adsabs/AstroCLIMB huggingface dataset:
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: Evolution of Li I as a function of age, as characterized by Equation (2).
Paper: The DECam Ecliptic Exploration Project (DEEP). I. Survey Description, Science Questions, and Technical Demonstration
Authors: David E. Trilling, David W. Gerdes, Mario Jurić, Chadwick A. Trujillo, Pedro H. Bernardinelli, Kevin J. Napier, Hayden Smotherman, Ryder Strauss, Cesar Fuentes, Matthew J. Holman, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, William J. Oldroyd, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Fred C. Adams, Colin Orion Chandler
Figure caption: A digital tracking recovery of 2002 PC171 detected in our B1f field on 2021 September 3. This object has m  V  = 24.1. These images are generated using the outputs of KBMOD and are used for human vetting. (All candidates are vetted by multiple people.) The two top left stamps show a simple sum and median coadd of the individual exposures stacked along the KBMOD trajectory. The top right plot shows the approximate KBMOD-estimated flux in each individual exposure. The bottom three rows show a subset of the individual exposures used in the KBMOD search aligned along the moving object trajectory. Although one row of stamps was excluded from this figure to save space, all individual stamps are included in the images used for human vetting. Many more details of our digital tracking approach are presented in Papers V (Napier et al. 2024) and VI (Smotherman et al. 2024).
Paper: The DECam Ecliptic Exploration Project (DEEP). I. Survey Description, Science Questions, and Technical Demonstration
Authors: David E. Trilling, David W. Gerdes, Mario Jurić, Chadwick A. Trujillo, Pedro H. Bernardinelli, Kevin J. Napier, Hayden Smotherman, Ryder Strauss, Cesar Fuentes, Matthew J. Holman, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, William J. Oldroyd, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Fred C. Adams, Colin Orion Chandler
Figure caption: Visualization of survey comparisons among published (dark blue), forthcoming (red), and DEEP (cyan). The forthcoming surveys are LSST wide fast deep, LSST Deep Drilling, and the JWST TNO pencil beam project. The contours (from 1 in the lower left to 106 in the upper right, logarithmically spaced) show the expected number of TNOs to be discovered, assuming ecliptic pointings, using the best-fit brightness distribution from B04. The symbol size shows the actual number of objects detected. The Dark Energy Survey, for example, which is shown by the symbol (5000, 23.8), “underperforms” relative to expectations because the majority of the sky coverage is away from the ecliptic. Our DEEP survey will produce the largest catalog of TNOs and faint TNOs to date.
Paper: The DECam Ecliptic Exploration Project (DEEP). I. Survey Description, Science Questions, and Technical Demonstration
Authors: David E. Trilling, David W. Gerdes, Mario Jurić, Chadwick A. Trujillo, Pedro H. Bernardinelli, Kevin J. Napier, Hayden Smotherman, Ryder Strauss, Cesar Fuentes, Matthew J. Holman, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, William J. Oldroyd, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Fred C. Adams, Colin Orion Chandler
Figure caption: Recovery of the KBO 2003 QL91. The panel on the left shows the object’s S/N as a function of rate of motion. The black teardrop-shaped region bounds the space of possible rates of motion for bound objects beyond 30 au. Two parameters describing a body’s proper motion are sufficient for the detection of KBOs over the 4 hr arcs, during which any nonlinear sky motion is undetectable at the resolution of our images. The panel on the right shows the characteristic elongation of a source as it is stacked at rates deviating from its true rate of motion.
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: Bias-corrected cumulative magnitude distribution of the L4 (left panel) and L5 (right panel) Jupiter Trojan populations based on G96 observations. The background population, shown by the upper curves, is separated from the major families: (i) Eurybates (label 1), Arkesilaos, Hektor, Thronium, and Teucer in the L4 population, and (ii) Deiphobus (label 1), Ennomos (label 2) and 2001 UV209 (label 3) in the L5 population. The red lines are the CSS observations (solid are the data in phase II, dashed are the data in phase I), and the black line is the bias-corrected model with σ interval (gray zone). The blue line is the whole background population from the MPC catalog. The vertical dashed lines show the magnitude segments used for the representation of the background population (Table 3).
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: differential magnitude distribution of the bias-corrected background Trojan populations: solid line is the median solution (red for L4 and blue for L5), and the gray zone is the σ uncertainty (0.1 mag bins wide). The Trojan populations in the families are not contributing. Right panel: the asymmetry factor f 45 = N 4/N 5 of the L4 and L5 Jupiter Trojans. The background population counts N 4 and N 5 are (i) their respective cumulative values at a certain magnitude limit (the abscissa), and (ii) correspond to the bias-corrected background population in our model. The solid black line is the median value, and the gray area is the σ envelope from the 10,000 posterior solutions by MultiNest. The vertical dashed line is the approximate observational completeness to date. The solid red line is the ratio of the observed L4/L5 populations with the Trojans in families removed. Up to the completion limit, we expect this fraction to reside inside the uncertainty limits of the model. The group of the largest Trojans below magnitude ≃9–9.5 exhibit symmetry, since f 45 = 1 is within the statistical uncertainty. Interestingly, the observed population fraction exceeds the σ interval of the model in the ≃9.5–10 range. This feature is due to the anomalous vacancy of the L5 Trojans in this magnitude range (see Figures 15 and 16). Trojan populations fainter than ≃10 deviate from symmetry, with the observed fraction returning to the σ interval of the model, and the statistical robustness increases with increasing H. At the approximate observational completeness limit, H ≃ 13.8, f 45 = 1.43 ± 0.05 (σ solution), with f 45 = 1 excluded at ≃7.9σ level.
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 solution of the L4 Trojan population using a model in which the maximum absolute magnitude has been extended to 15.5 (compare with the left panels in Figures 20 and 23). Left panel: Differential magnitude distribution of the G96 observations (blue for phase I and red for phase II) compared with the best-fitting biased model (black line with a σ interval depicted by the gray zone). Right panel: Bias-corrected cumulative magnitude distribution based on G96 observations. The background population, shown by the upper curves, is separated from the major families: (i) Eurybates (label 1), Arkesilaos, Hektor, Thronium, and Teucer. The red lines are the CSS observations (solid are the data in phase II, dashed are the data in phase I), and the black line is the bias-corrected model with σ interval (gray zone). The blue line is the whole background population from the MPC catalog. The vertical dashed lines show the magnitude segments used for the representation of the background population.
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 local slope of the cumulative absolute magnitude distribution for the bias-corrected background population of L4 (red) and L5 (blue) Trojans. The gray zone is the σ interval of the solution. The vertical dashed line indicates the often-quoted break at ≃9 mag, delimiting the transition from a very steep distribution of larger Trojans to a shallower distribution of smaller Trojans. The horizontal dashed line at 0.44 slope is the characteristic value for H > 9 mag Trojans in the previous literature (see, e.g., Uehata et al. 2022). In the last segment of our solution, magnitude range 14–15, the slope of the L4 population becomes gradually shallower reaching ≃0.38 at H = 15 mag. The solution of the L5 population in the same magnitude segment is even shallower, but we consider it unreliable for reasons discussed in the main text.
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: Projected distributions of the orbital parameters A (left), B (middle), and C (right) of the biased populations from our model (red lines) and the G96 observations (black histogram) using the phase I (bottom sectors) and phase II (top sectors) data: L4 data at the top panels, L5 data at the bottom panels. The shaded gray area delimits the σ region of the solution (created by 10,000 posterior random samples of the model). The blue histogram is the best-fitting model of the background population.
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: Differential magnitude distribution of the G96 observations (blue for phase I and red for phase II) compared with the best-fitting biased model (black line with a σ interval, based on analysis of 10,000 posterior random samples of the model, depicted by the gray zone). The left panel is for L4 Trojans, and the right panel is for L5 Trojans. The magnitude bin has a width of 0.1 mag for the model and 0.2 mag for the data.
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: Cumulative distribution of the orbital parameters (A, B, C) (left to right) based on our biased-corrected solution of the Trojan background populations: L4 in red and L5 in blue. Because the model parameters of the faint L5 Trojans are not reliable enough, we use a maximum 13.5 mag limit in computing the upper plots; the lower plots provide the same information but for a population limited to absolute magnitude 12. The color-coded curves are the best-fit solution, and the gray region is a σ interval. The B and C distributions appear to be statistically identical, but the A (inclination) distribution is different.
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 independent detections (gray symbols) for Jupiter Trojans observed by CSS station G96 during the phase I (top panels) and phase II (bottom panels) period (Section 2). The left panels are for the L4 swarm, and the right panels are for the L5 swarm. The abscissa is the absolute magnitude H. The black curves provide the predicted detection rate ﹩\bar{{ \mathcal R }}(H)﹩ for G96 determined by averaging over all long-term stable (A, B, C) bins using weights based on Equations (6)–(8). The blue curves are simply mean values of detection counts grouped in 0.5 wide bins in absolute magnitude, and the vertical bars represent the standard deviation within the respective magnitude bin. By their definition, the blue curves cannot decrease below one detection, while the predicted rates may. This produces an apparent mismatch beyond H ≃ 14.5–15.
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 posterior distribution of 15 model parameters characterizing the background population of the L4 Trojans from our nominal MultiNest fit to G96 observations (sometimes called the “corner diagram”; the L5 solution shows a fairly similar pattern). The individual plots are labeled (1)–(15) following the model parameter sequence given in Table 3; the first eight parameters determine the orbital distribution in A, B, and C elements, and the last seven parameters determine the absolute magnitude cumulative distribution (with the ninth parameter being the normalization at 14.5 mag), and the last six parameters the mean slope values in the chosen segments (Table 3).
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption:  m 162 − m 444 and m 162 vs. m 360 − m 444 for sources in NIRCam images of IC 348. The symbols indicate whether the sources are point-like (filled circles) or extended (crosses) based on the metric from Figure 3. We have marked the known members of IC 348 that are within the NIRCam images and are not saturated (red filled circles). We have performed NIRSpec observations on eight candidates for new members (open circles), which are labeled with the source numbers from Table 1. Colors for the planetary mass companion TWA 27B are included in the top diagram (open star, Luhman et al. 2023).
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption: JWST/NIRSpec spectrum of the substellar companion VHS 1256b after binning to a resolution of R = 200 (Luhman et al. 2023). We have marked the wavelengths spanned by the six NIRCam filters selected for imaging of IC 348. We have included a spectrum of background PAH emission extracted from our NIRSpec observations in IC 348.
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption:  m 162 vs. the median difference between 2 and 4 pixel aperture photometry among the available bands for sources in NIRCam images of IC 348. This metric is used to classify the sources as point-like (<0.1) or extended (≥0.1).
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption: Map of the known members of IC 348 and the field imaged by JWST/NIRCam in this study (red box).
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption: JWST/NIRSpec spectra of sources 1 and 3 (left and right, black) compared to various other spectra (red).
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption: JWST/NIRSpec spectra of brown dwarf candidates selected from NIRCam images of IC 348 (Figure 4). The spectra are labeled with the source numbers from Table 1. We also show NIRSpec data for a known cluster member (source 13), which has been normalized to source 4 at 3.9 μm and shifted upward. The dotted lines mark absorption features in sources 1 and 3 that we attribute to overtone and combination bands of C–H stretching modes in the same carrier that produces the fundamental band at 3.4 μm. Those wavelengths are also marked in the spectra of sources 2 and 4 for reference. We have included a spectrum of the brightest PAH feature appearing in the background emission in the NIRSpec data.(The data used to create this figure are available.)
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption: Spectra of sources 1 and 3 divided by the spectra of normal young objects (M5.5 standard and source 4), a laboratory reflectance spectrum of C5H12 (Clark et al. 2009), and a transmission spectrum of Saturn (Dalba et al. 2015). The strongest features in all spectra correspond to fundamental, overtone, and combination bands of C–H stretching modes. For reference, the central wavelength of the Q branch of CH4 is marked by the red dotted line (see Figure 2).
Paper: A JWST Survey for Planetary Mass Brown Dwarfs in IC 348 
Authors: K. L. Luhman, C. Alves de Oliveira, I. Baraffe, G. Chabrier, T. R. Geballe, R. J. Parker, Y. J. Pendleton, P. Tremblin
Figure caption: Luminosity estimates for new members of IC 348 identified with JWST (this work) compared to luminosities as a function of age predicted by the evolutionary models of Chabrier et al. (2023) for constant values of temperature and mass. For reference, we have included a luminosity estimate for the planetary mass companion TWA 27B (open star; Luhman et al. 2023).
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Time span over which integrated-light solar spectra were acquired by the SOLIS project, HARPS-N, EXPRES, and NEID. The left Y-axis is the number of sunspots, showing the extent of solar activity in Cycle 24 and now increasing in Cycle 25. The points in gray are the spatially averaged magnetic flux on the solar disk in Gauss as measured by the SOLIS spectromagnetograph (read Y-axis on the right).
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Sample SOLIS spectrum covering the region near the Mn I line at 539.5 nm compared to an average of HARPS-N spectra acquired on the same day. Both spectra represent the full data for that single day of observing, randomly selected as 2015 August 17 (a high-humidity season for the SOLIS data). The lower panel expands the upper 5% of the spectrum, so that the noise can be seen (compare fluctuations of the two spectra in regions near the continuum). The SOLIS spectrum is offset downward by 1% to facilitate the visual comparison.
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Span of the bisector of the Fe I line at 539.318 nm vs. date. The vertical blue lines mark the approximate times between which the Sun was most active in Cycle 24 (compare to Figure 1). In addition to the decrease in bisector span during the middle period of high solar activity, there are also fluctuations due to telluric effects (Section 3.2 and Figure 9). The green points with error bars are not real data; they illustrate the ±3σ envelope due to random variations per point in the three regions.
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Bisector span vs. the disk-averaged total magnetic flux in Gauss for three representative lines. The top panel illustrates the line having the clearest change in C-shaped bisector (positive span). The bottom panel shows the line with the clearest change in reversed-C bisector (negative span). The middle panel shows a line with no change in bisector span to high precision. For all lines, we divide the bisector measurements into quiet and active phases at a boundary of 6 G. Thus, quiet bisectors (blue points) have 〈∣B∣〉 < 6 G, and active bisectors (red points) have 〈∣B∣〉 ≧ 6 G. The horizontal lines indicate the median values in each phase.
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Average line bisectors (in m s−1) for the same three lines whose span is plotted vs. 〈∣B∣〉 in Figure 8. The active and quiet bisectors for Ti II 655.959 nm in the middle panel are almost identical and overlapping at this scale. Only the spans of the bisectors are meaningful here; the zero-point on the X-axis is affected by imprecision in the rest wavelengths of the lines. The ±1σ uncertainties on the difference in bisector span (quiet minus active) are listed in Table 1 and are 0.7, 1.2, and 5.1 m s−1 from the top to bottom panels. Lines in the top and bottom panels exhibit a statistically significant change in bisector span from quiet to active phases.
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Examples of bisectors that we measure using the SOLIS/ISS spectra. This example is for the spectral segment centered on the high-excitation line of neutral carbon at 538.032 nm. The two bottom panels expand two lines (left: Fe I 537.957 nm; right: Ti II 538.102 nm), with the average bisector for each line overplotted (in hot pink) on an even more expanded scale (refer to the 100 m s−1 legend). The bisectors plotted are average shapes over 3587 spectra. The rose-shaded region surrounding each bisector is the ±3σ uncertainty envelope of a single bisector measurement, and note that the velocity scale for the bisector is m s−1.
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Retrieval of the center-of-mass RV vs. orbital phase of the injected signal for the single Fe I line at 539.318 nm. This shows RV results extracted from 2672 line bisectors measured during 10.8 yr. The standard deviation of the points plotted here is 1.7 m s−1, so we do not expect to retrieve the injected signal without averaging over bins in phase, as well as over multiple lines. Because the injected signal has a 1 yr period (with zero RV on January 1), the orbital phase plotted here is the same as the terrestrial yearly calendar. The increase in humidity over Kitt Peak in the summer months affects the RV retrieved from this line, noticeable as increased scatter and a bias toward more positive (redder) RV values during July and August (see text for discussion).
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Bisector span (in m s−1) for the Fe I line at 539.318 nm vs. date. The blue line is the disk average of the total magnetic flux, plotted on an inverted scale (greater flux being downward) and matched to the amplitude of the bisector variations. The points are 100 day averages of the bisector span, and their scatter exceeds the error bars due to temporal variations on times less than the 11 yr magnetic cycle.
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Effect of spectral resolving power on line bisectors. This shows a synthetic absorption line with a bisector whose shape agrees with solar measurements at very high resolving power. The line bisectors are plotted on a greatly expanded wavelength scale (see 20 m s−1 legend). The black line is the fully resolved bisector, i.e., at infinite resolving power. After convolving to the spectral resolution of the NEID, HARPS-N, EXPRES, and SOLIS/ISS spectrometers, the spans of the bisectors (colored lines) are reduced from the fully resolved case but are still sufficiently prominent to serve as probes of solar activity and allow separation of center-of-mass RVs from activity-related RV variations.