adsabs/AstroCLIMB huggingface dataset:
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: Average noise-corrected LIBS spectra of “cemented” ice-regolith simulants, normalized to the total emission, containing between 0 and 38 wt% water ice. The blue curves represent measurements from LHS-based samples, while the red curves correspond to LMS-based samples. A vertical offset of 3 × 10−2 is applied for clarity. (a) Spectra in the UV–visible range captured by the first spectrometer. (b) Spectra in the visible–NIR range captured by the second spectrometer. (c) Close-up of the Balmer Hα line (656.48 nm), with no offset applied.
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: Photographs of six regolith simulants used in this study, including dry LMS and LHS samples, as well as “cemented” ice-regolith mixtures containing 5–20 wt% ice. Viewing angles vary slightly between images. All sample cups share a common diameter of 3.85 cm.
Paper: Laser-induced Breakdown Spectroscopy of Ice-regolith Mixtures: Implications for Measurements on Planetary Surfaces
Authors: Frédéric Diotte, Myriam Lemelin, François R. Doucet, Lütfü Ç. Özcan
Figure caption: Line-by-line variations in LIBS signal in “discrete” LHS ice samples. All measurements were taken from preprocessed spectra. (a) Average hydrogen intensity. (b) Average spectrum of 200 measurements made on a single scan line for a dry LHS sample. (c) Same as panel (b), but for a “discrete” LHS ice sample (15 wt% H2O). The shaded regions show the ±1σ range calculated from the spot-to-spot variation.
Paper: 2020 BX12—The Last Binary Asteroid Discovered at Arecibo
Authors: Luisa Fernanda Zambrano-Marin, Sean E. Marshall, Ellen S. Howell, Julia de León, Noemi Pinilla-Alonso, Anne K. Virkki, Jon Giorgini, Flaviane C. F. Venditti
Figure caption: Model for the data of day 2, with pole orientation at ecliptic (0, +15∘).
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Angular separation at quadrature as a function of distance to the system for planets receiving 67% of Earth’s instellation in the habitable zones of a range of host star types. The habitable zones of earlier-type M dwarfs reside at larger orbital radii than later-type systems and thus are less affected by observational configurations limited by coronagraphic IWA. However, achieving the necessary contrast for planets orbiting earlier-type hosts will inherently be more challenging, and early-type systems will indeed require higher integration times in general if we adopt constant instrumental contrast, as shown later in this work. Each planet is in its respective system’s habitable zone, and thus all planets receive a similar instellation to achieve a habitable climate, regardless of spectral type.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Stages of cross-correlation analysis, including telluric line removal (top), alias detrending (middle), and S/N estimation (bottom). The data CCF is shown in blue, and the model telluric and planet CCFs are shown in orange and green, respectively. The top panel shows the telluric CCF fit to the raw data CCF, which is subtracted off to remove the tellurics from the observation. The middle panel shows the telluric-subtracted data CCF (blue) and the planetary model CCF (green), which is used for detrending the aliasing patterns. The bottom panel shows the detrended CCF residuals in black and the planetary signal in red, as well as the telluric-subtracted data CCF curve (blue) for comparison. The S/N is calculated by dividing the maximum signal coefficient by the standard deviation of the detrended CCF residuals.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Example of simulated data for a 1000 hr observation of the O2 A band (bottom panel) for an Earth-like target orbiting an M6V host star 1.3 pc away using the 39 m ELT. The simulated data are constructed with two components: the light reflected from the planet and the shot noise, plotted in the top and middle panels, respectively. The shot noise is composed of planetary, stellar, and background sources (see Section 2.2.3), and we assume a 10% total throughput.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Mixing ratios for the major molecular species in the sub-Neptune atmosphere, and the atmospheric temperature profile (B. Charnay et al. 2015).
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: ELT integration time required to obtain a 3σ detection of a range of molecular bands for terrestrial atmospheres orbiting hypothetical 1.3 pc distant M2V–M8V host stars. Circles and triangles represent preindustrial Earth–like and Archean Earth–like atmospheres, respectively. Crosses and plus signs represent uninhabited ocean-loss and prebiotic Earth atmospheres, respectively. Filled and open symbols represent assumed instrumental contrasts of C = 10−3 and C = 10−4, respectively. We have limited the y-axis to ∼104 hr, i.e., ∼1 yr of continuous observation. This observational scenario assumes that each planet receives 66% of Earth’s insolation, the system has an RV of 20 km s–1 and is 1.3 pc away from Earth, and the observations are made with the E-ELT with an instrument capable of R = 100,000 observations and total throughput of 10%. While the biosignature disequilibrium pairs O2/CH4 and CO2/CH4 are potentially accessible for inhabited worlds, the abiotic gases O2 and CH4 in the uninhabited worlds may also be detectable in false-positive scenarios.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Detectability of H2O bands spanning the NIR for Proxima Centauri b with a modern Earth-like atmosphere. We assume an instrumental contrast of 10−3 and R = 100,000. We find that the 0.9 μm band is the most detectable H2O feature by at least a factor of three in some cases and by 1–2 orders of magnitude in the worst cases.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Integration time required to obtain a 3σ detection of a range of molecular bands for a sub-Neptune atmosphere (B. Charnay et al. 2015) orbiting Proxima Centauri b using simulated E-ELT and VLT observations with an assumed achieved contrast of C = 10−4 and total throughput of 10%. The molecules in this atmosphere are highly detectable with the ELT, requiring less than a few hours for most molecular species. The overall high detectability of all molecules, including H-bearing species, may help to identify the atmosphere of Proxima Centauri b as more likely to be sub-Neptune-like, rather than terrestrial, and this may be possible in the near term with smaller-aperture observatories. Note: symbols on the horizontal line at 1 hr (with arrows) are upper limits.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Comparison with previous work investigating the detectability of molecular features in an Earth-like atmosphere of Proxima Centauri b. Panels (a), (b), (c), (d), and (e) correspond to comparisons with C. Lovis et al. (2017), S. R. Vaughan et al. (2024), G. A. Hawker & I. R. Parry (2019), J. Wang et al. (2017), and H. Zhang et al. (2023), respectively. The studies we compare with use a variety of observing modes and configurations, which we attempt to control for in our comparisons by using the same or similar input parameters, and we list our assumptions for observing conditions and configurations in Table 5. Our results are largely consistent with these other studies, with the exception of more optimistic O2 and H2O detection when compared to H. Zhang et al. (2023).
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Time to a 3σ detection as a function of system RV for preindustrial Earth atmospheres orbiting M dwarf hosts. The host star is assumed to be 1.3 pc away and observed with E-ELT instrumentation capable of R = 100,000. Solid and dashed lines represent assumed instrumental contrasts of C = 10−3 and C = 10−4, respectively. We assume zero barycentric velocity and a total throughput of 10%. Our ability to detect molecular features depends strongly on the degree of telluric/target line blending and will be a consideration for minimizing the total observation time to detect molecular features in future observing campaigns by vetting targets for nonoptimal systemic velocities, observing the planet at orbital positions that minimize line blending, or taking into account observational seasonality if the barycentric velocity plays a significant role for a particular target.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Integration time to a 3σ detection for a range of terrestrial atmosphere types on Earth-sized planets orbiting analog nearby targets. Each panel represents a different molecular band, and each color represents a different nearby host star/planet analog. Filled and open circles represent assumed instrumental contrasts of C = 10−3 and C = 10−4, respectively, and we assume a total throughput of 10%. A Proxima Centauri b analog (1.3 pc away) is plotted in blue, and a sub-Neptune version of Proxima Centauri b is included for comparison. We may be able to detect several molecules within 100 hr of observing each target, and our Proxima Centauri b analog is the most favorable nearby target for thorough atmospheric characterization.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Integration time to detect O2, CO2, CH4, and H2O in a preindustrial Earth–like atmosphere orbiting an M6V host star 5 pc away using both transmission and reflected light (C = 10−4) techniques, both with R = 100,000. The transit transmission technique is overall more efficient for detecting O2, CO2, and CH4, but these techniques yield comparable results for H2O because reflected light observations are able to probe deeper into the atmosphere than in transmission and can detect the more abundant near-surface water. We emphasize that there is likely no transiting habitable zone terrestrial planet at 5 pc, and this figure should be only used as a reference for comparing differences in molecular detectability between the transmission and reflected light spectroscopy techniques.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Examples of TOA planetary flux spectral models for CH4 biosignature and false-positive cases. The left and right columns present the CH4 0.89 and 1.6 μm bands, respectively, for the biological CH4 Archean Earth–like case (top) and abiotic O2 prebiotic Earth-like case (bottom). The yellow and red curves represent spectra that are self-consistent with M2V and M6V host stars, respectively. We plot low spectral resolution (R = 500) curves over each high-resolution spectrum as black dashed curves. Note that we present the abiotic O2 with only an M6V host, as an atmospheric model consistent with an M2V host was unavailable.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Examples of TOA planetary flux spectral models for O2 biosignature and false-positive cases. The left and right columns present the O2 0.76 and 1.27 μm bands, respectively, for the biological O2 preindustrial Earth–like case (top) and abiotic O2 ocean-loss case (bottom). The yellow and red curves represent spectra that are self-consistent with M2V and M6V host stars, respectively. We plot low spectral resolution (R = 500) curves over each high-resolution spectrum as black dashed curves. Note that we present the abiotic O2 with only an M6V host, as an atmospheric model consistent with an M2V host was unavailable.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Time to a 3σ detection as a function of distance to the system for preindustrial Earth atmospheres orbiting M dwarf hosts with systemic RVs of 20 km s−1, observed with the E-ELT with instrumentation capable of R = 100,000 and C = 10−4, and with a total throughput of 10%. The time to detection scales as d2. For each curve, we plot a black symbol where the planetary separation falls below our assumed 2λ/D IWA for a 39 m mirror—targets with distances greater than this value will be challenging to observe. Later-type targets are more affected by the IWA limitation, and Proxima Centauri b (∼M6V, 1.3 pc away) will likely be the only nearby late-type target for which all tested molecular bands are accessible.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Time to a 3σ detection as a function of telescope collecting area for preindustrial Earth atmospheres orbiting M dwarf hosts 4.0 pc away with systemic RVs of 20 km s−1, observed with instrumentation capable of R = 100,000 and a total throughput of 10%. Solid and dashed lines represent assumed instrumental contrasts of C = 10−3 and C = 10−4, respectively. Current or planned telescopes are shown as dashed lines and labeled in the top panel. As expected, larger apertures improve the time to detection in all cases.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Time to a 3σ detection as a function of instrumental contrast for preindustrial Earth atmospheres orbiting M dwarf hosts for an E-ELT with instrumentation capable of spectral resolution R = 100,000 and a total throughput of 10%. The M dwarf hosts are assumed to be 1.3 pc and have systemic RVs of 20 km s−1.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Same as Figure 8, but for the GMT.
Paper: There’s More to Life in Reflected Light: Simulating the Detectability of a Range of Molecules for High-contrast, High-resolution Observations of Nontransiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows
Figure caption: Same as Figure 8, but for the TMT.
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: T1 bar–O/H–Zatm phase space for Jupiter with a scaling of Z by a solar value of Z⊙ = 0.015. (a) Observed 1 bar temperatures and the virtual 1 bar temperature of Li24. (b) Observationally inferred O/H values scaled by the solar O/H of K. Lodders (2021). (c) Conversion between O/H and Zatm, with the black dashed line indicating the 1:1 relation as a guide to the eye and with C/H varied from 0× (light) to 5× solar (dark) using the solar abundance values of K. Lodders (2021). (d) Interior model predictions for the T1 bar–Zatm relation by different H/He EOSs: REOS.3: [N17], MH13: [MH24], likelihood distributions with MLS22, CMS19, MH13 EOS at 1.0× solar but here slightly offset from 1.0: [MB22], same with CMS19 and CD21 EOS at 1.3× solar but slightly offset from 1.3: [HG23]. The intense bluish color indicates a high likelihood, while a pale or white color indicates a low likelihood. References: Gal = M. H. Wong et al. (2004), Gu22 = P. Gupta et al. (2022), Li20 = C. Li et al. (2020), Li24 = C. Li et al. (2024), Ca23 = T. Cavalié et al. (2023), Ca24 = T. Cavalié et al. (2024), MH24 = B. Militzer & W. B. Hubbard (2024), HG23 = S. Howard et al. (2023a), MB22 = Y. Miguel et al. (2022), MLS20 = S. Mazevet et al. (2022), N17 = N. Nettelmann (2017), NM21 = N. Nettelmann et al. (2021).
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Relative density differences (in %) at Jupiter’s 2 Mbar level between H/He P–T profiles with and without an OSL for different destabilizing He-depletion levels (color code). The bottom axis shows the pressure interval where the OSL is assumed to occur. The decrease in density is strongest if the OSL is placed at about 1 kbar (0.1 GPa), where the thermal expansion coefficient αT (black line for protosolar Y = 0.27, orange line for Y = 0.16) is high, while if placed at the dip of αT, the density at 2 Mbar increases dramatically.
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Illustration of the Jupiter layered structure model with an inverted He gradient ΔY < 0 across the OSL. The heavy element mass abundance Zdeep underneath PZ is shown with a gradient, although most models are computed with constant Zdeep and only a few models with a Gaussian gradient. Zatm extends from the 1 bar level either down to PZ as illustrated, or in models with an additional inverted Z gradient only to the top of the OSL. The He gradient in the He-rain zone is illustrated here to begin shallow and then be linear, while in the model computations we make a sharp transition at PHe. The radial positions of the layers are not to scale.
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Preferred Jupiter models with 1× solar in the atmosphere. As input, these models have an inverted He gradient dY = −0.07, PHe = 2.5 Mbar, T1 bar = 170 K, and PZ as given by the color code. A dilute core is possible with a substantial (factor of 5) increase in the heavy elements, in which case this strongly enriched region is confined to the very deep interior (0.2 MJ).
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Compilation of absolute wind velocity corrections and dynamical contributions to J6 (×106) that would bring the model values into agreement with the observed values. Gray vertical bar: observational uncertainty as in Figure 8; red ellipse: J6 model results from this work (Ne24) placed at Δvwind = 10 m s−1, and model results from N. Nettelmann et al. (2021), which led to a deviation from the observed winds by ≲15 m s−1; blue ellipse: ensemble of solutions in B. Militzer et al. (2022); green horizontal bar: wind modifications that are needed to bring the dynamical heights inferred from the zonal winds and Juno gravity data into agreement with the dynamical heights inferred from the Pioneer and Voyager occultation radii (E. Galanti et al. 2023).
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Nusselt number of particle transport in the regime of fingering double-diffusive convection according to the fit formula of J. Brown et al. (2013) for the three values of Rρ = 1 (red), Rρ = Rcrit (blue), and our choice for the OSL, Rρ = 1.11 (violet). Computation of Nuμ and Rcrit involves knowledge of thermophysical properties, which depend on pressure (x-axis) and temperature. On the right-hand y-axis, we plot Rcrit, which apparently adopts values between 1.5 and 2.5 across the OSL (0.1–2 GPa).
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Core mass and J6 values of models with an inverted He gradient (dots) and an additional inverted Z gradient (stars). As in Figure 4, open stars show models where Z3 ≲ 1× solar while pattern-filled stars show models with Z3 ≳ 1× solar. The vertical gray bar indicates the Juno measurement of J6. The level of additional He depletion ΔY in L3 with respect to YGal is indicated by the color code, with yellow indicating the strongest possible depletion.
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Atmospheric Z (right panel) and deep interior Z (left panel) of Jupiter models with an inverted He gradient ΔY≤0 (x-axis) across the OSL and different values of PHe (color code) as well as of PZ. Horizontal gray dashed lines indicate levels of enrichment over a solar Z⊙ = 0.015. Star symbols indicate models with an additional inverted Z gradient; among those, open stars show models where Z3 ≲ 1× solar while pattern-filled stars show models with Z3 ≳ 1× solar.
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: Diffusion of He through the OSL under simplified assumptions. Top panel: He-abundance profile at the present time for various enhancements fenh (color code) of the constant He diffusivity DHe; bottom panel: He-abundance profiles over time (color code) for DHe enhanced by a factor of 50 and assuming a linear decrease of Y(t) with time at the bottom of the OSL. The black symbol denotes YGal at the present time.
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: The same as Figure 5 but for selected models of 3× solar Z in the atmosphere. As input, the models have an inverted He gradient (dY = −0.08), an inverted Z gradient, PHe = 2.5 Mbar, T1 bar = 170 K, and PZ as given by the color code.
Paper: Jupiter’s Interior with an Inverted Helium Gradient
Authors: N. Nettelmann, J. J. Fortney
Figure caption: The same as Figure 5 but for selected models with 2× solar Z in the atmosphere. As input, the models have an inverted He gradient (dY = −0.09), PHe = 3 Mbar, T1 bar = 170 K, and PZ as given by the color code.