adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroid Collisions: Expected Visibility and Rate
Authors: Eran O. Ofek, David Polishook, Doron Kushnir, Guy Nir, Sagi Ben-Ami, Yossi Shvartzvald, Nora L. Strotjohann, Enrico Segre, Arie Blumenzweig, Michael Engel, Dennis Bodewits, John W. Noonan
Figure caption: The time-stretched light curve of the Dimorphos–DART impact shifted to a distance of 1 au from the observer, 1 au from the Sun and a phase angle of 53.3°. The time stretch is applied to account for the time it takes the flux to get out of the photometric aperture. See the text for details.
Paper: Asteroid Collisions: Expected Visibility and Rate
Authors: Eran O. Ofek, David Polishook, Doron Kushnir, Guy Nir, Sagi Ben-Ami, Yossi Shvartzvald, Nora L. Strotjohann, Enrico Segre, Arie Blumenzweig, Michael Engel, Dennis Bodewits, John W. Noonan
Figure caption: The normalized magnitude distribution of the expected DART-like impacts in the main belt, with Sun–observer–asteroid angle larger than 50°. The dashed lines show the limiting magnitude of the LAST epoch (20 s exposure), LAST visit (20 × 20 s exposure), and the Large Survey of Space and Time (LSST; Ivezić et al. 2019) single image. The fraction of events brighter than the limiting magnitude is given in parentheses. These fractions are already multiplied by the fraction of the asteroid with a Sun–observer–asteroid angle larger than 50° (0.63).
Paper: Asteroid Collisions: Expected Visibility and Rate
Authors: Eran O. Ofek, David Polishook, Doron Kushnir, Guy Nir, Sagi Ben-Ami, Yossi Shvartzvald, Nora L. Strotjohann, Enrico Segre, Arie Blumenzweig, Michael Engel, Dennis Bodewits, John W. Noonan
Figure caption: The probability distribution of the Sun–observer–target angle (elongation) for events brighter than magnitude 19.6 (blue line), 21.0 (magenta line), and 24.5 (yellow line). The drop near 180° is due to the nonzero ecliptic latitude of asteroids.
Paper: Asteroid Collisions: Expected Visibility and Rate
Authors: Eran O. Ofek, David Polishook, Doron Kushnir, Guy Nir, Sagi Ben-Ami, Yossi Shvartzvald, Nora L. Strotjohann, Enrico Segre, Arie Blumenzweig, Michael Engel, Dennis Bodewits, John W. Noonan
Figure caption: The magnitude vs. Δ of expected DART-like impacts in the main belt, which have Sun–observer–asteroid angles larger than 50°. Asteroids with constant Heliocentric distance (r) of 1.5, 2.5, and 3.5 au are marked in red.
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption: Mixing ratios of notable carbon- and oxygen-bearing molecules in chemical equilibrium, as predicted by FastChem 2 (Stock et al. 2018; Stocket al. 2022), compared to retrieved abundances (Section 5.2). The chemical equilibrium models are calculated for a solar metallicity with a uniform temperature profile of 1411 K, the equilibrium temperature of HIP 65Ab. The solid lines are the mixing ratios for a model with solar C/O, while the dashed lines represent a C/O of 1. The retrieved H2O and CO abundances are illustrated with their 1σ uncertainties. The other abundance constraints are shown as their 3σ upper limits. All shown molecules are included in our analysis, with the exception of OH, which is never expected to have measurable abundances at the pressures probed. The retrieved CO is slightly underabundant compared to equilibrium models. The H2O is also depleted relative to these solar abundance model predictions. SiO is poorly constrained due to it having almost no opacity in the IGRINS bandpass. Overall, our results are consistent with HIP 65Ab having a subsolar metallicity, and show a preference toward a supersolar C/O.
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption: Evolution of the cross-correlation detection strength as a function of number of principal components removed for both the real signal, and 200 injected samples. The orange line represents the detection of the real signal from HIP 65Ab observed in the data for different number of removed principal components. Each gray line represents an injection-recovery test (black line=the average), where we inject an atmospheric model at random orbital parameters away from the expected signal in K  p –V sys space and measure the strength at those parameters as a function of components removed. The strength of the injected model was calibrated to roughly match the real signal line. Both the real signal and the injected signal exhibit similar behavior when varying the number of principal components removed. In all cases, at least two principal components need to be removed to well-reveal the planetary signal, which then remains persistent up to at least 10 components removed. In our final analysis, we opted to remove three components.
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption: Overview of the data detrending steps applied to the observed 3.5 hr IGRINS spectroscopic time series targeting HIP 65Ab’s dayside atmosphere. (a) The extracted data from the IGRINS pipeline of an example spectral order in the K band. (b) The same data, but continuum alignment. (c) After the fitted median spectra is removed from each exposure. (d) With three principal components removed and noisy spectral channels masked. This last panel is fed to the cross-correlation and retrieval frameworks. The applied steps help remove undesirable telluric and stellar contributions, leaving behind the underlying planetary signal buried in noise.
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption: To scale diagram of the phase cover of our HIP 65Ab observations. The phase covered is from ϕ = 0.57 to 0.717 where ϕ = 0 is the center of the transit and ϕ = 0.5 is the middle of the secondary eclipse. The 3.5 hr observation used in this analysis is of the post-eclipse (western) dayside of HIP 65Ab.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Predicted C/O ratio of ROXs 42B b as a function of the final atmospheric metallicity and the carbon abundance of the gas accreted by the planet, assuming formation outside the CO snow line. Our derived metallicity constraints from our high-resolution fits are shown as white lines.
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: Comparison of the literature standard abundance tables of Fe, O, and S with the values of this work derived from FUV and X-ray observations presented in Table 5. The log(O/Ne) ratio is the sum of the predicted O I abundance that we obtain from a simultaneous X-ray and FUV fit and the solid-phase oxygen. For the log(Fe/Ne) ratio, we used the combined contribution of solid iron and atomic Fe II. Please note that the log(S/Ne) ratio comes from the S II value only resulting from the FUV fit. The Ne abundance is determined through the fit of the Ne K-edge in the X-ray spectrum from Psaradaki et al. (2023); in particular, it represents the summed abundance of Ne I, Ne II, and Ne III.
Paper: Elemental Abundances in the Diffuse Interstellar Medium from Joint Far-ultraviolet and X-Ray Spectroscopy: Iron, Oxygen, Carbon, and Sulfur
Authors: I. Psaradaki, L. Corrales, J. Werk, A. G. Jensen, E. Costantini, M. Mehdipour, R. Cilley, N. Schulz, J. Kaastra, J. A. García, L. Valencic, T. Kallman, F. Paerels
Figure caption: Comparison between the X-ray atomic database of SPEX (red) and Schippers et al. (2021; black) for Fe I, Fe II, Fe III, and Fe IV. The Fe I, Fe II, and Fe IV data in Schippers et al. (2021) have been taken from Richter et al. (2004), Schippers et al. (2017), and Beerwerth et al. (2019), respectively.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of X-complex asteroids selected as heterogeneous candidates in this study. Visible spectrophotometric and spectroscopic data were taken from Zellner et al. (1985), Bus & Binzel (2002), Sergeyev et al. (2022), and Gaia Collaboration et al. (2023). Data of Sergeyev & Carry (2021) were also used in the case of few visible spectral data. The green and yellow error bars represent the observational uncertainty of Marsset et al. (2020b). They are shown for the two most extreme spectra (Section 5). Different colors are used only for better readability. The black arrows show the slope uncertainty centered at the reflectance value of the spectra at 2.40 μm, as marked by the black dashed lines.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: The absolute differences ∣I ext,starry − I full∣ and ﹩| {I}_{\mathrm{ext},\cos \xi \cos {\theta }^{{\prime} }}-{I}_{\mathrm{full}}| ﹩ for three exoplanets are shown at the substellar point. From top to bottom, the exoplanets are KELT-9 b, Kepler-91 b, and Trappist-1 d. The dashed line and dotted–dashed line show the average values of ∣I ext,starry − I full∣ and ﹩| {I}_{\mathrm{ext},\cos \xi \cos {\theta }^{{\prime} }}-{I}_{\mathrm{full}}| ﹩, respectively. Odd values of N are plotted with unfilled markers, and even values with filled markers. Note that all of the averages are nonzero, but they approach zero for larger star–planet separations. Both models demonstrate a “wiggle” of the absolute error. I ext,starry performs better for large star–planet separations for which the host star is more point-like.
Paper: Hyper Illumination of Exoplanets: Analytical and Numerical Approaches
Authors: Jennifer L. Carter, Risinie D. Perera, M. J. Way
Figure caption: Shown are intensity calculations using I ext,starry and ﹩{I}_{\mathrm{ext},\cos \xi \cos {\theta }^{{\prime} }}﹩ along the intensity equator for three exoplanets and varying the numbers of source points N. Included for reference is the analytically determined values within the fully illuminated zone I full. See legend for line styles. From top to bottom, the exoplanets are KELT-9 b, Kepler-91 b, and Trappist-1 d. Within the fully illuminated zone, we see that ﹩{I}_{\mathrm{ext},\cos \xi \cos {\theta }^{{\prime} }}﹩ performs better than I ext,starry for the two hot Jupiter exoplanets. Both models perform well for Trappist-1 d, with I ext,starry matching better.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of S-complex V-, R-, and K-type asteroids identified as candidates for surface heterogeneity.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of A-type asteroids identified as candidates for surface heterogeneity. There are two types of graphs for 863 and 289: one where the scale of the vertical axis is similar to other graphs and one where the entire spectrum is shown.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of Ch/Cgh- and D-type asteroids identified as candidates for surface heterogeneity.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: This figure shows the spectral reddening of meteorite samples in response to laser bombardment as a function of the laser energy level. The vertical axis indicates the reflectance value of the bombarded sample at 2.4 μm after normalization of the spectrum to a value of 1 at 0.55 μm. The horizontal axis corresponds to the laser energy. Data for the olivine, L6 Chateau Renard meteorite, and CM2 Murchison meteorite were taken from Sasaki et al. (2001, 2003), Matsuoka et al. (2015, 2020), and Hasegawa et al. (2019). The olivine spectrum is on the verge of maturation after 150–300 mJ of laser irradiation. As an archetype of ordinary chondrites, we show the L6 Chateau Renard meteorite because there are a large number of data available for that meteorite. In the case of that meteorite, maturation is reached at an irradiation of 60–80 mJ. A multiplication factor was applied to the results obtained for the chip sample in order to match the results obtained for pellet samples. Data from the CM2 Murchison meteorite were used as carbonaceous chondrites. The spectrum of the Murchison meteorite is in a mature state after 5–10 mJ laser irradiation. The lime area indicates the distribution range of S-complex asteroids with confirmed heterogeneity. The observation uncertainty (gray star) is taken from Marsset et al. (2020b).
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Left panel: comparison between the spectra of 1 Ceres obtained in this study and the average spectrum from the DAWN spacecraft (de Sanctis et al. 2018). Middle panel: comparison between the sp06 spectrum of 1 Ceres obtained in this study and spectra of the Occator crater (De Sanctis et al. 2016). Five regions are located in the ∼90 km Occator crater on 1 Ceres. Spectra 5 and 1 correspond to the brightest area and dark floor in Occator, respectively. As the numbers in the spectrum become smaller, their reflectances are decreasing (e.g., absolute reflectance values of craters 5, 4, 3, 2, and 1 at 1.0 μm are 0.25, 0.13, 0.10, 0.05, and 0.03, respectively). Right panel: comparison between the sp06 spectrum of 1 Ceres obtained in this study and spectra of exposed water-rich areas (Combe et al. 2019).
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Fraction of heterogeneous candidates for each asteroid size and taxonomic type. We emphasize that nondetection does not necessarily imply intrinsic surface homogeneity. Hence, this fraction of heterogeneity candidates is a lower limit. The numbers in the parentheses above the graph indicate conservative heterogeneous candidates/optimistic+conservative heterogeneous candidates/total number.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Distribution of spectral slope variation at 2.4 μm in our data set. Pink: nondetection for surface heterogeneity (66 objects). Gray: optimistic candidates (52 objects). Yellow: conservative candidates (12 objects). Since optimistic candidates and noncandidates for surface heterogeneity are not determined using reflectance differences at 2.4 μm, the value of 1 on the abscissa is intentionally left out.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of B/C-type asteroids identified as candidates for surface heterogeneity.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of asteroids not identified as candidates for surface heterogeneity.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of asteroids observed multiple times with low S/N.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of unpublished asteroids in MITHMBAs observations.