adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Evolution of the total magnetic field energy EB in all our models, as a function of time since the first contact. The growth rate varies, depending on the number of contacts before the final merger. However, in all cases, EB grows by more than 8 orders of magnitude over a few tens of hours via small-scale dynamos, and then saturates at 1044–1045 erg or rises substantially more slowly.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Radial magnetic field strength of the products, mass-weighted averaged over the spherical equipotential surfaces of collision products produced in collisions between 0.7 M⊙ and 0.6 M⊙ stars with different impact parameters b, as a function of the enclosed mass. The thinner lines indicate the dipole component defined as ﹩\sqrt{{({B}^{{\rm{r}}})}^{2}+{({B}^{{\rm{z}}})}^{2}}﹩, where Br(Bz) is the radial (vertical) component of magnetic fields.
Paper: Discovery of the Richest Pulsating Ultramassive White Dwarf
Authors: Francisco C. De Gerónimo, Murat Uzundag, Alberto Rebassa-Mansergas, Alex Brown, Mukremin Kilic, Alejandro H. Córsico, Gracyn C. Jewett, Adam G. Moss
Figure caption: Light curve obtained with APO on December 23 (upper panel) and September 1 (bottom panel; see Section 2 for more details).
Paper: The Cold Jupiter Eccentricity Distribution is Consistent with EKL Driven by Stellar Companions
Authors: Grant C. Weldon, Smadar Naoz, Bradley M. S. Hansen
Figure caption: Panel (a): diagram (not to scale) illustrating important angles. In this example, the coordinate system ﹩\hat{x},\hat{y},\hat{z}﹩ is defined by the total angular momentum of the system (﹩{{\boldsymbol{G}}}_{{\rm{tot}}}\parallel \hat{z}﹩) and is related to the observer frame ﹩{\hat{x}}^{{\prime} },{\hat{y}}^{{\prime} },{\hat{z}}^{{\prime} }﹩ by a rotation about the ﹩\hat{x}={\hat{x}}^{{\prime} }﹩ axis. The angular momentum of the inner (outer) orbit is shown as the vector ﹩{{\boldsymbol{G}}}_{{\bf{1}}}﹩ (﹩{{\boldsymbol{G}}}_{{\bf{2}}}﹩), and the respective angle with the ﹩\hat{z}﹩-axis is i1 (i2). The mutual inclination i is the angle between ﹩{{\boldsymbol{G}}}_{{\bf{1}}}﹩ and ﹩{{\boldsymbol{G}}}_{{\bf{2}}}﹩. The inclination of G1 with respect to the line of sight is iobs. The stellar obliquity ψ is the angle between the spin vector ﹩{\boldsymbol{s}}﹩ of the star and ﹩{{\boldsymbol{G}}}_{{\bf{1}}}﹩. The projection of the obliquity onto the sky plane is λ. Panel (b): isotropic distribution of inclinations (solid gray region), distribution of mutual inclinations in the r0.13 simulation run (solid orange line), and distribution of iobs (solid black line) calculated by rotating the simulations into the observer frame. Panel (c): planetary mass in the r0.13 simulations. We show the line-of-sight masses assuming an isotropic inclination distribution (dashed black line) and the line-of-sight masses produced by EKL (solid orange line). Panel (d): observed line-of-sight masses for planets in the SSSP (dashed black line) and MSSP (solid blue line) samples. Panel (e): Distribution of stellar obliquities ψ produced by EKL in the r0.13 simulation run (solid orange line) and the sky-projected obliquities λ (solid black line). All systems have spin–orbit angles initially aligned.
Paper: A Diverse, Overlooked Population of Type Ia Supernovae Exhibiting Mid-infrared Signatures of Delayed Circumstellar Interaction
Authors: Geoffrey Mo, Kishalay De, Eli Wiston, Nayana A. J., Raffaella Margutti, Danielle Frostig, Jesper Sollerman, Yashvi Sharma, Takashi J. Moriya, Kevin B. Burdge, Jacob Jencson, Viraj R. Karambelkar, Nathan P. Lourie
Figure caption: The phase space of MIR light curves for SNe Ia. We show NEOWISE W2 light curves for the SNe Ia showing delayed CSM interaction from our sample in the colored stars. For comparison, we also plot previously published SNe Ia with delayed CSM interaction, including PTF 11kx, SN 2015cp, and SN 2020eyj (blue circles, squares, and triangles, respectively). Plotted with blue diamonds is the Spitzer IRAC Ch2 light curve of SN 2014dt, an SN Iax that exhibits an analogous rise and fall to the interacting SNe Ia, but at a much lower luminosity (O. D. Fox et al. 2016; J. E. Jencson et al. 2019). The SNe Ia-CSM, for which we show selected W2 light curves in dark red (these include SN 2016iks, SN 2017eby, SN 2017hzw, SN 2018crl, SN 2018evt, SN 2018gkx, SN 2019agi, SN 2020aekp), display similar behavior to most of the SNe Ia with delayed CSM interaction. Finally, we show Spitzer Ch2 light curves of normal SNe Ia from T. Szalai et al. (2019) in magenta.
Paper: A Diverse, Overlooked Population of Type Ia Supernovae Exhibiting Mid-infrared Signatures of Delayed Circumstellar Interaction
Authors: Geoffrey Mo, Kishalay De, Eli Wiston, Nayana A. J., Raffaella Margutti, Danielle Frostig, Jesper Sollerman, Yashvi Sharma, Takashi J. Moriya, Kevin B. Burdge, Jacob Jencson, Viraj R. Karambelkar, Nathan P. Lourie
Figure caption: Optical spectroscopic and MIR photometric signatures of CSM interaction. Left: spectra of the known delayed CSM-interacting SNe PTF11kx (M. L. Graham et al. 2017) and SN 2015cp (M. L. Graham et al. 2019), compared to spectra we obtained for SN 2020yex and SN 2022bbt, zoomed in to the region around Hα. Both Hα lines (>1000 km s−1) from CSM interaction, as well as unresolved host galaxy lines, are visible for PTF11kx and SN 2015cp. In contrast, only narrow lines from the host galaxy are visible for SN 2020yex, while no trace is detected in SN 2022bbt. Right: comparison of the evolution of MIR (NEOWISE; orange) and Hα (blue) luminosity for SNe Ia displaying delayed CSM interaction (labeled Ia-dCSM in the legend). We also show the corresponding luminosity evolution for SN 2015da (SN IIn; L. Tartaglia et al. 2020), SN 2018evt (SN Ia-CSM; L. Wang et al. 2024), SN 2020aekp (SN Ia-CSM; Y. Sharma et al. 2023), and three SNe Ia that show late-time nebular Hα emission (SN 2016jae, N. Elias-Rosa et al. 2021; SN 2018cqj, J. L. Prieto et al. 2020; SN 2018fhw, J. A. Kollmeier et al. 2019; P. J. Vallely et al. 2019). We show 5σ upper limits on the broad/intermediate Hα line (see Appendix B) for two events in our sample in blue as the open hexagon and square, respectively.
Paper: A Diverse, Overlooked Population of Type Ia Supernovae Exhibiting Mid-infrared Signatures of Delayed Circumstellar Interaction
Authors: Geoffrey Mo, Kishalay De, Eli Wiston, Nayana A. J., Raffaella Margutti, Danielle Frostig, Jesper Sollerman, Yashvi Sharma, Takashi J. Moriya, Kevin B. Burdge, Jacob Jencson, Viraj R. Karambelkar, Nathan P. Lourie
Figure caption: The evolution of dust properties, derived from fitting the NEOWISEW1 and W2 bands for events in our sample, as well as for SN 2015cp. Top: lower limits on the blackbody radii compared to the speed of light (blue line), 104 km s−1 ejecta (black line; relevant for typical SNe Ia), and 3000 km s−1 ejecta (magenta line; relevant for SNe Iax). Note that the dust radii at early phases are far outside the ejecta, as shown in the inset. Middle: dust temperatures assuming 0.1 μm carbonaceous grains. There is a rise in the dust temperature at  ≈1 yr after explosion, indicating the reheating of preexisting dust by radiation produced by CSM interaction. Bottom: the evolution of the dust mass shows an increase at later phases, consistent with the formation of new dust.
Paper: The Cold Jupiter Eccentricity Distribution is Consistent with EKL Driven by Stellar Companions
Authors: Grant C. Weldon, Smadar Naoz, Bradley M. S. Hansen
Figure caption: Comparison of the eccentricity CDF between the observed MSSP sample (solid blue line) and the r0.13 simulation run in this work (solid orange line). We also show, from low to high median eccentricity, the distribution produced by EKL with circular orbits in C. Petrovich (2015b) (dashed orange line), the scattering distribution in J.-L. Zhou et al. (2007) (dashed gray line), the scattering distribution in S. Chatterjee et al. (2008) (solid red line), and the scattering distribution in M. Jurić & S. Tremaine (2008) (dashed light blue line).
Paper: The Cold Jupiter Eccentricity Distribution is Consistent with EKL Driven by Stellar Companions
Authors: Grant C. Weldon, Smadar Naoz, Bradley M. S. Hansen
Figure caption: Time evolution of the mutual inclination i (black line, upper panel), stellar obliquity ψ (violet line, upper panel), eccentricity e1 (green line, middle panel), semimajor axis a1 (red line, lower panel), and pericenter a1(1 − e1) (blue line, lower panel) for a simulated initially cold planet that undergoes high-eccentricity tidal migration. We shade the regions where the planet is considered a cold Jupiter (blue region), warm Jupiter (thin orange region), and hot Jupiter (red region). The system is initially set with m1 = 1.04 M⊙, m2 = 6.20 MJ, m3 = 0.94 M⊙, a1 = 3.92 au, a2 = 721.00 au, e1 = 0.01, e2 = 0.55, i = 86﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4, ω1 = 82﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4, and ω2 = 141﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1.
Paper: A Diverse, Overlooked Population of Type Ia Supernovae Exhibiting Mid-infrared Signatures of Delayed Circumstellar Interaction
Authors: Geoffrey Mo, Kishalay De, Eli Wiston, Nayana A. J., Raffaella Margutti, Danielle Frostig, Jesper Sollerman, Yashvi Sharma, Takashi J. Moriya, Kevin B. Burdge, Jacob Jencson, Viraj R. Karambelkar, Nathan P. Lourie
Figure caption: Optical and MIR light curves of our sample of SNe Ia showing evidence for delayed CSM interaction. We show NEOWISE MIR light curves alongside Gaia, ATLAS, and ZTF photometry of the SNe in our sample. Upper limits are displayed as downward-pointing open symbols. In parentheses next to each SN’s label is its peak-light classification.
Paper: Discovery of the Richest Pulsating Ultramassive White Dwarf
Authors: Francisco C. De Gerónimo, Murat Uzundag, Alberto Rebassa-Mansergas, Alex Brown, Mukremin Kilic, Alejandro H. Córsico, Gracyn C. Jewett, Adam G. Moss
Figure caption: Light curve obtained with HiPERCAM on September 17 (see Section 2). HiPERCAM filters us, gs, rs, is, and zs are shown from top to bottom. The increased scatter at BJD 2460571.7 is due to an increase in the seeing and is unrelated to the target.
Paper: The Cold Jupiter Eccentricity Distribution is Consistent with EKL Driven by Stellar Companions
Authors: Grant C. Weldon, Smadar Naoz, Bradley M. S. Hansen
Figure caption: Panel (a): distributions of initial conditions (dashed black line), simulated eccentricities (solid black line), and observed eccentricities in the MSSP sample (shaded blue) for six different simulation runs. The Poisson uncertainty for each bin is shown in blue. Each plot is labeled with the name of the run. The KS test p-values comparing the simulated and observed distributions are shown. Panel (b): comparison of the simulated eccentricity distribution (shaded orange) in the r0.13 simulations with the distribution for multistar, single-planet systems (MSSP, solid blue line), single-planet, single-star systems (SSSP, dashed black line), and multiplanet systems (MP, solid black line). Panel (c): two-dimensional histogram with simulated systems in the r0.13 run binned based on eccentricity and semimajor axis. The color code shows the number of counts in each bin. Darker regions correspond to a higher amount of time spent in that region. Here, we show systems with a > 0.5 au to examine the boundary between the warm and cold populations. The observed population of 0.3–10 MJ planets (blue dots, single-planet systems) is overplotted.
Paper: Measurement of Turbulence Injection Scale Down to the Chromosphere
Authors: Zachary Bailey, Riddhi Bandyopadhyay, Shadia Habbal, Miloslav Druckmüller
Figure caption: Variation of perpendicular correlation length as a function of height above the solar surface, given in units of a solar radius (﹩{R}_{\odot }\approx 700\,﹩ Mm). The red squares are measurements in the chromosphere and the blue round symbols are measurements in the transition region and the lower corona from this work, using a white light eclipse image. The previous closest estimate of L⊥ in the corona (R. Sharma & R. J. Morton 2023) is shown by a magenta triangle. A scaled version of the theoretical model of L⊥ (S. R. Cranmer & A. A. van Ballegooijen 2012), based on the equation ﹩{L}_{\perp }\alpha {{B}_{0}}^{-1/2}﹩(J. V. Hollweg 1986) is plotted in a black solid line. The typical width of solar granules is (∼1.5 Mm) shown by a red cross at the left edge.
Paper: Measurement of Turbulence Injection Scale Down to the Chromosphere
Authors: Zachary Bailey, Riddhi Bandyopadhyay, Shadia Habbal, Miloslav Druckmüller
Figure caption: White light image taken during the 2017 August 21 TSE. (A) Overview of the full eclipse image. S1 and S2 point to the regions of strong chromospheric emission (pink) and are the locations closest to the solar surface in these images. (B) and (C) are close-up views of the two sections studied in this work. We start at the base of the chromosphere and move toward the outer dashed white lines above the solar limb. We divide both S1 and S2 into six sections shown by the dashed white lines to measure ﹩{L}_{\perp }﹩ 12 times at each given radius. Also shown in panel (B) is a sample plot that gives pixel intensity (in arbitrary units) vs. distance for three one-dimensional cuts at different radial distances in the chromosphere (red), transition region (black), and the corona (yellow).
Paper: The Cold Jupiter Eccentricity Distribution is Consistent with EKL Driven by Stellar Companions
Authors: Grant C. Weldon, Smadar Naoz, Bradley M. S. Hansen
Figure caption: Grid of initial eccentricities and inclinations (﹩\theta =\cos i﹩), where the color code corresponds to the maximum eccentricity obtained by integrating for 100tquad. We note that the color code is spaced nonlinearly to observe features at both low and high eccentricities. Each system is set with a1 = 5 au, a2 = 165 au, and e2 = 0.5, such that ϵ = 0.02. Here, we set m1 = 1 M⊙, m2 = 1 MJ, m3 = 1 M⊙, ω1,0 = 0°, and ω2,0 = 0°.
Paper: Measurement of Turbulence Injection Scale Down to the Chromosphere
Authors: Zachary Bailey, Riddhi Bandyopadhyay, Shadia Habbal, Miloslav Druckmüller
Figure caption: Schematic diagram (not to scale) of the expansion of the magnetic field, starting from the chromosphere into the corona as inferred from the ﹩{{L}}_{{\boldsymbol{\perp }}}﹩ measurements. This is similar to the schematics by T. R. Rimmele et al. (2020) and F. Wöger et al. (2021), except for the heights, which are different.
Paper: The Cold Jupiter Eccentricity Distribution is Consistent with EKL Driven by Stellar Companions
Authors: Grant C. Weldon, Smadar Naoz, Bradley M. S. Hansen
Figure caption: The eccentricities and semimajor axes of observed planets (black dots) with mass 0.3–10 MJ. In this work, we consider hot Jupiters to have a < 0.1 au (red region), warm Jupiters to have 0.1 au < a <​​​​​​ 0.8 au (orange region), and cold Jupiters to have 0.8 au < a < 6 au (blue region).
Paper: Measurement of Turbulence Injection Scale Down to the Chromosphere
Authors: Zachary Bailey, Riddhi Bandyopadhyay, Shadia Habbal, Miloslav Druckmüller
Figure caption: Correlation function derived from TSE white light image. An example of normalized correlation function ﹩R({\mathscr{l}})/R(0)﹩ (black solid line) vs. spatial lag ﹩{\mathscr{(}}{\mathscr{l}}{\mathscr{)}}﹩, computed from the TSE white light image. The thin red line is an exponential fit ﹩{{e}}^{{\mathscr{-}}{\mathscr{l}}{\mathscr{/}}{{L}}_{{\boldsymbol{\perp }}}}﹩ to the correlation function, with ﹩{L}_{\perp }=1325\,﹩ km.
Paper: Measurement of Turbulence Injection Scale Down to the Chromosphere
Authors: Zachary Bailey, Riddhi Bandyopadhyay, Shadia Habbal, Miloslav Druckmüller
Figure caption: Pixel intensities in the different color channels of the detector vs. height.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Ratios of the thermal (Etherm, black solid), kinetic (EK, blue-family lines), and magnetic (EB, red-family lines) energy to the absolute potential energy ∣Epot∣, as a function of time since the first contact. There is a clear energy hierarchy such that Epot > Etherm > EK ≫ EB. The sum of the thermal (Etherm) and kinetic energy (EK) is ≃0.5∣Epot∣, while Etherm/EK ≃ 3–4. In addition, each component of EK and EB reveals a similar hierarchical structure, independent of the collision parameters: ﹩{E}_{{\rm{K}}}^{\theta }\gg {E}_{{\rm{K}}}^{{\rm{r}}}\simeq {E}_{{\rm{K}}}^{z}(\lesssim 1 \% )﹩ and ﹩{E}_{{\rm{B}}}^{\theta }\gg {E}_{{\rm{B}}}^{{\rm{r}}}\simeq {E}_{{\rm{B}}}^{z}(\lesssim 10 \% )﹩.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Fraction of mass in the central part of collision products (inner 10% in mass) that originally belonged to the primary star F1, 10%, as a function of the core density ratio of the original two stars. F1, 10% = 0.5 (horizontal gray line) indicates that two stars are equally mixed, while F1, 10% > 0.5 indicates that the chemical abundances in more than 50% of the central part originated from the primary. The collisions with the same mass ratio (impact parameter b) share the same color (shape). We further differentiate collisions with the primary mass M1 = 0.7 M⊙ (solid markers) from those with M1 = 0.8 M⊙ (hollow markers). The general trend is that mixing becomes more efficient (F1, 10% ⟶ 0.5) if collisions occur between stars with similar masses and smaller b. In addition, collisions of a primary star that is easily destroyed (lower central density or higher core H mass fraction) lead to efficient mixing, indicated by generally smaller F1, 10% for M1 = 0.7 M⊙ than that for M1 = 0.8 M⊙.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Mass-weighted average of the temperature Tmid in the midplane (top) and the ratio of the rotational velocity in the midplane to the Keplerian velocity ﹩{v}_{{\rm{mid}}}^{\phi }/{v}_{{\rm{Kep}}}^{\phi }﹩ (bottom), as a function of distance from the center of mass of the collision products in collisions involving M1 = 0.7 M⊙, with different impact parameters b. The temperature profile shows a noticeable slope change at 0.7–0.8 R⊙ for b ≤ 0.25 (except for one case with M2 = 0.4 M⊙ and b = 0.25) and 1–2 R⊙ for b = 0.5 (solid lines). The velocity ratio profiles show the similar features.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Mass-weighted average of the hydrogen mass fraction within the collision products, as a function of enclosed mass. The models are divided into four groups depending on the primary mass and mass ratio: M1 = 0.7 M⊙, q = M2/M1 = 0.97 (top-left), M1 = 0.7 M⊙, q = 0.86 (top-right), M1 = 0.7 M⊙, q = 0.57 (bottom-left), and M1 = 0.8 M⊙, q ≲ 0.88 (bottom-right). The gray lines in each top panel indicate the profiles of the initial stars: less massive stars have higher core hydrogen mass fraction at the same age.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Density distribution of the products in collisions between a 0.7 M⊙ star and 0.68 M⊙ star with b = 0.25 (top) and 0.5 (bottom) along an x–z slice passing through the center of mass, overlaid with equidensity lines (white contours). The density is measured at t ≃ 45 hr since the first contact. As b increases, the overall shape of the product becomes more oblate because of larger angular momentum. Markedly, for b = 0.5, a noticeably flattened structure along the midplane appears between the central part of the product and the outermost envelope, potentially indicative of disk formation.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Spin frequency with respect to the critical frequency (top) and midplane spin velocity (bottom) in all our models, as a function of enclosed mass. The models are divided into four groups depending on the primary mass and mass ratios: M1 = 0.7 M⊙, q = M2/M1 = 0.97 (leftmost), M1 = 0.7 M⊙, q = 0.86 (left middle), M1 = 0.7 M⊙, q = 0.57 (right middle), and M1 = 0.8 M⊙, q ≲ 0.88 (rightmost).
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Evolution of the total magnetic field energy EB as a function of time with varying number of cells per star N (0.25M to 4M, different colors) and the initial magnetic field strength at the stellar surface Bs (1G, 10G, and 100G, different line styles). The magnetic energy saturates at similar levels, independent of N and Bs.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Density and hydrogen mass fraction profiles of initial models for main-sequence stars with a metallicity of Z = 0.001 and at an age of 12 Gyr, as a function of enclosed mass.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: Left: Raw spectroscopic lightcurves, as extracted with Eureka! and binned to Δλ = 0.02 μm. The gray areas mark the separations between the data from the NRS1 and NRS2 detectors, as well as the integrations that were trimmed out of the NRS2 lightcurves of transits 2 and 4. Right: White lightcurves and best-fit models. We also show the lightcurve data points binned by a factor of 80 to more easily identify the small undulations. On the right axes, we show the histograms of the unbinned residuals.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: The average Eureka! transmission spectrum of L 98-59 b from the four JWST NIRSpec/G395H transits compared against the 98% SO2 model predicted in D. Z. Seligman et al. (2024) and a self-consistent photochemical model assuming an SO2-dominated atmosphere. We also show the best-fit flat-line and atmosphere models retrieved with Aurora on the Δλ = 0.01 μm data and the corresponding 2σ uncertainty bands. All models include an offset between the two detectors.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: Aurora retrieval results for L 98-59 b. Top: The retrieved transmission spectrum on the Eureka! reduction of the L 98-59 b observations. The inference is performed on the Δλ = 0.01 μm resolution observations, but the Δλ = 0.04 μm data are overplotted for visual clarity. The orange shading shows the retrieved median model as well as 1σ and 2σ confidence intervals. Bottom: Posterior distributions for the gases of interest. Most gases are unconstrained, with inferred abundances suggestive of an atmosphere rich in SO2.