adsabs/AstroCLIMB huggingface dataset:
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Comparison of emissivity spectra, normalized at their 15 μm emissivity peaks, of L-chondrite analog mixtures (from Bramble et al. 2021b) to Didymos. The finest fraction of the analog mixture is qualitatively similar to the Didymos spectrum across much of the wavelength range, though the asteroid emissivity features are generally muted longward of ∼8 μm. The lack of an emissivity drop longward of 8 μm in Didymos’ spectrum could be due to differences in porosity, hyperfine particles, or other physical causes vs. compositional ones. The coarsest fraction of the analog is a poor match across the wavelength range, and only the finest fraction shows a TF like Didymos does.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: MIRI spectrum of Didymos compared to the finest fraction of several OC meteorites from Bramble (2020) measured in simulated asteroidal conditions. The spectra are all qualitatively similar, though the Didymos spectrum has emissivity features near 10 and 17 μm not present in the OC spectra, and it has generally higher emissivity than them at λ > 9 μm. The position of the ∼15 μm peak is more consistent with the LL chondrites than the other chondrites, though the number of available comparison spectra is small.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: MIRI emissivity spectrum as calculated using the ATM (Section 4). The shaded area is affected by limitations in the JWST calibration, as discussed in the text, and the artifact position near 12.2 μm is shown. Also shown are the interpreted positions of the Christensen Feature (CF) and Reststrahlen bands (RF), and a possible location of Transparency Features (TF). The precise CF location is difficult to determine, given the observational uncertainties.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Didymos compared to Eros from Rivkin et al. (2018) and the low-albedo asteroid Winchester from Rivkin et al. (2022). Eros has a discernible absorption in the 3 μm region, interpreted as due to hydrated minerals with an estimated concentration of a few hundred ppm of hydrogen. The uncertainties on the Eros spectrum are smaller than the data points when they are not seen. Didymos shows no indication of an absorption in this region, consistent with an anhydrous surface. Because the scatter is large enough to encompass the Eros spectrum, we suggest that a possible upper limit on hydration on Didymos is similarly a few hundred ppm of water.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Comparison of Didymos NIRSpec data and XSHOOTER data from 2022 September 27 (de León et al. 2023, in preparation), scaled to match at 1.5 μm. The overall agreement is excellent. The uncertainties in the NIRSpec data are not well-represented by the formal error bars, which are smaller than the data points, but they are better represented by the point-to-point scatter. Also shown are the average S-class and Q-class asteroids from DeMeo et al. (2009). Didymos is best matched by the S-class spectrum.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: 7–20 μm spectra of Didymos and OC-relevant minerals. The minerals were taken from the RELAB database and measured in reflectance, and (1-reflectance) is plotted for them. The most prominent features in Didymos’ emissivity spectrum fall at wavelengths where features can be found in olivine, (low-Ca) pyroxene, or diopside. Features near 10 and 17.5 μm seen in Didymos’ spectrum but not the OC spectra in Figure 11 are consistent with olivine.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Comparison of the NIRSpec data to RELAB spectra of Chelyabinsk (Jenniskens PI), normalized to 1.5 μm. Didymos is a closer match to the powdered light-colored lithology of Chelyabinsk than a chip of the light-colored lithology or either of the dark lithology spectra, suggesting cm-sized particles and shock-darkened regions are not important contributors to the overall reflectance spectrum at hemispheric scales in the Didymos system.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: The thermal inertia of Didymos (open and closed red circles) is similar to that of other measured thermal inertias for asteroids <5 km in diameter. There does not appear to be a compositional dependence on thermal inertia that can be discerned from this sample. The data for asteroids other than Didymos were compiled from the literature by MacLennan & Emery (2021), with original citations found in that work.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Spectral energy distribution for Didymos from MIRI compared to the best-fit ATM. The shaded region covers Channel 4 of MIRI, which currently has some unresolved calibration problems.
Paper: Detectability of the Yarkovsky Effect in the Main Belt
Authors: Denise Hung, David J. Tholen, Davide Farnocchia, Federica Spoto
Figure caption: The A 2 uncertainty as a function of observational arc length L and asteroid semimajor axis a. With the semimajor axis fixed in the left panel, the arc length L and A 2 uncertainty A 2,unc follow a power law. With the arc length fixed in the right panel, a and A 2,unc follow an exponential function. Note that the A 2 uncertainty decreases as the arc length increases from 10 to 200 yr in 10 yr steps, but we only include four arc lengths in the legend for the purpose of brevity. The fitted lines are plotted from our two-dimensional fit, f(L, a) = k10 c(a−2.6) L  α , where the values of the coefficients are k = 1.852 × 105, c = 0.556, and α = −2.488.
Paper: Detectability of the Yarkovsky Effect in the Main Belt
Authors: Denise Hung, David J. Tholen, Davide Farnocchia, Federica Spoto
Figure caption: We compare the observational arc lengths of our observed sample of MBAs with the minimum arc lengths needed for a Yarkovsky detection. The dashed line shows where the two axes are equal. The error bars on the minimum arc lengths are based on the error bars on the predicted A 2 values derived from our TPM fitting as described in Section 3.1. They are best taken strictly as lower limits due to the caveats described in Section 6.2. None of our observed asteroids have long enough arcs to meet the threshold for Yarkovsky detection.
Paper: Detectability of the Yarkovsky Effect in the Main Belt
Authors: Denise Hung, David J. Tholen, Davide Farnocchia, Federica Spoto
Figure caption:  A 2 fitted by orbit determination for our sample of 134 MBAs, one Mars-crosser, and two NEAs plotted in terms of the S/N and indicator parameter ﹩{ \mathcal S }﹩. We define the A 2 to be valid if it has both S/N > 3 and ﹩{ \mathcal S }\leqslant 2﹩. All of our MBAs fall outside of this range, while the two NEAs are our only valid detections. Notably, the two NEAs are also the only asteroids in our sample with a previously found A 2 in the literature.
Paper: Detectability of the Yarkovsky Effect in the Main Belt
Authors: Denise Hung, David J. Tholen, Davide Farnocchia, Federica Spoto
Figure caption: The diameters of the nearly 2000 MBAs thermophysically modeled in Hung et al. (2022) plotted against the absolute values of their predicted A 2, which was estimated from their derived parameters. The scaling relation from Equation (9) using the values of Bennu produces consistently higher expected A 2 values than predicted, but we see better agreement if we reduce the relation by a factor of 3.
Paper: Detectability of the Yarkovsky Effect in the Main Belt
Authors: Denise Hung, David J. Tholen, Davide Farnocchia, Federica Spoto
Figure caption: Semimajor axes, eccentricities, and inclinations of our 134 MBA targets. The vertical lines in semimajor axis are drawn at the boundaries of the inner (a < 2.0 au), central (2.0 au < a < 3.2 au), and outer (3.2 au < a < 4.6 au) main belt regions. Nearly all of our observed MBAs fall within the central main belt region.
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: Analyses of the silicate feature ratios of 10 μm to 19 μm. (a) ζ vs. λ 9P/Tempel 1 (20050702.52). For 9P/Tempel 1, we define ζ model = (F  λ,total − F(ac))/F(ac) and ζ observed = (F  λ,observed − F(ac))/F(ac). ζ(10) is the flux averaged over Δλ = 2 μm centered at 10.3μm, and ζ(19) uses Δλ = 2 μm centered at 19.02 μm. (b) Silicate feature ratios of 19 μm to 10 μm vs. a  p . The models’ silicate feature ratio 19 μm to 10 μm ([ζ(19)/ζ(10)]model) is dependent upon the grain size distribution peak grain size a  p . However, [ζ(19)/ζ(10)]observed/[ζ(19)/ζ(10)]model is independent of a  p . (c) [ζ(19)/ζ(10)]observed/[ζ(19)/ζ(10)]model vs. λ HM 10μm rise observed. A linear regression using the python statsmodels linregress (Seabold & Perktold 2010) yields a slope of 0.350 ± 0.170, intercept of −2.109 ± 1.462, and p-value of 0.05. A firm correlation requires a p-value of ≤0.007 (97.3% probability of the failure of the null hypothesis of a zero-valued slope), so the p-value of 5% indicates that there is only 95% confidence that this non-zero-valued slope represents a correlation.
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: The derived silicate crystalline mass fraction, f cryst. Filled red circles are OCCs, and filled green circles are JFCs, where each point represents the average values over all observations for the parameter f cryst if multiple observations of the same comet were obtained. The vertical bars represent the range of f cryst within the 95% confidence interval.
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: Atomic carbon-to-silicate ratio vs. f cryst for the comet spectra in our sample. JFCs (short period) are shown in blue and OCCs (long period) in orange. (a) All comet spectra in the survey. (b) Comet spectra where f cryst is constrained to the 95% confidence level.
Paper: Effects of Airless Bodies’ Regolith Structures and of the Solar Wind’s Properties on the Backscattered Energetic Neutral Atoms Flux
Authors: S. Verkercke, J.-Y. Chaufray, F. Leblanc, E. M. Bringa, D. Tramontina, L. Morrissey, A. Woodson
Figure caption: Left: field of view of the CENA instrument mapped on the lunar surface. The red and blue colored bands show the seven channels of the field of view (FOV), which is within the sphere of the lunar surface at the equator, and the spacecraft trajectory is shown in green. Right: projection of the FOV of each channel on the lunar surface at the subsolar point as reported by Bhardwaj et al. (2005).
Paper: Effects of Airless Bodies’ Regolith Structures and of the Solar Wind’s Properties on the Backscattered Energetic Neutral Atoms Flux
Authors: S. Verkercke, J.-Y. Chaufray, F. Leblanc, E. M. Bringa, D. Tramontina, L. Morrissey, A. Woodson
Figure caption: Angular distribution maps for reflected H ENA of a flat surface as predicted by MD for SZA 0° (right) and 80° (left).
Paper: Effects of Airless Bodies’ Regolith Structures and of the Solar Wind’s Properties on the Backscattered Energetic Neutral Atoms Flux
Authors: S. Verkercke, J.-Y. Chaufray, F. Leblanc, E. M. Bringa, D. Tramontina, L. Morrissey, A. Woodson
Figure caption: Reflection coefficient as a function of SZA. The blue, red, and orange solid curves correspond, respectively, to regoliths with porosities of 0.55 (Figure 1(a)), 0.71, and 0.85 (Figure 1(b)). The blue and red regoliths are composed of 50 and 10 μm grains, respectively, with a surface energy γ = 0.025 J m−2, while the orange regolith is composed of 50 μm grains with a surface energy of 1.5 J m−2. The blue and orange dashed curves are the reflection coefficients retrieved by Szabo et al. (2022) for regoliths of porosities 0.55 and 0.83, respectively. The numbers in brackets correspond to the numbers in Figure 3. The black solid and dashed lines represent, respectively, the reflection coefficient dependency on SZA for a flat surface as predicted by MD (Leblanc et al. 2023) and SDTrimSP (Szabo et al. 2022). The observed reflection coefficients derived from CENA observations by Vorburger et al. (2013) are also plotted in gray. The error bars on the solid curves are based on the standard deviation of the reflection coefficient of protons launched from different random initial conditions.
Paper: Effects of Airless Bodies’ Regolith Structures and of the Solar Wind’s Properties on the Backscattered Energetic Neutral Atoms Flux
Authors: S. Verkercke, J.-Y. Chaufray, F. Leblanc, E. M. Bringa, D. Tramontina, L. Morrissey, A. Woodson
Figure caption: Graphic representation of slices of regolith models created with LAMMPS while using a JKR contact model with γ = 0.025 J m−2 (a) and γ = 1.5 J m−2 (b). Both are formed of 50 μm grains. The brighter grains are closer to the simulation box sides, while the darker ones are occluded by surrounding grains. The simulation box is represented in black.
Paper: Effects of Airless Bodies’ Regolith Structures and of the Solar Wind’s Properties on the Backscattered Energetic Neutral Atoms Flux
Authors: S. Verkercke, J.-Y. Chaufray, F. Leblanc, E. M. Bringa, D. Tramontina, L. Morrissey, A. Woodson
Figure caption: Reflection coefficient as a function of the regoliths’ roughness ratio at (left) SZA 0° and (right) SZA 70°. The numbers in brackets correspond to the regoliths of Figure 2. The stars serve as indicators in Section 3.2. The error bars are based on the standard deviation of the reflection coefficient of protons launched from different random initial conditions. The different colors stand for the different types of grains composing the regoliths. The “hexagonal lattice” regoliths were created based on a hexagonal lattice to achieve compact packing.
Paper: Effects of Airless Bodies’ Regolith Structures and of the Solar Wind’s Properties on the Backscattered Energetic Neutral Atoms Flux
Authors: S. Verkercke, J.-Y. Chaufray, F. Leblanc, E. M. Bringa, D. Tramontina, L. Morrissey, A. Woodson
Figure caption: Sunward vs. antisunward fluxes ratio as a function of the average roughness evaluated for multiple regolith structures at SZA 20° (a) and 80° (b). Normalized angular distribution maps for two extreme regolith structures at SZA 20° (c) and (d), and at SZA 80° (e) and (f). The bottom half of each map represents the sunward direction hemisphere and the upper half the antisunward hemisphere. The error bars are based on the standard deviation of the ratios of protons launched from different random initial conditions.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Earth thermal infrared spectrum from MGS-TES (Christensen & Pearl 1997) trimmed to 7–40 μm, as described in text. Adopted error bars are constant in wavelength and yield S/N of 20 at 10 μm. Forward model spread from retrieval analysis is shown as darker and lighter swaths for 16th–84th and 5th–95th percentiles, respectively.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Photometric (below 1 μm) and spectroscopic (above 1 μm) reflected light observation of Earth from NASA’s EPOXI mission, rotationally averaged from the 2008 March 18–19 data set (Livengood et al. 2011). Simulated wavelength-independent error bars yielding a V-band S/N of 20 are indicated, and only every fifth error bar is shown for spectroscopic data for clarity. Forward model spread from retrieval analysis is shown as darker and lighter swaths for 16th–84th and 5th–95th percentiles, respectively.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Simulated spectrum of an exo-Earth orbiting a solar twin at characteristic HabEx/LUVOIR spectral coverage and resolving power (ultraviolet [0.2–0.4 μm], visible [0.4–1.0 μm], and near-infrared [1.0–1.8 μm] at a resolving power of 7, 140, and 70, respectively). Gas spectral impacts are indicated by showing sensitivity to mixing ratio changes for key species. For the sensitivity test, and relative to fiducial values, the water vapor and ozone mixing ratios were halved, the molecular oxygen mixing ratios were doubled, and the carbon dioxide and methane mixing ratios were increased by a factor of 5.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Constraints on key atmospheric species for three different HabEx/LUVOIR-like observing scenarios where spectral coverage and S/N are traded. One scenario has S/N of 20 across the ultraviolet, optical, and near-infrared bands, a second scenario has optical-only coverage at an enhanced S/N of 35, and a third has a reduced optical S/N of 10 and an enhanced near-infrared S/N of 45.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Two-dimensional histograms of thermal structure models randomly selected from retrievals on MGS-TES Earth observations. Standard Earth thermal structures from McClatchey et al. (1972) are shown as gray lines. The left panel is from a retrieval with a three-parameter thermal structure model (power-law troposphere profile and isothermal stratosphere), while the right panel is from a retrieval with a four-parameter thermal structure model (power laws in both the troposphere and stratosphere).
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Gas mixing ratio constraints from retrievals performed on EPOXI observations of Earth degraded to V-band S/N of 10 (filled) and 20 (unfilled). Gases are represented with different colors, and vertical lines indicate known “truth” values. At S/N = 10, gas posteriors include a peak near a realistic value and a second, unrealistic peak due to an inability to rule out solutions with a deep atmosphere.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Visualized posterior distribution for 11 parameters from the rfast tool when retrieving on the simulated observations in Figure 7. One-dimensional marginal distributions are shown along the diagonal, with associated 16th/50th/84th percentile values indicated above. Values used to generate the faux observation (i.e., “truth” values) are indicated as orange vertical and horizontal lines.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Correlation between inferred cloud coverage fraction and surface pressure for retrievals performed on EPOXI data at S/N = 10. Two classes of solutions emerge: one with realistic surface pressures (horizontal line) and cloud coverages, and another with a deep atmosphere and near-global coverage of modest-thickness clouds.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Gas mixing ratio constraints from retrievals performed on the MGS/TES observations of Earth shown in Figure 14. Gases are represented with different colors, and vertical lines indicate known “truth” values.