adsabs/AstroCLIMB huggingface dataset:
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: Radial [El/H] gradients of OCs at different vertical distances from the Galactic plane. The filled circles in blue and red represent OCs within different distance bins from the Galactic plane. The colored lines correspond to the linear fits for the clusters within these respective bins.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: Time evolution of radial [El/H] gradients for the OCs. The purple, green, and red filled circles represent OCs in three distinct age bins.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: Radial [El/H] gradients of OCs above (the red circles) and below (the blue circles) the Galactic plane. The red and blue lines indicate the corresponding linear fits for these two sets of clusters.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Phase curves of GJ 1214 b, integrated from 5 to 12 μm. The dashed gray line and surrounding shaded region show a fit (with an imposed positive flux requirement) to the observed data from E. Kempton et al. (2023) and the corresponding 3σ uncertainty. The black dotted line and surrounding shaded region show a reanalysis of the same data, with the methodology presented in the Appendix of this work. In the top-left panel, dashed lines show clear and hazy SPARC/MITgcm models from E. Kempton et al. (2023). In all other panels, sets of RM-GCM models were chosen to show trends with metallicity, cloud coverage, and hazes. In agreement with the original analysis, we find that the presence of atmospheric aerosols (and likely clouds and hazes together) is required to explain the large observed phase-curve amplitude and lower overall planetary flux, but no model is currently able to match the data.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Pressure–temperature profiles for models of GJ 1214 b with varying metallicity and aerosol distributions. From left to right, columns correspond to extended cloud models with no hazes, soot haze models with no clouds, and models with both extended clouds and soot hazes. The top row shows models at 1× solar metallicity, and the bottom row shows models at 100× solar metallicity. Equatorial profiles are represented by colored lines, where the longitude is denoted by the color (zero corresponds to the substellar point). Pressure–temperature profiles for all nonequatorial profiles are represented by gray lines. The condensation curves for the KCl clouds are shown as additional dashed blue lines. Atmospheric aerosols, particularly hazes, drive large day–night temperature differences.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Emission spectra from the dayside (left) and nightside (right) of GJ 1214 b. The gray diamonds show the observed spectra from E. Kempton et al. (2023). The black squares show the reanalysis. The black dashed lines show a 553 K blackbody (right) and a 437 K blackbody (left), the best-fit values from E. Kempton et al. (2023). We use the same PHOENIX (T. O. Husser et al. 2013) stellar model as in E. Kempton et al. (2023) to convert the SPARC/MITgcm models to planetary flux. Simulated spectra are also shown for 1× solar metallicity (top row), 30× (middle row), and 100× (bottom row). The dotted lines show SPARC/MITgcm models, while the solid lines show RM-GCM models for varying aerosol parameterizations (convolved down to R = 100). An atmosphere with a combination of clouds, hazes, and a higher-metallicity atmosphere best fits the day- and nightside emission spectra.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Vertical aerosol profiles of GJ 1214 b simulated with extended clouds and soot hazes at 100× solar metallicity. Cloud and haze radiative properties are shown at 0.5 μm (top row) and at 5.00 μm (bottom row), corresponding to the starlight and thermal channels of the double-gray radiative transfer. The red lines show the substellar profile, and the black lines show the antistellar profile. (For the hazes the substellar and antistellar profiles are identical.) Across all panels, the vertical lavender and turquoise lines mark the pressure level where the thermal and starlight photospheres would be, respectively, if no aerosols were present. The profiles reveal that hazes dominate the thermal channel at pressures less than approximately 10−1 bar, but that both hazes and clouds are optically thick at the optical photosphere.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: White-light (5–10.5 μm) phase curves of GJ 1214 b, with (blue) and without (green) fitting for a step function at 1.0278 days (gray dashed line). In the top panel, the blue and green curves look nearly identical because the phase curve and systematic models are able to compensate for the lack of a step function. The bottom panel highlights the significant difference between best-fit phase-curve models. The increase in nightside flux alters the planet’s energy budget by decreasing its inferred Bond albedo. The blue light curve more closely matches the phase-curve models shown in Figure 7.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Bond albedos (the energy reflected by the planet divided by the total energy incident across all wavelengths) of GJ 1214 b models with aerosols for metallicities of 1×, 30×, and 100× solar. All models have an additional imposed top-of-the-atmosphere Bond albedo of 0.10, following I. Malsky et al. (2024). KCl clouds or extra-reflective soot haze models result in Bond albedos above 0.3.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Temperature maps and wind structure (white arrows) of different GJ 1214 b models around a pressure of 1 mbar. The panels show 1× solar metallicity (top row) and 100× solar metallicity (bottom row). From left to right, the columns show extended cloud models, models with soot hazes, and models with both extended clouds and soot hazes. Hazes absorb more starlight by this pressure level, resulting in larger day–night temperature differences.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Revised nightside emission spectrum of GJ 1214 b. All three reanalyses (blue, orange, and purple) generally yield consistent results; however, the two Eureka! spectra are slightly higher than the SPARTA spectrum. At longer wavelengths, the differences between the original nightside spectrum by E. Kempton et al. (2023) and the reanalyses becomes increasingly apparent. The measured nightside emission from the blue and orange spectra more closely match the models shown in Figure 8.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Measured step size (i.e., flux offset) vs. wavelength for three different reanalyses. All three reanalyses detect a jump in flux to high confidence at longer wavelengths; however, they disagree on the magnitude of the step size at >11 μm where the measured flux and resulting phase-curve fits are least reliable.
Paper: The Infrared-bright SW Knots in the Complex Ejecta of VY CMa
Authors: Roberta M. Humphreys, Terry J. Jones, Kris Davidson, A. M. S. Richards, R. Ravi, A. P. Singh, L. M. Ziurys
Figure caption: Left panel: gray scale of the 249 GHz continuum emission.The large feature in the upper left includes the star and the ALMA clumps. Middle panel: the 249 GHz continuum emission contours in red plotted overlaying a gray-scale image of the 3.6 μm emission. The contours are linear, but arbitrarily chosen to emphasize the comparison between mm-wave dust emission and the NIR scattered emission. Right panel: the 249 GHz continuum emission contours plotted overlaying a gray-scale image of the CO line emission integrated over 16–23 km s−1. Each frame is 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 wide, east to west. The small red dot or green cross marks the position of the star.
Paper: The Infrared-bright SW Knots in the Complex Ejecta of VY CMa
Authors: Roberta M. Humphreys, Terry J. Jones, Kris Davidson, A. M. S. Richards, R. Ravi, A. P. Singh, L. M. Ziurys
Figure caption: Images of the SW knots from the 12CO image cube with the cross identifications with the knots in the HST image, Figure 1. (a) Knot S-D at VLSR 38 km s−1. (b) SW-A at VLSR 25 km s−1. (c) Knots S-E1, S-E2 and the S-arc in the arc that marks the east edge of the SW knots, at VLSR 20 km s−1. (d) SW-B at VLSR 10 km s−1 also showing S-arc at this velocity. ALMA clump D is visible close to the star in images (a) and (b), clump C in image (c), and clump A in (c) and (d) to the north of the star. The + marks the position of the star in all the frames.
Paper: The Infrared-bright SW Knots in the Complex Ejecta of VY CMa
Authors: Roberta M. Humphreys, Terry J. Jones, Kris Davidson, A. M. S. Richards, R. Ravi, A. P. Singh, L. M. Ziurys
Figure caption: The 12CO contours in red on the F656N 1999 image from HST at two LSR velocities showing the offset in 22.8 yr for knots S-D and SW-A on the left and the S-E and S-arc on the right. The contours are linear with the 26.8 km s−1 blue contour corresponding to 0.09 Jy Beam–1 and a spacing of 0.035 Jy Beam–1; and the 21.5 km s−1 blue contour corresponding to 0.1 Jy Beam–1 with a spacing of 0.02 Jy Beam–1. The star’s LSR velocity is 22 km s−1. The small red spot in the black box marks the position of the star.
Paper: The Infrared-bright SW Knots in the Complex Ejecta of VY CMa
Authors: Roberta M. Humphreys, Terry J. Jones, Kris Davidson, A. M. S. Richards, R. Ravi, A. P. Singh, L. M. Ziurys
Figure caption: CO emission contours at three different velocities are plotted overlaying a gray-scale image of the 3.6 μm emission. The CO emission was averaged over a 4 km s−1 bandpass for each plotted velocity. The contours are linear, but arbitrarily chosen to emphasize the comparison between CO molecular emission and the scattered light seen at NIR wavelengths. The dashed white circle is the saturation level in the 3.6 μm. Each frame is 3″ wide, east to west.
Paper: The Infrared-bright SW Knots in the Complex Ejecta of VY CMa
Authors: Roberta M. Humphreys, Terry J. Jones, Kris Davidson, A. M. S. Richards, R. Ravi, A. P. Singh, L. M. Ziurys
Figure caption: The continuum-subtracted 12CO line profiles. The short vertical line marks the velocity of the star at 22 km s−1.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Top panels and bottom-left panel: The same as in Figure 6, but now the long-term unstable Hilda asteroids are highlighted by the red symbol. These objects were eliminated from the population in a numerical simulation spanning 4 Gyr and accounting for gravitational perturbations from all planets. The currently observed population of 6094 Hilda asteroids represented the initial data of the simulations. The eliminated Hildas were located near the border of the stability zone (see, in particular, the bottom-left panel and compare with a similar results in Figure 6 of M. Brož & D. Vokrouhlický 2008). An excessive fraction of the Schubart family members at high-eccentricity orbits would be eliminated, confirming its age younger than 4 Gyr (see M. Brož & D. Vokrouhlický 2008). Bottom-right panel: (ap, ep) projection of the known Hilda population as in the bottom-left panel, but now the color-coded asteroids are those, which were eliminated in the simulation lasting 4 Gyr, which included the effect of the thermal accelerations. In this case, all bodies were given  ≃4 km size and maximum estimated value of the thermal accelerations: (i) red symbols had positive along track acceleration, and (ii) blue symbols had negative along track acceleration. The usual secular drift in semimajor axis transfers to a drift in eccentricity due to the resonance lock (e.g., M. Brož & D. Vokrouhlický 2008); the sense of the drift is indicated by the arrows.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Left panel: statistical distribution of the eccentricity factor κ (Equation (B12), red) and the inclination factor ﹩{\kappa }^{{\prime} }﹩ (Equation (B13), blue) numerically determined for 6094 orbits of the observed Hilda population. Their median values  ≃1.47 are close to each other and highlighted by the gray vertical line. Right panel: correlation of the eccentricity factor κ (ordinate) and the proper eccentricity parameter ep (abscissa) numerically determined from the sample of 6094 observed Hildas.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Resonant variables Φ vs. ϕ for (1911) Schubart. The gray contours are isolines of constant Hamiltonian ﹩\overline{{ \mathcal H }}=C﹩ for different values of C. Critical curves are highlighted in red: (i) the stable stationary center of the resonance at ϕ = 0 corresponds to a maximum value of C ≃ −1.965258, and (ii) the separatrix of the resonant regime connects the unstable stationary centers at ϕ = ±180∘ and has C ≃ −1.966212. The black curve is a result of a numerical integration of the real orbit of (1911) Schubart with perturbations from all planets taken into account (the green dot specifies the initial conditions of the simulation). The simulation span 5 kyr time interval. In order to eliminate a slight blur by short-period perturbations, terms with periods smaller than 20 yr have been digitally filtered out (equivalent to averaging the Hamiltonian over λ1). Remaining behavior is a simple libration about the stationary point (red dot) with a period of Pϕ = 262.5 yr. The grid in ap, schematically shown by the dashed lines, corresponds to the bins used in our populations analysis (see Table 1).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Projected distributions of the proper orbital parameters ap (left), ep (middle), and ﹩\sin {I}_{{\rm{p}}}﹩ (right) of the biased Hilda population from our model (red lines) and the G96 observations (black histogram) using the phase I (bottom panels) and phase II (top panels) data. The shaded gray area delimits the σ region of the solution (created by 10,000 posterior random samples of the model). The blue histogram is the best-fitting model of the background population. The residual mismatch is most likely expression of two effects: (i) a slight inaccuracy (or simplicity) in the template masks of the families accounted for and absence of smaller clusters, and (ii) possible correlations of the orbital distribution in the orbital elements.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The posterior distribution of 15 model parameters (p1, …, p15) characterizing the background population of Hildas from our nominal fit to G96 observations (also called the “corner diagram”). The individual plots are labeled (1)–(15) following the model parameter sequence given in Table 2; the first nine parameters determine the orbital distribution in proper parameters, and the last six parameters determine the absolute magnitude cumulative distribution (with the tenth parameter being the normalization at 16 mag, and the last five parameters being the mean slope values in the chosen segments). The near-to-circular distribution of the parameter solution indicates uncorrelated parameters. In some cases though, correlations exist and are shown by quasi-linear parameter dependence (e.g., p1 vs. p2, p1 vs. p3, etc.). These are well understood from the functional form of the distribution functions Di(pi) given in Equation (4).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Projected distributions of the proper orbital longitude of perihelion ϖp of the biased Hilda population from our model (red line) and the G96 observations (black histogram) using the phase I (bottom panel) and phase II (top panel) data. We used here data for faint objects, the H value in between 15.5 and 17. The shaded gray area delimits the σ region of the solution (created by 10,000 posterior random samples of the model). The quality of the phase II (both in time span and sky coverage) results in a rather good match between the observations and the model. Except for a mismatch in the ϖp range 120∘−180∘, the model performs acceptably well even in the phase I (bottom panel).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Bias-corrected cumulative magnitude distribution of the Hilda population based on G96 observations. The background population, shown by the upper curve, is separated from the major families (see Table 3): Hilda (label 1), Schubart (label 2), and Potomac (label 3). The red lines are the CSS observations (solid lines are the data in phase II, dashed lines are the data in phase I), and the black line is the bias-corrected model with σ interval (gray zone). The blue line is the whole background population from the MPC catalog. The vertical dashed lines show the magnitude segments used for the representation of the background population (Table 2).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Depletion of the observed Hilda population with time (6094 initial bodies identified in Section 2 initially, horizontal dashed line). Solid lines show results from three simulations: (i) only gravitational perturbations from planets (black line), (ii) thermal accelerations as if all bodies had H ≃ 16 and an estimated maximum outward drift (red line), and (iii) thermal accelerations as if all bodies had H ≃ 16 and an estimated maximum inward drift (blue line). The runs with the thermal accelerations thus correspond to bodies with sizes modestly smaller than 4 km for pV ≃ 0.055 (e.g., T. Grav et al. 2012) and assume the objects have bulk densities of 1.5 g cm−3.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The local slope of the cumulative absolute magnitude distribution for the bias-corrected background population of Hildas. The gray zone is the σ interval of the solution. The horizontal dashed line at 0.34 slope is the value found by I. Wong & M. E. Brown (2017) using the simple power-law fit.
Paper: Revised Masses for Low-density Planets Orbiting the Disordered M-dwarf System TOI-1266
Authors: Dakotah Tyler, Erik A. Petigura, James Rogers, Jack Lubin, Andreas Seifhart, Jacob L. Bean, Madison Brady, Rafael Luque
Figure caption: Mass–radius context figure showing the iso-composition curves and current known exoplanets up to 4 R⊕. TOI-1266 b and c and shown with gold and blue squares, respectively. The gray points represent data from the NASA Exoplanet Science Institute (2020) as of 2024 November 21 filtered to only include planets that have published mass and radius uncertainties <30%. The red data points represent such planets that orbit low-mass stars (M* < 0.6M⊙). The solid lines represent various iso-composition curves. The gold and blue 1%–4% H/He curves represent the predicted mass–radius curves for planets with various envelope mass fractions of exclusively H/He for planets at Teq,b = 425 K and Teq,c = 354 K, respectively. The iso-composition curves for the solid structure models are from L. Zeng & D. Sasselov (2013), the water mass fraction curves are from A. Aguichine et al. (2021), and the envelope mass fraction curves were determined by interpolating in between precomputed grids from thermal evolution models from E. D. Lopez & J. J. Fortney (2014) that assume solar metallicity, H/He envelopes and “Earth-like” cores, hot start thermal evolution and no atmospheric escape.
Paper: Revised Masses for Low-density Planets Orbiting the Disordered M-dwarf System TOI-1266
Authors: Dakotah Tyler, Erik A. Petigura, James Rogers, Jack Lubin, Andreas Seifhart, Jacob L. Bean, Madison Brady, Rafael Luque
Figure caption: Context plot showing the sample of exoplanets from the NEA in Figure 4. Planets orbiting stars less than 0.6 M⊙ are indicated in red. Along the x-axis we show insolation and on the y-axis we show the planet radius compared to the predicted radius for a rocky planet of the same mass.
Paper: Revised Masses for Low-density Planets Orbiting the Disordered M-dwarf System TOI-1266
Authors: Dakotah Tyler, Erik A. Petigura, James Rogers, Jack Lubin, Andreas Seifhart, Jacob L. Bean, Madison Brady, Rafael Luque
Figure caption: Top panel: the RVs phase-folded at the period of TOI-1266 b, after subtracting the RV components from the other planet based on our best-fit model. The gray points represent the MAROON-X and HARPS-N measurements. The model RV curve is plotted in blue. The phase-folded weighted mean RVs and their uncertainties are shown in red. Bottom panel: same as top panel, but for TOI-1266 c.