adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Dynamical separatrices of high-order and secondary spin–orbit resonances in the phase space (left-hand column panels), as well as their comparisons to numerical structures arising in Poincaré sections (right-hand column panels) for spin–orbit problems with different asphericity parameters. The red-dashed lines stand for dynamical separatrices of the synchronous primary resonance, which are expressed by Equation (10).
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Analytical structures (dynamical separatrices) of the synchronous primary resonance and the secondary 1:1 spin–orbit resonance together with the associated numerical structures arising in Poincaré sections at different eccentricities for binary asteroid systems (65803) Didymos (top panels) and (4383) Suruga (bottom panels). The blue lines stand for the dynamical separatrices of the 1:1 secondary resonance and red-dashed lines stand for the dynamical separatrices of the synchronous primary resonance. The asphericity parameter is α = 1.1 for binary asteroid system (65803) Didymos and it is α = 1.36 for binary asteroid system (4383) Suruga.
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: Left: An example of the decrement of EqW of H lines in the Balmer series, normalized by EqW of Hγ (n  u  = 5). The black line shows the best-fitted model from Kwan & Fischer (2011). Hϵ is likely contaminated from Ca H. Right: Distribution of the derived Temp and log n models for the sources with cleanly defined decrements in Balmer lines. Points are color coded by the uncertainty in log n. We note that most confident measurements tend to have log n > 11.
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: An example of a spectral lines (Hα and Li I) of a PMS star in BOSS spectra. The red line is centered on the feature, and the blue line is the manually defined continuum over which the line is integrated to measure EqW.
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: Top: Kiel diagram of the sample, color coded by the photometrically derived probability of a star being on the PMS using Sagitta (McBride et al. 2021). Bottom: Adopted ages for the stars in the sample; for the sources with PMS prob.<0.5, the assumed age is that of the closest high-probability neighbor.
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: Distribution of Hα as a function of temperature for the YSOs in our sample. The red line shows the adopted separation between CTTSs and WTTSs. The yellow lines are the ranges for the selection from White & Basri (2003).
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: EqW measurements in BOSS spectra for some of the lines used in this study. The colored background (color coded by the density of points) represents field stars of different evolutionary stages. Black contours are the sources identified as YSOs.
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: On-sky distribution of identified YSO candidates with probability >0.5.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Upper panel: histogram of the absolute magnitude H values for detections of L4 (left) and L5 (right) Trojans during the CSS phase I operations (the ordinate is the number of such detections within the bin). The vertical dashed line shows the magnitude at the center of a bin in which the number of detections dropped below 5% of the bin with a maximum number of detections. This value is about ≃15.1 for both L4 and L5 clouds. Bottom panel: correlation between the absolute magnitude H at the abscissa and visual magnitude m at the ordinate for detections of L4 (left) and L5 (right) Trojans during the CSS phase I operations. At an ideal opposition, m − H ≃ 6.7 (neglecting the phase function correction) from simple distance arguments (the dashed line). The nearly 2 mag spread toward larger m values are detections at different phase angles. The dotted lines between visual magnitudes 20 and 21 indicate a typical 50% photometric efficiency of detections. Objects brighter than m ≃ 15 (lower dotted line) may saturate exposures and be undetected due to their slow motion. Luckily, there are detection losses due to this effect for Trojan populations because even the largest of them at opposition barely reach this limit. The only photometric limit, indicated by the vertical dashed line from the upper panel, thus occurs at the faint end of the spectrum.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Number of Trojan detections throughout the CSS operations in phases I and II: left for L4 cloud, right for L5 cloud. Apart from the obvious annual variation, due to the Earth's revolution about the Sun changing the viewing geometry of the Trojan clouds at the night sky, there is also a longer-term variation due to Jupiter's motion. This dictates when a particular cloud, L4 or L5, appears projected in the direction of the galactic plane. For instance, the major minimum of L4 object detection around 2018 is when the cloud overlaps with the galactic center direction. Finally, data during the phase II operations of CSS are roughly 4 times more numerous than during phase I operations due to a 4 times larger field of view.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Projection of the MPC Trojan clouds as of 2023 February onto the λ − λ J (abscissa) and da = a − a J (ordinate) plane (using osculating elements at MJD 60,000, and a J = 5.204 au). The left panel is for L4, and the right panel is for L5. Red symbols among the L4 population highlight the Eurybates family members, those among the L5 population show the more dispersed Ennomos/Deiphobus family members. The blue lines are the isolines of the first integral of the Trojan motion Equation (3) for selected values of the C parameter: (i) C = 1.68 (solid) and C = 1.95 (dashed) in the L4 panel, and (ii) C = 1.88 (solid) and C = 2 (dashed) in the L5 panel. In spite of its huge simplicity, representation using Equation (3) helps to parameterize the population for our purposes.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Upper panel: intrinsic distribution of the apparent motion of Jupiter Trojans in the fields of view of CSS phase II (determined from a modeled synthetic population of objects) is shown by the black histogram with gray shading. The color-coded histograms are the apparent motion distributions of the detected Trojans (red for L4 and blue for L5 Trojans); all distributions are normalized to maximum. Detected populations miss the tail of very slowly moving objects (see below). Lower panel: mean value of the bright-end detection probability ϵ 0 of the CSS observations during phase I (red) and phase II (blue) as a function of the apparent motion w on the CCD detector of G96 (abscissa in deg day−1). The horizontal dashed lines are global average values of ϵ 0 over all w values, and the vertical dotted lines denote a critical w value for which ϵ 0 drops to ≃0.25. The drop in the detection efficiency below ≃0.04 deg day−1 (phase I) and ≃0.08 deg day−1 (phase II) is related to a finite pixel size of the detector, preventing the identification of a clear tracklet for a slowly moving Trojan image.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Jupiter Trojan detections by the CSS operations between 2016 May 31 and 2022 June 14 (phase II). There are 40,832 detections of 6307 individual bodies librating about the L4 center (left panel) and 18,293 detections of 3041 individual bodies librating about the L5 center (right panel). The blue symbols are topocentric R.A. (abscissa) and decl. (ordinate) of the observations. The red line is the Jupiter track in the same period of time near the ecliptic plane (dotted line). The solid black line is the projection of the galactic plane surrounded by the ±15° latitude strip (gray region). The black star is the direction of the galactic center. The observations primarily avoid pointing toward crowded stellar fields near the galactic center.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Cartesian representation of ﹩z-{e}_{{\rm{J}}}\exp (\pm {\imath }\pi /3)﹩ for 7903 L4 Trojans (left) and 4177 L5 Trojans (right) from the MPC catalog as of 2023 February (using osculating elements at MJD 60,000). The red symbols show the major families in the respective Trojan clouds: Eurybates at L4 and Ennomos/Deiphobus at L5, using their identifications in Appendix A. At the zero level, the population distribution is independent of the polar angle ψ in these coordinates, depending only on the radial coordinate B (see Equation (2)).
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Jupiter Trojan detections by the CSS operations between 2013 January 2 and 2016 May 14 (phase I). There are 14,303 detections of 4551 individual bodies librating about the L4 center (left panel) and 7230 detections of 2460 individual bodies librating about the L5 center (right panel). The blue symbols are topocentric R.A. (abscissa) and decl. (ordinate) of the observations. The red line is the Jupiter track in the same period of time near the ecliptic plane (dotted line). The solid black line is the projection of the galactic plane surrounded by the  ±15° latitude strip (gray region). The black star is the direction of the galactic center.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The same as in Figure 5, but now for the CSS phase II operations containing roughly 3 times more detections. The vertical dashed lines are now different for the two Trojan clouds: ≃15.35 for L4 and ≃14.95 for L5.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Cartesian representation of ζ − ζ J for 7903 L4 Trojans (left) and 4177 L5 Trojans (right) from the MPC catalog as of 2023 February (using osculating elements at MJD 60,000). The red symbols show the major families in the respective Trojan clouds: Eurybates at L4 and Ennomos/Deiphobus at L5, using their identifications in Appendix A. At the zero level, the population distribution is independent of the polar angle φ in these coordinates, depending only on the radial coordinate A (see Equation (1)).
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Detections of the L4 Trojans during phase II of the CSS observations (calendar date at the abscissa; see also Figure 4). The ordinate shows the Trojan ecliptic longitude λ referred to as the ecliptic longitude of the Earth λ Earth at the moment of detection. The upper panel is for H ≤ 14 Trojans (population of large and bright objects), and the lower panel is for H ≥ 15 Trojans (population of small and faint objects). The dashed curves are the extremal configurations defined by (i) the Sun being 10° below the local horizon, (ii) the Trojan being at the ecliptic and 15° above the local horizon (the cyclic nature is due to longer nights as well as the higher maximum position of the ecliptic above the horizon in winter). At each season, the Trojans start to be observable in the extreme morning sky, and over a period of little less than a year, they move to the extreme evening sky. This is due to the Earth's faster mean motion about the Sun, such that the L4 swarm near Jupiter’s libration center is being caught by the Earth-bound observed; the dotted line has the relevant synodic frequency n − n J. The scatter of detections in λ − λ Earth at any given moment corresponds to Trojans at different libration amplitudes about L4. A combination of geometric, CSS-operation-dependent, and photometric selection effects impact detections. Bright Trojans are detectable during the whole season unless a galactic plane interferes (pre-2019 observations; see Figures 3 and 4) or the observations are interrupted by summer maintenance (see the example in 2019 shown by the arrow). Faint objects are observed selectively near the opposition (λ ≃ λ Earth), which decreases their apparent magnitude in both factors on the right-hand side of Equation (23): (i) the product RΔ is minimum, as well as (ii) the magnitude-phase correction P(α). Due to the galactic-plane disturbance, no faint Trojans near L4 were detected during phase II until the opposition in late 2019.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Trojans in the L4 swarm detected by the CSS in the 2021 April and 2022 April seasons (see Figures 4 and 33), projected on the plane of osculating nonsingular elements ﹩(e\cos \varpi ,e\sin \varpi )﹩. The left panel is for bright objects with H < 14, and the right panel is for faint objects with H > 15. The green star is the forced center of the quasi-proper elements (B, ψ), namely at e J polar distance from the center and polar angle 60° + ϖ J (Equation (2)); several constant B circles are shown for the sake of illustration. The bright objects are distributed symmetrically about the forced center. The faint objects are mostly detected in the first quadrant, though clearly their complete population should follow the symmetric distribution shown by the bright objects. The symbols on the right panel are colored in red when the detection occurred at a 20° angular distance from the pericenter; this is the case for nearly all detected faint objects. The light blue annulus depicts B ∈ (0.06, 0.08) interval of values that we have chosen for testing the validity of the detection probability ﹩{ \mathcal P }(A,B,C;H)﹩ averaging over the polar angle ψ (defined from the shifted axis as shown by the arrow).
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Left panel: detection probability of L4 Trojans in the quasi-proper orbital element bin defined by (i) A ∈ (0.2, 0.225), (ii) B ∈ (0.06, 0.08), and (iii) C ∈ (1.58, 1.60). Here we use only CCS observations between 2021 April and 2022 April. The bold black line is the ψ-averaged detection probability ﹩{{ \mathcal P }}_{\mathrm{ave}}={ \mathcal P }(A,B,C;H)﹩, and the gray curves show the ψ-resolved detection probabilities ﹩{{ \mathcal P }}_{i}﹩ in 20° wide bins. Four individual values are color-highlighted. At H = 15 mag, the minimum and maximum detection probabilities ﹩{{ \mathcal P }}_{i}﹩ are more than 1 order of magnitude different (see the arrow). The diamond symbol is the ﹩{{ \mathcal P }}_{\mathrm{ave}}﹩ value. Right panel: the appropriately scaled ﹩{{ \mathcal P }}_{i}﹩ values (red histogram), compared to the actual number N  i  of detected Trojans in the (B, ψ) annulus with B ∈ (0.06, 0.08), but all (A, φ, C, θ) values (in order to increase statistics); for simplicity, the N  i  are assumed to have ﹩\sqrt{{N}_{i}}﹩ uncertainties shown by vertical intervals.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The newly determined proper elements of L4 (left) and L5 (right) Jupiter Trojans with the input orbital information as of April 2023. The top panels show a projection onto the da P vs. ﹩\sin {I}_{{\rm{P}}}﹩ plane, and the bottom panels show a projection onto the da P vs. e P plane. Distinct clusters, especially among the L4 Trojans, are the subject of our analysis, resulting in a new catalog of the Trojan families.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Trojan families highlighted in the plane of the proper eccentricity e P and the proper sine of inclination ﹩\sin {i}_{{\rm{P}}}﹩ (compare with the rightmost panel in Figure 11); the objects librating about the leading point L4 on the left panel, those librating about the trailing point L5 on the right panel. The scale of gray and the size of the symbols are proportional to the absolute magnitude H (see the vertical bar). The family location is indicated by the largest remnant (color-coded open circles and labels); the newly discovered families are identified by the asterisk (*).
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The same as Figure 29 (left panel), but now zoomed on the individual families among the L4 Trojans. The family members are black (the symbol size proportional to the physical size of the body), non-members projecting onto the same ﹩({e}_{{\rm{P}}},\sin {I}_{{\rm{P}}})﹩ zone (but having offset the da P third coordinate) are shown in gray. The family identification is at the top label, and the position of the largest remnant is highlighted by the open circle. The low-inclination families (﹩\sin {I}_{{\rm{P}}}\lt 0.2﹩) are typically resolved by having a large population of members, and the high-inclination ones may be resolved more easily because of the low background population of Trojans. In the case of the Hektor family (top and right panel), we show its dense core consisting of only very small fragments, while previous studies considered its more extended version (e.g., Rozehnal et al. 2016).
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The same as in Figure 30, but now for the three families identified among the L5 Trojans. We argue that the former Ennomos family, shown on the leftmost panel, is in fact composed of two overlapping families: (i) Ennomos, at the right bottom corner, and (ii) Deiphobus, extending toward the high inclinations.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Population of L4 (left) and L5 (right) Jupiter Trojans from the MPC catalog (as of 2023 February 22) projected onto the “quasi-proper” elements used in our debiasing procedure: (i) ﹩{{da}}_{{\rm{P}}}(C)={a}_{{\rm{J}}}\sqrt{8\mu (C-1.5)/3}﹩ vs. A (top), and (ii) ﹩{{da}}_{{\rm{P}}}(C)={a}_{{\rm{J}}}\sqrt{8\mu (C-1.5)/3}﹩ vs. B (bottom). While these variables are much simpler than the true proper elements, they provide a picture nearly as accurate (compare with Figure 28).
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The same as in Figure 33, but now for the L5 Trojans. The upper panel is for detections of the H ≤ 14 Trojans, and the lower panel is for detections of the H > 14.5 Trojans.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Measured i * values for hot (orange) and warm (blue) Jupiters plotted as a function of a/R *. The dashed line is the separation between hot and warm Jupiters for an a/R * of 20 around a Sun-like star. The y-axis spans 90°–0° to emphasize aligned systems at i * = 90°. The top panel shows all of the 36 hot Jupiters and 24 warm Jupiters compiled for our analysis. In the bottom panel, we have isolated the sample to 25 hot Jupiter and 22 warm Jupiter host stars below the Kraft break.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Planet-hosting stars in our sample plotted on a Gaia M G vs. G  BP  − G  RP  color–magnitude diagram. Host stars are color coded based on whether they harbor a hot Jupiter (orange) or a warm Jupiter (blue). Most systems in our analysis are main-sequence FGK dwarfs. The star with the reddest color is TOI-1227, a young (11 ± 2 Myr), low-mass (0.17 M ⊙) member of the Lower Centaurus Crux OB association.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Posterior distributions of stellar inclination for stars hosting hot (orange) and warm (blue) Jupiters in our sample. Shaded regions show the 68% and 95% credible intervals.