adsabs/AstroCLIMB huggingface dataset:
Paper: Brown Dwarf Formation through Gravitational Collapse: Insights from 3D Numerical Simulations
Authors: Adnan Ali Ahmad, Benoît Commerçon, Gilles Chabrier, Antonin Borderies
Figure caption: A timeline of the evolution of collapse. Panel (a) displays the temperature-density evolution of the densest cell in our runs. Panels (b), (c) display the maximum density and magnetic field strength as a function of time since first core formation, respectively.
Paper: Astrometric Methods for Detecting Exomoons Orbiting Imaged Exoplanets: Prospects for Detecting Moons Orbiting a Giant Planet in α Centauri A’s Habitable Zone
Authors: Kevin Wagner, Ewan Douglas, Steve Ertel, Kyran Grattan, S. Pete Worden, Aniket Sanghi, Billy Quarles, Charles Beichman
Figure caption: Left: an illustrative example of a 30 M⊕ moon orbiting a Saturn-mass planet, with their CoM in a ∼1.8 au orbit around a 1.0 MSun star at 1.3 pc (similar to the planet candidate around α Centauri A described in K. Wagner et al. 2021; C. Beichman et al. 2025; A. Sanghi et al. 2025). Such a large moon is not representative of moons that would be likely found in nature, but it serves to better illustrate several following points via its larger gravitational effect on the planet. The blue curve shows the orbit fit for the observed dates. The dashed curve shows the orbit of the CoM of the planet and moon. Right: the same as the left, but zoomed in. The moon and planet orbits about their CoM are shown at their actual scale, rather than enlarged, as in the left panel. While the orbit fit is performed for the measured planet position (red points), note that the orbit fit (blue points) most closely matches the position of the CoM (black dotted curves)—illustrating that the moon’s effect on the planet’s position does not significantly affect the Keplerian orbit fit of the planet.
Paper: Astrometric Methods for Detecting Exomoons Orbiting Imaged Exoplanets: Prospects for Detecting Moons Orbiting a Giant Planet in α Centauri A’s Habitable Zone
Authors: Kevin Wagner, Ewan Douglas, Steve Ertel, Kyran Grattan, S. Pete Worden, Aniket Sanghi, Billy Quarles, Charles Beichman
Figure caption: Left column: χ2 difference for moon mass (Mmn) vs. moon orbital semimajor axis (amn) for observing cadence = 1 hr, with no gaps between observations and a 2 month nonobservability window per year for a 5 yr campaign. Center columns: sidereal period error and semiamplitude error for Mmoom vs. amn. Rows correspond to varying cases of astrometric precision. Right column: success (blue) defined as the exomoon candidate being recovered with χ2 difference >5, period error <5%, and amplitude error <25%. All results are averaged over 20 runs for each combination of Mmn vs. amn.
Paper: Astrometric Methods for Detecting Exomoons Orbiting Imaged Exoplanets: Prospects for Detecting Moons Orbiting a Giant Planet in α Centauri A’s Habitable Zone
Authors: Kevin Wagner, Ewan Douglas, Steve Ertel, Kyran Grattan, S. Pete Worden, Aniket Sanghi, Billy Quarles, Charles Beichman
Figure caption: Top left: separation residuals after subtracting the predicted positions of the planet based on a Keplerian orbit fit to the astrometry. The black curve shows a 10× smoothed version of the data. Top right: the same residuals, shown over a smaller range. Bottom left: phase-folded separation residuals (gray points, binned by 1 day as red points) with maximum χ2 difference between the sine fit (blue curve) and null hypothesis (dashed line). Bottom right: separation residuals with sine fit subtracted. The star–planet–moon system configuration corresponds to that in Figure 1.
Paper: Astrometric Methods for Detecting Exomoons Orbiting Imaged Exoplanets: Prospects for Detecting Moons Orbiting a Giant Planet in α Centauri A’s Habitable Zone
Authors: Kevin Wagner, Ewan Douglas, Steve Ertel, Kyran Grattan, S. Pete Worden, Aniket Sanghi, Billy Quarles, Charles Beichman
Figure caption: Results for astrometric precision = 0.1 mas, observing cadence of 1 hr, and a 5 yr observing campaign for various moon masses assuming a 0.3 MJup planet orbiting α Centauri A. Left column: first 90 days of the observing campaign, with best-fit planet orbit subtracted (red points, black curve: smoothed by a running mean of 10 points). Center column: phase-folded data for the full 5 yr campaign corresponding to the largest χ2 difference from a period grid search. Right column: χ2 difference for each of the tested periods. The dashed line represents the known sidereal period of the simulated moon.
Paper: Astrometric Methods for Detecting Exomoons Orbiting Imaged Exoplanets: Prospects for Detecting Moons Orbiting a Giant Planet in α Centauri A’s Habitable Zone
Authors: Kevin Wagner, Ewan Douglas, Steve Ertel, Kyran Grattan, S. Pete Worden, Aniket Sanghi, Billy Quarles, Charles Beichman
Figure caption: Results for astrometric precision = 0.1 mas, observing cadence of 1 day and a 5 yr observing campaign for an Earth-mass moon orbiting a 0.3 MJup planet orbiting α Centauri A. Left: first 90 days of the observing campaign, with best-fit planet orbit subtracted (red points; smoothed by 10 observations—black curve). Center: phase-folded data for the full 5 yr campaign corresponding to the largest χ2 difference from a period grid search. Right: χ2 difference for each of the tested periods. The dashed line represents the known sidereal period of the simulated moon.
Paper: 3D Simulations of Convective Entrainment in Gas Giants: Rotation and Decreasing Luminosity as Barriers to Mixing
Authors: Shu Zhang, 舒 张, J. R. Fuentes, Andrew Cumming
Figure caption: Panel (a): vertical component of the rms flow velocity, averaged over the convection zone, as a function of convection zone thickness h and imposed heat flux FT. The quantity plotted on the x-axis is f = hFT for the nonrotating case and ﹩f=h{F}_{T}^{2}﹩ for the rotating case. The dashed and solid lines represent the theoretical predictions from Equation (2) (with prefactors of 0.7 and 0.95, respectively, to obtain agreement with the measured values). Panel (b): thickness of the convection zone, h, as a function of time, t, for all our simulations. The vertical line marks t⋆ = 0.005, the time at which the cooling flux at the top boundary begins to decrease with time. The dashed lines correspond to the analytic predictions in Equations (4)–(7), with best-fit values γ = 0.58, 1.9, 0.41, 0.022 from top to bottom.
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: Observed spectrum of CT Cha b. Top left: calibrated JWST/MIRI MRS data of the CT Cha system, showcasing the stellar point-spread function dominating the image at 13.3–15.6 μm. Bottom left: a spectral cross-correlation map of the same field of view revealing the companion. A gray star marks the location of the host star. Right: continuum-subtracted spectrum of CT Cha b (black) compared to a total model (red shaded area) composed of molecular emission from C2H6, C2H2, 13CCH2, HCN, C6H6, CO2, C3H4, and C4H2, shown with models in the colors below. The four panels on top show selected wavelength regions that contain important molecular features.
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: Observed spectrum of CT Cha A. Left: CT Cha A (black line) extracted spectrum in the same spectral region in which the disk around the companion showcases emission features from carbon-bearing molecules, but where no such emission is detected in CT Cha A (regions indicated). The total best-fit model is shown in the blue shaded region with the individual molecular models from warm water (T ∼ 400 K, H2O #1), cold water (T ∼ 200 K, H2O #2), and OH shown below. Right: at longer wavelengths, bright lines from cold water dominate the spectrum.
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: Molecular SCC maps of the CT Cha system. For all of the molecules besides H2O (bottom right), the SCC provides a signal at the location of CT Cha b, while no signal is present from CT Cha A, which is located in the lower-left corner and indicated by the gray star. Conversely, the H2O SCC is dominated by residual stellar features, and the shape of the stellar point-spread function from the original cube can still be recognized (white dashed line in the H2O panel).
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: χ2 maps for the molecules detected in the spectrum of CT Cha b. The model corresponding to the best fit is represented by the black plus. The 1σ, 2σ, and 3σ contours are shown in yellow, orange, and red, respectively. Equivalent emitting radii are shown in the labeled white contours with the radii in astronomical units. The explored parameter space goes up to temperatures of 1500 K, but we show a zoomed-in temperature range for clarity.
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: Extraction process of the CT Cha b spectrum. Left: 2D SCC map (top) showing the signal of CT Cha b (black) and the neighboring apertures (blue) used to sample the instrumental and stellar noise from the calibrated data (bottom). Right: the spectrum extracted at the location of the companion is shown in black, while the projection of the principal-component analysis (PCA) basis obtained from the noise apertures is shown in blue. This spectrum encapsulates various noise sources, like the signal from the stellar point-spread function, the background, and instrumental and detector effects.
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: Postprocessing of the spectrum of CT Cha A. Top row: original extracted 1D spectrum from the star (black, left panel) and the corresponding modes (right panel). The modes highlighted in orange have been used to reconstruct the low-frequency modulation of the spectrum, shown in orange in the left panel. Middle row: same as the top panels, but for the modes with the highest amplitudes. Bottom row: final continuum-subtracted spectrum of CT Cha A in channel 4B. Vertical lines at the top of the panel indicate the location of expected H2O (blue) and OH (pink) emission lines. Our method is able to retain most of the expected emission lines in this range, distinguishing them from the systematic noise initially present.
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: The C2H2 to H2O flux ratio as a function of host luminosity. The MINDS sample is shown in gray (S. L. Grant et al. 2025). CT Cha b is shown in red and CT Cha A in blue. Upward arrows are 3σ lower limits (H2O not detected) and downward arrows are 3σ upper limits (C2H2 not detected).
Paper: A Carbon-rich Disk Surrounding a Planetary-mass Companion
Authors: Gabriele Cugno, Sierra L. Grant
Figure caption: Same as Figure 7, but for the molecules identified in the CT Cha A spectrum.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: HAT-P-18 b extracted light curves. The top panel shows the 10 Å bin light curve centered around the He triplet in red, together with the white light curve in blue. The bottom panel shows the binned residuals, illustrating both the larger depth and asymmetry present in the helium light curve.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Schematic representation of the parameterization proposed in this study for an envelope of escaping gas around a planet (gray circle) moving in the direction of the blue arrow. The red semiellipse represents the trailing tail of length l1, while the blue semiellipse represents the leading tail of length l2. The two semiellipses share a common semimajor axis h, which describes the height of the envelope. The black dashed–dotted line shows the 12 harmonic representation of the envelope.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Main results from the injection-recovery test for the uniform-envelope 2000 ppm case. The injected data are shown in red, and the recovered results are shown in blue. The top left panel shows the simulated light curve, together with the fitted model in blue. The top right panel shows the posteriors of the four fitted parameters, with the injected values shown in red. The bottom panel shows the shape of the injected envelope in red, together with the median retrieved envelope in blue. The blue shaded region shows the 1σ uncertainty region, while the gray line represents the star, and the purple circle illustrates the planet.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Results from the injection-recovery test for the helium envelope with a variable opacity. The top panel shows the inputted absorbance profiles (red curves), together with the empirically retrieved absorbance profiles (light and dark blue points with error bars) for the two-layer envelope 200 ppm case. The bottom panel shows the injected variable envelope in different shadings of red, with the dashed lines indicating the position and shape of the fitted layers.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Main results of HAT-P-18 b uniform helium envelope fit. The top left panel shows the NIRISS/SOSS light curve in red, corresponding to the 10 Å bin centered around the He triplet, together with the fitted model light curve in blue. The top right panel shows the posteriors of the four fitted parameters (l1, l2, h, α). The bottom panel shows the median retrieved envelope in blue, with the shaded region showing the 1σ uncertainty region. The gray line represents the star, and the purple circle illustrates the planet.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Example of the degeneracy between the envelope height h and the opacity α. The red shaded region illustrates a smaller, more opaque envelope, while the blue shaded region represents a larger, more transparent envelope. The right panel shows the corresponding light curves, with the difference plotted in the lower panel.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Main results of the injection-recovery test for the two-layer, 200 ppm precision case. The top panel shows the injected light curve in red together with the fitted model light curve in blue, while the bottom panel shows the posterior distribution of the fitted parameters.
Paper: Modeling Tails of Escaping Gas in Exoplanet Atmospheres with Harmonica
Authors: Carlos Gascón, Mercedes López-Morales, Shreyas Vissapragada, Morgan MacLeod, Hannah R. Wakeford, David Grant, Ignasi Ribas, Guillem Anglada-Escudé
Figure caption: Transit light curves corresponding to different envelope morphologies. The left panel shows several envelopes with a prominent increasing leading tail. The height h and trailing tail l1 are kept constant. The right panel, on the other hand, shows envelopes with a constant prominent trailing tail but an increasing height and leading tail. In all cases, the opacity is left constant.
Paper: A Black Hole Is Born: 3D General-relativistic Magnetohydrodynamic Simulation of Black Hole Formation from Core Collapse
Authors: Goni Halevi, Swapnil Shankar, Philipp Mösta, Roland Haas, Erik Schnetter
Figure caption: Snapshots of the specific entropy s, in units of kB baryon−1, shown as 2D slices through our 3D GRaM-X simulation at various times (from left to right: 50, 100, 200, 300, and 325 ms postbounce). The entropy generally increases from low values (blue) to higher ones (red) as time progresses. The contraction of the core region and the early shock expansion, followed by a later stalling, are also visible. The shock propagation and convective motions exhibit inherent asymmetries. A movie of the simulation is available at this link: https://www.youtube.com/shorts/4sisdNGLUL0.
Paper: A Black Hole Is Born: 3D General-relativistic Magnetohydrodynamic Simulation of Black Hole Formation from Core Collapse
Authors: Goni Halevi, Swapnil Shankar, Philipp Mösta, Roland Haas, Erik Schnetter
Figure caption: Postbounce evolution of the central density (top panel), shock radius (middle panel), and PNS mass (bottom panel) for both our GR1D simulation (dashed lines) and our 3D GRaM-X simulation (solid lines). The 3D evolution of the central density and PNS mass are both closely approximated by the 1.5D evolution. The time of BH formation, where the central density exponentially rises, is also nearly identical between the two simulations. However, the shock radius differs dramatically between the 3D and 1.5D evolution at times after it has reached its maximum value.
Paper: A Black Hole Is Born: 3D General-relativistic Magnetohydrodynamic Simulation of Black Hole Formation from Core Collapse
Authors: Goni Halevi, Swapnil Shankar, Philipp Mösta, Roland Haas, Erik Schnetter
Figure caption: Spatial trajectory of the BH as measured by the centroid of the apparent horizon over time. Circle markers in the 3D projection represent the horizon at each time after BH formation, with color indicating time after BH formation tBH in microseconds, and size representing the proper area A of the horizon. The horizon expands at a decreasing rate while the black hole moves along a complex trajectory. 2D projections of this trajectory on each plane are drawn with square markers and connected with dashed gray lines.
Paper: A Black Hole Is Born: 3D General-relativistic Magnetohydrodynamic Simulation of Black Hole Formation from Core Collapse
Authors: Goni Halevi, Swapnil Shankar, Philipp Mösta, Roland Haas, Erik Schnetter
Figure caption: The evolution of mass accretion rate, measured in solar masses per second, after core bounce. For the 3D GRaM-X simulation, we show the accretion rate measured through 3 different radii: 50 km (coral), 70 km (turquoise), and 90 km (pink). At early times, the accretion rate is higher through smaller radii, but at late times, the rate converges at a few solar masses per second. We also include the accretion rate measured at 50 km from our GR1D simulation (gray) for comparison; it shows a similar trend to the 3D results but ends with overall lower accretion.
Paper: A Black Hole Is Born: 3D General-relativistic Magnetohydrodynamic Simulation of Black Hole Formation from Core Collapse
Authors: Goni Halevi, Swapnil Shankar, Philipp Mösta, Roland Haas, Erik Schnetter
Figure caption: Volume rendering of specific entropy s, in units of kB baryon−1, at 300 ms after core bounce (corresponding to the fourth panel of Figure 1).
Paper: Ion-scale Turbulence and Energy Cascade Rate in the Solar Corona and Inner Heliosphere
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Alexander Pitňa
Figure caption: Left: KAW-normalized PSDs of magnetic field (red), velocity (blue), and ion density (black) fluctuations (computed using K2 = βi(1 + βi)), for an event observed by both Spektr-R and Wind on 2012 April 27 at approximately 21:00 UT. The gray dotted lines show the analytic approximations to the spectrum, with a k−5/3 power-law form in the inertial range, and a steeper k−8/3 form in the dissipative range. The dashed and solid vertical gray lines show the approximate spacecraft-frame frequencies ﹩{f}_{{d}_{i}}﹩ and ﹩{f}_{{\rho }_{i}}﹩, respectively (see Table 1). Right: model wavenumber spectra of the magnetic field (red) and ion density (black) fluctuations. The spectrum of magnetic fluctuations breaks from the ﹩{k}_{\perp }^{-5/3}﹩ Kolmogorov form of the inertial range to the steeper ﹩{k}_{\perp }^{-\delta }﹩ form (with δ ≃ 8/3) in the dissipative range, at a wavenumber ﹩{d}_{r}^{-1}﹩. The density fluctuations exhibit a similar break, but at a higher wavenumber corresponding to the thermal proton gyroradius ρi.
Paper: Ion-scale Turbulence and Energy Cascade Rate in the Solar Corona and Inner Heliosphere
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Alexander Pitňa
Figure caption: Left: magnetic fluctuations ﹩{P}_{B}({f}_{{d}_{r}})\,{f}_{{d}_{r}}﹩ at the break and the predicted magnitude from radio-inferred density fluctuations. The solid and dashed lines show the expected values from kinetic Alfvén waves, for the slow and fast solar wind parameters given in the Appendix, and the plus and diamond symbols are based on measurements by PSP (D. Duan et al. 2021; J. Šafránková et al. 2023). The bands represent a scaling factor from 0.5 to 2 that accounts for the spread in measurements (E. P. Kontar et al. 2023). Additional data are from R. J. Leamon et al. (1998), R. Bruno & L. Trenchi (2014), as indicated. Right: density fluctuations ﹩{P}_{n}({f}_{{\rho }_{i}})\,{f}_{{\rho }_{i}}﹩ at the break, using Equation (6) with data at 1 au from L. M. Celnikier et al. (1987), P. J. Kellogg & T. S. Horbury (2005), and C. H. K. Chen et al. (2014b), as shown in Figure 10 of E. P. Kontar et al. (2023).
Paper: Ion-scale Turbulence and Energy Cascade Rate in the Solar Corona and Inner Heliosphere
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Alexander Pitňa
Figure caption: Energy cascade rate (Equation (8)) using two models of the corona: an equatorial active region with slow solar wind (solid lines), and a coronal hole with fast solar wind (dashed lines). The bands represent a scaling factor ranging between 0.5 and 2. The overplotted data are from in situ measurements by R. J. Leamon et al. (1999), R. Bandyopadhyay et al. (2020), D. Telloni et al. (2023), F. S. Mozer et al. (2023), and T. A. Bowen et al. (2024).
Paper: Ion-scale Turbulence and Energy Cascade Rate in the Solar Corona and Inner Heliosphere
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Alexander Pitňa
Figure caption: Radial variation of various plasma parameters, as observed by the Parker Solar Probe covering the time between between 2018 October 31 and 2023 July 31. From top to bottom: magnetic field strength B (G), ambient ion density n (cm−3), ion temperature Ti (K), and the ion plasma beta: βi = 8π n kB Ti/B2. In each plot power-law fits (red) to the median observed values (black histograms) are shown. The solid and dashed lines show the analytic models provided in the Appendix, for the slow and fast solar wind, respectively.