adsabs/AstroCLIMB huggingface dataset:
Paper: Theoretical Perspective on the Occurrence of Electrostatic Solitary Waves and Double Layers in Ganymede’s Wake Region
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Variation of (a) pseudopotential, S(ϕ) with ϕ, (b) electrostatic potential ϕ, and (c) electric field with ξ for the fast ion-acoustic mode 2 corresponding to Set 2.
Paper: Theoretical Perspective on the Occurrence of Electrostatic Solitary Waves and Double Layers in Ganymede’s Wake Region
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Variation of ϕ with ξ for varied κ values for (a) slow ion-acoustic solitons (M = 0.245), (b) fast ion-acoustic 1 solitons (M = 0.732), and fast ion-acoustic 2 solitons (M = 0.9).
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: Time series of the H+ integrated flux J in the two bands: JI (80–300 keV) and JII (300–2000 keV) plotted in magenta plus and cyan square symbols, respectively. The sampling rate is one sample/minute. In the same diagram, we also depict and number the start (higher black impulse) and end (lower black impulse) of each one of the SEP events reported in Table 1. The radial distance R (right scale) of PSP during orbit 15 is shown by the green line.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: Examples of Gaussian white noise in natural time: panels (A) and (B) depict pk and ﹩{ \mathcal T }{p}_{k}={p}_{N-k+1}﹩, respectively, in an excerpt of N = 100. The transformation of the measured signal Xi (red) to the z-scores Zi (blue) and then to Wi, which are positive and can be analyzed as Qk in natural time, is shown in (C). (D): Log–log plot of the fluctuations of natural time under time reversal Δχs vs. s obtained from the analysis of Wi, where the validity of Equation (4) is shown.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: Spectrogram of proton energy, as a function of time, color-mapped to proton intensity for the entirety of orbit 15. Black color indicates low flux, while gray indicates data gaps. This plot includes data that is smoothed to 1 hr from the provided 1 minute resolution.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: The integrated fluxes J1 (dark blue cross symbols) and J2 (blue open squares) to be read on the right scale together with ΔS300 for band I (red) and band II (magenta) to be read on the left scale vs. time in minutes for the case of SEP events 1 and 2 of Table 1. The values of ΔS300 for band II (magenta line) have been vertically displaced by −0.1 for the sake of clarity. In the same figure, we mark with gray impulses the start and end of each event as reported in Table 1 together with the OT of FNT for J1 (dark green vertical lines) and for J2 (thick black impulses), and the OT of the Hurst method for J1 (orange impulses). The corresponding min(ΔS300) are connected to the baseline with red and magenta impulses, respectively. We also depict for J1 the values of 1 + χH (green circles) and H (purple triangles) divided by 10 (so as to fall within the left scale) when they exceed the 99.9% confidence interval for white noise. The numbers “1” and “2” are vertically positioned at ﹩{J}_{{\rm{\max }}}﹩ for each band, colored accordingly, and indicate the number of the SEP event in Table 1.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: The integrated flux J for energy band I (upper panel labeled (A)) and II (lower panel labeled (B)) vs. time in minutes. In each of these two panels, we also present the time series of the scaling exponents H, aDFA, hCMA, and 1 + χH, estimated at each point by using J during the last 5 hr (300 measurements, only when the fitting of Equations (1)–(4) is reliable a scaling exponent appears in the diagram). The corresponding probability densities are shown vertically on the right. The green color corresponds to values of the scaling exponents that are inside the 99.9% confidence interval for Gaussian white noise, while red color to values that are outside this interval and hence are highly unlikely to come from white noise pointing to persistence.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: The same as in Figure 5 but for band I of orbit 15, see Figures 1 and 2. For convenience we also mark with blue color the start (higher impulses) and end (lower impulses) of the events of Table 1.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: The integrated proton flux J for band I (blue, right scale) together with the entropy change ΔS300 of natural time under time reversal (red, left scale) estimated when analyzing the preceding 300 values of J in natural time (see Section 2.7) vs. time elapsed from the beginning of Figure 4. For this band, the first OT was identified by means of FNT and the cyan shaded area corresponds to a 100 minute interval around this OT. It is this interval that N. V. Sarlis et al. (2024) used to count the minimum value of ΔS300 to get an estimate of ﹩{J}_{{\rm{\max }}}﹩. In the present paper, we found that pursuing for minimum the ΔS300 time series up to 300 minutes after the OT improves the results. Hence, we adopted this new definition of min(ΔS300) here.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: Excerpts of Figure 5 in an expanded timescale to depict the earliest OT for band I (A) and band II (B). The red arrows indicate the OT, which corresponds to the first time the scaling exponent exceeds the 99.9% confidence interval for white noise for three consecutive measurements (minutes in our case). In each panel, we also depict by black circles the integrated flux J, which can be read on the right scale.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: Values of Δtx for each scaling exponent and band vs. the SEP event labels (events 17 and 18 of Table 1 could not be checked due to a lack of data, see Figure 2). On the right part of the figure, we depict the log-normal (Gaussian after taking logarithms) distribution that according to the Kolmogorov–Smirnov–Lilliefors test can be used to describe the data (with values less than 1500 minutes). It has a mean value of ≈90 minutes (101.95±0.87 minutes).
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: Receiver Operating Characteristics diagram for PSP orbit 15 in which the red star corresponds to a hit rate of 87.5% and false alarm rate of 2.2% estimated as lower and higher limits, respectively, for the alarms issued based on the FNT method OT for J1 (see Sections 2.6 and 3). This star is far away from the (blue) diagonal that corresponds to random predictions while the colored contours present the p value (%) to obtain by chance an ROC point when attempting to predict the 16 SEP events of orbit 15 (see Sections 2.8 and 4 as well as N. V. Sarlis & S.-R. G. Christopoulos 2014); the limits with p = 10%, 5%, and 1% are also shown.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: Spectrogram of proton energy, as a function of time, for an SEP event that started on 2023 January 3.
Paper: Persistent Behavior of Low-energy Solar Energetic Particles Observed by Parker Solar Probe During Orbit 15
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. E. Cuesta, L. Y. Khoo, M. M. Shen, J. S. Rankin, N. A. Schwadron
Figure caption: The same as in Figure 8 but for band II of orbit 15, see Figures 1 and 2.
Paper: Spectral Properties of Globally Distributed ENA Fluxes across Diverse Regions of the Heliosphere
Authors: Thomas K. Kim, Daniel B. Reisenfeld, Eric J. Zirnstein, Paul H. Janzen, Asher S. Merrill, Sung Jun Noh, Nehpreet K. Walia, Yue Chen, Fan Guo, Dave Osthus, Lauren J. Beesley, Dae-Kyu Shin, Justyna M. Sokół, Maciej Bzowski, Marzena A. Kubiak, Czeslaw Porowski, Herbert O. Funsten
Figure caption: Top panel: termination shock distance from Zirnstein–Heerikhuisen model. Middle panel: heliosheath thickness obtained through the technique outlined in D. B. Reisenfeld et al. (2021), utilizing GDF-only Theseus maps. Bottom panel: estimated GDF source distance calculated by summing the termination shock distance and half of the heliosheath thickness. The B–V plane is indicated by black curves containing the upwind velocity vector and the LISMF magnetic field vector (E. Zirnstein et al. 2016). Note: in the tail direction, the heliosheath “thickness” does not represent the full physical extent of the heliotail, but rather the distance to the ENA horizon, the observational limit of the D. B. Reisenfeld et al. (2021) method for ENAs in the IBEX-Hi energy range. See the text for further details.
Paper: Spectral Properties of Globally Distributed ENA Fluxes across Diverse Regions of the Heliosphere
Authors: Thomas K. Kim, Daniel B. Reisenfeld, Eric J. Zirnstein, Paul H. Janzen, Asher S. Merrill, Sung Jun Noh, Nehpreet K. Walia, Yue Chen, Fan Guo, Dave Osthus, Lauren J. Beesley, Dae-Kyu Shin, Justyna M. Sokół, Maciej Bzowski, Marzena A. Kubiak, Czeslaw Porowski, Herbert O. Funsten
Figure caption: IBEX-Hi observation date (first column), ENA travel time from heliosheath midpoint (second column), and effective IBEX-Hi observation date at heliosheath midpoint (third column) observed across IBEX-Hi energy channels for 2013 ram maps. The ENA travel time (column Y) is fixed throughout our study, as we use the same average distance to the ENA source region (see Figure 3(c)). So, the structure of the resultant yearly map (column Z) would be same but with different time offset.
Paper: Spectral Properties of Globally Distributed ENA Fluxes across Diverse Regions of the Heliosphere
Authors: Thomas K. Kim, Daniel B. Reisenfeld, Eric J. Zirnstein, Paul H. Janzen, Asher S. Merrill, Sung Jun Noh, Nehpreet K. Walia, Yue Chen, Fan Guo, Dave Osthus, Lauren J. Beesley, Dae-Kyu Shin, Justyna M. Sokół, Maciej Bzowski, Marzena A. Kubiak, Czeslaw Porowski, Herbert O. Funsten
Figure caption: Comparing IBEX-Hi ram sky maps for energies ranging from 0.71–4.29 keV between the standard and Theseus in 2013. All sky maps are Compton-Getting and survival probability corrected. The Theseus sky maps benefit from the combined data of triple and double coincidences, yielding superior statistics and lower noise in the maps. The coordinates of the upwind direction used in this figure and hereafter are based on P. Swaczyna et al. (2022).
Paper: Spectral Properties of Globally Distributed ENA Fluxes across Diverse Regions of the Heliosphere
Authors: Thomas K. Kim, Daniel B. Reisenfeld, Eric J. Zirnstein, Paul H. Janzen, Asher S. Merrill, Sung Jun Noh, Nehpreet K. Walia, Yue Chen, Fan Guo, Dave Osthus, Lauren J. Beesley, Dae-Kyu Shin, Justyna M. Sokół, Maciej Bzowski, Marzena A. Kubiak, Czeslaw Porowski, Herbert O. Funsten
Figure caption: Ribbon and GDF separation examples for energies 0.71, 1.74, and 4.29 keV with Theseus sky maps from 2011–2014. The presented ribbon separation results are based on the approach described in L. G. Beesley et al. (2023).
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: WISE-selected dwarf AGNs mapped onto the trained SOM, shown as pink squares overlaid on cyan circles, which represent the full sample of NSA dwarf AGNs selected by various methods. Two distinct WISE AGN clumps are visible: the right clump is associated with bluer sources, while the left clump corresponds to redder AGNs. Among the 83 WISE-selected AGNs, 22 are mapped to the right clump and 55 to the left clump. The SOM background is color coded by the logarithmic median stellar mass of the training galaxies in each cell.
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: SOM trained on the photometric colors of dwarf galaxies. Top row: SOM cells color coded by the logarithmic median stellar mass (left) and photometric redshift (right) of the training galaxies mapped to each cell. Bottom row: SOM cells color coded by the number density of training galaxies (left) and the median Hα/Hβ line ratio (right). White regions along the lower edges of the SOM correspond to cells where Hα or Hβ measurements were unavailable.
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: Distribution of NSA dwarf AGNs mapped onto the trained SOM, with cells color coded by the [O II]/z flux ratio of the training dwarf galaxies. The z corresponds to SDSS z-band photometry, tracing the stellar continuum near 9000 Å. Pink squares indicate AGNs associated with representative selection methods.
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: Distribution of NSA dwarf AGNs mapped onto the trained SOM, with cells color coded by the [O III]/([O II] × z) flux ratio of the training dwarf galaxies. The z corresponds to SDSS z-band photometry, tracing the stellar continuum near 9000 Å. Pink squares indicate AGNs associated with representative selection methods.
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: Distribution of NSA dwarf AGNs mapped onto the trained SOM, with cells color coded by the logarithmic median stellar mass of the training dwarf galaxies. Pink squares indicate AGNs associated with representative selection methods.
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: Component maps of the trained SOM, showing the learned seven-dimensional color manifold. Each panel corresponds to one of the color dimensions, with the color bars indicating the variation in that color across the SOM cells.
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: Comparison of the stellar mass distributions of WISE-selected dwarf AGNs and those selected through other methods. WISE AGNs show a clear preference for lower-mass hosts relative to the broader dwarf AGN sample.
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: SDSS images of a sample of WISE-selected AGNs from the left (top) and right (bottom) clumps. The scale is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 pixel−1. Galaxies in the left clump appear less blue, and several of them have a bright source in the center of the galaxy. Galaxies in the right clump appear bluer, indicating a higher likelihood of starburst activity.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: Spectrum from AIR-Spec showing the three new coronal lines, indicated with bold italic text in the lower plot. The upper plot shows the measured spectrum in black and a fit to the coronal continuum in red. Telluric absorption is prominent in the continuum spectrum and was modeled using ATRAN (S. D. Lord 1992). In the lower plot, the fitted continuum has been subtracted from the measured spectrum to make the lines easier to identify. We also indicate the known lines from neutral H, He, and the known S XI coronal line.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: Image from the AIR-Spec slit-jaw camera showing the slit position used to measure the new lines. The dashed line indicates the solar limb, and the solid line, the lunar limb.
Paper: TiDES: The 4MOST Time Domain Extragalactic Survey
Authors: C. Frohmaier, M. Vincenzi, M. Sullivan, S.F. Hönig, M. Smith, H. Addison, T. Collett, G. Dimitriadis, R. S. Ellis, P. Gandhi, O. Graur, I. Hook, L. Kelsey, Y.-L. Kim, C. Lidman, K. Maguire, L. Makrygianni, B. Martin, A. Möller, R. C. Nichol, M. Nicholl, P. Schady, B. D. Simmons, S. J. Smartt, E. Tempel, P. Wiseman
Figure caption: Flowchart of our end-to-end simulation framework. We begin with a database input of an LSST OpSim realization that is transformed into an SNANA SIMLIB file. Along with transient spectral templates and a host-galaxy library to draw from, we use SNANA to create realistic light curves of transient phenomena. The resulting database of events is then queried as if data were flowing in real-time, such that we can trigger for immediate follow-up of live transients or time-insensitive observations of galaxies. These observational requests are merged with our predetermined AGN targets and ingested into the 4MOST Facility Simulator (4FS) along with all other 4MOST member surveys. 4FS allocates fiber-time and scheduling during a mock 5 yr survey, returning a description of all observations at the catalog-level. This data product allows us to generate synthetic spectra with realistic observational effects. These spectra are then assessed for their quality and sent to their appropriate science channels. This allows us to perform a mock cosmology analysis of SNe Ia cosmology, study our final population statistics, and enables other analyses to be performed.
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: Radio luminosity–peak frequency parameter space plot (R. A. Chevalier 1998) recreated from Figure 2 of B. Margalit & E. Quataert(2024). The black dashed lines denote lines of constant (Γβ)sh. The bottom gray line indicates the region above which emission at the peak frequency is dominated by thermal electrons. The top gray line labeled Lcrit shows a theoretical upper bound for points within this parameter space (B. Margalit & E. Quataert 2024). We have plotted points corresponding to AT 2022cmc at 24, 260, 370, and 910 days.
Paper: TiDES: The 4MOST Time Domain Extragalactic Survey
Authors: C. Frohmaier, M. Vincenzi, M. Sullivan, S.F. Hönig, M. Smith, H. Addison, T. Collett, G. Dimitriadis, R. S. Ellis, P. Gandhi, O. Graur, I. Hook, L. Kelsey, Y.-L. Kim, C. Lidman, K. Maguire, L. Makrygianni, B. Martin, A. Möller, R. C. Nichol, M. Nicholl, P. Schady, B. D. Simmons, S. J. Smartt, E. Tempel, P. Wiseman
Figure caption: The overlap in footprints of the 4MOST and LSST surveys. The heatmap represents the number of visits in the wide–fast–deep LSST program under the baseline v3.4 survey strategy during the overlap with 4MOST operations. Due to the nonuniform sky coverage of LSST over this time period, relics of the rolling cadence seasons can be seen as density difference along decl. stripes. The dashed blue lines represent the extent of the 4MOST footprint. Within this footprint, certain areas such as the WAVES fields (S. P. Driver et al. 2019) or LMC/SMC observations (M. R. L. Cioni et al. 2019), are observed more frequently to meet the science requirements of the other 4MOST consortium surveys. The green circles show the location of the four DDFs in 4MOST that coincide with the LSST DDFs. 4MOST will observe these locations at a higher cadence–at least every 14 days for the TiDES-RM experiment.
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: The number density of the circumnuclear environment as a function of distance from the SMBH for a sample of radio-detected TDEs including the other well-studied relativistic TDE, Swift J1644 (K. D. Alexander et al. 2016, 2017; T. Eftekhari et al. 2018; Y. Cendes et al. 2021a; A. J. Goodwin et al. 2022, 2023a, 2023b, 2024). Also shown is the density profile for AT 2022cmc, which shows the same density profile as the rest of the TDE population.