adsabs/AstroCLIMB huggingface dataset:
Paper: The Debiased Compositional Distribution of MITHNEOS: Global Match between the Near-Earth and Main-belt Asteroid Populations, and Excess of D-type Near-Earth Objects
Authors: Michaël Marsset, Francesca E. DeMeo, Brian Burt, David Polishook, Richard P. Binzel, Mikael Granvik, Pierre Vernazza, Benoit Carry, Schelte J. Bus, Stephen M. Slivan, Cristina A. Thomas, Nicholas A. Moskovitz, and Andrew S. Rivkin
Figure caption: Observed vs. debiased compositional distribution of the MITHNEOS survey for the overall NEO population (top left) and individual escape/source regions. Regions are ordered by increasing distance from the Sun. Each percentage indicates the average probability for an NEO in our data set of originating from the source region. A total of 11 objects in our data set were not included in this plot owing to uncertain spectral classification (Section 2.2). This figure shows the compositional mixing of the NEO population and, therefore, of the asteroid belt at small object sizes, as well as the global trend of increasing dark-to-bright object ratio as a function of ER distance from the Sun.
Paper: The Debiased Compositional Distribution of MITHNEOS: Global Match between the Near-Earth and Main-belt Asteroid Populations, and Excess of D-type Near-Earth Objects
Authors: Michaël Marsset, Francesca E. DeMeo, Brian Burt, David Polishook, Richard P. Binzel, Mikael Granvik, Pierre Vernazza, Benoit Carry, Schelte J. Bus, Stephen M. Slivan, Cristina A. Thomas, Nicholas A. Moskovitz, and Andrew S. Rivkin
Figure caption: Observed (blue) and debiased (orange) fractional abundances of spectral classes of NEOs, compared to their predicted source populations in the asteroid belt (green). Escape regions are ordered by increasing distance from the Sun, and their name is indicated in the upper left corner of the panels. See Section 3.4 for a description of the selection criteria of the main-belt data sets. Carbonaceous C- and P-type objects were merged into a single class “C/P,” and silicate-rich S- and Q-type objects into “S/Q” (see Section 3.5). For these two broad classes, the plotted bars are divided into two shades of color, with the darker shade corresponding to C and S types and the lighter shade to P and Q types. The least populated taxonomic classes (A, K, L, E, and M types) are not displayed here for better readability. A second version of the figure including every taxonomic class is provided in Appendix C. This figure highlights the compositional match between NEOs and their predicted source regions after bias correction. The red arrows underline local composition differences discussed in Section 4.2.2.
Paper: The Debiased Compositional Distribution of MITHNEOS: Global Match between the Near-Earth and Main-belt Asteroid Populations, and Excess of D-type Near-Earth Objects
Authors: Michaël Marsset, Francesca E. DeMeo, Brian Burt, David Polishook, Richard P. Binzel, Mikael Granvik, Pierre Vernazza, Benoit Carry, Schelte J. Bus, Stephen M. Slivan, Cristina A. Thomas, Nicholas A. Moskovitz, and Andrew S. Rivkin
Figure caption: Same as Figure 4, but with the inclusion of the minor (least populated) taxonomic classes.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: The motion of Wolf 359. The first three images are from Digital Sky Survey taken in (a) 1953, (b) 1988, and (c) 1995, whereas the last image (d) was taken in 2020 as a part of this work, all shown with J2000 coordinates.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: Example images with Wolf 359 each marked with a red circle depicting the maximal photometric aperture size used in light-curve extraction: eight pixels for NOWT (left image), and nine pixels for TAOS (right image).
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: The NOWT light curves of Wolf 359 (in black) and of the two reference stars (in gray). Each flare event detected is marked by a vertical red line. The observations from April 23 to 27 were taken in the R band, whereas on April 28 and 29 they were in V. The sudden flux drop on April 27 around HJD 2458967.2 was due to weather conditions, manifest also in the reference light curves. The major event on 2020 April 26 detected also with TAOS was analyzed separately and not shown here.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: The major event detected on 2020 April 26 by both NOWT (in red) and TAOS (in blue). For each telescope, the measured instrumental magnitudes of Wolf 359 and of a comparison star are displayed to validate the variability. Typical photometric errors are about 0.01 mag so smaller than the sizes of the symbols.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: (a) Cumulative frequency (or occurrence timescale) distribution and (b) duration vs. flare energy of the Wolf 359 flares reported in this work. The dashed line in (a) is not meant for a fit but for illustration only because the data seem more complex than a linear fit.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: As in Figure 4 for the superflare observed in 2020 April 26, but now each light curve has been detrended and rescaled relative to the quiescent stellar brightness, in flux/count unit instead of magnitude. The horizontal segments mark the sampling function for NOWT (in red) and for TAOS (in blue), with the filled parts for exposure and open (or a dark bar for TAOS) for dead time intervals.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: The observed (filled symbols, NOWT in red and TAOS in blue) vs. computed (open symbols) light curves for (a) a single-exponential, (b) a double-exponential, (c) a power-law decay function with an instantaneous impulse rise, and (d) a power-law decay function with a finite-time rise (16 s). For each model, the analytic function is represented as a black curve, and the residuals (O − C, the observed minus the computed) are also shown. For (c) the peak amplitude is ΔF/F0 = 2.92, while in (d) it is ΔF/F0 = 1.63.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: Effect of observing cadence of a continuous (a) power-law, or (b) a double-exponential function.
Paper: Simultaneous Detection of Optical Flares of the Magnetically Active M-dwarf Wolf359
Authors: Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, and Wing Ip
Figure caption: The computed light curves of the intrinsic flare profile with a peak of 1.6 times of the stellar brightness (Figure 7(d)) sampled at a cadence of 20 s (in blue), 2 minutes (in orange), and 20 minutes (in green); (a) with a zero phase lag, or (b) with a 0.5 phase lag.
Paper: Scheduling Direct Imaging Observations Based on Radial Velocity Orbital Fits: Best Practices for Translating Orbits and Failure Modes
Authors: Corey Spohn, Dmitry Savransky, and Rhonda Morgan
Figure caption: Comparison of how the four different orbit construction methods (max KDE, max likelihood, credible interval, and multivariate Gaussian) perform at calculating the probability of detection at two different ratios of RV error to RV semiamplitude. The “True planet” line has a value of 1 when the defined planet is detectable by a HabEx-like instrument, and a value of zero when it is not.
Paper: Scheduling Direct Imaging Observations Based on Radial Velocity Orbital Fits: Best Practices for Translating Orbits and Failure Modes
Authors: Corey Spohn, Dmitry Savransky, and Rhonda Morgan
Figure caption: Distributions in α vs. Δmag space for the different orbit construction techniques at the time of fitting. The point represents the true planet’s location. The planet has a of 2 au, e of 0, i of 100°, Rp of 3.48R⊕, geometric albedo of 0.367, and is around a Sun-like star at a distance of 10 parsecs. Each column uses the same output from RadVel with a set ratio of RV error to RV semiamplitude and assumes 10 yr of RV measurements.
Paper: Scheduling Direct Imaging Observations Based on Radial Velocity Orbital Fits: Best Practices for Translating Orbits and Failure Modes
Authors: Corey Spohn, Dmitry Savransky, and Rhonda Morgan
Figure caption: Temporal evolution of orbits constructed with the multivariate-Gaussian method shown in Figure 2.
Paper: Scheduling Direct Imaging Observations Based on Radial Velocity Orbital Fits: Best Practices for Translating Orbits and Failure Modes
Authors: Corey Spohn, Dmitry Savransky, and Rhonda Morgan
Figure caption: Probability of detection curve demonstrating both kinds of failure. The green triangles represent steps when all conditions for intermittent failures are met. The end of the curve, highlighted, represents the point in time when dispersion failure has occurred. This is a somewhat extreme example as it is unlikely that a planet with an error to semiamplitude ratio of 1.25 would be considered for observation.
Paper: Scheduling Direct Imaging Observations Based on Radial Velocity Orbital Fits: Best Practices for Translating Orbits and Failure Modes
Authors: Corey Spohn, Dmitry Savransky, and Rhonda Morgan
Figure caption: Failure mode statistics for the four different construction methods for different ratios of RV error to signal semiamplitude. We see that the failure percentage increases at different rates for each construction method as the ratio of error to semiamplitude increases. Max likelihood and max KDE perform poorly for all ratios tested. Credible interval performs the best for very low ratios, and multivariate Gaussian significantly outperforms credible interval for ratios of 0.5 or greater. Note that, while max likelihood and max KDE appear to perform well, this is only the case when the planet is always detectable, which makes it a trivial result.
Paper: Scheduling Direct Imaging Observations Based on Radial Velocity Orbital Fits: Best Practices for Translating Orbits and Failure Modes
Authors: Corey Spohn, Dmitry Savransky, and Rhonda Morgan
Figure caption: Results for multivariate-Gaussian construction method with 10000 planets generated to test how representative the smaller sample of Figure 5 is. In all cases, the percentages match to better than 1.38% and most below 0.35%, lending confidence to the smaller sample size used in Figure 5.
Paper: Scheduling Direct Imaging Observations Based on Radial Velocity Orbital Fits: Best Practices for Translating Orbits and Failure Modes
Authors: Corey Spohn, Dmitry Savransky, and Rhonda Morgan
Figure caption: Violin plots showing the variation of intermittent failure based on the ratio of RV error to RV semiamplitude for the multivariate-Gaussian method. Each violin shows the median (the horizontal black bar), the quartiles (the vertical green bars), and the kernel density estimate (the green curve to the left and right). The number of data points used for each ratio is labeled above the upper plot. We see that the distribution of the time of the first intermittent failure is weighted heavily near the start of the simulation with long tails for all ratios. The intermittent failure rate is the number of intermittent failures divided by the number of times when the planet is not detectable. It is more variable, with low ratios having their distributions skewed to higher failure rates. This is due to the dense clustering of orbits for low ratios, causing large failure rates when there is a period offset from the true planet.
Paper: Confirming the 3:2 Resonance Chain of K2-138
Authors: Mariah G. MacDonald, Leonard Feil, Tyler Quinn, and David Rice
Figure caption: Evolution of the orbital periods, eccentricities, period ratios, and three-body resonance angles in an example simulation of K2-138. Here we define resonance as the libration of a resonance angle, which occurs if the angle oscillates between two values. We say that the system contains a resonance chain if three or more planets are in resonance with one another.
Paper: Confirming the 3:2 Resonance Chain of K2-138
Authors: Mariah G. MacDonald, Leonard Feil, Tyler Quinn, and David Rice
Figure caption: Kernel density estimations of various planetary masses and orbital periods, separated by whether a resonance angle was librating. For K-S p-values and parameter estimates from this analysis, see Table 3.
Paper: Confirming the 3:2 Resonance Chain of K2-138
Authors: Mariah G. MacDonald, Leonard Feil, Tyler Quinn, and David Rice
Figure caption: A five-planet resonance chain of K2-138 is consistent with in situ formation. Here we show the evolution of one of our short-scale migration simulations. We start the planets out of resonance and then apply a small damping to the semimajor axis of the outer planet with a timescale of τa = 4.6 × 104 yr. We force the planets to undergo this small migration for 1.5 × 104 yr, before stopping the migration and allowing the system to evolve for an additional 105 yr to confirm long-term stability and resonance. We show the evolution of the orbital periods, eccentricities, period ratios, and three-body resonance angles.
Paper: Confirming the 3:2 Resonance Chain of K2-138
Authors: Mariah G. MacDonald, Leonard Feil, Tyler Quinn, and David Rice
Figure caption: Mass–radius diagram with the radius and mass estimates of K2-138's planets. These estimates were pulled from normal distributions centered on the values from Lopez et al. (2019), with standard deviations equal to the uncertainties. We overplot composition curves of Earth-like (solid), 1% H/He atmosphere (short dashed), and 100% water (long dashed). We find that K2-138b is consistent with an Earth-like and terrestrial compositions, but that planets c–f require at least 1% H/He envelopes to satisfy their densities.
Paper: Confirming the 3:2 Resonance Chain of K2-138
Authors: Mariah G. MacDonald, Leonard Feil, Tyler Quinn, and David Rice
Figure caption: Ternary diagram showing solutions from MAGRATHEA to 1000 samples of each planet’s observed mass and radius. Here the axes are the percentage of mass in a core, mantle, and hydrosphere. Thin lines show the WMF needed to match the observed radius across core-to-mantle mass ratios. The thick solid lines correspond to the median WMF, while dashed lines are the 1σ bounds. The gray dashed line shows a constant Earth-like core-to-mantle ratio. K2-138b (blue) is the only planet where all 1000 samples have nonatmosphere solutions. The median samples of K2-138 c (green) and K2-138d (orange) require an atmosphere, and so we include only the lower 1σ bound of WMF. K2-138e requires an atmosphere to satisfy its density and is therefore not included. We use python-ternary by Harper et al. (2015).
Paper: Confirming the 3:2 Resonance Chain of K2-138
Authors: Mariah G. MacDonald, Leonard Feil, Tyler Quinn, and David Rice
Figure caption: The water and atmosphere mass fractions needed to match samples of mass and radius for each planet. We fix the core-to-mantle mass ratio to 1:2, similar to Earth. Thin background lines are solutions to each sample, and thick lines are the mean (solid) and 1σ bounds (dashed) of samples with solutions at the given water mass. We use an isentropic temperature profile with the surface temperature set to the equilibrium temperature from Lopez et al. (2019). We only include the statistics for K2-138b until more than 50% of the samples result in solutions that require less than 10−4% atmospheric mass. A total of 19% of K2-138b samples are too dense to require an atmospheric mass of more than 10−4% and are not shown.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: Architecture of five quadruple systems. Green circles denote subsystems, and small pink circles show individual stars with masses indicated below.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 7852 Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: CCF (top) and RV curve (bottom) of HIP 9148 Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: RV curves of the components B (top) and A (bottom) of HIP 12548. The RV measurements derived from strongly blended dips (plus signs) are assigned large errors.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: The outer orbit of HIP 12548 A,B. Top: positional measurements (plus signs denote visual micrometer measurements, squares are accurate speckle measurements, the wavy line is the orbit with wobble); bottom: the RV curve.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: The RV curve of HIP 21079 Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: The RV curves of single-lined spectroscopic subsystems Aa,Ab (top) and Ba,Bb (bottom) of the HIP 24320 quadruple.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: The RV curves of the inner (top) and outer (bottom) orbits in HIP 27970. Plus signs correspond to the RVs from Gorynya & Tokovinin (2018), and squares correpond to the CHIRON RVs.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 34212 Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: RV curves of HIP 56282. Top: inner orbit; bottom: intermediate orbit. Plus signs denote the less accurate RVs from Gorynya & Tokovinin (2018). The intermediate orbit is still tentative.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: CCF (top) and RV curve (bottom) of HIP 57860 Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: CCF (top) and RV curve (bottom) of HD 108938.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: CCF (top) and RV curve (middle) of HIP 76400 Aa1,Aa2 with the trend subtracted. The bottom plot shows the RV curve in the 70 yr visual orbit of Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 76816 Ba,Bb.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: CCF (top) and RV curve (bottom) of HIP 81395 Ba,Bb, the visual companion of HIP 81394.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: CCF (top) and RV curve (bottom) of HIP 98278 Ba,Bb, the visual companion of HIP 98294. Crosses and plus signs denote inaccurate RVs deduced from blended dips.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: CCF (top) and RV curve (bottom) of HIP 100420.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.
Authors: Andrei Tokovinin
Figure caption: Periods and eccentricities of inner subsystems with solar-type components in the MSC (plus signs). The orbits determined here are plotted by large red triangles.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The tangential velocity differences (Δ∣vT∣) and 2D separations for neighboring stars relative to their TOI hosts (blue circles). The black line shows the Keplerian velocity as a function of semimajor axis for a binary pair with a total mass of 2 M⊙ assuming circular orbits. The bound companions identified by our statistical analysis are shown in red.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The distribution of projected separations for the 170 non-false-positive TOI hosts and their 172 detected stellar companions (blue). The red histogram corresponds to the sample of companions to solar-like field stars reported in Raghavan et al. (2010). The separations of TOI hosts and companions span 40–10,000 au (our search limit, delineated by gray shading), though most companions are found within 300–4000 au. The lack of TOI host companions at separations <40 au is due to the Gaia resolution limit of 0.″7, though the number of missed companions may be negligible (see Section 6).
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The distribution of ΔG (left) and mass ratios (right) for all 172 detected companions compared to their non-false-positive TOI hosts. The companions are comparatively fainter than the TOI hosts, with ΔG ranging from −11.5 to +4.8 and peaking at ∼−5.0. The mass ratio distribution of the companions relative to the TOI hosts spans ∼0.10–1.17 and peaks at ∼0.3, identifying approximately half of the companions as low-mass main-sequence stars.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The total sample of 2140 TOIs plotted in period–radius space (gray). Non-false-positive TOIs with one detected stellar companion (binary systems) and two detected companions (triple systems) are overplotted in blue and red, respectively. There does not appear to be a preferred location for TOIs with stellar companions in period–radius space. Six TOIs fall outside this period–radius space and are not shown for easier visualization. We also delineate the regions of parameter space that harbor Kepler-like (blue) and close-in giant systems (red).