adsabs/AstroCLIMB huggingface dataset:
Paper: Assembling GW231123 in Star Clusters through the Combination of Stellar Binary Evolution and Hierarchical Mergers
Authors: Lavinia Paiella, Cristiano Ugolini, Mario Spera, Marica Branchesi, Manuel Arca Sedda
Figure caption: Masses and effective spin distributions for YCs, GCs, and NCs in our fiducial simulation. The metallicity is set to Z = 0.002. The contour lines refer to the 68%, 95%, 99% (solid line) and 99.99% (dotted–dashed line) contours. The 1D distributions are normalized to 1 and displayed in log scale.
Paper: Assembling GW231123 in Star Clusters through the Combination of Stellar Binary Evolution and Hierarchical Mergers
Authors: Lavinia Paiella, Cristiano Ugolini, Mario Spera, Marica Branchesi, Manuel Arca Sedda
Figure caption: BBH populations for different metallicities (Z = 0.02 in the left column, Z = 0.002 in the central column, and Z = 0.0002 in the right column) and cluster environments, namely YCs (upper row), GCs (central row), and NCs (bottom row). The bins are normalized over the number of BBHs, with brighter (darker) colors corresponding to more (less) BBHs. The GW231123 primary and secondary masses are indicated with a red cross. The fraction of BBHs falling within the event mass ranges is indicated for each metallicity–environment combination in the plots.
Paper: Assembling GW231123 in Star Clusters through the Combination of Stellar Binary Evolution and Hierarchical Mergers
Authors: Lavinia Paiella, Cristiano Ugolini, Mario Spera, Marica Branchesi, Manuel Arca Sedda
Figure caption: Delay times of mergers in the GW231123 mass CI for different cluster environments in our simulations. The filled histograms refer to Z = 0.002 runs, while the empty histograms refer to Z = 0.0002 runs. In the latter case, the solid lines refer to primary BHs undergoing a single merger event (“Stellar”), while the dashed lines refer to BHs that also underwent previous mergers (“Hierarchical”).
Paper: Assembling GW231123 in Star Clusters through the Combination of Stellar Binary Evolution and Hierarchical Mergers
Authors: Lavinia Paiella, Cristiano Ugolini, Mario Spera, Marica Branchesi, Manuel Arca Sedda
Figure caption: Masses and effective spin distributions for stellar BBHs in YCs in our fiducial simulation. The metallicity is set to Z = 0.002. The contour lines refer to the 68%, 95%, 99% (solid line), and 99.99% (dotted–dashed line) contours. The 1D distributions are normalized to 1 and displayed in log scale.
Paper: Assembling GW231123 in Star Clusters through the Combination of Stellar Binary Evolution and Hierarchical Mergers
Authors: Lavinia Paiella, Cristiano Ugolini, Mario Spera, Marica Branchesi, Manuel Arca Sedda
Figure caption: Mass spectrum of BHs produced in primordial stellar binaries for Z = 0.002 and Z = 0.0002. The black line denotes the primary mass of GW231123 while the gray band indicates the 90% C.I.. The dashed lines show the maximum mass that a BH can attain as a product of single stellar evolution.
Paper: The ODYSSEUS Survey. Spatial Correlation of Magnetospheric Inclinations Points to Parsec-scale Star–Cloud Connection
Authors: Caeley V. Pittman, Catherine C. Espaillat, Thanawuth Thanathibodee, Nuria Calvet, Lee W. Hartmann, Sylvie Cabrit
Figure caption: Comparison between imag and idisk,gas. The dashed line indicates equality, and the shaded region marks ±20°. Red outlines indicate transition disks, and blue outlines indicate measurements from AGE-PRO (L. Trapman et al. 2025; M. Vioque et al. 2025; K. Zhang et al. 2025).
Paper: Colors of Life in the Clouds: Biopigments of Atmospheric Microorganisms as a New Signature to Detect Life on Planets like Earth
Authors: Lígia F. Coelho, Lisa Kaltenegger, William Philpot, Adam J. Ellington, Noelle Bryan, Stephen Zinder, Brent C. Christner
Figure caption: Modeled reflectance spectra of different Earth-like planets: ocean worlds (left column), snowball planets (right column), both with clouds covered by strain L9-9A-1 (see Table 1 and Figure 1), resampled for an HWO resolution of R = 140. Purple lines represent planets with aerial biota in clouds. Top row: 100% clouds with 100% covered by aerial biota. Middle row: 100% clouds with 50% covered by aerial biota. Bottom row: 50% clouds with 50% covered by aerial biota. Dashed gray lines show “lifeless cloudy planet,” solid blue shows “lifeless ocean planet,” and solid pink shows “lifeless snowball planet” scenarios. Atmospheric features are labeled O2 at 690, 760, and 1260 nm, and H2O at 1490 and 1900 nm. Individual spectra of albedos are shown in Figure B1.
Paper: Colors of Life in the Clouds: Biopigments of Atmospheric Microorganisms as a New Signature to Detect Life on Planets like Earth
Authors: Lígia F. Coelho, Lisa Kaltenegger, William Philpot, Adam J. Ellington, Noelle Bryan, Stephen Zinder, Brent C. Christner
Figure caption: Individual spectra of surface albedos used in Figure 2.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: (a) Probability density functions of the normalized magnetic field-line curvature, κlc, from simulations with different δB0/B0. Power-law slopes κ+1 and κ−2.5 are shown for reference. (b) Probability density functions of the normalized magnetic field-line contraction, (vE · κ)lc/c, for the same set of simulations, with symmetric Pareto distribution fits plotted as dashed lines.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Probability density functions of field increments at different spatial separations, from the outer scale r = 42di down to the ion inertial scale r = di, including intermediate scales. Results are from the reference simulation (δB0/B0 = 1) at t = 2 lc/c. The increments Δf(r) are (a) ΔBx(r) and (b) ΔEx(r), each normalized by their standard deviation at the corresponding r. At small separations, the pdfs show pronounced non-Gaussian heavy tails, while at large r they approach a Gaussian distribution (dashed curve).
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Two-dimensional slices in the x–y plane at fixed z from the reference simulation (δB0/B0 = 1) at t = 2 lc/c, showing the normalized magnetic field strength B/Brms and the normalized magnetic field-line curvature magnitude κ/κrms. The bottom panel shows the joint distribution of B/Brms and κ (measured in units of the inverse coherence length, ﹩{l}_{c}^{-1}﹩), showing that regions of strong curvature tend to coincide with weaker magnetic fields. A power-law slope of −1/2 is provided for reference.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Probability density functions of ΔW⊥ and ΔWtot, normalized to the particle energy γ0mic2, accumulated over Δt = 0.5 lc/c  starting at t0 = 2 lc/c (γ0 is the particle Lorentz factor at t0) in the reference simulation. Different colors correspond to three distinct ranges of γ0.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Perpendicular and parallel spectra of (a) magnetic and (b) electric fluctuations, from the simulation with δB0/B0 = 1 at t = 2 lc/c. Power-law slopes of ﹩{k}_{\perp }^{-5/3}﹩ and ﹩{k}_{\parallel }^{-2}﹩ are shown for reference. Here, perpendicular (⊥) and parallel (∥) are measured with respect to B0.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Time evolution of the proton energy spectrum ﹩dN/d\mathrm{ln}(\gamma -1)﹩ for the reference simulation (δB0/B0 = 1). Over time, the particle spectrum develops a high-energy power-law tail with index p = ﹩-d\mathrm{log}N/d\mathrm{log}(\gamma -1)\simeq 2.7﹩.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Second-order structure function of magnetic fluctuations (a) and anisotropy of magnetic and electric fluctuations (b), from the simulation with δB0/B0 = 1 at t = 2 lc/c. Here, perpendicular (⊥) and parallel (∥) are measured with respect to the scale-dependent local mean magnetic field, as detailed in J. Cho & E. T. Vishniac (2000).
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Dependence of curvature-drift energization and other contributions on δB0/B0. (a) Pdfs of ΔWc/γ0mic2 accumulated over Δt = 0.5 lc/c starting at t0 = 2 lc/c, from particles with γ0 ∈ (3, 8). (b)–(d) Pdfs of the ratios vc/v∇B, vc/vp, and ∣qE⊥ · vc∣/∣μM∂t(B/γE)/γ∣, respectively, obtained from the tracked particles.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Example trajectory of a proton from the reference simulation (δB0/B0 = 1). The top panel shows the trajectory color-coded by the particle Lorentz factor γ. The bottom panel shows the same trajectory color-coded by the magnetic field-line contraction (vE · κ)lc/c at the particle location. The trajectory is plotted over a duration of 4 lc/c.
Paper: Magnetic Field-line Curvature and Its Role in Particle Acceleration by Magnetically Dominated Turbulence
Authors: Samuel T. Sebastian, Luca Comisso
Figure caption: Probability density functions of ΔWc and ΔW⊥, normalized to the particle energy γ0mic2, accumulated over Δt = 0.5 lc/c starting at t0 = 2 lc/c (γ0 is the particle Lorentz factor at t0) in the reference simulation. Different colors correspond to three distinct ranges of γ0.
Paper: A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
Authors: W. V. Jacobson-Galán, L. Dessart, C. D. Kilpatrick, P. J. Patel, K. Auchettl, S. Tinyanont, R. Margutti, V. V. Dwarkadas, K. A. Bostroem, R. Chornock, R. J. Foley, H. Abunemeh, T. Ahumada, P. Arunachalam, M. J. Bustamante-Rosell, D. A. Coulter, C. Gall, H. Gao, X. Guo, D. O. Jones, J. Hjorth, M. Kaewmookda, M. M. Kasliwal, R. Kaur, C. Larison, N. LeBaron, H.-Y. Miao, G. Narayan, Y.-C. Pan, S. H. Park, K. C. Patra, Y. Qin, C. L. Ransome, A. Rest, J. Rho, S. Rose, H. Sears, J. J. Swift, K. Taggart, V. A. Villar, Q. Wang, Y. Zenati, H. Zhou
Figure caption: Left: Hα/[O I] spectral region shown in velocity space relative to Hα rest wavelength for phases δt = 110–708 days. Spectra have been normalized to peak flux. Hα shows a multicomponent structure where the narrow emission line profile comes from the inner ejecta (v < 5000 km s−1) and the “boxy” underlying profile comes from the CDS (v > 5000 km s−1), both of which are heavily affected by dust attenuation. Middle: optical-to-MIR hydrogen emission lines at δt = 364–374 days. Blue/red asymmetry in the narrow component of Hα confirms dust formation in the inner ejecta, which is also supported by the wavelength dependence of such line asymmetry on IR wavelengths. Right: Hα, Paα, and He I λ1.083 μm spectral regions in velocity space at δt = 656–658 days. The possible wavelength-dependent blue/red asymmetry in the “boxy” profile suggests the presence of dust in the CDS.
Paper: A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
Authors: W. V. Jacobson-Galán, L. Dessart, C. D. Kilpatrick, P. J. Patel, K. Auchettl, S. Tinyanont, R. Margutti, V. V. Dwarkadas, K. A. Bostroem, R. Chornock, R. J. Foley, H. Abunemeh, T. Ahumada, P. Arunachalam, M. J. Bustamante-Rosell, D. A. Coulter, C. Gall, H. Gao, X. Guo, D. O. Jones, J. Hjorth, M. Kaewmookda, M. M. Kasliwal, R. Kaur, C. Larison, N. LeBaron, H.-Y. Miao, G. Narayan, Y.-C. Pan, S. H. Park, K. C. Patra, Y. Qin, C. L. Ransome, A. Rest, J. Rho, S. Rose, H. Sears, J. J. Swift, K. Taggart, V. A. Villar, Q. Wang, Y. Zenati, H. Zhou
Figure caption: Left: pseudobolometric light curves of SN 2023ixf constructed using NUV–NIR bands (0.16–2.5 μm; salmon circles), NUV (0.16–0.3 μm; magenta circles), FUV–NUV (0.1–0.3 μm; magenta stars), optical (0.3–1.0 μm; blue circles), NIR (1.0–2.5 μm; orange circles), and MIR (2.5–30.0 μm; orange circles). The unabsorbed 0.3–10 keV X-ray light curve is shown as cyan circles. Right: fractional flux emitted in UV (0.1–0.3 μm; magenta), optical (0.3–1.0 μm; blue), IR (1–30 μm; orange), and X-ray (0.3–10 keV; cyan) wavelengths at δt = 374 days.
Paper: A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
Authors: W. V. Jacobson-Galán, L. Dessart, C. D. Kilpatrick, P. J. Patel, K. Auchettl, S. Tinyanont, R. Margutti, V. V. Dwarkadas, K. A. Bostroem, R. Chornock, R. J. Foley, H. Abunemeh, T. Ahumada, P. Arunachalam, M. J. Bustamante-Rosell, D. A. Coulter, C. Gall, H. Gao, X. Guo, D. O. Jones, J. Hjorth, M. Kaewmookda, M. M. Kasliwal, R. Kaur, C. Larison, N. LeBaron, H.-Y. Miao, G. Narayan, Y.-C. Pan, S. H. Park, K. C. Patra, Y. Qin, C. L. Ransome, A. Rest, J. Rho, S. Rose, H. Sears, J. J. Swift, K. Taggart, V. A. Villar, Q. Wang, Y. Zenati, H. Zhou
Figure caption: Zoomed-in comparison of SN 2023ixf UVOIR spectra at δt = 374 days with respect to CMFGEN model spectra at δt = 350 days for a variety of shock powers and dust parameters (e.g., masses, grain sizes, and temperatures).
Paper: A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
Authors: W. V. Jacobson-Galán, L. Dessart, C. D. Kilpatrick, P. J. Patel, K. Auchettl, S. Tinyanont, R. Margutti, V. V. Dwarkadas, K. A. Bostroem, R. Chornock, R. J. Foley, H. Abunemeh, T. Ahumada, P. Arunachalam, M. J. Bustamante-Rosell, D. A. Coulter, C. Gall, H. Gao, X. Guo, D. O. Jones, J. Hjorth, M. Kaewmookda, M. M. Kasliwal, R. Kaur, C. Larison, N. LeBaron, H.-Y. Miao, G. Narayan, Y.-C. Pan, S. H. Park, K. C. Patra, Y. Qin, C. L. Ransome, A. Rest, J. Rho, S. Rose, H. Sears, J. J. Swift, K. Taggart, V. A. Villar, Q. Wang, Y. Zenati, H. Zhou
Figure caption: Left: best-matched CMFGEN model spectra (red and gold lines) at δt = 350 days, with CDS dust and shock power included, compared to SN 2023ixf at δt = 374 days (black). CMFGEN model spectra with no added dust plotted in blue shows the need for dust in the CDS to match the overall SN luminosity and spectral features. Right: shock power CMFGEN model spectra at δt = 600 days with no dust (blue), CDS dust (red), and ejecta dust (gold) compared to SN 2023ixf at δt = 620 days (black). The PWR1e40 model at δt = 600 days would better match the Hα emission but overpredicts the line emission in the UV. The disappearance of emission lines such as Mg I] and [Ca II] confirms the presence of dust within the inner SN ejecta.
Paper: A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
Authors: W. V. Jacobson-Galán, L. Dessart, C. D. Kilpatrick, P. J. Patel, K. Auchettl, S. Tinyanont, R. Margutti, V. V. Dwarkadas, K. A. Bostroem, R. Chornock, R. J. Foley, H. Abunemeh, T. Ahumada, P. Arunachalam, M. J. Bustamante-Rosell, D. A. Coulter, C. Gall, H. Gao, X. Guo, D. O. Jones, J. Hjorth, M. Kaewmookda, M. M. Kasliwal, R. Kaur, C. Larison, N. LeBaron, H.-Y. Miao, G. Narayan, Y.-C. Pan, S. H. Park, K. C. Patra, Y. Qin, C. L. Ransome, A. Rest, J. Rho, S. Rose, H. Sears, J. J. Swift, K. Taggart, V. A. Villar, Q. Wang, Y. Zenati, H. Zhou
Figure caption: Single-temperature thermal bremsstrahlung model fit (black dashed lines) to three late-time epochs of Swift-XRT data (red circles). Temperature is fixed in these models following the decline rate derived by A. J. Nayana et al. (2025).
Paper: A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
Authors: W. V. Jacobson-Galán, L. Dessart, C. D. Kilpatrick, P. J. Patel, K. Auchettl, S. Tinyanont, R. Margutti, V. V. Dwarkadas, K. A. Bostroem, R. Chornock, R. J. Foley, H. Abunemeh, T. Ahumada, P. Arunachalam, M. J. Bustamante-Rosell, D. A. Coulter, C. Gall, H. Gao, X. Guo, D. O. Jones, J. Hjorth, M. Kaewmookda, M. M. Kasliwal, R. Kaur, C. Larison, N. LeBaron, H.-Y. Miao, G. Narayan, Y.-C. Pan, S. H. Park, K. C. Patra, Y. Qin, C. L. Ransome, A. Rest, J. Rho, S. Rose, H. Sears, J. J. Swift, K. Taggart, V. A. Villar, Q. Wang, Y. Zenati, H. Zhou
Figure caption: Best-fit three-component (Si+C dust) dust models using standard analytic prescriptions for optically thin dust (e.g., O. D. Fox et al. 2011; S. Tinyanont et al. 2019; M. Shahbandeh et al. 2023; J. Pearson et al. 2025) with opacities from B. T. Draine & A. Li (2007).
Paper: A Panchromatic View of Late-time Shock Power in the Type II Supernova 2023ixf
Authors: W. V. Jacobson-Galán, L. Dessart, C. D. Kilpatrick, P. J. Patel, K. Auchettl, S. Tinyanont, R. Margutti, V. V. Dwarkadas, K. A. Bostroem, R. Chornock, R. J. Foley, H. Abunemeh, T. Ahumada, P. Arunachalam, M. J. Bustamante-Rosell, D. A. Coulter, C. Gall, H. Gao, X. Guo, D. O. Jones, J. Hjorth, M. Kaewmookda, M. M. Kasliwal, R. Kaur, C. Larison, N. LeBaron, H.-Y. Miao, G. Narayan, Y.-C. Pan, S. H. Park, K. C. Patra, Y. Qin, C. L. Ransome, A. Rest, J. Rho, S. Rose, H. Sears, J. J. Swift, K. Taggart, V. A. Villar, Q. Wang, Y. Zenati, H. Zhou
Figure caption: Top: multiepoch UVOIR spectra of SN 2023ixf covering a phase range of δt = 253–659 days. Middle/bottom: best-matched CMFGEN model spectra (red lines) at δt = 350 and  600 days compared to UVOIR spectrum of SN 2023ixf at δt = 374 and 620 days (black). Model spectra include (0.5 = 1) × 1040 erg s−1 of shock power and (0.5–1) × 10−3 M⊙ of silicate dust with a grain size of 1 μm and temperature of 600–650 K.
Paper: Ultra-High-energy Cosmic Ray Production in Binary Neutron Star Mergers
Authors: Glennys R. Farrar
Figure caption: Black dashed line: rigidity cutoff ﹩{{ \mathcal R }}_{{\rm{cut}}}﹩ as a function of radius from Equation (2), with field initialized to the K. Kiuchi et al. (2024) simulation and evolving with expansion as B ∝ r−3/2 and lcoh = r/3. Colored solid lines: maximum rigidity for various nuclei as a function of radius, consistent with tsynch = taccel. The radii where these intersect are denoted rcrit for each composition.
Paper: Ultra-High-energy Cosmic Ray Production in Binary Neutron Star Mergers
Authors: Glennys R. Farrar
Figure caption: Rigidity-weighted escaping spectrum for Fe, ﹩{ \mathcal R }\,d{N}^{{\rm{esc}}}/d\,{{\rm{log}}}_{10}{ \mathcal R }﹩ (au), after expansion to progressively larger radii 1014, 1014.1, 1014.3,1015, 1016 cm (shown in blue, orange, green, red, and purple, respectively), in the simple approximation outlined in Appendix B; a more complete treatment leads to greater suppression of late-time and low-energy contributions.
Paper: Ultra-High-energy Cosmic Ray Production in Binary Neutron Star Mergers
Authors: Glennys R. Farrar
Figure caption: The Poynting flux on a sphere of r = 500 km, 150 ms post-merger, in the high-resolution neutrino radiation GRMHD simulation of a BNS merger reported in Figure 4 of K. Kiuchi et al. (2024).
Paper: Ultra-High-energy Cosmic Ray Production in Binary Neutron Star Mergers
Authors: Glennys R. Farrar
Figure caption: Same as in Figure 2, but initializing for the jet, where B is 10 times larger and lcoh ≈ 0.2r.
Paper: Ultra-High-energy Cosmic Ray Production in Binary Neutron Star Mergers
Authors: Glennys R. Farrar
Figure caption: Acceleration timescale divided by synchrotron loss timescale vs. rms magnetic field strength, for various nuclei, at ﹩{{ \mathcal R }}_{{\rm{cut}}}﹩=6.8 EV; He is a factor 4 below O and crosses unity at 3700 G.
Paper: Separating Flare and Secondary Atmospheric Signals with RADYN Modeling of Near-infrared JWST Transmission Spectroscopy Observations of TRAPPIST-1
Authors: Ward S. Howard, Adam F. Kowalski, Michael Radica, Laura Flagg, Valeriy Vasilyev, Benjamin V. Rackham, Guadalupe Tovar Mendoza, Meredith A. MacGregor, Alexander I. Shapiro, Jake Taylor, Louis-Philippe Coulombe, Olivia Lim, David Lafrenière
Figure caption: Top: the wavelength-integrated (0.6–2.83 μm) transit-normalized flare light curves of our sample. The flare temperatures of the integrations used for model validation and mitigation are scaled by color. Bottom left: fiducial Teff flare spectra are computed from similar-temperature integrations. Best-fitting blackbody curves are shown with the dashed gray lines. Bottom right: quiescent features appear in the residual spectra after subtracting the best-fit blackbody curves.
Paper: Separating Flare and Secondary Atmospheric Signals with RADYN Modeling of Near-infrared JWST Transmission Spectroscopy Observations of TRAPPIST-1
Authors: Ward S. Howard, Adam F. Kowalski, Michael Radica, Laura Flagg, Valeriy Vasilyev, Benjamin V. Rackham, Guadalupe Tovar Mendoza, Meredith A. MacGregor, Alexander I. Shapiro, Jake Taylor, Louis-Philippe Coulombe, Olivia Lim, David Lafrenière
Figure caption: Top: peak flare spectrum of each event overlaid with the best-fit RADYN model, where fits are color-coded by reduced χ2 value. The full model grid is shown for reference in gray, where each gray model is scaled by the filling factor of the highlighted model. The models qualitatively describe the line and 0.82–2.83 μm continuum emission, but predict a large Paschen jump not present in the observations. The daggers denote NIRSpec flares. Bottom: a close-up of the best-fit RADYN line models for the F4 event compared with the NIRISS data. Although not included in RADYN, Pγ is shown to alleviate blending concerns for HeI IRT.
Paper: Separating Flare and Secondary Atmospheric Signals with RADYN Modeling of Near-infrared JWST Transmission Spectroscopy Observations of TRAPPIST-1
Authors: Ward S. Howard, Adam F. Kowalski, Michael Radica, Laura Flagg, Valeriy Vasilyev, Benjamin V. Rackham, Guadalupe Tovar Mendoza, Meredith A. MacGregor, Alexander I. Shapiro, Jake Taylor, Louis-Philippe Coulombe, Olivia Lim, David Lafrenière
Figure caption: Flowchart illustrating the empirical flare correction procedure. We note the steps in the physics-based procedure are similar to those in the empirical procedure.
Paper: Early Evidence for Isotropic Planetary Obliquities in Young Super-Jupiter Systems
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Jiayin Dong, Joshua S. Speagle, 佳士 沈, Dang Pham
Figure caption: We test whether our hierarchical model can distinguish between planet-like and brown-dwarf-like formation using simulated obliquity measurements. Top: planet-like formation assumes a Fisher distribution with κ = 5 (top left), while brown-dwarf-like formation is modeled as an isotropic distribution with κ = 0 (top right). Vertical lines mark the obliquities of Earth, Mars, Saturn, and Neptune, which distinctly cluster together. Bottom: for 100 draws of 4 obliquities from the above distribution, we simulate noisy observations for the spin axis and orbital inclinations and infer posteriors on κ. The median posteriors show qualitatively distinct structure, demonstrating that even four measurements can inform formation pathways.
Paper: Early Evidence for Isotropic Planetary Obliquities in Young Super-Jupiter Systems
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Jiayin Dong, Joshua S. Speagle, 佳士 沈, Dang Pham
Figure caption: Planet spin axis inclinations (ip, orange) compared with orbital inclinations (io, gold). These line-of-sight inclinations are relative to an observer along the ﹩{X}^{{\prime} }﹩-axis (left side), while the vertical axis represents the sky plane (﹩{Y}^{{\prime} }-{Z}^{{\prime} }﹩), following Figure 1. ip is mirrored about the sky plane due to an observational degeneracy. These diagrams were inspired by B. P. Bowler et al. (2023).