adsabs/AstroCLIMB huggingface dataset:
Paper: Possibility of Secondary i- and s-processes Following r-process in the Collapsar Jet
Authors: Zhenyu He, Toshitaka Kajino, Motohiko Kusakabe, Shan-Gui Zhou, Hiroyuki Koura, Satoshi Chiba, Haining Li, Yangming Lin
Figure caption: (a): Time evolution of neutron mole fraction Y  n  (black lines) and neutron number density n  n  = ρ N A Y  n  (blue lines), for decelerated expansion α = 0.62 (solid lines) and free expansion α = 1 (dashed lines). (b)–(d): Illustration of the isotopic abundances (red) and main nuclear flows (blue lines) for α = 0.62 at (n  n /cm−3, t/s)= (1.75 × 1020, 4.5), (2.36 × 1013, 3.8 × 102), and (2.13 × 107, 2.1 × 106) for (b), (c), and (d), respectively. The gray region covers nuclei included in the network, and the black squares correspond to the stable nuclei. The logarithmic isotopic abundances are illustrated by the darkness of red.
Paper: Possibility of Secondary i- and s-processes Following r-process in the Collapsar Jet
Authors: Zhenyu He, Toshitaka Kajino, Motohiko Kusakabe, Shan-Gui Zhou, Hiroyuki Koura, Satoshi Chiba, Haining Li, Yangming Lin
Figure caption: Top panel: relative abundance of heavy elements as a function of atomic number. Black dots are observed abundances in the CEMP-r/s star CS31062-050 (see Hampel et al. 2016 and references therein). The red solid line corresponds to the best fit combining solar s-process abundances (Asplund et al. 2009; Bisterzo et al. 2014) and collapsar nucleosynthesis yields in this study. The blue dashed line is the best fit achieved by combining solar s-process abundances and solar r-process residuals (Goriely 1999). For comparison, we also show the final yields of collapsar nucleosynthesis scaled to Eu (green dotted line). Bottom panel: the differences between observations and two best-fit models. Values of Y (Z = 39) are out of this region, which have Δlog(Y) = 1.60 (red circle) and 1.65 (blue triangle). Note that χ 2 values in the legend are estimated only for elements from Ba (Z = 56) to Hf (Z = 72).
Paper: Possibility of Secondary i- and s-processes Following r-process in the Collapsar Jet
Authors: Zhenyu He, Toshitaka Kajino, Motohiko Kusakabe, Shan-Gui Zhou, Hiroyuki Koura, Satoshi Chiba, Haining Li, Yangming Lin
Figure caption: (a) Mass-weighted sum of final abundances in collapsar jet nucleosynthesis for decelerated propagation (α = 0.62; red solid line). The black solid line is the result without the effect of residual neutron captures at a later phase t > 5 s. (b) Solar s-process abundances (open squares; Bisterzo et al. 2014) and solar r-process residuals (filled circles) derived by subtracting the s-process yields from observed solar abundances (Lodders et al. 2009).
Paper: Possibility of Secondary i- and s-processes Following r-process in the Collapsar Jet
Authors: Zhenyu He, Toshitaka Kajino, Motohiko Kusakabe, Shan-Gui Zhou, Hiroyuki Koura, Satoshi Chiba, Haining Li, Yangming Lin
Figure caption: Percentage of the i-process contribution F  i  of 31 r-only nuclei in the mass region 70 < A < 210, for decelerated expansion α = 0.62 (red circles) and free expansion α = 1 (blue circles). The labeled circles represent the nuclei dominated by the i-process contribution F  i  > 50% for α = 0.62.
Paper: Possibility of Secondary i- and s-processes Following r-process in the Collapsar Jet
Authors: Zhenyu He, Toshitaka Kajino, Motohiko Kusakabe, Shan-Gui Zhou, Hiroyuki Koura, Satoshi Chiba, Haining Li, Yangming Lin
Figure caption: Nuclear flow paths related to the synthesis of 151Eu. The corresponding r-, i-, and s-process flows are depicted by red, blue, and green arrows, respectively. The value in the parenthesis indicates the half-life of each unstable nuclide.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: The top panels, respectively, compare the time variations of the QPO count rate and instantaneous phase between the decomposed QPO IMF (in blue) and synthetic QPO signal (in gray) in a representative 20 s time range. The two middle panels present the parameter correlations between decomposed and synthetic QPO signals using all time bins. The two bottom panels show the histograms of count rate difference and phase difference between the simulated QPO and decomposed QPO signals from all time bins. The orange dashed lines displayed in the middle and bottom panels represent the case that the two signals are in perfect alignment.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: Left: simulated light curve composed of a red noise and a QPO component. In this simulated signal, the Poisson noise is also considered. Right: Fourier power spectra that are produced from the original total light curve (in black), simulated QPO component (in gray), and decomposed QPO component (in blue), respectively.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: Phase-folding profiles of the simulated total (in blue) and noise (in red) light curves. The phase-folding is performed by using the instantaneous phase function of the decomposed QPO IMFs and by combining the seven simulated light curves (see the corresponding main text for details).
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: The top two panels, respectively, present relationships between QPO fractional rms and significance of modulations in the total (in blue) and QPO-subtracted (in red) profiles in the energy ranges of 150–170 and 170–200 keV, where the red noise fractional rms is fixed at 30%. The bottom two panels present relationships between red noise fractional rms and the significance of modulations in the total and QPO-subtracted profiles, where the QPO fractional rms is fixed at 15%. The purple dotted lines plotted in four panels represented that the modulation in profiles can be determined at a 5σ confidence level.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: The top two panels, respectively, present phase-folding profiles of total (in blue) and QPO-subtracted (in red) light curves sampled from 104 simulated light curves in the energy ranges of 150–170 and 170–200 keV. The bottom two panels present the distributions of the maximum cross-correlations between phase-folding profiles of the simulated total (in blue), QPO-subtracted (in red), pure Poisson noise (in gray) light curves in the two high energy bands and the profile of the total light curve in the low energy band presented in Figure 11.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: Examples of cross-correlation of 120–130 and 170–200 keV QPO waveforms with the 30–120 keV QPO waveform. The upper panels plot the cross-correlation vs. phase lag for a specified waveform with the 30–120 keV QPO waveform. The lower panels show the cross-correlation distribution from 104 Monte Carlo simulations of two noncorrelated waveforms. The dashed vertical lines plotted in the lower panels indicate the peak cross-correlation values as observed in the upper panels.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: Power density spectra of the simulated pure Poisson noise (in black) and the corresponding VMD IMFs (in colors). The decomposed IMFs are evenly distributed in frequencies, suggesting that VMD is essentially a set of adaptive Wiener filter banks capable of separating modes with different center frequencies.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: Power density spectra of the simulated light curves in the energy ranges of 150–170 (in orange) and 170–200 (in blue) keV.
Paper: A Candidate Supermassive Black Hole in a Gravitationally Lensed Galaxy at Z ≈ 10
Authors: Orsolya E. Kovács, Ákos Bogdán, Priyamvada Natarajan, Norbert Werner, Mojegan Azadi, Marta Volonteri, Grant R. Tremblay, Urmila Chadayammuri, William R. Forman, Christine Jones, Ralph P. Kraft
Figure caption: BH growth tracks for different initial seed masses and accretion rates assuming continuous accretion with a radiative efficiency of 10%. Light BH seeds only reach 104–105 M ⊙ mass by z ≈ 10.4 accreting at their Eddington limit. The estimated ∼8.0 × 107 M ⊙ mass for its redshift of z ≈ 10.37, however, places the candidate BH of GHZ 9 as originating from a heavy seed, similar to UHZ 1 (Bogdán et al. 2024). While sustained accretion above the Eddington limit is unlikely (Willott et al. 2010; Smith et al. 2018), we also show the growth curves assuming f Edd = 2 for light seeds with the hatched region, which would also be able to produce BH masses estimated for GHZ 9 and UHZ 1. We show three previously known highest redshift quasars at z ∼ 7.5 identified in large-area optical surveys (Mortlock et al. 2011; Bañados et al. 2018; Wang et al. 2021b).
Paper: A Candidate Supermassive Black Hole in a Gravitationally Lensed Galaxy at Z ≈ 10
Authors: Orsolya E. Kovács, Ákos Bogdán, Priyamvada Natarajan, Norbert Werner, Mojegan Azadi, Marta Volonteri, Grant R. Tremblay, Urmila Chadayammuri, William R. Forman, Christine Jones, Ralph P. Kraft
Figure caption: The 0.5–3 keV band Chandra image of GHZ 9-X and its surroundings centered around the neighboring star. A source region of a r = 2″ circle (green region) and a background wedge centered around the star (black region) were applied to account for the net counts in our second approach (Section 4.1). A circle with r = 3″ around the star (red region) was excluded from the analysis. The color bar indicates the scaled number of counts.
Paper: A Candidate Supermassive Black Hole in a Gravitationally Lensed Galaxy at Z ≈ 10
Authors: Orsolya E. Kovács, Ákos Bogdán, Priyamvada Natarajan, Norbert Werner, Mojegan Azadi, Marta Volonteri, Grant R. Tremblay, Urmila Chadayammuri, William R. Forman, Christine Jones, Ralph P. Kraft
Figure caption: Chandra ACIS and JWST NIRCam images of the z ≈ 10.4 galaxy, GHZ 9, and its surroundings. Panel (a) shows the 0.5–3 keV band X-ray mosaic of A2744 marking the position of GHZ 9. Panels (b) and (c) are zoomed-in JWST NIRCam images showing the surroundings of GHZ 9. Panel (d) presents postage stamp NIRCam images of GHZ 9 and its projected neighbor, a z ≈ 1.6 galaxy, in seven bandpass filters. GHZ 9 is not detected in the two shortest wavelengths, indicating its Lyman-break nature. Panel (e) is the Chandra and JWST composite image of the immediate vicinity of GHZ 9. The z ≈ 10.4 galaxy, GHZ 9, is cospatial with the X-ray source, while panel (f) is the Chandra counts image of GHZ 9.
Paper: A Candidate Supermassive Black Hole in a Gravitationally Lensed Galaxy at Z ≈ 10
Authors: Orsolya E. Kovács, Ákos Bogdán, Priyamvada Natarajan, Norbert Werner, Mojegan Azadi, Marta Volonteri, Grant R. Tremblay, Urmila Chadayammuri, William R. Forman, Christine Jones, Ralph P. Kraft
Figure caption: Predicted luminosity function of AGN at z = 8 (left panel) and z = 10 (right panel) for light and heavy SMBH seed models (adapted from Ricarte & Natarajan 2018). Overplotted are the observed lower limits on the number density at z = 8 (Greene et al. 2024) and at z = 10 based on the detections of AGN behind A2744 (i.e., UHZ 1 and GHZ 9). The number density of AGN at z = 10 drastically exceeds theoretical expectations.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: Hilbert–Huang transform analysis of a representative example of a 14 s long light curve with a 0.05 s time resolution of HE in the energy range of 30–120 keV. (a) Representative example of a 14 s long light curve and corresponding five IMFs obtained from VMD algorithm. (b) Power density spectra of the original HE light curve, as well as the second and third IMFs. (c) The QPO (the second) IMF and corresponding phase function, instantaneous frequency, and amplitude.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: The Hilbert–Huang transform (HHT) phase-folded QPO waveforms of MAXI J1535–571 from Insight-HXMT/HE light curves. To enhance the S/N, waveforms from all selected observations have been collectively combined, and the final combined waveform is normalized by the mean value of the count rate. These QPO phases are obtained through HHT analysis of light curves in the 30–120 keV energy band. Each panel showcases the significance level determined via the cross-correlation technique, as detailed in Appendix C.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: The long-term combined power density spectra (PDS) of 30–100 (in blue) and 100–200 (in red) keV energy bands. The shaded region highlights the frequency range where the QPO fundamental is observed.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: Power density spectrum of the HXMT/HE observation P011453500201 in the 30–120 keV energy band fitted with a model consists of a broken power-law function (plotted in red) and two Lorentzian functions (plotted in blue). In the plotted power density spectrum, Poisson noise has been subtracted.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: The fitting results of the waveforms with the jet precession model in the energy bands between 130 and 200 keV. Sequentially from left to right, the fitting results for the energy bands of 130–150, 150–170, and 170–200 keV are depicted. All data points displayed have undergone background subtraction. The red solid lines represent the jet precession model plotted from the posterior distribution derived with the Markov Chain Monte Carlo method.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: The best-fitting phases (a) and amplitudes (b) of two harmonically related cosine functions are plotted as a function of the photon energy.
Paper: Recovery of High-energy Low-frequency Quasiperiodic Oscillations from Black Hole X-Ray Binary MAXI J1535–571 with a Hilbert–Huang Transform Method
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Jing Q. Peng, L. Ji, Peng J. Wang, Z. Chang, Zhuo L. Yu, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, X. Ma, L. Zhang, W. Yu, J. Li
Figure caption: HE light curves of MAXI J1535–571. In this plot, red triangles denote observations with type-C QPO detection, while blue circles represent those without type-C QPO detection. Each point represents one observation, and the shaded area indicates the selected observations for detailed timing analyses.
Paper:  tdescore: An Accurate Photometric Classifier for Tidal Disruption Events
Authors: Robert Stein, Ashish Mahabal, Simeon Reusch, Matthew Graham, Mansi M. Kasliwal, Marek Kowalski, Suvi Gezari, Erica Hammerstein, Szymon J. Nakoneczny, Matt Nicholl, Jesper Sollerman, Sjoert van Velzen, Yuhan Yao, Russ R. Laher, Ben Rusholme
Figure caption: “Waterfall plots” produced by SHAP for a TDE (top) and an SN Ia (bottom), demonstrating the thinking behind the tdescore classifications. In both plots, red/right is more TDE-like, while blue/left is less TDE-like. The four most salient features for each source are shown, with the actual value for each parameter given in the leftmost column. Top: the TDE (ZTF19aapreis) has WISE colors inconsistent with an AGN host (W1–W2 = 0.0), has a blue color at peak (g − r = −0.3), is very nuclear (0.″1 offset to PS1), and has very little cooling (0.003 mag per day). All these variables lead to a TDE classification. Bottom: the SN (ZTF19aanyuyh) also has WISE colors inconsistent with an AGN host (W1–W2 = 0.0) and a high detection rate (one data point per 1.3 days), supporting a possible TDE classification. However, the source also fades very rapidly (9.3 days), and is somewhat offset from its PS1 host (0.″4). In combination, these other variables lead to a non-TDE classification. In both cases, the tdescore use of features closely approximates the reasoning that would be employed by an astronomer.
Paper:  tdescore: An Accurate Photometric Classifier for Tidal Disruption Events
Authors: Robert Stein, Ashish Mahabal, Simeon Reusch, Matthew Graham, Mansi M. Kasliwal, Marek Kowalski, Suvi Gezari, Erica Hammerstein, Szymon J. Nakoneczny, Matt Nicholl, Jesper Sollerman, Sjoert van Velzen, Yuhan Yao, Russ R. Laher, Ben Rusholme
Figure caption: Prediction-normalized confusion matrices (left) and truth-normalized confusion matrices (right), showing the performance of tdescore on the real data for different thresholds. The data set is highly imbalanced, as seen in Figure 2. The source shuffling is performed ten times, yielding averaged performance across the iterations, with the average expected number of sources for each category shown in parentheses. Top: an inclusive threshold, optimized for recall. At the cost of 5% loss of TDEs, a sample is produced with a TDE fraction increased from ∼2% to ∼46%. Center: an intermediate threshold, chosen to achieve >80% precision. It achieves relatively high recall (77.5%). Bottom: a strict threshold, optimized for precision. >70% of TDEs pass this requirement, yielding a clean sample with <5% contamination rate.
Paper:  tdescore: An Accurate Photometric Classifier for Tidal Disruption Events
Authors: Robert Stein, Ashish Mahabal, Simeon Reusch, Matthew Graham, Mansi M. Kasliwal, Marek Kowalski, Suvi Gezari, Erica Hammerstein, Szymon J. Nakoneczny, Matt Nicholl, Jesper Sollerman, Sjoert van Velzen, Yuhan Yao, Russ R. Laher, Ben Rusholme
Figure caption: An example of the light-curve fitting procedure on a real TDE, ZTF20achpcvt/AT2020vwl (Hodgkin et al. 2020; Hammerstein et al. 2021b), for which limited data were available at peak. Using the two-step fit, the approximate g-band peak time and the color at peak can be inferred for use in classification. AT2020vwl is relatively red with (g − r) ≈ 0, but bluer TDEs with (g − r) > 0 are detected more frequently in g-band. Nonetheless, the fitting procedure still works well for this TDE.
Paper: Ultradeep Cover: An Exotic and Jetted Tidal Disruption Event Candidate Disguised as a Gamma-Ray Burst
Authors: R. A. J. Eyles-Ferris, C. J. Nixon, E. R. Coughlin, P. T. O'Brien
Figure caption: The dependence of the viscous timescale on β and α for rotating (left) and nonrotating 105.5 M ⊙ SMBHs (right). We show to r  p  = r dc, and α is varied from 0.3 to 1 in steps of 0.1. In each panel, the black horizontal line indicates GRB 191019A’s rest frame t 90, and the gray vertical line indicates β  c  = 41.5 for a 105.5 M ⊙ SMBH.
Paper:  tdescore: An Accurate Photometric Classifier for Tidal Disruption Events
Authors: Robert Stein, Ashish Mahabal, Simeon Reusch, Matthew Graham, Mansi M. Kasliwal, Marek Kowalski, Suvi Gezari, Erica Hammerstein, Szymon J. Nakoneczny, Matt Nicholl, Jesper Sollerman, Sjoert van Velzen, Yuhan Yao, Russ R. Laher, Ben Rusholme
Figure caption: Top: breakdown of the various cuts applied to the ZTF nuclear sample. Of 11,699 ZTF sources; 5264 have a secure classification; 3040 also have a well-measured fade; and 2744 sources pass all cuts. Bottom: of these 2744 sources used to train tdescore, 55 (2.0%) are TDEs.
Paper:  tdescore: An Accurate Photometric Classifier for Tidal Disruption Events
Authors: Robert Stein, Ashish Mahabal, Simeon Reusch, Matthew Graham, Mansi M. Kasliwal, Marek Kowalski, Suvi Gezari, Erica Hammerstein, Szymon J. Nakoneczny, Matt Nicholl, Jesper Sollerman, Sjoert van Velzen, Yuhan Yao, Russ R. Laher, Ben Rusholme
Figure caption: Precision and recall as a function of tdescore threshold. The balanced threshold (chosen such that precision is at least 80%) is illustrated by the central dotted vertical line. The inclusive (>95% recall) and clean (>95% precision) thresholds are illustrated by the left and right dotted vertical lines, respectively. The corresponding confusion matrices for these three scenarios are shown in Figure 4.