adsabs/AstroCLIMB huggingface dataset:
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: Schematic workflow diagram summarizing the BLADE algorithmic framework. Each analytical step is indicated sequentially, beginning with data ingestion and metadata matching (Step 1) from the CNEOS database, followed by digitization, normalization (Step 2), adaptive Savitzky–Golay filtering (Step 3), prominence-based peak detection (Step 4), gradient analysis (Step 5), and subsequent classification into defined fragmentation categories (Step 6). An optional altitude extrapolation step (Step a), requiring velocity-vector data, can be performed concurrently and then integrated after gradient analysis (Step b) to assign altitudes to detected peaks, using the known altitude at peak brightness as an anchor. Parameter settings employed at each stage, including Savitzky–Golay filtering parameters and peak detection thresholds, are explicitly indicated. The resulting fragmentation classification categories (continuous fragmentation, discrete fragmentation, airburst, single peak, and no significant peaks) and their defining criteria are also shown.
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: Analysis of the 2015 May 10 07:45:01 UTC event demonstrating continuous fragmentation. (a) Intensity-vs-time plot showing a multipeaked structure. (b) Intensity-vs-altitude plot highlighting primary and secondary peaks at ∼30 km and ∼27 km, respectively. (c) Normalized-intensity-vs-time plot emphasizing relative peak dominance. (d) Gradient analysis with detected peaks (red markers) identifying multiple fragmentation events.
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: Analysis of the 2019 November 28 (20:30:53 UTC) event, classified as a continuous fragmentation. (a) Intensity-vs-time plot showing a broad primary peak and multiple subpeaks, indicative of complex energy deposition. (b) Intensity vs altitude. (c) Normalized-intensity-vs-time plot. (d) Normalized light curve with gradient overlay and detected peaks, showing significant intensity changes and fragmentation dynamics.
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 2018 December 18 23:48:18 UTC airburst event. (a) Intensity vs time showing a dominant peak at ~0.35 s. (b) Intensity vs altitude indicating a peak energy release at ~26 km. (c) Normalized light curve. (d) Gradient analysis with the detected peak marked at 0.35 s, confirming a single energy release characteristic of an airburst.
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 2015 June 14 03:03:06 UTC event, classified as discrete fragmentation. (a) Intensity vs time. (b) Intensity vs altitude shows the primary fragmentation at ∼30 km, with secondary events at ∼35 and ∼28 km. (c) Normalized light curve emphasizes the prominence of individual peaks. (d) Gradient and detected peaks confirm discrete fragmentation.
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: Global detections of bolides reported on the CNEOS website from 1988 to 2024 (plotted are 808 events, which have the geographical location). Cyan circles and yellow stars show all events within the subset selected for this study, with the latter having the velocity vector available.
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: Box-plot statistical comparison of bolide classification categories (airburst, single peak, discrete fragmentation (Dis. Frag.), and continuous fragmentation (Cont. Frag.)) across (a) altitude, (b) entry angle, (c) impact energy, and (d) entry velocity. Box boundaries represent the lower (Q1) and upper (Q3) quartiles, with the central line indicating the median. Whiskers extend to ±1.5 × IQR (interquartile range), and outliers beyond this range are plotted individually. The legend shown in panel (a) is applicable to all panels.
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 for the 2018 June 21 01:16:20 UTC event. (a) Intensity vs time showing a single peak. (b) Intensity vs altitude indicating localized energy deposition. (c) Normalized light curve. (d) Gradient analysis with detected peak, supporting single-peak classification, though evidence suggests an airburst event requiring further algorithm refinement.
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: Distribution of bolide events classified into four categories: airburst, continuous fragmentation, discrete fragmentation, and single peak.
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: Relationships between impact energy and altitude, velocity, and entry angle across different classification categories.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Top: the normalized and telluric corrected stellar spectrum over all orders are plotted, arranged in descending order from left to right, with order 9 on the far left and order 1 on the far right. Orders with observations included in our cross correlation analyses are marked in black, orders discarded in gray. Bottom: the input synthetic transmission spectrum for a 3 R⊕, 5 M⊕ planet hosting a clear, solar metallicity atmosphere is plotted. All modeled lines within the spectral region observed come from water absorption.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: We make use of a median out-of-transit stellar spectrum to remove the stellar spectral signal over the helium line triplets range. Temporal variations of the stellar spectrum are shown. The median removal is performed on a per-visit, per nodding position basis, as each visit and nodding position has its own associated systematics. Top: observations over the first CRIRES+ visit, from nodding position A, prior to median division. Stellar absorption features appear as deep vertical stripes that are constant in velocity within the stellar rest frame. Bottom: the spectral residuals after applying median division, demonstrating the removal of stellar spectral features while preserving any potential planetary signal.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Environmental variations over the course of both transit observations. Included are variations in airmass, seeing, and per pixel signal to noise over the helium triplet at 1083 nm over the course both nights. The vertical lines across all plots represent times of ingress and egress for both visits, respectively.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Lightcurves for visit 1 (top) and visit 2 (bottom) that trace along where we would expect the metastable helium triplet of lines to be present. The optical transit of HIP94235b is depicted by shaded gray regions. Lightcurves with transit depths based on different mass-loss rates are shown in teal (﹩\dot{M}﹩ = 1011 g s−1) and blue (﹩\dot{M}﹩ = 1012 g s−1).
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Cross-correlation peak signal to noise as a function of the assumed orbital and systemic velocities of the planet, averaged over both nights of observations. For a circular orbit, the expected velocities of the planetary system are Kp = 111 km s−1 and Vsys = 9 km s−1. We find no evidence of excess absorption originating from the planet.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: One example CRIRES+ spectrum of HIP94235b obtained during visit 1. Top Extracted spectrum from all nine spectral orders, arranged in descending order from left to right, with order 9 on the far left and order 1 on the far right. Middle Normalized stellar spectrum over the helium infrared triplet at 1083 nm. The wavelengths of the helium infrared triplet are marked by the vertical lines. Bottom Telluric corrected portion of the spectrum over the helium infrared triplet region.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Evolution tracks for HIP94235b’s radius (left) and envelope mass fraction (right) evolution over the first Gyr. The top panel shows the allowed tracks before these CRIRES+ results, with the bottom panel showing the observationally constrained tracks. HIP94235b has formed with a radius of 3.5–4.2 R⊕ and an initial envelope mass fraction of 3%–10%. The transparent blue bars in each figure show the error on the planet radius (R = 3.00﹩{}_{-0.28}^{+0.32}﹩ R⊕) as the horizontal transparent region, and planet age (120 ± 50 Myr) as the vertical transparent region.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Cross-correlation-function variations over the two transit visits. Cross correlations are performed against a high-resolution line-by-line spectral model of a 3 R⊕, 5 M⊕, solar metallicity atmosphere. The expected velocity variation of the planet, assuming a circular orbit, over the observations is marked by the dashed line. The times of ingress and egress are marked by the horizontal lines.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Spectral residuals as a function of time since mid-transit (hours) and wavelength (nm). Visit 1 is in pink and visit 2 is in orange. The solid horizontal lines represent ingress and egress. The slanted dashed lines mark the wavelengths of the metastable helium triplet of lines, Doppler shifted to the rest frame of the planet. The colorbar on the right represents the amount of excess absorption within the plot in percent.
Paper: Searching for Helium Escape and a Low-density Atmosphere Around the 120 Myr Old Sub-Neptune HIP94235b Using CRIRES+
Authors: Ava Morrissey, George Zhou, Chelsea X. Huang, Duncan Wright, Neale Gibson, Keighley E. Rockcliffe, Elisabeth R. Newton, James Kirk, Daniel Bayliss
Figure caption: Recovery of the injected transmission signal of a clear, solar metallicity planetary model. Top: we find the planetary signal can only be recovered at the 2σ level when the stellar signals are subtracted via a simple removal of the median spectrum. Bottom: SYSREM removal of the stellar signal (over 4 iterations) removes the injected planetary signal, with no signals retrieved. The velocities of the injected signal are marked by the dashed lines.
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: The TESS folded light curves for six DWD systems whose periodograms are displayed in Figure 1. The name of each system is mentioned inside the panel. The binned data are represented by red circles. To better discern the periodic trends in data, we have included horizontal blue lines indicating constant flux in each panel.
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: The LS periodograms related to the TESS light curves of six known DWD systems. The name of each target is reported at the top of each panel. The thick colored and vertical lines specify the orbital period, its half, double, triple, etc. These lines are depicted to compare the orbital period and its proper fractions/multiples with the period of their most-dominant signal with the maximum LS power.
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: The expected amplitude in the normalized flux due to Doppler boosting (given by Equation (3)) varies with the inclination angle and when considering different values for the mass of the secondary companion in LP400−22. We assume a circular orbit in the simulation.
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: The amplitudes of ellipsoidal variations for two targets J2132+0754 and LP400−22 vary with the inclination angle and by considering different values for the mass of the secondary components (represented by different colors) and the radius of the primary components (represented by different line styles). The thick red lines represent the amplitudes of the observed periodic trends in their TESS light curves Δn. We utilize the analytical relation provided by S. L. Morris & S. A. Naftilan (1993) to evaluate the amplitude of the ellipsoidal variation.
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: Left panel: The target pixel file drawn from the TESS data at the position TIC 1101113865. The flux of this target is extracted from pixels specified with a dashed pattern. Right panel: The map of blending stars around this target (TIC 1101113865 or J1449+1717 as identified with a green star) extracted from the Gaia data archive. The variable and bright star in this field is marked by a blue triangle.
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: The expected light curve for the DWD J1717+6757 taking into account self-lensing (plotted by dashed green curve), eclipsing effect (dotted–dashed red curve), and ellipsoidal variation (dotted blue curve). The overall flux due to the two components is shown by the solid black curve. The parameters used to create this light curve are reported in the first row of Table 3.
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: The folded and denoised light curves due to two DWD systems J0112+1835 (left panel) and J0056−0611 (right panel), respectively. TTESS values are periods of trends with the maximum LS powers (mentioned in the sixth column of Table 1).
Paper: Probing Periodic Trends in the TESS Light Curves of the Seventeen Known Double White Dwarf Systems
Authors: Sedighe Sajadian, Aref Asadi
Figure caption: The LS periodograms related to the TESS light curves of DWD systems J0112+1835 (left panel) and J0056−0611 (right panel). The colored and thick lines are plotted at their orbital periods, and proper fractions or multiples of their orbital periods.
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: Simulated hot Jupiter occurrence as a function of Rbirth based on the hot Jupiter-metallicity power law from D.-C. Chen et al. (2023). The mean occurrence and standard deviation of 1000 sets of injections are plotted. Top left: GALAH (green squares), APOGEE (purple circles), and NIHAO simulation (gray diamonds) data show decreased rates of hot Jupiter occurrence from 5 to 14 kpc. The NIHAO simulation and APOGEE distributions are similar. Top right: GALAH and APOGEE data colored by mean absolute vertical velocity. Discrepancies in planet occurrence between the two surveys at Rbirth < 5 kpc are correlated to differences >5 km s−1 in mean stellar vertical velocities, where APOGEE stars are kinematically hotter. Bottom left: mean [Fe/H] binned by Rbirth for GALAH and APOGEE sample as solid markers and planet host population as unfilled markers. The mean metallicity reflects the simulated planet occurrence trends in the top left panel, where APOGEE stars with Rbirth < 5 kpc are more metal poor by 0.2–0.4 dex compared to GALAH stars at the same Rbirth. Bottom right: mean [α/Fe] binned by Rbirth for GALAH and APOGEE sample as solid markers and planet host population as unfilled markers.. APOGEE stars with Rbirth < 5 kpc are more α-enriched by 0.2 dex compared to GALAH stars at the same Rbirth. The net increase in mean [Fe/H] in the planet host population vs. the entire sample reflects the planet frequency–metallicity power law used to inject stars with hot Jupiters. Because of this exponential weighting, even small shifts in the distribution of metal-rich stars in APOGEE across Rbirth shift the peak of planet occurrence and thus the mean [Fe/H] of the planet host population inward by 2 kpc independently of the peak in mean [Fe/H] at 7 kpc.
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: GALAH (left) and APOGEE (right) identified planet hosts in the [Fe/H]–[α/Fe] plane colored by inferred Rbirth. While most planet hosts were born at 5 kpc, just inward of the current solar neighborhood at 8 kpc, there are stars that have migrated from Rbirth of 0–13 kpc. The colored lines trace different chemical evolution sequences across the disk, as defined in Equations (1) and (2) from K. Wang et al. (2024) and J. Mills et al. (2025, in preparation) with each line corresponding to a distinct Rbirth bin (in 2 kpc intervals). In this figure only, we show Rbirth tracks that are slightly shifted from those presented in Equations (1) and (2) to reflect a more physically motivated Rbirth calibration. The rest of our plots and analysis use the unshifted calibration. We discuss the shift in Section 5.5, where we also show that the relative trends and core conclusions of our work are unaffected.
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: Overview of stellar properties in the APOGEE sample. Left: Rcurrent and Z distribution. Top right: [Fe/H]–[Mg/Fe] plane colored by density with low and high-α sequence boundary shown by red line. 13% of the APOGEE sample’s stars belong to the high-α sequence. Bottom right: distribution of stars in the Teff–﹩﹩ plane colored by [Fe/H].
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: Rcurrent and Z coordinates (left) and [Fe/H]–[O/Fe] plane colored by their ages (right) of stars from the NIHAO-UHD (T. Buck 2020) simulation in the same spatial range as known planet hosts. We show the low and high-α sequence boundary with the red dashed line that was fit by eye following Figure 3 of T. Buck (2020). The NIHAO sample is made up of 30% high-α sequence stars.
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: Spatial and kinematic distribution of APOGEE stars colored by calculated phase-space densities following the calculation and visualization outlined in Figure 1 of A. J. Winter et al. (2020). Left: Rcurrent–Z spatial distribution APOGEE catalog colored by P(dense). Right: VR–VZ velocity distribution colored by P(dense). The stars classified as being in the overdense environments are evident, given their close proximity to neighbors spatially and kinematically compared to the stars classified as being in underdense environments.
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: Overview of stellar properties in the GALAH sample. Left: Rcurrent and Z distribution. Top right: [Fe/H]–[α/Fe] plane colored by density with low and high-α sequence boundary shown by red line; 5% of the GALAH sample’s stars belong to the high-α sequence. Bottom right: distribution of stars in the Teff–﹩{\mathrm{log}}g﹩ plane colored by [Fe/H].