adsabs/AstroCLIMB huggingface dataset:
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) for the high-luminosity reference samples with MBol < −9.7 (Table 3): early O-types (purple), mid O-types (blue), late O-types (cyan), and early B-types (green).
Paper: The Evolution of Jupiter and Saturn as a Function of the Rρ Parameter
Authors: Ankan Sur, Adam Burrows, Roberto Tejada Arevalo, Yubo Su
Figure caption: Evolutionary model for Jupiter with an initial fuzzy core that experiences Schwarzschild convection (Rρ = 0). This model reproduces, within ∼0.7% of the various measured quantities, the current values of the effective temperature, equatorial radius, atmospheric helium abundance, outer envelope metallicity, and J2 and J4 gravitational moments. The initial outer entropy is 7.8 kB/baryon, while the interior entropy is 5.8 kB/baryon. The panels display: (top left) the evolution of the temperature profile; (top middle) the evolution of the helium mass fraction (Y) profile; (top right) the evolution of the effective temperature and equatorial radius; (bottom left) the evolution of the entropy profile; (bottom middle) the evolution of the Z profile; and (bottom right) the evolution of the gravitational moments J2 and J4. This Jupiter model contains 38 M⊕ of heavy elements, including a compact core of 1 M⊕ (Z = 1). The outer metallicity starts at 1.9 Z⊙ and increases to 3.66 Z⊙. Helium rain begins at ∼3.5 Gyr, based on the LHR0911 miscibility curves with a −75 K temperature shift, resulting in outer helium depletion to Y = 0.233, consistent with Galileo entry probe measurements (U. von Zahn et al. 1998).
Paper: The Evolution of Jupiter and Saturn as a Function of the Rρ Parameter
Authors: Ankan Sur, Adam Burrows, Roberto Tejada Arevalo, Yubo Su
Figure caption: Best-fit Saturn evolutionary model assuming an initially fuzzy core and Schwarzschild convection (Rρ = 0). This model reproduces Saturn’s present-day effective temperature, equatorial radius, outer envelope metallicity, and gravitational moment, J2, within 0.5% of their measured values. The initial entropy is 7.0 kB/baryon at the outer boundary and ∼4.0 kB/baryon in the deep interior. The six panels mirror those shown in Figure 1: (top left) temperature profile evolution; (top middle) helium mass fraction (Y) profile; (top right) evolution of effective temperature and equatorial radius; (bottom left) entropy profile; (bottom middle) heavy-element mass fraction (Z) profile; and (bottom right) gravitational moments J2 and J4. The model contains a total of 24.5 M⊕ in heavy elements, including a compact 1.5 M⊕ core. The outer envelope metallicity rises from an initial value of 2.0 to 9 Z⊙ due to interior mixing. The LHR0911 hydrogen–helium miscibility curve shifted by –75 K (equivalent to the corresponding Jupiter model) leads to an atmospheric helium mass fraction of Yatm ∼ 0.168, in agreement with constraints from B. J. Conrath & D. Gautier (2000) and T. T. Koskinen & S. Guerlet (2018) (pink shaded region in the top middle panel). The miscibility boundary and helium rain region for the current epoch of the best-fit model are highlighted using a blue field in the top left panel.
Paper: The Evolution of Jupiter and Saturn as a Function of the Rρ Parameter
Authors: Ankan Sur, Adam Burrows, Roberto Tejada Arevalo, Yubo Su
Figure caption: Best-fit evolutionary models for Jupiter with varying Rρ. Only the initial and final (4.56 Gyr) timestamps are shown for comparison. The dark blue curve corresponds to our updated Ledoux model (Rρ = 1), while the red curve shows the Schwarzschild model (Rρ = 0). The light blue, green, and orange curves represent intermediate cases with Rρ = 0.75, 0.50, and 0.25. All quantities are within 1σ of their measured central values.
Paper: The Evolution of Jupiter and Saturn as a Function of the Rρ Parameter
Authors: Ankan Sur, Adam Burrows, Roberto Tejada Arevalo, Yubo Su
Figure caption: Same as Figure 3, but for Saturn: best-fit evolutionary models with varying Rρ values. As Rρ decreases, the models exhibit higher effective temperatures during early evolution, enhanced final envelope metallicities, broader helium rain regions, and more helium depletion at the surface. The total heavy-element mass and initial entropies are adjusted accordingly to reproduce Saturn’s present-day structure, with the Schwarzschild model requiring lower initial central temperatures and a more compact core.
Paper: The Evolution of Jupiter and Saturn as a Function of the Rρ Parameter
Authors: Ankan Sur, Adam Burrows, Roberto Tejada Arevalo, Yubo Su
Figure caption: Brunt–Väisälä frequency ratios for Jupiter and Saturn at 4.56 Gyr for models with varying Rρ. The shaded region in panel (b) indicates the seismologically inferred stratified zone from C. R. Mankovich & J. Fuller (2021; MF2021), with a characteristic ratio of 2 extending to 60% of Saturn’s radius. Our models reveal comparable stable regions—one associated with the dilute core and another arising from the helium rain layer in both planets. The location of the peaks of our distributions for Saturn matches well with the predictions of MF2021. The raw Brunt data have been smoothed out for better visualization in this plot.
Paper: Type Ia Supernova Growth-rate Measurement with LSST Simulations: Intrinsic Scatter Systematics
Authors: Bastien Carreres, Rebecca C. Chen, Erik R. Peterson, Dan Scolnic, Corentin Ravoux, Damiano Rosselli, Maria Acevedo, Julian E. Bautista, Dominique Fouchez, Lluís Galbany, Benjamin Racine
Figure caption: Bias in estimated velocity as a function of fitted SALT color parameter c. The contours represent the 25%, 50% and 75% density levels of the SN Ia sample, and points are the velocity bias in different c bins. The blue contours correspond to SP23, while the yellow contours are obtained using a variation of the ﹩{\tau }_{{E}_{\mathrm{dust}}}﹩ parameter.
Paper: The Evolution of Jupiter and Saturn as a Function of the Rρ Parameter
Authors: Ankan Sur, Adam Burrows, Roberto Tejada Arevalo, Yubo Su
Figure caption: Initial entropy profiles for our Jupiter models with varying Rρ values, compared against hot-start (solid lines) and cold-start (dashed lines) initial conditions from A. Cumming et al. (2018; maroon) and S. Müller et al. (2020; green). Our results show that models initialized with cold-start conditions yield the best match to Jupiter’s present-day observables.
Paper: Type Ia Supernova Growth-rate Measurement with LSST Simulations: Intrinsic Scatter Systematics
Authors: Bastien Carreres, Rebecca C. Chen, Erik R. Peterson, Dan Scolnic, Corentin Ravoux, Damiano Rosselli, Maria Acevedo, Julian E. Bautista, Dominique Fouchez, Lluís Galbany, Benjamin Racine
Figure caption: Average result over the eight mocks as a function of variations of the value of the ﹩{\tau }_{{E}_{{\rm{dust}}}}﹩ with respect to the baseline value used in SP23.
Paper: The Sonora Substellar Atmosphere Models. VI. Red Diamondback: Extending Diamondback with SPHINX for Brown Dwarf Early Evolution
Authors: C. Evan Davis, Jonathan J. Fortney, Aishwarya Iyer, Sagnick Mukherjee, Caroline V. Morley, Mark S. Marley, Michael Line, Philip S. Muirhead
Figure caption: The solar metallicity ([M/H] = +0.0) Teff–log(g)–T10 table used as a boundary condition in our thermal evolution model. The T10 values are tabulated for the Sonora Diamondback (M24) and SPHINX  (I23) atmospheres as indicated in the plot. The process used to determine the boundary condition in the “weighted transition” region, where these two atmosphere grids overlap in Teff, is described in Section 2.2. A structure model with a particular T10 and surface gravity determines its Teff by interpolating within this table.
Paper: The Sonora Substellar Atmosphere Models. VI. Red Diamondback: Extending Diamondback with SPHINX for Brown Dwarf Early Evolution
Authors: C. Evan Davis, Jonathan J. Fortney, Aishwarya Iyer, Sagnick Mukherjee, Caroline V. Morley, Mark S. Marley, Michael Line, Philip S. Muirhead
Figure caption: Evolution tracks of Teff (top panel), radius (middle panel), and surface gravity (bottom panel) of selected solar metallicity (thick solid lines), metal-rich (thin dashed lines), and metal-poor (thin dotted lines) model objects. Models are labeled by their mass in MJ. In general, the objects tend to be hotter, smaller, and of higher surface gravity as metallicity decreases, with these patterns becoming more apparent at higher masses and younger ages. Most of the modeled properties here become less sensitive to metallicity as these objects age, but objects that are close to or above the hydrogen-burning limit (M ≳ 0.06 M⊙ = 62.9 MJ) retain differences due to metallicity well after a few Gyr.
Paper: The Sonora Substellar Atmosphere Models. VI. Red Diamondback: Extending Diamondback with SPHINX for Brown Dwarf Early Evolution
Authors: C. Evan Davis, Jonathan J. Fortney, Aishwarya Iyer, Sagnick Mukherjee, Caroline V. Morley, Mark S. Marley, Michael Line, Philip S. Muirhead
Figure caption: Luminosity evolution tracks of selected models from our work (thin solid lines) compared to the M24 tracks (thick dotted–dashed lines) and the recent C23 models (thin dotted lines). Models are labeled by their mass in MJ. The bottom panel shows the logarithmic ratios of the M24 and C23 models to those of this work (i.e., a value of 0.25 means the model is ∼1.78 times as luminous as our models at that age). Our luminosity tracks are typically within 1% of the M24 luminosities at late ages (≳ 1 Gyr), but are more luminous at young ages due to higher initial entropy and the inclusion of I23 atmospheric boundary conditions. As the C23 models do not account for the L/T transition, they tend to be more luminous before and less luminous after the L/T transition than our models, except for the very lowest-mass cases, which are less luminous at all young ages and more luminous beyond several Gyr.
Paper: The Sonora Substellar Atmosphere Models. VI. Red Diamondback: Extending Diamondback with SPHINX for Brown Dwarf Early Evolution
Authors: C. Evan Davis, Jonathan J. Fortney, Aishwarya Iyer, Sagnick Mukherjee, Caroline V. Morley, Mark S. Marley, Michael Line, Philip S. Muirhead
Figure caption: The metal-rich ([M/H] = +0.5) Teff–log(g)–T10 table used as a boundary condition in our thermal evolution model. The T10 values are tabulated for the Sonora Diamondback  (M24) and SPHINX  (I23) atmospheres, as indicated in the plot. The process used to determine the boundary condition in the “weighted transition” region, where these two atmosphere grids overlap in Teff, is described in Section 2.2. A structure model with a particular T10 and surface gravity determines its Teff by interpolating within this table.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: An example of LINER-AGN. (a) The SDSS g, r, i-band image. (b) The [S II]-BPT diagram. (c) The spatially resolved [S II]-BPT diagram, which is color coded in the same way as panel (b). The regions within the yellow circle follow Σ(r) ∼ 1/r2. (d) The normalized [O III] λ5007 surface brightness as a function of radius. The gray points are the surface brightness of all the spaxels with S/N of [O III] λ5007 greater than 3, while purple squares correspond to [S II]-LINERs. The black solid line is the 1/r2 model convolved with the PSF. The blue dotted vertical line with R ∼ 4″ represents the yellow circle region in panel (c). (e) ﹩\mathrm{log}([{\rm{O}}\mathrm{III}]/[{\rm{O}}\mathrm{II}])﹩ for each spaxel as a function of radius. Purple squares represent [S II]-LINER emission. The blue dashed line is the linear fitting within the yellow region in panel (c).
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: AGN fraction as a function of ΔPA. In the left panel, blue circles represent blue and green galaxies, while red triangles represent red galaxies. In the right panel, blue circles represent the fraction of high Eddington ratio AGNs, while red triangles represent the fraction of low Eddington ratio AGNs. The demarcation line between low and high Eddington ratios is Lbol/LEdd ∼ 10−3 (L. C. Ho 2008).
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: AGN fraction as a function of ΔPA for three galaxy subsamples (align, prograde, retrograde) with similar global M* and Dn4000 distributions. In the left panel, blue circles represent blue and green galaxies, while red triangles represent red galaxies. In the right panel, blue circles represent the fraction of high Eddington ratio AGNs, while red triangles represent the fraction of low Eddington ratio AGNs. The demarcation line between low and high Eddington ratios is Lbol/LEdd ∼ 10−3.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: AGN fraction for misaligned galaxies and their control sample. The red histograms with hatched lines are for misaligned galaxies, while gray histograms are for their control samples, which are aligned galaxies with similar global M* and Dn4000. In the left panel, galaxies are divided into three stellar populations (blue, green, and red galaxies). In the right panel, AGNs are divided by the Eddington ratio at Lbol/LEdd ∼ 10−3.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: The AGN fraction as a function of ΔPA for AGN samples selected through three different aperture sizes: 1 kpc (left), 2 kpc (middle), and 4 kpc (right), with blue circles being blue and green galaxies and red triangles being red galaxies.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: Fraction of galaxies with positive Dn4000 gradient as a function of ΔPA. Blue circles represent blue and green galaxies, while red triangles represent red galaxies.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: AGN fraction as a function of ΔPA after removing galaxies with interaction/merger remnant. In the left panel, blue circles represent blue and green galaxies, while red triangles represent red galaxies. In the right panel, blue circles represent the fraction of high Eddington ratio AGNs, while red triangles represent the fraction of low Eddington ratio AGNs.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The mass of the flare-associated LASCO CMEs with halo CMEs plotted along the X-ray peak flux of associated GOES X-ray flares that occurred during Cycles 23 and 24 (a), Cycle 23 (b), and Cycle 24 (c); the kinetic energy of the corresponding CMEs along the X-ray peak flux during Cycles 23 and 24 (d), Cycle 23 (e), and Cycle 24 (f); and the linear speed of the CMEs along the X-ray peak flux during Cycles 23 and 24 (g), Cycle 23 (h), and Cycle 24 (i). The solar X-ray-flare-associated regular CMEs are plotted as gray dots, while flare-associated halo CMEs are plotted as black dots. We binned the data with respect to the associated solar X-ray flares’ peak flux to derive a log-linear correlation. Each bin, ordered from the lowest to highest flare peak flux, contains 94, 325, 744, 651, 372, and 274 samples for Cycle 23 and 24; 65, 217, 425, 429, 265, and 192 for Cycle 23; and 29, 108, 319, 222, 107, and 82 for Cycle 24. The median values of the bins are presented as blue dots. The error bars indicate the interquartile range (IQR) of the samples in the respective bins. The correlation derived from A. N. Aarnio et al. (2011), which includes LASCO CMEs from 1996 to 2006, is presented as a green solid line in (a), (b), and (c), whereas the best fit derived from the blue dots is presented as a blue solid line. The shaded region around each best-fit line represents the 1σ confidence interval of the regression model, reflecting the uncertainty in the slope and intercept estimates.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: (Left) Histogram of solar CMEs that occurred within ±2 hr of the solar X-ray flare event start time in the GOES database as a function of angular separation between the corresponding CME and a flare. The dashed lines indicate spatial constraint used to pair flares and CMEs (±45° of angular separation). (Right) Histogram of selected CMEs within the spatial constraint among the flare–CME pairs that are within ±2 hr start time differences as a function of time differences between the flare event start time and the CME detection time in minutes. The dashed lines indicate temporal constraint, showing CMEs that started 10–80 minutes after the onset of their paired X-ray flare events. We found similar distribution peaks observed in A. N. Aarnio et al. (2011), which indicates that these constraints can also be applied to our extended LASCO CME and GOES X-ray flare database.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The mass distribution of solar CMEs in the Large Angle Spectrometric Coronagraph (LASCO) CME catalog data set that occurred from 1996 to 2019. The mass values of CMEs that propagated toward or away from the line of sight of the instrument are labeled as halo CMEs in the LASCO CME database. The mass distribution of halo CMEs is presented as a dashed histogram. In total, we started with 21,945 LASCO CMEs, including 708 halo CMEs, in our analyses.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: 1 hr averaged solar spectral irradiance at 1600 Å (left) and 1 hr averaged detrended FUV flux from AIA1600 images (right). For clarity in this 10 yr time series, 1 hr averages are plotted; however, all detrending and quantitative analyses were performed using 1 minute averaged data.
Paper: Constraining the Mass Loss and the Kinetic Energy of Stellar Coronal Mass Ejections with Solar Far-ultraviolet Flares
Authors: Nuri Park, Evgenya L. Shkolnik, Joe Llama
Figure caption: The solar X-ray flare peak flux distribution of the GOES solar flare report from 1996 to 2019. We excluded flares without position values, since we require flares that are spatially and temporally coincident with CMEs.
Paper: Wakes from Companion Interactions in Type Ia Supernovae Nebular Emission Line Profiles
Authors: Kathlynn Simotas, Lars Bildsten, Logan J. Prust
Figure caption: Modeled emission line profiles for [Co III] 11.89 μm (or the innermost velocity tracer as displayed in the top of Figure 2) on the top row and [Ar III] 8.99 μm (the first shell-like tracer shown in the bottom of Figure 2). The solid black line shows the undisturbed (no-wake) ejecta modeled by the Gaussian fit of T. L. S. Wong et al. (2024). In all panels the red line is the profile along the axis of the wake, the blue line is 40∘ from the wake axis along the bow shock, and the orange line is 90∘ from the wake axis. The first column uses linear sampling j ∝ ρ. The second column uses squared sampling j ∝ ρ2  and the third column uses electron density sampling using the values of ncrit for each ion at 270 days after explosion.
Paper: Wakes from Companion Interactions in Type Ia Supernovae Nebular Emission Line Profiles
Authors: Kathlynn Simotas, Lars Bildsten, Logan J. Prust
Figure caption: Demonstrating the impact of 3 choices of innermost velocity scheme for the electron density sampled [Co III] line. The gray line shows the most extreme case where all material at ≤1500 km s−1 is replaced with a hole. The blue line shows the case where a hole is cut out only within the angular extent of the bow shock (≈40∘). The green line shows an extension of our velocities at exactly 1500 km s−1 extrapolated inward to the edge of the simulation domain.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Mass fraction of water and hydrogen dissolved in melt as a function of the total ambient pressure. Shown are temperatures representative of Earth-like melt (1600 K) and sub-Neptune core surfaces (5000 K). The dotted curves show the same solubility laws but with the fugacity coefficient set to unity (ϕi = 1). For illustration, the volume mixing ratio of water has been set to ﹩{X}_{{{\rm{H}}}_{2}{\rm{O}}}=1{0}^{-6}﹩ (for converting ﹩{P}_{{{\rm{H}}}_{2}{\rm{O}}}={X}_{{{\rm{H}}}_{2}{\rm{O}}}P﹩) and we have assumed ﹩{P}_{{{\rm{H}}}_{2}}=P﹩ for hydrogen. Sub-Neptunes have characteristic surface pressures of P ∼ 104 bar.
Paper: Wakes from Companion Interactions in Type Ia Supernovae Nebular Emission Line Profiles
Authors: Kathlynn Simotas, Lars Bildsten, Logan J. Prust
Figure caption: Composition profiles of passive scalars in velocity space at an angle of 10° relative to the explosion axis. The red line indicates the element group that was initially moving at the highest velocities, which is now highest in the innermost region moving at <4000 km s−1. All other groups remain in the order, if not the exact velocity range, of their initial distribution.
Paper: Wakes from Companion Interactions in Type Ia Supernovae Nebular Emission Line Profiles
Authors: Kathlynn Simotas, Lars Bildsten, Logan J. Prust
Figure caption: Comparison of the [Co III] 11.89 μm line shape from J. DerKacy et al. (2023), Blondin 1D nLTE radiative transfer code output (S. Blondin et al. 2023), and our three sampling methods with an input of a spherically symmetric Gaussian density profile with equivalent ejecta mass and energy values as the model in S. Blondin et al. (2023) and S. Gronow et al. (2021).
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Fugacity coefficients for H2, H2O, CO, CO2, and CH4 as functions of pressure. The shaded region is bounded by calculations for 1600 K (upper bound) and 5000 K (lower bound), corresponding to the temperatures of Earth-like melt and sub-Neptune core surfaces, respectively. The dotted curves are the lower bounds for CO and CO2, which are otherwise obscured by the shaded regions for H2 and CH4.
Paper: The Gradient of Mean Molecular Weight across the Radius Valley
Authors: Kevin Heng, James E. Owen, Meng Tian
Figure caption: Schematic describing how geochemical outgassing calculations are combined with data-driven radius-valley constraints to produce molecular abundances and the mean molecular weight.
Paper: Wakes from Companion Interactions in Type Ia Supernovae Nebular Emission Line Profiles
Authors: Kathlynn Simotas, Lars Bildsten, Logan J. Prust
Figure caption: The intensity-weighted velocity as a function of viewing angle. The blue line corresponds to the lowest velocity tracer, and the orange line corresponds to the first shell-like tracer.