adsabs/AstroCLIMB huggingface dataset:
Paper: TiDES: The 4MOST Time Domain Extragalactic Survey
Authors: C. Frohmaier, M. Vincenzi, M. Sullivan, S.F. Hönig, M. Smith, H. Addison, T. Collett, G. Dimitriadis, R. S. Ellis, P. Gandhi, O. Graur, I. Hook, L. Kelsey, Y.-L. Kim, C. Lidman, K. Maguire, L. Makrygianni, B. Martin, A. Möller, R. C. Nichol, M. Nicholl, P. Schady, B. D. Simmons, S. J. Smartt, E. Tempel, P. Wiseman
Figure caption: The observed 4MOST redshift distribution for all simulated transient types after five years of 4MOST operations. The solid lines show the expected number of transients with an SNR15Å  ≥ 5, while the dashed lines show the expectation for an SNR15Å  ≥ 3 in the spectrum’s continuum. The legend shows the total number of objects for each subclass satisfying the SSC. Different science cases will require different qualities of data, so these numbers are presented as a guide to the final sample size.
Paper: TiDES: The 4MOST Time Domain Extragalactic Survey
Authors: C. Frohmaier, M. Vincenzi, M. Sullivan, S.F. Hönig, M. Smith, H. Addison, T. Collett, G. Dimitriadis, R. S. Ellis, P. Gandhi, O. Graur, I. Hook, L. Kelsey, Y.-L. Kim, C. Lidman, K. Maguire, L. Makrygianni, B. Martin, A. Möller, R. C. Nichol, M. Nicholl, P. Schady, B. D. Simmons, S. J. Smartt, E. Tempel, P. Wiseman
Figure caption: The spectroscopic efficiency of targeted objects as a function of their observed magnitude. Our measurements are shown for objects meeting the SNR15Å ≥ 5 (purple diamonds) and ≥3 (green squares) parameter. 1σ statistical-only uncertainties on efficiencies are calculated using Bayes' theorem following the method presented in M. Paterno (2004) and, in the context of supernova survey efficiencies, C. Frohmaier et al. (2017). The table shows the best-fit parameters for Equation (2), m50 is the magnitude corresponding to a recovered fraction of 50%, and τ describes the steepness of the exponential fall off.
Paper: TiDES: The 4MOST Time Domain Extragalactic Survey
Authors: C. Frohmaier, M. Vincenzi, M. Sullivan, S.F. Hönig, M. Smith, H. Addison, T. Collett, G. Dimitriadis, R. S. Ellis, P. Gandhi, O. Graur, I. Hook, L. Kelsey, Y.-L. Kim, C. Lidman, K. Maguire, L. Makrygianni, B. Martin, A. Möller, R. C. Nichol, M. Nicholl, P. Schady, B. D. Simmons, S. J. Smartt, E. Tempel, P. Wiseman
Figure caption: Mock 4MOST spectra based on the 4MOST ETC output. A typical maximum-light SN Ia template spectrum at several different redshifts (red line) and r-band magnitudes is shown. The template is “observed” by 4MOST with the raw data shown in light gray and then rebinned to 15 Å (black line). The mock spectra are calculated assuming a typical 4MOST exposure time of 2700 s, conditions of seeing of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩8, airmass 1.4, in gray time. The mean S/N per 15 Å bin over 4500–8000 Å is also given.
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: The 86/87, 15, and 5 GHz luminosity light curves for both AT 2022cmc and Swift J1644. While Swift J1644 is systematically more luminous than AT 2022cmc, the two events show remarkably similar light curves, but Swift J1644 has yet to be interpreted within a thermal+nonthermal scenario.
Paper: New TeV-emitting BL Lac Candidates from the eROSITA X-Ray Survey
Authors: Cassidy Metzger, Andrea Gokus, Manel Errando
Figure caption: Example of the synchrotron SED of selected source THC J0819-079 (green triangles) compared to potential candidate WISEA J095233.24+114520.4 that is discarded by the αR-IR cut (red squares). Quasar-like sources can make it through our selection criteria based on infrared flux and spectrum and display an αIR-X similar to that of TeV HBLs, even though their synchrotron peak is probably in the infrared band and their X-ray flux, showing a very hard spectrum, samples the rising edge of their high-energy spectral component. These quasar-like objects will tend to display larger jet powers than BL Lacs, and their excess radio flux can be used to discriminate them from BL Lacs using the αR-IR criterion (see Section 3).
Paper: New TeV-emitting BL Lac Candidates from the eROSITA X-Ray Survey
Authors: Cassidy Metzger, Andrea Gokus, Manel Errando
Figure caption: The flux and counts distribution in the 2.0–5.0 keV band for the main eRASS1 catalog (black) and hard eRASS1 catalog (blue) compared with the flux and counts for TeV-detected HBLs (red).
Paper: New TeV-emitting BL Lac Candidates from the eROSITA X-Ray Survey
Authors: Cassidy Metzger, Andrea Gokus, Manel Errando
Figure caption: Distribution of X-ray fluxes for the TeV candidate blazars in different bands from the eRASS1 catalog, compared to the fluxes of all sources in the eROSITA survey.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Example Monte Carlo simulation results for an Earth-mass planet with a CO2 atmosphere orbiting a 1 M⊙ star (Upper) and a four-Earth-mass planet with a N2-dominated atmosphere orbiting a 0.2 M⊙ star (Lower). Left: bolometric instellation, scaled to Earth’s value (S/S⊕), plotted against the total carbon or N2 mass lost. Blue dots indicate Monte Carlo outcomes in which the planet retains its atmosphere (with an initial carbon mass of 0.01 M⊕), while red dots indicate outcomes in which the atmosphere is stripped. The middle red line marks the critical instellation at p0 = 0.1, meaning there is a 90% probability of atmospheric retention at that flux level. The shaded region spans from p0 = 0.01 (lower boundary) to p0 = 0.5 (upper boundary), illustrating instellation thresholds for 99% and 50% retention probability, respectively. To obtain a robust estimate of the critical instellation S* at a given p0, we draw 5000-point bootstrap samples from our 10,000-point Monte Carlo data set (in 10 iterations), refit the logistic model each time, and then average the resulting S* values. Right: Histograms of the instellation values for planets that retain atmosphere (blue) vs. those that lose it (red). For our implementation of the CP2024 N2-escape, in the volatile-rich limit, the probability of atmospheric loss does not reach one due to the plateau in escape rates for the highest XUV fluxes. To capture this behavior, we apply a three-parameter logistic fitting. In contrast, for CO2 and other atmospheres where the escape rate continues to increase with XUV flux, the loss probability approaches one at infinite high XUV flux, so it is reduced to a two-parameter fitting.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Trend of the scaled density of the solid body only: the upper row shows 2D histograms of the scaled density of the solid body (﹩{\rho }_{\mathrm{solid}}/{\rho }_{\oplus }^{* }﹩) as a function of planetary mass (Mp), while the lower row shows its relationship with equilibrium temperature (Teq). The left column (c) assumes that solid density variations follow a normal distribution, with a standard deviation equal to 1/3 of the difference between Rearth-like(Mp) and Rsilicate(Mp). The right column (d) corresponds to a uniform distribution spanning the range between Rsilicate(Mp) (pure MgSiO3) and Riron(Mp) (pure Fe). The black lines and black text indicate the results of linear regression for the solid-body scaled density, while the red ones represent the linear regression of the total density derived from the transit radius (see Figure 7). In (c), the slope of the solid-body density trend is an order of magnitude lower than that of the final total density, suggesting an insignificant contribution from variations in the solid composition. However, in (d), the solid-body density trend significantly influences the overall density slope, even changing the sign for the slope of ﹩{\rho }_{\mathrm{solid}}/{\rho }_{\oplus }^{* }-{M}_{p}﹩. We also tested uniformly sampling density instead of radius, but the trend caused by the solid portion alone persists.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Mass–radius relationship for solid-body planets under three composition assumptions: given a planetary mass (Mp), the radius is assigned based on different composition assumptions: (a) a fixed Earth-like composition (Rearth-like(Mp)), (b) a normal distribution centered at Rearth-like(Mp) with a standard deviation equal to one-third of the difference between Rearth-like(Mp) and Rsilicate(Mp), (c) a normal distribution centered at Rearth-like(Mp) with a standard deviation equal the difference between Rearth-like(Mp) and Rsilicate(Mp), and (d) a uniform distribution spanning the range between Rsilicate(Mp) (pure MgSiO3) and Riron(Mp) (pure Fe). The shaded blue region represents a 2D histogram of our Monte Carlo samples, with darker colors indicating higher number density. The dots are observed rocky planet candidates from the NASA Exoplanet Archive, with error bars representing measurement uncertainties. The colors represent the measured density relative to Earth’s composition.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Left Panel: temperature–pressure profiles for atmospheres with surface pressures of 10 bar (pink) and 100 bar (blue). The solid lines correspond to the two-layer model (Scenario (1) in Figure 5), where the atmosphere consists of a convective lower layer and an isothermal upper layer beyond the radiative-convective boundary (RCB). The dashed lines represent the three-layer model (Scenario (2) in Figure 5), where an additional radiative layer forms near the surface. Right Panel: altitude–temperature profiles for the same cases shown in the left panel. Triangular markers indicate the pressure level probed by the transit method, with filled symbols representing the two-layer model (Scenario (1)) and open symbols representing the three-layer model (Scenario (2)).
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Same configuration and markers as Figure 3. Here we plot only the 90% cosmic shoreline for two initial volatile fractions, but instead of sampling the escape onset from Table 2, we delay and fix the start of escape at 500 Myr and 1 Gyr. This illustrates the potential retention of the atmosphere outgassed from the volatiles sequestered in the solid mantle after magma-ocean crystallization, under the assumptions that the initial volatile atmosphere and dissolved magma-ocean volatiles were completely removed and that escape is not supply-limited.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Cosmic shorelines as functions of planetary mass and instellation scaled to Earth’s value (S/S⊕). Each line corresponds to results computed for stellar masses within a range of 0.01 M⊙. For example, the lowest (darkest) line represents stellar masses between 0.10 and 0.11 M⊙. The priority scores listed in Table 3 and Table B1 are derived from these shoreline calculations.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: High-redshift Meudon model radiation field, including the cosmic microwave background (pink), IR (blue), visible (green), and the B. T. Draine (1978) UV component, which is scaled to provide an incident G0 = 106 at the cloud’s edge (red).
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: The mass–radius relationship for different planetary compositions: pure iron (100% Fe), Earth-like rocky (32.5% Fe + 67.5% MgSiO3), and pure rock (100% MgSiO3).
Paper: A Tale of Two Sightlines: Comparison of Hydrocarbon Dust Absorption Bands toward Cygnus OB2-12 and the Galactic Center
Authors: Yvonne J. Pendleton, T. R. Geballe, Laurie E. U. Chu, Marjorie Decleir, Karl D. Gordon, A. G. G. M. Tielens, Louis J. Allamandola, Jeroen Bouwman, J. E. Chiar, Curtis Dewitt, Burcu Gunay, Thomas Henning, Vito Mennella, M. E. Palumbo, Alexey Potapov, Maisie Rashman, Sascha Zeegers
Figure caption: Optical depth near- and mid-IR spectra for Cyg OB2-12 (black dots) and the Quintuplet (blue dots) compared to three laboratory spectra (black lines). Wavelength scales are at the bottom of each spectrum; frequency scale is at the top of the figure. Scaling factors shown apply to both near- and mid-IR data. Dashed vertical lines are at 3.08 μm (corresponding to water ice), 3.289 μm (the central wavelength of the Gaussian used to fit the 3.3 μm CH aromatic band), 3.415 μm (the 3.4 μm aliphatic band), 5.85 μm (the aliphatic carbonyl band), 6.05 μm (the aromatic, quinone carbonyl band), 6.2 μm (the blended olefinic and aromatic bands), and 6.85 μm (the scissor band). See Table 1 for details. Top: hydrogenated amorphous carbon (HAC) produced by hydrogen atom irradiation of carbon grains under simulated diffuse ISM conditions, resulting in predominantly surface aliphatic hydrocarbons (V. Mennella et al. 2002). Middle: an interstellar dust analog synthesized from a carbon-rich plasma using an acetylene precursor under simulated circumstellar conditions, yielding predominantly aromatic particles with an aliphatic hydrocarbon component (B. Günay et al. 2018). Bottom: UV-irradiated H2O:CH3OH:silicate mixture in which the components were deposited together at low temperature and then exposed to UV light (A. Potapov et al. 2021). This mid-IR spectrum has been flattened by dividing it by a linear continuum matching the spectrum at 5.55 and 7.35 μm. The three laboratory analogs were specifically prepared to reproduce the 3.4 μm aliphatic CH stretch complex. Differences between the laboratory spectra and the interstellar absorption at other wavelengths (e.g., the 3.3 μm aromatic CH stretch or carbonyl bands near 5.85 μm) are expected, as these experiments did not attempt to replicate the full chemical complexity of interstellar carbonaceous dust.
Paper: A Tale of Two Sightlines: Comparison of Hydrocarbon Dust Absorption Bands toward Cygnus OB2-12 and the Galactic Center
Authors: Yvonne J. Pendleton, T. R. Geballe, Laurie E. U. Chu, Marjorie Decleir, Karl D. Gordon, A. G. G. M. Tielens, Louis J. Allamandola, Jeroen Bouwman, J. E. Chiar, Curtis Dewitt, Burcu Gunay, Thomas Henning, Vito Mennella, M. E. Palumbo, Alexey Potapov, Maisie Rashman, Sascha Zeegers
Figure caption: The 2.86−3.70 μm optical depth spectrum of Cyg OB2-12 obtained with SpeX on the NASA IRTF. The spectrum is displayed at a resolution of 0.004 μm. Telluric-line residuals were removed as described in Section 2.1. Three H I Pfund series (n–5) absorption lines and a weak He II emission line are labeled. The wavelengths of the H I Humphreys series (n–6) lines and the series limit at 3.283 μm are indicated by short vertical lines. Data points in the interval 3.31−3.32 μm are spurious due to incomplete correction of the nearly totally opaque telluric absorption by closely spaced lines of the methane ν3 Q-branch, and are not shown. The noise level varies with wavelength but can be estimated from the point-to-point fluctuations in the signal in regions devoid of absorption features, such as 2.90−3.00 μm and 3.12−3.20 μm.
Paper: A Tale of Two Sightlines: Comparison of Hydrocarbon Dust Absorption Bands toward Cygnus OB2-12 and the Galactic Center
Authors: Yvonne J. Pendleton, T. R. Geballe, Laurie E. U. Chu, Marjorie Decleir, Karl D. Gordon, A. G. G. M. Tielens, Louis J. Allamandola, Jeroen Bouwman, J. E. Chiar, Curtis Dewitt, Burcu Gunay, Thomas Henning, Vito Mennella, M. E. Palumbo, Alexey Potapov, Maisie Rashman, Sascha Zeegers
Figure caption: Comparison of spectral profiles of the 3.3 μm absorption bands toward Cyg OB2-12 (black) and the GC Quintuplet (blue, scaled down by a factor of 3.5; data from Figure 3, this paper), and the 3.25 μm band in the deeply embedded YSO Mon R2 IRS3 (K. Sellgren et al. 1995, shown with its Gaussian fit, both in gray). The Gaussian used to fit the 3.3 μm bands in the spectra of Cyg OB2-12 and the Quintuplet is shown in red.
Paper: A Tale of Two Sightlines: Comparison of Hydrocarbon Dust Absorption Bands toward Cygnus OB2-12 and the Galactic Center
Authors: Yvonne J. Pendleton, T. R. Geballe, Laurie E. U. Chu, Marjorie Decleir, Karl D. Gordon, A. G. G. M. Tielens, Louis J. Allamandola, Jeroen Bouwman, J. E. Chiar, Curtis Dewitt, Burcu Gunay, Thomas Henning, Vito Mennella, M. E. Palumbo, Alexey Potapov, Maisie Rashman, Sascha Zeegers
Figure caption: The 2.90−3.70 μm (NASA IRTF) and 5.50−7.34 μm (Spitzer IRS) spectra of Cyg OB2-12 on a common optical depth scale. The resolutions of the two spectra are 0.004 μm and 0.09 μm, respectively. The gap at 3.025−3.10 μm is due to interference by the H I 10−5 absorption and He II 7−6 emission lines. The gap at 3.29−3.32 μm is due to interference by the H I 9−5 absorption line at 3.297 μm and nearly total absorption of the spectrum by telluric methane in the 3.31−3.32 μm interval.
Paper: A Tale of Two Sightlines: Comparison of Hydrocarbon Dust Absorption Bands toward Cygnus OB2-12 and the Galactic Center
Authors: Yvonne J. Pendleton, T. R. Geballe, Laurie E. U. Chu, Marjorie Decleir, Karl D. Gordon, A. G. G. M. Tielens, Louis J. Allamandola, Jeroen Bouwman, J. E. Chiar, Curtis Dewitt, Burcu Gunay, Thomas Henning, Vito Mennella, M. E. Palumbo, Alexey Potapov, Maisie Rashman, Sascha Zeegers
Figure caption: Optical depth spectra of Cyg OB2-12 (black) and Quintuplet (blue) sightlines. Both the near- and mid-IR optical depth spectra of the Quintuplet (both from J. E. Chiar et al. 2013) are divided by 3.5 so that the strengths of the 3.4 μm band match and thus facilitate comparison of relative band intensities. The continuum level of the mid-IR spectrum of the Quintuplet is slightly shifted from that in J. E. Chiar et al. (2013), as discussed in the text.
Paper: A Tale of Two Sightlines: Comparison of Hydrocarbon Dust Absorption Bands toward Cygnus OB2-12 and the Galactic Center
Authors: Yvonne J. Pendleton, T. R. Geballe, Laurie E. U. Chu, Marjorie Decleir, Karl D. Gordon, A. G. G. M. Tielens, Louis J. Allamandola, Jeroen Bouwman, J. E. Chiar, Curtis Dewitt, Burcu Gunay, Thomas Henning, Vito Mennella, M. E. Palumbo, Alexey Potapov, Maisie Rashman, Sascha Zeegers
Figure caption: Normalized flux (F; left and right y-axes) and optical depth (τ; middle y-axes) 3.1−3.7 μm spectra of Cyg OB2-12 (left) and Quintuplet (right) (observations shown by black solid lines) with Gaussian fits to the 3.289 μm (aromatic CH) in red and to the aliphatic CH stretch bands in green at 3.376 μm (CH3 asymmetric), 3.420 μm (CH2 asymmetric), 3.474 μm (CH3 symmetric), and 3.52 μm (CH2 symmetric). The Quintuplet spectrum (a composite of ISO and Spitzer data) and the fit to it are directly from J. E. Chiar et al. (2013, their Figure 2). The sums of the Gaussian fits are shown by purple lines for both sightlines. Details of the fits are summarized in Table 1.
Paper: A Tale of Two Sightlines: Comparison of Hydrocarbon Dust Absorption Bands toward Cygnus OB2-12 and the Galactic Center
Authors: Yvonne J. Pendleton, T. R. Geballe, Laurie E. U. Chu, Marjorie Decleir, Karl D. Gordon, A. G. G. M. Tielens, Louis J. Allamandola, Jeroen Bouwman, J. E. Chiar, Curtis Dewitt, Burcu Gunay, Thomas Henning, Vito Mennella, M. E. Palumbo, Alexey Potapov, Maisie Rashman, Sascha Zeegers
Figure caption: Normalized flux (F; left and right y-axes) and optical depth (τ; middle y-axes) spectra are depicted by thin black lines for Cyg OB2-12 and the Quintuplet sources, left and right panels, respectively, over the 5.5−7.0 μm range. Gaussian fits to the 5.85 (C=O; blue), 6.05 (quinone; aqua), 6.19 (olefinic; yellow), 6.25 (aromatic; red), and 6.85 (CH2 scissor; green) μm absorption bands are color-coded as listed in the legend. The sums of the Gaussians are shown by dashed purple lines.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: The star’s y-direction acceleration (upper panel) and the mass accretion rate per area at x = −Lx (lower panel) of the JET-x, JET-y, and JET-z models. Both models consider the scenario with stellar outflow.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Time-averaged azimuthal acceleration of the sBH in the BH-jet-z models for different values of r0.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Similar to Figure 6 but for the JET-x (left panel), JET-y (middle panel), and JET-z (right panel) models.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Similar to Figure 2 but for the ACCD-anti (red lines) and ACCD-fric (blue lines) models. The dashed lines represent acceleration in the y-direction, while the dotted lines represent acceleration in the x-direction.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Similar to Figure 6 but for the ACCD-anti (left panel) and ACCD-fric (right panel) models. The white dashed circles indicate the characteristic standoff distance R0 in the left panel and the Bondi radius RB on the right.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Similar to Figure 1 but for the GAMMA-anti model.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Gas density ρ in the x = 0 plane at tevo = 0.1 P for the BH-jet-z models.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Similar to Figure 3 but for the PG-45 and PG-0 models.
Paper: A Novel Approach to Identifying Substructures through Analysis of Metallicity Distribution Functions
Authors: Young Kwang Kim, Young Sun Lee, 영선 이, Timothy C. Beers
Figure caption: Distribution of stars in the Etot–LZ plane for LRS 1 (top panel), LRS 2A and LRS 2B (middle panel), and LRS 3 and LRS 4 (bottom panel). The solid orange boxes mark the locations of Sequoia, Thamnos 1, and Thamnos 2 used by H. H. Koppelman et al. (2019) and GSE by D. Horta et al. (2023), scaled to the St﹩\ddot{a}﹩ckel potential used in this study. The solid green box indicates the region of the ED-2 stars from E. Dodd et al. (2023) and the ED-2 candidates from our sample.