adsabs/AstroCLIMB huggingface dataset:
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: First: PCA-template-based best-fit model (shown in colored solid lines) of a galaxy spectrum. We can see the flux discontinuity in the z camera (λ ∼ 7550 Å). Second: zoomed version of PCA model of the same spectrum, showing the expected location of emission lines. The continuum is not well-fitted with PCA at the camera boundary. [O III] doublet is also not well fitted. Third: archetype-based per-camera best-fit model of the same spectrum. The fit looks better visually and absorbs the flux discontinuity in the z camera more accurately, also evident by smaller χ 2. Fourth: zoomed version of archetype-based per-camera model of the same spectrum, showing the expected location of emission lines. [O II] emission line (λ ∼ 9200 Å) is more accurately modeled. The black curve is the observed flux, the purple curve shows the error spectra in all panels, and the fitted model is shown in solid color lines.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption:  g − r vs. stellar mass for parent galaxy sample (left) and archetypes (right). In both panels, we show the properties of ELGs (blue), LRGs (red), and BGS (orange). We see that galaxies lie in different regions on this plane, and archetypes also span a similar range in the color space. In the right panel, the open circles denote the archetype that we selected randomly to show their spectra in Figure 14 in Appendix A.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: First: PCA-template-based model of the same galaxy spectrum (shown in Figure 6) at right redshift. Second: zoomed version of the model. We can see that χ 2 is higher than the best-fit model (see Figure 6). Third: archetype-based fit of the same spectrum at wrong redshift. Fourth: zoomed version of the archetype model. We see that our archetype model does not fit any unphysical feature, and χ 2 is higher than the best-fit model (see third panel of Figure 6). The black curve is the observed flux, the purple curve shows the error spectra in both panels, and the model is shown in solid color lines.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Empirical determination of optimal threshold for archetype generation using the SetCoverPy method. We show the ﹩{s}_{\mathrm{red}}^{2}﹩ as a function of the number of galaxy archetypes for each galaxy subtype. Our optimal value for ﹩{s}_{\mathrm{red}}^{2}\approx 0.003﹩ lies where the number of LRG archetypes significantly decreases (as shown in the inset). Beyond this threshold, the number of archetypes begins to saturate at higher ﹩{s}_{\mathrm{red}}^{2}﹩ values.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Analytical structures arising in phase portraits (left-column panels) and comparison to numerical structures arising in Poincaré sections (right-column panels) at different maximum eccentricities when the total angular momentum is characterized by a ref = 10. Red dashed lines stand for the separatrices of the synchronous (1:1) resonance, blue lines stand for separatrices of secondary spin–orbit resonances, and green lines represent separatrices of high-order spin–orbit resonances. An excellent agreement can be observed between analytical and numerical structures.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Analytical structures arising in phase portraits and numerical structures arising in Poincaré sections for three representative binary asteroid systems (Didymos, VO123, and Suruga). Red dashed lines stand for the dynamical separatrices of the synchronous (1:1) resonance and the blue lines represent the separatrices of the secondary resonances. Green lines are level curves of the resonant Hamiltonian (i.e., phase portraits). Chaotic motions can be observed in the regions around dynamical separatrices of the primary synchronous (1:1) resonance as well as around dynamical separatrices of secondary resonance.
Paper: Search for Young Stellar Objects within 4XMM-DR13 Using CatBoost and SPE
Authors: Xiangyao Ma, Yanxia Zhang, Jingyi Zhang, Changhua Li, Zihan Kang, Ji Li
Figure caption: Confusion matrix of classification for the known samples, the above panel for CatBoost while the below panel for SPE.
Paper: Search for Young Stellar Objects within 4XMM-DR13 Using CatBoost and SPE
Authors: Xiangyao Ma, Yanxia Zhang, Jingyi Zhang, Changhua Li, Zihan Kang, Ji Li
Figure caption: The distribution of stars, galaxies, quasars and YSOs in 2D spaces; the red open circles represent stars, the blue open squares for YSOs, the green open diamonds for galaxies, and the purple open triangles for quasars.
Paper: Search for Young Stellar Objects within 4XMM-DR13 Using CatBoost and SPE
Authors: Xiangyao Ma, Yanxia Zhang, Jingyi Zhang, Changhua Li, Zihan Kang, Ji Li
Figure caption: The feature importance of the XMM-WISE-SDSS sample. The above panel is feature importance by CatBoost, and the below panel is feature importance by SPE.
Paper: A Geodetic and Astrometric VLBI Experiment at 22/43/88/132 GHz
Authors: Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang
Figure caption: The closure group delay, closure delay rate, and closure phase in the KVN triangle baseline (KTN-KUS-KYS), with different frequency bands represented by dots of different colors. Top panels: closure group delay without/with FPT; Middle panels: closure delay rate without/with FPT; and Bottom panels: closure phase without/with FPT. The 43 GHz result is not presented and has large uncertainties due to the low SNR issues on KUS station.
Paper: A Geodetic and Astrometric VLBI Experiment at 22/43/88/132 GHz
Authors: Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang
Figure caption: Postfitting residuals at different bands.
Paper: The Components of Cepheid Systems: The FN Vel System 
Authors: Nancy Remage Evans, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Charles Proffitt, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: The standard deviations from the spectrum-model comparison as the temperature of the models is changed. Dots: the standard deviation; triangles: the parabola fit. Left: E(B – V) = 0.60 mag. Right: E(B − V) = 0.56 mag.
Paper: The Components of Cepheid Systems: The FN Vel System 
Authors: Nancy Remage Evans, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Charles Proffitt, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: The difference between the model and the spectrum for E(B − V) = 0.60 mag. The temperatures for the models are on the right of each difference spectrum. The wavelengths between 1180 and 1250 Å are omitted because of contamination by interstellar Lyα absorption. The difference spectrum in black is the best fit.
Paper: The Components of Cepheid Systems: The FN Vel System 
Authors: Nancy Remage Evans, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Charles Proffitt, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: Comparison between BOSZ models and the STIS spectrum unreddened for E(B − V) = 0.60 mag. Flux for all panels is in erg cm−2 s−1 Å−1; wavelength is in Å. Models are in red; spectrum is in black. The temperature for the models is at the lower right of each panel.
Paper: The Components of Cepheid Systems: The FN Vel System 
Authors: Nancy Remage Evans, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Charles Proffitt, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: The pulsation velocity (left) and the orbital velocity (right) are shown as a function of their respective phases. The dashed line in the left figure is the systemic velocity. The colors of the symbols indicate the date of observation from the earliest data in yellow to more recent data in blue. (Adapted from S. Shetye et al. 2024).
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: Histograms of Δ (the deviation from perfect period commensurability; Equation (1)) for planet pairs near first-order resonances (left panel, including the 6:5, 5:4, 4:3, 3:2, and 2:1 MMRs) and second-order resonances (right panel, including the 9:7, 7:5, 5:3, and 3:1 MMRs), across all ages (known and unknown). The translucent histograms are drawn from all 734 confirmed multiplanet systems, and the dashed red lines mark our chosen bounds on Δ, inside of which pairs are deemed “resonant.” We used an asymmetrical boundary −0.015 ≤ Δ ≤ 0.03 for first-order resonances to reflect how their libration widths are intrinsically asymmetric (K. Batygin & A. Morbidelli 2013b; N. Choksi & E. Chiang 2020), and a symmetrical boundary of −0.015 ≤ Δ ≤ 0.015 for second-order resonances (N. Bailey et al. 2022). Note how the excess population or “peak” in the left panel is captured by our Δ bounds. Systems identified to have more than one resonant pair—these are arguably self-validating, since resonances congregate in a system more than they would if they were distributed randomly (Section 4.1)—are used to generate the opaque histograms, most of which lie self-consistently within our Δ bounds (not all of the opaque points lie inside, since a given multiresonant system can also contain nonresonant pairs).
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: Given a system with one resonant pair, what is the probability that this same system has a second resonant pair? We experiment using observed multiplanet systems across all ages (known and unknown). The rows indicate the given first resonant pair (either first-order or second-order, with their raw probabilities), while the columns label the second pair. The first entry in the left panel shows that, using real observed systems, there are 61 cases where both pairs are near first-order resonances. This corresponds to a observed probability of 61/(61 + 27 + 99) = 32.6% ± 3.4% for finding a second first-order resonance given a first first-order resonance. This probability is twice as high as in a simulated uncorrelated sample that scrambles observed period ratios across all systems (right panel; the corresponding probability is 15.6% ± 1.1%, which is just the raw incidence of first-order resonances). Resonances among observed systems thus “congregate”: where there is one resonant pair, there are better-than-random odds that there will be another in the same system.
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: The fractions of observed neighboring pairs of planets across all ages near various first- and second-order resonances. Resonances with smaller period ratios (4:3, 5:4, and 6:5) are progressively less populated because a pair of planets must avoid all earlier resonances to reach them. Another possibility is that these resonances may start to overlap and destabilize (e.g., J. Rath et al. 2022).
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Right: B, V, I image of NGC 1614 with detected clusters overlaid; the color-coding shows the maximum E(B − V) allowed during the age-dating fits. Left: uncorrected U − B vs. V − I color–color diagrams of four example regions with assigned maximum allowed E(B − V) of 0.1 mag (top left), 0.5 mag (top right), 1.0 mag (bottom left), and 2.0 mag (bottom right). A reddening vector of A  V  = 1.0 is shown in the bottom right image. Diamonds indicate clusters with V-mag ≤ 23.5, filled circles represent 23.5 <= V-mag < 24.5, and open circles represent V-mag ≥ 24.5. Data points outlined and filled in black indicate that the cluster has Hα emission and is younger than ≈6 Myr. These regions illustrate the different amounts of reddening due to dust found for clusters in different regions within NGC 1614.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Color–color diagrams for clusters in NGC 1614 with B − V vs. V − I (left) and NUV – B vs. V − I (right). The grayscale showing the V-band magnitude is to the right of the diagrams. Predictions from solar-metallicity (BC03) tracks (cyan) for cluster evolution are shown in blue for log (τ/yr) = 6, 7, 8, 9, and 10. A reddening vector with A  V  = 1.0 is shown in the upper right corner of each panel.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Cumulative mass functions for clusters in NGC 1614 in age intervals of 1–10 Myr, 10–100 Myr, and 100–400 Myr. The adopted completeness limit, where each distribution flattens from a power law, is shown as the dashed vertical line. Fits to a power-law fit are shown as the dotted–dashed lines, and fits to a truncated power law are shown as the dotted line. The best-fit values of β for a power law (PL) and the statistic N  C , which represents the upper end of a truncated power law (TPL), are given in the upper right corner of each panel. See text for details.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Comparison of Γ values of different galaxies and age intervals. Γ1−10 is plotted in blue, Γ10−100 in green, and Γ100−400 in red. Values for NGC 1614 in this work are plotted as diamonds, and Γ1−10 for NGC 1614 from A. Adamo et al. (2020) are plotted as black crosses. Blue compact dwarf galaxies from R. Chandar et al. (2023b) are plotted as triangles. Binned dwarfs in the LEGUS from D. O. Cook et al. (2023) are plotted as circles. The relationships found in R. Chandar et al. (2017) are the lines with shaded error regions in each color.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption:  U − B vs. V − I color–color diagram with the BC03 model in black, Hα training set clusters shown as blue circles, UV-arm training set shown as green triangles, and old cluster training set shown as red squares. A reddening vector with an A  V  = 1.0 is shown in the upper right corner.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Cluster age–mass diagram for NGC 1614. The dashed line represents M  V  = −8 mag, the approximate completeness limit for individual clusters in our sample. Median error bars are plotted for clusters above the completeness limits for the 1–10 Myr, 10–100 Myr, and 100–400 Myr age intervals (see text).
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Maximum likelihood fit results to the power-law index β and upper mass cutoff M * are shown for <10 Myr, 10–100 Myr, and 100–400 Myr clusters. The most massive cluster in each age range is plotted as the green triangle. The most likely −β and M ⋆ values are shown as the horizontal and vertical dashed lines, respectively. The 1σ (black), 2σ (gray), and 3σ (light gray) confidence intervals are also shown. There is no convergence for M ⋆ in any age range, indicating that the data do not prefer an exponential upper mass cutoff.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Age distributions of star clusters in NGC 1614 in the three indicated mass intervals. Fitted lines show power laws, ﹩{dN}/d\tau \propto {\tau }^{\gamma }﹩, with the best-fit value of γ indicated.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Same as the left panel of Figure 5, but with cluster colors corrected for best-fit values from age-dating.
Paper: The Radiative–Convective Gap: Fact or Fiction?
Authors: Wolfgang Brandner, Artur Sorg, Siegfried Röser, Elena Schilbach
Figure caption: Left: color–magnitude diagram of the Hyades, Praesepe, Pleiades, and α Persei clusters for 0.3 ≤ BP0 − RP0 ≤ 0.7 mag. Stars in Praesepe fill in the gap in the Hyades stellar sequence. Similarly, the combined Praesepe and α Persei sequence does not exhibit a pronounced gap. Right: one instance of Monte Carlo simulations of clusters as populous as the Hyades in the mass range 0.5–2.5 M ⊙. The stochastic population of the stellar sequence according to the initial mass function results in a gap similar to the gap in the Hyades.
Paper: The Radiative–Convective Gap: Fact or Fiction?
Authors: Wolfgang Brandner, Artur Sorg, Siegfried Röser, Elena Schilbach
Figure caption: Instances of Monte Carlo–generated synthetic color–magnitude diagrams of a Hyades-type cluster. The random drawing from an initial mass function combined with small number statistics, and the nonlinear relation between stellar mass and BP − RP color can result in gaps in the sequence.
Paper: The Radiative–Convective Gap: Fact or Fiction?
Authors: Wolfgang Brandner, Artur Sorg, Siegfried Röser, Elena Schilbach
Figure caption: Cumulative distribution of extinction-corrected absolute G abs magnitudes (left) and BP − RP colors (right) of bona fide single stars in the Hyades, Pleiades, Praesepe, and α Persei. The vertical dashed lines mark the color range of the “radiative–convective” gap seen in the Hyades CMD.
Paper: The Radiative–Convective Gap: Fact or Fiction?
Authors: Wolfgang Brandner, Artur Sorg, Siegfried Röser, Elena Schilbach
Figure caption: Absolute color–magnitude diagram of the bona fide single stars in the Praesepe open cluster based on Gaia DR3. The uncertainties in absolute magnitude and color are indicated by red error bars. Overplotted as dotted blue lines is the family of best-fitting PARSEC isochrones.
Paper: The Radiative–Convective Gap: Fact or Fiction?
Authors: Wolfgang Brandner, Artur Sorg, Siegfried Röser, Elena Schilbach
Figure caption: Color–color diagrams of the Praesepe (left) and α Persei (right) open clusters based on Gaia DR3 photometry. Blue plus and green crosses mark stars and white dwarfs, respectively, with valid photometry in all three Gaia photometric bands. Orange “tri-ups” indicate likely binary stars. Red circles mark stars with suspect photometry in at least one of the photometric bands. For α Persei (A V = 0.3 mag), we plot an extinction vector corresponding to A V = 1.0 mag.
Paper: The Radiative–Convective Gap: Fact or Fiction?
Authors: Wolfgang Brandner, Artur Sorg, Siegfried Röser, Elena Schilbach
Figure caption: The minimum distance in color–magnitude space of stars on the single star sequence in Praesepe from the best-fitting PARSEC isochrone.