adsabs/AstroCLIMB huggingface dataset:
Paper: Catalog of Ultraviolet Bright Stars: Strategies for UV Occultation Measurements, Planetary Illumination Modeling, and Sky Map Analyses Using Hybrid IUE-Kurucz Spectra
Authors: Michael A. Velez, Kurt D. Retherford, Vincent Hue, Joshua A. Kammer, Tracy M. Becker, G. Randall Gladstone, Michael W. Davis, Thomas K. Greathouse, Philippa M. Molyneux, Shawn M. Brooks, Ujjwal Raut, Maarten H. Versteeg
Figure caption: (a) Comparison of IUE (blue), Juno-UVS (red), and Kurucz (green) spectra for HD 78548. The gray lines are the total data for both IUE and Juno-UVS with the colored lines being the averages. The dashed lines are the cutoff of 130–175 nm used for the confidence factors. It should be noted that Juno-UVS is experiencing a localized gain loss at Lyα (gain sag), an effect previously documented (Hue et al. 2019). This is one of many examples showing how effective the Kurucz models can be to construct CUBS spectra. (b) Histogram of quality ranking [0, 10] for all IUE stars in CUBS based on the relative difference (RD) between IUE and Kurucz spectra between 130 and 175 nm. (c) Histogram of quality ranking [0, 10] for all IUE stars in CUBS based on the S/N of IUE spectra between 130 and 175 nm.
Paper: Catalog of Ultraviolet Bright Stars: Strategies for UV Occultation Measurements, Planetary Illumination Modeling, and Sky Map Analyses Using Hybrid IUE-Kurucz Spectra
Authors: Michael A. Velez, Kurt D. Retherford, Vincent Hue, Joshua A. Kammer, Tracy M. Becker, G. Randall Gladstone, Michael W. Davis, Thomas K. Greathouse, Philippa M. Molyneux, Shawn M. Brooks, Ujjwal Raut, Maarten H. Versteeg
Figure caption: Example spectra from CUBS with both the flux of the star (black) and the estimated count rate (blue) as expected to be viewed by Europa-UVS. IUE data are used between 116 and 196 nm, and a Kurucz model is used between 50–116 and 196–210 nm.
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: Raw FTICR spectra obtained for WS with LDI+ (top), ESI− (middle), and LDI+ postextraction (bottom). The scale has been chosen to allow comparison of the main distributions but cuts off some large intensity peaks (mostly fatty acid contaminants in the ESI− spectrum). The repetitive peaks above m/z 800 in the LDI+ spectra are fullerenes, which are a by-product of the LDI process (this includes the large peak at 720, which is C60).
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: Cation LILBID mass spectra of p-toluene sulfonic acid, recorded at a concentration of 0.05 mol L−1 in a pure water matrix, simulating the mass spectra of SUDA on board the Europa Clipper.
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: WAr sample: DBE vs. number of carbon atoms (#C) in the formula for all annotations in a sample (top) and only S-bearing compounds (bottom), LDI+ analysis (left), ESI− (middle), and LDI+ after extraction. Note: while dot size relates to the intensity of the formula, S-bearing compounds for the LDI+ analysis (bottom left, bottom right) have been enlarged for visibility.
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: Example of blanks. Top: LDI+ blanks, obtained with laser shots aimed at the sample-free part of the window. Bottom: blank obtained with methanol that was deposited on a MgF2 window on which tape (that was used to hold the sample windows in the LDI cell) was applied and removed.
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: Error (in ppm) vs. m/z graph for WS (left) and WAr (right), with LDI+ (top), ESI− (middle), and LDI+ after extraction (bottom).
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Reflectance spectra of Jovian irregular satellites in the JVI Himalia prograde (i = 28°) cluster: JVI Himalia, JVII Elara (in 2006), JVII Elara (in 2009), and JX Lysithea. The absolute values are determined by scaling the average value of the relative reflectance across a 100 Å spectral width around 0.55 μm by the NEOWISE geometric albedo (Table 3; Grav et al. 2015; Mainzer et al. 2016). The best indication of the quality of the spectrum is the peak-to-peak scatter within a spectrum. Red bars beneath each spectrum mark the spectral beginning (lower wavelength) and ending (higher wavelength) of the 0.7 and 0.43 μm features for the C-complex asteroids as shown by the spectrum of 19 Fortuna as a proxy (Figure 5).
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Panel (A): the heliocentric distance scaling of the collisional mass-production rate M + for Scenario A, where the total m loss = 430.6 kg s−1 for the best-fit parameters. The dashed orange line shows the PSP measurements derived from Szalay et al. (2021). The four realizations of our collisional model for JFCs are shown in color-coded solid lines: our preferred model A  s  = 5 × 105 J kg−1 (blue), 3× stronger particles A  s  = 1.5 × 106 (green) J kg−1, 200× stronger particles A  s  = 108 J kg−1 (yellow), and 1000× weaker particles A  s  = 300 J kg−1 (gray). We also show the theoretically predicted scaling of M + based on brightness observations of the Zodiacal Cloud with a slope α = −3.33 (dashed black line). Our preferred model shows a good match to PSP measurements as well as the predicted slope down to heliocentric distance of 0.1 au, where the effects of the dust depletion zone near the Sun are evident. Panel (B): the same as Panel A but now for Scenario B, where the total mass loss is m loss = 164.5 kg s−1 for the best-fit parameters. In Scenario B, we assumed a smaller total cross section of the Zodiacal Cloud and thus all models give smaller values of M +. Here, the 3× stronger particle model with A  s  = 1.5 × 106 J kg−1 underestimates M + compared to that derived from PSP measurements and provides an upper limit for A  s  in Scenario B.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Scenario B collisional lifetimes for D = 50 μm meteoroid. Panels (A)–(C) show the collisional lifetime in years for the full range of bound orbits; eccentricity 0 < e < 1, inclination 0 < I < 180°, where the color-coding represents logarithmically spaced collisional lifetime. Panel (A) is for a particle with semimajor axis a = 0.3 au, panel (B) for a = 1.0 au, and panel (C) for a = 3.0 au. Contours show boundaries between color-coded logarithmic steps. Panel (D) shows the ratio between collisional lifetimes in our model T coll and T coll(SE86) with ﹩{{ \mathcal F }}_{\mathrm{coll}}=20﹩ used in, for example, Pokorný et al. (2014, 2018), i.e., the color-coding shows ﹩{ \mathcal R }={T}_{\mathrm{coll}}/{T}_{\mathrm{coll}}(\mathrm{SE}86)﹩. The hatching shows areas within a factor of 1.78 of unity, i.e., ﹩{ \mathcal R }=0.56\mbox{--}1.78﹩. Our model provides ∼3× longer collisional lifetimes for meteoroids on low-e and low-I orbits and 1–2 orders of magnitude shorter collisional lifetimes for high-e and high-I orbits (dark blue regions).
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Panel (A): distribution of M + in the ecliptic plane in our preferred model in Scenario B. The plot shows the average M + within 0.025 au from the ecliptic plane. The value of M + in the ecliptic is radially symmetric in our model and decreases as ﹩{M}^{+}\propto {r}_{\mathrm{hel}}^{-3.83}﹩ between 0.1 < r hel < 1.0 au, which is steeper than the radially averaged value of M + shown in Figure 13. The color-coded contours show the order-of-magnitude increase in M +, where our model predicts 9 orders of magnitude difference between M + at r hel = 5 au and r hel = 0.1 au. Panel (B): the same as Panel (A) but now for a slice through the Y-axis, a side view of the JFC dust cloud, where the values of M + are averaged over 0.025 au away from the Y-axis in our model. Due to rotational symmetry these two images can be used to reconstruct the entire three-dimensional image of the distribution of M + in our JFC model.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: The same as Figure 6 but now for Scenario B assuming meteoroid binding energy close to that used in Grun et al. (1985), i.e., ﹩{{ \mathcal P }}_{{A}_{s}}=10﹩ (A  s  = 1000 J kg−1). Assuming much smaller A  s  than those providing best fit to our constraints leads to short dynamical lifetimes that prevent meteoroids detectable by CMOR to assume more circular orbits at semimajor axes close to 1 au. The SFD at 1 au is also affected by removal of meteoroids with diameters 100 < D < 1000 μm. The mass-accretion rate is at 37% of the best-fit value in Figure 6.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Estimated value of the collisional lifetime multiplier F coll for a particle with D = 50 μm and a full range of bound orbits phase space. We use the Grun et al. (1985) binding energy estimate A  s  = 300 J kg−1 and A  s  = 500,000 J kg−1 derived from our best-fit model to derive the value of F coll. For most of the orbital phase space the Grun et al. (1985) binding energy underestimates the collisional lifetimes by a factor of 40−100.
Paper: Catalog of Ultraviolet Bright Stars: Strategies for UV Occultation Measurements, Planetary Illumination Modeling, and Sky Map Analyses Using Hybrid IUE-Kurucz Spectra
Authors: Michael A. Velez, Kurt D. Retherford, Vincent Hue, Joshua A. Kammer, Tracy M. Becker, G. Randall Gladstone, Michael W. Davis, Thomas K. Greathouse, Philippa M. Molyneux, Shawn M. Brooks, Ujjwal Raut, Maarten H. Versteeg
Figure caption: Example (a) stellar occultation spectra and (b) transmission spectra from star HD 52089 showing how the stellar signal decreases in intensity at specific wavelengths related to the composition of a model for Europa’s atmosphere as the star gets closer to the surface (altitude Z TAN = 0 km) from the reference frame of the observing spacecraft. The gray region represents the 1σ uncertainty for the transmission spectra. (c) Absorption cross sections for key species in Europa’s atmosphere (O2, H2O, and C2H2) used in the present model (references shown in Table 1).
Paper: Catalog of Ultraviolet Bright Stars: Strategies for UV Occultation Measurements, Planetary Illumination Modeling, and Sky Map Analyses Using Hybrid IUE-Kurucz Spectra
Authors: Michael A. Velez, Kurt D. Retherford, Vincent Hue, Joshua A. Kammer, Tracy M. Becker, G. Randall Gladstone, Michael W. Davis, Thomas K. Greathouse, Philippa M. Molyneux, Shawn M. Brooks, Ujjwal Raut, Maarten H. Versteeg
Figure caption: (a) FUV sky map created using CUBS integrated from 115 to 210 nm. (b) EUV sky map integrated from 50 to 115 nm.
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: WS sample, LDI+ analysis (left) and ESI− (right). The top and middle figures show the DBE vs. number of carbon atoms (#C) in the formula for all annotations in a sample (top) and only S-bearing compounds (middle). The bottom figures show the number of oxygen atoms (#O) vs. the number of carbon atoms (#C). Note: dot size relates to the intensity of the formula in all graphs, but S-bearing compounds for the LDI+ analysis (middle left) have been enlarged for visibility.
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: FT-IR spectra of a 2:1 water:propane mixture layer: Top: comparison between the sample after deposition (black) and after 30 mn irradiation with S7+ ions (red). Bottom: comparison between the sample after deposition (black) and the spectrum of 15 similar layers, each individually irradiated with the 105 keV S7+ beam (red).
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: DBE vs. number of carbon atoms (#C) in the formula for all annotations (top) and only for S-bearing compounds (bottom). Note: while dot size relates to the intensity of the formula, S-bearing compounds have been enlarged for visibility.
Paper: Sulfur Implantation into Water Ice with Propane: Implications for Organic Chemistry on the Surface of Europa
Authors: Alexis Bouquet, Cíntia Aparecida Pires da Costa, Philippe Boduch, Hermann Rothard, Alicja Domaracka, Grégoire Danger, Isabelle Schmitz, Carlos Afonso, Philippe Schmitt-Kopplin, Vincent Hue, Tom A. Nordheim, Alexander Ruf, Fabrice Duvernay, Maryse Napoleoni, Nozair Khawaja, Frank Postberg, Thomas Javelle, Olivier Mousis, Laura Isabel Tenelanda Osorio
Figure caption: Evolution of the main features linked to CH4, CO2, and C–H bonds over the course of the irradiation of one layer of water:propane mixture with S7+ ions (left), compared to experiments with electrons (Hand & Carlson 2012; right, reproduced from the original paper).
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption: HBM framework. Hyperparameters are shown in blue, local parameters in white, and observed parameters in gray. The observed and local parameters always have N  p  members corresponding to the number of planets in the sample. N  c  = 1, 2, and 3 when the one-, two-, and three-population model is considered, respectively. Observed masses and density ratios are modeled as Gaussian random variables centered on their unknown true values (local parameters) with a standard deviation equal to their observational uncertainties (Equations (2) and (6), respectively). The local and hyperparameters are linked through the mixture model defined in Equation (5).
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption: Water grid (cyan) and reduced rock grid (black). The ρ scaled parameter corresponds to the density at mass of a water- and volatile-free rocky planet with a liquid pure-iron core and Fe-free silicate mantle with Fe/Mg = 0.71, Si/Mg = 0.79, Ca/Mg = 0.09, and Al/Mg = 0.07.
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption: Density ratio as a function of mass for our N  c  = 1 (left) and N  c  = 2 (right) models applied to the Luque & Pallé (2022) sample of small transiting planets in orbit around M dwarfs. We color code the highest-density population as green and the lowest-density population as purple. The planets are assigned the same color as the population to which they most likely belong. The solid lines are the isocomposition lines for each ﹩{\mu }_{\mathrm{comp}}^{j}﹩. The bands are the corresponding intrinsic density ratio scatter parameter ﹩{\sigma }_{{\rho }_{\mathrm{ratio},\mathrm{pop}}}^{j}﹩. For all ﹩{\mu }_{\mathrm{comp}}^{j}﹩ and ﹩{\sigma }_{{\rho }_{\mathrm{ratio},\mathrm{pop}}}^{j}﹩, we use the median values given in Table 3.
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption: Density ratio as a function of mass for the preferred N  c  = 1 model (left) and the N  c  = 2 model (right) applied to the Adibekyan et al. (2021) sample. We color code the highest-density population as green and the lowest-density population as purple. The planets are assigned the same color as the population to which they most likely belong. The solid lines are the isocomposition lines for each ﹩{\mu }_{\mathrm{comp}}^{j}﹩. The bands are the corresponding intrinsic density ratio scatter parameter ﹩{\sigma }_{{\rho }_{\mathrm{ratio},\mathrm{pop}}}^{j}﹩. For all ﹩{\mu }_{\mathrm{comp}}^{j}﹩ and ﹩{\sigma }_{{\rho }_{\mathrm{ratio},\mathrm{pop}}}^{j}﹩, we use the median values given in Table 4.
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption:  B 21 (left vertical axis) and n  σ  (right vertical axis) as a function of N  p  for average observational uncertainties of ﹩{\sigma }_{{M}_{p}}=5 \% ﹩ and ﹩{\sigma }_{{R}_{p}}=1 \% ﹩ (cyan), ﹩{\sigma }_{{M}_{p}}=6 \% ﹩ and ﹩{\sigma }_{{R}_{p}}=2 \% ﹩ (purple), and ﹩{\sigma }_{{M}_{p}}=10 \% ﹩ and ﹩{\sigma }_{{R}_{p}}=2.5 \% ﹩ (red).
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption: Summary of results for a synthetic 20-planet sample of planets with two populations: a Mercury-like one with ﹩{\mu }_{\mathrm{comp}}^{\mathrm{ml}}=0.7﹩ CMF and w ml = 0.25 and an Earth-like population with ﹩{\mu }_{\mathrm{comp}}^{\mathrm{el}}=0.325﹩ CMF and w el = 0.75.
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption: Hyperparameter posterior corner plot for the one-population model applied to our synthetic sample. The +/− values correspond to the 95% credible intervals. This figure was generated with the dynesty dynamic nested sampling software package (Speagle 2020).
Paper: A Gap in the Densities of Small Planets Orbiting M Dwarfs: Rigorous Statistical Confirmation Using the Open-source Code RhoPop 
Authors: J. G. Schulze, Ji Wang, 吉 王, J. A. Johnson, B. S. Gaudi, R. Rodriguez Martinez, C. T. Unterborn, W. R. Panero
Figure caption: Hyperparameter posterior corner plot for the two-population model applied to our synthetic sample. The +/− values correspond to the 95% credible intervals. This figure was generated with the dynesty dynamic nested sampling software package (Speagle 2020).
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: Plots illustrating the clustering of steep-sloped, unclassified asteroids in spectral slope and the IRPC space defined in DeMeo et al. (2009). Asteroids are plotted according to spectral slope and IRPC 2 (panel (a)), spectral slope and IRPC 3 (panel (b)), and IRPC 2 and IRPC 3 (panel (c)). Each asteroid’s Bus–DeMeo classification is represented by the shape of the plot marker, with unclassified asteroids shown with a “-” symbol. Asteroids observed in this paper are plotted in dark red, while asteroids from the original Bus–DeMeo sample (DeMeo et al. 2009) are plotted in semitransparent gray. The clustering of the unclassified asteroids in slope and principal component space suggests that this population of steeply sloped asteroids may represent a distinct taxonomic class not described in the Bus–DeMeo taxonomic system.
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: Distribution of orbital elements of all the asteroids presented in this work. Panel (a) shows the distribution of asteroids in semimajor axis (a, in au) and eccentricity (e) space, while panel (b) shows the distribution of asteroids in semimajor axis (a, in au) and inclination (i, in degrees) space. Asteroids with slopes exceeding the average spectral slope of the R-group Trojans in either the LDT or IRTF data are plotted in red as steep-sloped asteroids. Bus–DeMeo classifications for each asteroid are given by the shape of the marker. Osculating orbital elements were computed using the JPL Horizons ephemeris service for Julian Date 2460000.5.