adsabs/AstroCLIMB huggingface dataset:
Paper: Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+
Authors: Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Steven Giacalone, W. Garrett Levine, Morgan Saidel, Shreyas Vissapragada, David R. Ciardi, Karen A. Collins, David W. Latham, Cristilyn N. Watkins, Polina A. Budnikova, Dmitry V. Cheryasov, Akihiko Fukui, Allyson Bieryla, Avi Shporer, Benjamin M. Tofflemire, Catherine A. Clark, Chris Stockdale, Colin Littlefield, Emily Gilbert, Enric Palle, Eric Girardin, Felipe Murgas, Galen J. Bergsten, Hugh P. Osborn, Ian J. M. Crossfield, Jerome de Leon, Jesus Higuera, Keisuke Isogai, Mark E. Everett, Michael B. Lund, Norio Narita, Richard P. Schwarz, Roberto Zambelli, Steve B. Howell
Figure caption: Top: TRICERATOPS+ fit (red curve) for the TP scenario (transiting planet around target star) to the observations of TOI-1254.01. Bottom: TRICERATOPS+ fit (red curve) for the SEBx2P scenario (an unresolved eclipsing binary with twice the orbital period around a secondary star) compared to the same observational data set. This scenario has a relative probability of 0.9999.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Star fields for Roslund 3 (left panel) and Ruprecht 174 (right panel) in the equatorial coordinate system. The red boundaries indicate the fields observed with the T100 telescope, that is, ﹩21\mathop{.}\limits^{{\rm{^{\prime} }}}5\times 21\mathop{.}\limits^{{\rm{^{\prime} }}}5﹩. Each chart is ﹩4{0}^{{\prime} }\times 4{0}^{{\prime} }﹩. North and east correspond to the up and left directions, respectively.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The histograms illustrate the distribution of stars in the direction of Roslund 3 (panels (a) and (b)) and Ruprecht 174 (panels (c) and (d)) as a function of V and G magnitudes. The red dashed lines indicate the photometric completeness limits for each band.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: CMDs based on UBV and Gaia photometry for the clusters Roslund 3 (panels (a), (b), (c)) and Ruprecht 174 (panels (d), (e), (f)). The blue solid lines represent the PARSEC isochrones that best match the observed data, allowing for the determination of the clusters’ distance moduli and ages. The purple solid lines indicate the uncertainties associated with the age estimates. The color scales and symbols are consistent with those defined in Figure 4.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: King profiles of Roslund 3 (upper panel) and Ruprecht 174 (lower panel), with black solid curves representing the best-fit models. The shaded red and gray regions indicate the confidence intervals of the model and the background stellar density, respectively, while the red arrows show the limiting radii of the OCs.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The corner plot presents both the one-dimensional marginalized and two-dimensional joint posterior probability distributions for the inferred parameters of Roslund 3 and Ruprecht 174. In the two-dimensional panels, the overlaid contours correspond to confidence levels of 68%, 90%, and 95%, delineating the regions of highest probability density. The one-dimensional histograms display the posterior distributions for each parameter individually, where the vertical lines mark the median values along with the 16th and 84th percentiles, representing the 1σ credible intervals.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: CMDs of the Roslund 3 ((a)–(b)) and Ruprecht 174 ((c)–(d)) OCs are shown in both the UBV ((a) and (c)) and Gaia ((b) and (d)) photometric systems. Stars with membership probabilities P < 0.5 are represented by gray circles, while those with P ≥ 0.5 are denoted by colored circles. The continuous and dashed blue curves correspond to the ZAMS lines from H. Sung et al. (2013) and PARSEC models (A. Bressan et al. 2012).
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The fields of Roslund 3 (upper panels) and Ruprecht 174 (lower panels) OCs: Gaia DR3 proper-motion components (left panels) and sky orientation vectors in equatorial coordinates (right panels). The color scale and circles are consistent with those in Figure 4. Black plus signs in the right panels mark the central equatorial coordinates of the clusters.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: (U − B)0 vs. (B − V)0 TCDs for nine F–G-type main-sequence stars with membership probabilities P ≥ 0.5 are presented for Roslund 3 (top panel (a)) and Ruprecht 174 (top panel (b)). The Hyades main sequence, shown as blue curves, is used as a reference. The bottom panels display the histograms of the normalized (δ0.6) values, along with Gaussian fits represented by blue curves to model the distributions.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The TCDs of the main-sequence members (P ≥ 0.5) of Roslund 3 (a) and Ruprecht 174 (b). The reddened ZAMS (H. Sung et al. 2013), is represented by the red dashed curves, with the green solid curves indicating ±1σ uncertainty intervals.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Trigonometric parallax histograms of stars with membership probabilities P ≥ 0.5, within the G ≤ 20.5 mag limit, and relative parallax errors σϖ/ϖ < 0.2 for the Roslund 3 (a) and Ruprecht 174 (b). The red dashed lines represent the Gaussian curve fitted to the distribution.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The membership probability distributions for all stars in the cluster fields of Roslund 3 (a) and Ruprecht 174 (b) are shown, based on Gaia data. The blue histograms represent the membership probabilities of all stars detected in the cluster regions.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The orbital motions of the Roslund 3 ((a), (b)) and Ruprecht 174 ((c), (d)) in the (Z vs. Rgc) and (Rgc vs. t) planes.The filled yellow circles and triangles represent the present-day and early orbital positions of the clusters in the Galaxy, respectively. Red arrows indicate the direction of their motion.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: PDMFs for Roslund 3 (a) and Ruprecht 174 (b). The red points represent the mass distributions, while the blue line shows the best-fit linear trend. Green lines mark the one standard deviation boundaries of the fit.
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The cumulative radial distribution of stars across various mass ranges for Roslund 3 (a) and Ruprecht 174 (b).
Paper: A Multidata Approach to Open Clusters: Roslund 3 and Ruprecht 174 in CCD UBV and Gaia DR3 Context
Authors: Hülya Karagöz, Talar Yontan, Selçuk Bilir, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: LF histograms for Roslund 3 (a) and Ruprecht 174 (b).
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Top panel: above view of the L 98-59 planetary system on BJD = 2460000 assuming circular orbits. The line of sight toward Earth is to the right. The Habitable Zone defined in R. K. Kopparapu et al. (2013) is shown in green for runaway/maximum greenhouse (conservative) and pale green for early recent Venus/early Mars (optimistic). Bottom panel: comparative exoplanetology of M-dwarf multiplanetary systems ordered by stellar effective temperature and planetary instellation. An arbitrary shift of +100 K in Teff has been applied to TOI-700 and Teegarden’s star for clarity. In both panels, transiting (nontransiting) exoplanets are shown as filled (open) circles, with circle size proportional to planetary radius. For planets with only a minimum mass constraint, the radius is set to the 95th percentile of the prediction from spright (H. Parviainen et al. 2024).
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Family portrait of the five planets in the L 98-59 system showing their transit (or absence of transit) observed by TESS in the top panels and their Doppler signature from HARPS (red circles) and ESPRESSO (white/black circles for pre/post data) in the bottom panels. Only the error bars for ESPRESSO are shown to improve visibility. Black curves represent best-fit models from the transit analysis (top) and joint RV–TTV fit (bottom, using fixed orbital inclinations; see Section 4.5). For L 98-59 e and f, 1000 predicted transit curves are shown in red using posterior samples from the RV–TTV fit and radii estimated from their minimum masses using spright (H. Parviainen et al. 2024). Planets e and f do not transit L 98-59.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Sub-kelvin differential temperature measurements of L 98-59 from ESPRESSO and HARPS, with only the error bars for ESPRESSO displayed for clarity. The posterior distributions on the hyperparameters for a quasiperiodic GP regression are shown above with the median GP prediction shown with the orange curve and 1σ uncertainty envelope. The dTemp indicator revealed that L 98-59 is a relatively quiet star with a rotational period of 76.7 ± 1.5 days.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Mass–radius constraints on the L 98-59 planets (b: green, c: purple, d: red, e: blue, f: teal) with other exoplanets around M dwarfs in the background (gray points). The previous values from D21 are shown in black attached to revised measurements. For L 98-59 e and f, 1σ and 2σ confidence contours are shown with the radius estimated using spright (H. Parviainen et al. 2024) and with a cross symbol showing the two modes (rocky and volatile-rich). Rocky composition curves from L. Zeng et al. (2019) are drawn from pure iron to pure silicate rocks. Water-rich interior models at T = 400 K from A. Aguichine et al. (2021) are shown with dotted blue curves. The orange region delimits a degeneracy (H2- or H2O-rich) in composition (J. G. Rogers et al. 2023).
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Marginalized 1D and 2D posterior distributions of internal structure parameters for L 98-59 b (left), c (center), and d (right) derived with smint (C. Piaulet et al. 2023). The 2D posteriors display the 1σ and 2σ contours. The analysis constrains the core- and water-mass fractions (﹩f{{\prime} }_{{\rm{core}}}﹩, ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩) using priors on planetary mass (Mp) and irradiation temperature (Tirr; not shown), while requiring consistency with the observed planetary radius (Rp). The sub-Earth L 98-59 b is assumed to be purely rocky (﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}=0﹩). We explored a pure rocky model for L 98-59 c and water-rich models for L 98-59 c and d with either a uniform prior on ﹩f{{\prime} }_{{\rm{core}}}﹩ (“up”) or using ﹩f{{\prime} }_{{\rm{core}}}﹩ from planet b as a prior (“bp”). L 98-59 b has an ﹩f{{\prime} }_{{\rm{core}}}﹩ consistent with a wide range of iron content in the interior (from coreless to super-Mercury), with a mode close to Earth’s value (﹩f{{\prime} }_{{\rm{core}}}=0.325﹩; H. S. Wang et al. 2018). L 98-59 c likely has a small ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}\sim 0.03﹩ to explain its mass and radius. For L 98-59 d, we infer a statistically significant ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ = 0.16–0.18 irrespective of the choice of prior.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Internal energy balance inferred with melt (M. S. Peterson et al. 2023) for L 98-59 b (top panel) and c (bottom panel) as a result of tidal heating. We show the tidal heating flux per unit surface area (solid lines) and the convective heat flux (dashed lines) as a function of mantle temperature, with the equilibrium points shown as circles, colored according to the value of the melt fraction coefficient B adopted in the model (methods in Appendix C.3). The solidus temperature is shown as the vertical black line. The equilibrium happens beyond the solidus for L 98-59 b, at similar heat fluxes to those inferred for Jupiter’s moon Io, implying a potential molten magma layer under the planets’ surfaces, which could be conducive to active volcanic activity. The lower eccentricity-driven tidal flux for planet c results in equilibrium mantle temperatures consistent with a solidified mantle or marginally beyond the solidus. Under these conditions, we cannot conclude that L 98-59 c has a partially molten mantle layer.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Transit timing variations (TTVs) of L 98-59 c (top) and L 98-59 d (bottom) from TESS (white circles), HST (red cross), and JWST (green circles) with a zoomed-in region shown on the right. The HST partial transit of L 98-59 c was not included in the fit. The blue curve depicts the median TTV model from the joint RV–TTV fit using a fixed inclination for all planets. A 68% confidence envelope is shown in lighter blue and was determined from 1000 random solutions drawn from the posterior distribution. The red dashed curve shows a TTV model without the outer nontransiting planets L 98-59 e and f.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Summary of the RV component from the joint RV–TTV fit. Left panels: radial velocity (RV) of L 98-59 from ESPRESSO and HARPS decomposed into many components (activity and planets). For clarity, only the error bars from ESPRESSO are shown. The first row shows the raw RVs with systemic offsets removed. Each subsequent row sequentially subtracts one component at a time in decreasing order of variance (activity GP, then planets c, e, f, d, and b). Right panels: Lomb–Scargle periodograms computed on the combined data at each step. The false-alarm probability (FAP) of 0.1% is shown with a dotted horizontal line.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Normalized PDCSAP light curve of L 98-59 from TESS between 2018 August 23 (sector 2) and 2025 April 9 (sector 90). Photometry taken during the transit of L 98-59 b, c, and d is highlighted in green, purple, and red, respectively. The black line is the median GP model of the out-of-transit light curve (details in Section 3.1). The GP amplitude (σphot) and coherence timescale (τ) are indicated for each sector. Our GP models were compatible with a baseline flux f0 = 1 and no additional jitter (σjitter = 0 ppm) for all sectors.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Marginalized posterior distributions of the orbital eccentricities of the L 98-59 planets from the joint TTV–RV fit (fixed inclinations) using the full data set (black) and TTVs from TESS only (red). The 2D posteriors show 1σ, 2σ, and 3σ contours.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Detection sensitivity map of Keplerian signals in the ESPRESSO and HARPS data. The semiamplitudes of L 98-59 b–f are depicted with inverted triangles for transiting and circles for nontransiting planets. The detection significance is calculated from the false-alarm probability in a Lomb–Scargle periodogram, corresponding to a blind search for periodic signals in a data set. Orange dashed and dotted vertical lines highlight the stellar rotational period (Prot) and its first harmonic (Prot/2). Our activity modeling with a quasiperiodic GP suppresses small injected signals (K ≈ 1–2 m s−1) at long periods and close to the stellar rotation period and harmonics. The ESPRESSO and HARPS RVs are sensitive to planets c–f in a blind search, and to planet b in an informed search using the period and phase constrained by transit.
Paper: Detailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Authors: Charles Cadieux, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, René Doyon, Étienne Artigau, Neil J. Cook, Louis-Philippe Coulombe, Pierre-Alexis Roy, David Lafrenière, Pierrot Lamontagne, Michael Radica, Björn Benneke, Eva-Maria Ahrer, Drew Weisserman, Ryan Cloutier
Figure caption: Posterior distributions of Kk (left), ek (center), and ωk (right) for the L 98-59 planets from an RV-only fit and the joint RV–TTV fit (fixed-inclination model). The eccentricity distributions are normalized so that their heights are equal to improve visibility. The small TTVs detected on L 98-59 c and d provide significant constraints on the orbital architecture of the system.
Paper: BLADE: An Automated Framework for Classifying Light Curves from the Center for Near-Earth Object Studies Fireball Database
Authors: Elizabeth A. Silber, Vedant Sawal
Figure caption: Light curve analysis of the event on 2006 October 14 at 18:10:49 UTC. (a) Intensity-vs-time plot showing two dominant peaks corresponding to distinct fragmentation events. (b) Intensity-vs-altitude plot indicating that the primary peaks occurred at altitudes of ~47 and 44 km, with additional fluctuations suggesting possible secondary fragmentation. (c) Normalized light curve. (d) Gradient analysis and peak detection plot, where the green dashed line represents the gradient, the blue line indicates the normalized light curve, and red dots mark the detected peaks.