Magenta and blue stars denote the position of the LMC and SMC; green, orange and sky blue diamonds denote the position of the Sculptor, Draco, and Ursa Minor dwarf galaxies (SclI, DraI, and UMiI); yellow and red triangles denote the Sgr core (C) and stream (S), respectively. The position of these dwarf galaxies are taken from T. K. Fritz et al. (2018).
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: Three representative light curves provided by Gaia DR3 from the bronze sample are shown, which should be carefully used. The light curve in the left panel appears too symmetric to be consistent with a typical RR Lyrae star, yet it is classified as an RRab. The middle panel shows a steep rise and an amplitude exceeding 0.8 mag, suggesting it should be classified as an RRab rather than an RRc. The light curve in the right panel contains few and scattered data points, making it difficult to reliably identify it as an RR Lyrae star.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: Spatial distribution of HV-RRL candidates in the gold and silver samples in the Galactic frame. Red dots represent the HV-RRL candidates in the gold sample; green dots represent candidates in the silver sample. Error bars are computed by Monte Carlo sampling. Gray dots represent the rest of RRLs in the total sample, with the depth of gray indicating logarithm of density.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: Period–amplitude distribution of the HV-RRL candidates for golden and silver samples. Blue circle dots are RRab types; orange triangles are RRc types.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: Plots of perpendicular displacement of the particles ﹩\sqrt{{\langle \delta \widetilde{z}\rangle }^{2}}/{L}_{{\rm{inj}}}﹩ versus the CRs’ gyroperiods t · Ω in transonic Ms ≈ 1 conditions, corresponding to simulations A1, A3, and A4. ldiss is the numerical dissipation scale, and Linj is the injection scale. Panels (a), (b), and (c) correspond to an initial cosine of the pitch angle μ ≈ 1, μ ≈ 0.25, and μ ≈ 0.1, respectively.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: An example of the scattering diffusion and mirror diffusion. A particle with a Larmor radius of 10 cells and an initial pitch-angle cosine of 0.25 is ejected into simulation A4 (Ms = 1.24 and MA = 1.21). The particle trajectory is plotted in the 3D volume rendering cube of normalized magnetic field strength. Panel (a): the trajectory is colored to show the time, increasing from blue to red. Panel (b): the trajectory is colored to show ∣μ∣, where μ is the cosine pitch angle, increasing from dark blue to yellow. Magnetic field lines are colored to show the normalized magnetic field strength. In the regimes dominated by a magnetic field mirror, the particle is reflected back and forth by multiple mirrors while undergoing superdiffusion perpendicular to the mean magnetic field. It can reenter the scattering diffusion regime due to the gradual stochastic change of pitch angle.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: Left three panels: x−z slices of ion velocity (vi; top) and neutral velocity (vn; bottom) at three different neutral–ion coupling statuses: strong coupling, intermediate coupling, and decoupling. Right panel: the kinetic energy spectrum. The theoretically expected parallel and perpendicular components of the neutral–ion decoupling wavenumber are denoted as kdec,∥ and kdec,⊥, respectively. To guide the eye, the dashed and dashed–dotted black lines represent power-law slopes of –5/3 and –2, for comparison with Kolmogorov and Burgers turbulence scaling, respectively.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: Left three panels: x–z slices of ion density (ρi; top) and neutral density (ρn; bottom) at three different neutral–ion coupling statuses: strong coupling, intermediate coupling, and decoupling. Right panel: the density spectrum. The neutral–ion decoupling wavenumber’s theoretically expected parallel and perpendicular components are denoted as kdec,∥ and kdec,⊥, respectively. To guide the eye, the dashed and dashed–dotted black lines represent power-law slopes of –5/3 and –2, for comparison with Kolmogorov and Burgers turbulence scaling, respectively.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: The velocity distribution of the RRLs as member stars of the dwarf galaxies in the Galactic rest frame. Blue dots represent the selected unbound candidates of the Milky Way, while gray dots represent other RRLs. Orange stars mark the position and velocity of the dwarf galaxies’ centers.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: Left three panels: x–z slices of magnetic field strength at three different neutral–ion coupling statuses: strong coupling, intermediate coupling, and decoupling. Right panel: the magnetic field spectrum. To guide the eye, the dashed and dashed–dotted black lines represent power-law slopes of −5/3 and −2, respectively.
Paper: Search for Distant Hypervelocity Star Candidates Using RR Lyrae Stars
Authors: Haozhu Fu, Yang Huang, Huawei Zhang
Figure caption: The velocity distribution of the RRLs as member stars of the dwarf galaxies in the LMC rest frame. Blue dots represent the selected unbound candidates of the Milky Way, while gray dots represent other RRLs. Blue line denotes the simulated LMC escape velocity in Figure 4 from D. Boubert et al. (2017); red line denotes the LMC escape velocity computed by the Hernquist profile constructed in Section 3.1.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: The parallel mean free path 〈λ∥〉 in units of the turbulence injection scale Linj as a function of coupling strength (γdρi)/(vinj/Linj), which is the ratio of the neutral–ion collisional frequency to the eddy turnover rate at the injection scale.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: Histograms of ion velocity (red) and neutral velocity (blue) in transonic (top) and supersonic (bottom) conditions.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: Same as Figure 7 but for the logarithmic mass density ﹩{\mathrm{log}}_{10}(\rho /\langle \rho \rangle )﹩.
Paper: Cosmic-ray Perpendicular Superdiffusion and Parallel Mirror Diffusion in a Partially Ionized and Turbulent Medium
Authors: Yue Hu, Siyao Xu, Alex Lazarian, James M. Stone, Philip F. Hopkins
Figure caption: Histograms of magnetic field strength in transonic (left) and supersonic (right) conditions.
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: The high-luminosity (MBol < −9.7) LBVs, candidate LBVs, and the B[e]sgs plotted with red circles on H-alpha emission images of the LMC from MCELS (R. C. Smith & MCELS Team 1999). The plots also include the reference samples in the matching luminosity range (Table 3): early O-types (purple), mid O-types (blue), late O-types (cyan), and early B-types (green).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An HR diagram of the B[e]sgs in the LMC sorted into three luminosity groups: high-luminosity B[e]sgs (green triangles, MBol < −9.7), mid-luminosity B[e]sgs (orange diamonds, −9.7 ≤ MBol < −7.0), and low-luminosity B[e]sgs (red pentagons, MBol ≥ −7.0). The zero-age main sequence and evolutionary tracks are adopted from P. Eggenberger et al.’s (2021) Z = 0.006 nonrotating models, which is consistent with the range of spectroscopic abundances measured for luminous stars in the LMC (A. Mucciarelli et al. 2008; A. V. Ahumada et al. 2019; M. Romaniello et al. 2022).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An HR diagram of the 126 of 152 WRs in the LMC which have published temperatures and luminosities (G. Testor & V. Niemela 1998; P. Massey et al. 2000; J. M. Bestenlehner et al. 2014; V. V. Gvaramadze et al. 2014; R. Hainich et al. 2014; K. F. Neugent et al. 2017; E. Aadland et al. 2022). WN type are gold triangles. WNh type are purple Xs. WN3/O3 are orange crosses, WC type are blue squares, WO type are green circles. O2-3If*/WN slash stars are red asterisks. The zero-age main sequence and evolutionary tracks are adopted from P. Eggenberger et al.’s (2021) Z = 0.006 nonrotating models, which is consistent with the range of spectroscopic abundances measured for luminous stars in the LMC (A. Mucciarelli et al. 2008; A. V. Ahumada et al. 2019; M. Romaniello et al. 2022).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: The HR diagram for the most luminous and massive stars in the LMC. The zero-age main sequence (ZAMS) is noted with a solid black line. The Humphreys/Davidson limit (R. M. Humphreys & K. Davidson 1979, 1994) is noted with the dashed black line. Stars are color coded: O-type = dark blue, B-type = light blue, A-type = green, YSG = orange, RSG = red. The vertical striping is due to the spectroscopic temperature scale we have adopted (J. C. Martin & R. M. Humphreys 2023). ZAMS and evolutionary tracks are adopted from P. Eggenberger et al.’s (2021) Z = 0.006 nonrotating models, which are consistent with the range of spectroscopic abundances measured for luminous stars in the LMC (A. Mucciarelli et al. 2008; A. V. Ahumada et al. 2019; M. Romaniello et al. 2022).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: A schematic HR diagram of the LBVs in the LMC discussed in the text. The apparent transits of the LBV during outburst are shown as straight blue lines. The LBV/S Dor instability strip is outlined in pink and the empirical upper luminosity boundary is shown in orange. Evolutionary tracks for nonrotating models from P. Eggenberger et al. (2021) are shown in gray for 20 M⊙, 40 M⊙, 60 M⊙, and 85 M⊙.
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An H-alpha emission image of the LMC from MCELS (R. C. Smith & MCELS Team 1999) with earlier type WNs (WN2–WN4, cyan crosses), later-type WNs (WN5–WN11, yellow crosses), WNhs (red Xs), and WN3/O3s (green diamonds) in the luminosity range from −9.7 ≤ MBol < −8. WCs (magenta circles) of all luminosity types are also plotted.
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An H-alpha emission image of the LMC from MCELS (R. C. Smith & MCELS Team 1999) with earlier type WNs (WN3–WN4, cyan crosses), later-type WNs (WN4.5-WN7, yellow crosses), WNhs (magenta Xs), and Of/WN slash stars (red circles) in the highest luminosity range for stars brighter than MBol < −9.7. Note that all but one of the WNhs are found in and around the 30 Doradus region.
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An H-alpha emission image of the LMC from MCELS (R. C. Smith & MCELS Team 1999) including the reference samples of the earliest types for −8 > MBol <≥ −9.7 (Table 3): early + mid O-types (purple), late O-types + early B-types (blue), and mid + late B-types (cyan).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An H-alpha emission image of the LMC from MCELS (R. C. Smith & MCELS Team 1999) including the reference samples of the late types for −8 > MBol ≥ −9.7 (Table 3): ASGs (green), YSGs (gold), RSGs (red), and post-RSGs (magenta squares).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An H-alpha emission image of the LMC from MCELS (R. C. Smith & MCELS Team 1999) including the reference samples for −5.0 > MBol ≥ −7.0 (Table 3): O-types + early B-types (purple), mid B-types (blue), and late B-types (cyan).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An H-alpha emission image of the LMC from MCELS (R. C. Smith & MCELS Team 1999) including the reference samples of the late types for −5 > MBol ≥ −7.0 (Table 3): ASGs (green), YSGs (gold), and RSGs (red).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: Luminosity (MBol) as a function of relative transverse velocity (J. A. Deman & M. S. Oey 2024) with one sigma error bars for LBVs (top panel), candidate LBVs (middle panel), and B[e]sgs (bottom panel). Top panel: Higher luminosity LBVs (purple circles, MBol < −9.7) and less-luminous LBVs (blue squares, MBol ≥ −9.7). Bottom panel: High-luminosity B[e]sgs (green triangles, MBol < −9.7), mid-luminosity B[e]sgs (orange diamonds, −9.7 ≤ MBol < −7.0), and low-luminosity B[e]sgs (red pentagons, MBol ≥ −7.0).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: The relative transverse speed with one sigma error bars computed by J. A. Deman & M. S. Oey (2024) as a function of separation from the nearest neighbor of similar luminosity and spectral type (Tables 4 and 5). The gray lines note the distance a star will move in 3, 5, 8, 10, and 20 Myr at a given speed. The colors for each class and luminosity grouping are the same as used in Figure 20. Top panel: Higher luminosity LBVs (purple circles, MBol < −9.7), less-luminous LBVs (blue squares, MBol ≥ −9.7), and candidate LBVs (cyan crosses). Bottom panel: High-luminosity B[e]sgs (green triangles, MBol < −9.7), mid-luminosity B[e]sgs (orange diamonds, −9.7 ≤ MBol < −7.0), and low-luminosity B[e]sgs (red pentagons, MBol ≥ −7.0).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: Cumulative distribution plots of the nearest neighbors for the less-luminous WNs separated into groups by early types (WN2–WN4, black) and later types (WN5–WN11, gray). The distribution of less-luminous WNhs is plotted as a thin red line Each sample is plotted relative to different mid-luminosity −8.0 > MBol ≥  −9.7 reference samples (colored-dotted line).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: Cumulative distribution plots of the nearest neighbors for the highest luminosity WN separated into groups by early types (WN3–WN4, black) and later types (WN4.5—WN7, gray). The WNh (all later type) are plotted as a thin red line that overlaps the later-type WN. Each sample is plotted relative to different high-luminosity MBol < −9.7 reference samples (colored-dotted line).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: Cumulative distribution plots of the nearest less-luminosity −8.0 > MBol ≥ −9.7 WN neighbors for the WNs themselves (black), WNhs (thin red line on the right), and all 23 WCs (gray).
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: An H-alpha emission image of the LMC from MCELS (R. C. Smith & MCELS Team 1999), including LBVs (red crosses), candidate LBVs (CLBVs, smaller yellow crosses), and B[e]sgs (blue boxes) in the LMC. The largest symbols for the LBVs and B[e]sgs are for those with Mbol < −9.7, the next largest symbols are for those between −8 > Mbol ≥ 9.7, and the smallest boxes are for B[e]sg with Mbol > −7. The green arrows show the direction and amount of transverse motion that the highest velocity stars and most separated B[e]sgs (labeled) will experience over 5 Myr at the relative transverse velocity that J. A. Deman & M. S. Oey (2024) has computed for them.
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: Cumulative distribution plots of the nearest neighbors for all 23 WCs (black) plotted relative to different mid luminosity −8.0 > MBol ≥ −9.7 reference samples (colored-dotted line). The YHG sample is also plotted relative to the YSG as a gray line in that panel.
Paper: On the Spatial Distribution of Luminous Blue Variables, B[e] Supergiants, and Wolf–Rayet Stars in the Large Magellanic Cloud
Authors: John C. Martin, Roberta M. Humphreys, Kris Davidson
Figure caption: Cumulative distribution plots of the nearest neighbors for the classical LBVs (black) and candidate LBVs (gray) plotted relative to early (WN3–WN4) and late (WN4.5-WN7) higher luminosity (MBol < −9.7) WN stars (colored line).