adsabs/AstroCLIMB huggingface dataset:
Paper: Linear and Circular Polarimetry of the Optically Bright Relativistic Tidal Disruption Event AT 2022cmc
Authors: Aleksandar Cikota, Giorgos Leloudas, Mattia Bulla, Lixin Dai, Justyn Maund, Igor Andreoni
Figure caption: Linear polarization of AT 2022cmc (this work, blue star) compared to the polarization of TDEs AT 2018dyb, AT 2019dsg, AT 2019azh, AT 2019qiz, and AT 2020mot (Leloudas et al. 2022; Patra et al. 2022; Liodakis et al. 2022b; red triangles); relativistic TDEs Swift J164449.3+573451 and Swift J2058+0516 (Wiersema et al. 2012, 2020; green squares); the superluminous transient ASASSN-15lh (Maund et al. 2020; black circles); and GRBs collected by Covino & Gotz (2016; gray circles) with N > 4 epochs. The polarization is shown as a function of days relative to peak brightness. Note that the time of first detection approximately coincides to peak brightness for GRBs. TDEs J164449.3+57345 and AT 2019qiz are marked with open symbols to mark uncertain values because they have not been corrected for the host galaxy dilution (see Section 4).
Paper: Linear and Circular Polarimetry of the Optically Bright Relativistic Tidal Disruption Event AT 2022cmc
Authors: Aleksandar Cikota, Giorgos Leloudas, Mattia Bulla, Lixin Dai, Justyn Maund, Igor Andreoni
Figure caption: Constraints to the ratio of the nonthermal to the thermal component for AT 2022cmc at 7.2 days, based on our linear polarimetry observations and the degree of polarization of the putative jet. The black line shows the measured linear polarization of 0.14%, and the gray shaded areas indicate the 1σ, 2σ, and 3σ uncertainties.
Paper: Linear and Circular Polarimetry of the Optically Bright Relativistic Tidal Disruption Event AT 2022cmc
Authors: Aleksandar Cikota, Giorgos Leloudas, Mattia Bulla, Lixin Dai, Justyn Maund, Igor Andreoni
Figure caption: Linear polarization of AT 2022cmc (red star) in the Stokes q–u plane at 7.22 rest-frame days after first detection. The light blue circles display the ISP measured through field stars, and the blue square is their weighted mean. The polarization of AT 2022cmc measured in the individual sequences is displayed in the four subplots on the top of the figure. The gray concentric circles in the subplots denote polarization degrees of 1%, 2%, 3%, and 4%. The polarization of AT 2022cmc is consistent with zero, and this is also true for the ISP.
Paper: Linear and Circular Polarimetry of the Optically Bright Relativistic Tidal Disruption Event AT 2022cmc
Authors: Aleksandar Cikota, Giorgos Leloudas, Mattia Bulla, Lixin Dai, Justyn Maund, Igor Andreoni
Figure caption: Circular polarization of AT 2022cmc at 12.23 days after first detection in the rest frame. The left and middle panels show the circular polarization measured at two different orientations of the instrument, separated by 90°, and the right panel shows the average of both measurements. The circular polarization is consistent with zero.
Paper: SDSS J134441.83+204408.3: A Highly Asynchronous Short-period Magnetic Cataclysmic Variable with a 56 MG Field Strength
Authors: Colin Littlefield, Paul A. Mason, Peter Garnavich, Paula Szkody, John Thorstensen, Simone Scaringi, Krystian Iłkiewicz, Mark R. Kennedy, Natalie Wells
Figure caption: Top: long-term ATLAS light curve of J1344, consisting of c- and o-band observations. The shaded region indicates the time of the TESS observations. Middle: TESS light curve of J1344. Bottom: power spectrum of the TESS light curve. As we discuss in the text, we interpret the Thorstensen et al. (2020) spectroscopic frequency as the spin frequency ω, but it is conceivable that it is actually the orbital frequency Ω. However, the identification of the beat frequency ω − Ω and its harmonics is secure, and the very presence of this frequency establishes that J1344 is an asynchronous rotator.
Paper: SDSS J134441.83+204408.3: A Highly Asynchronous Short-period Magnetic Cataclysmic Variable with a 56 MG Field Strength
Authors: Colin Littlefield, Paul A. Mason, Peter Garnavich, Paula Szkody, John Thorstensen, Simone Scaringi, Krystian Iłkiewicz, Mark R. Kennedy, Natalie Wells
Figure caption:  P spin/P orb as a function of orbital period in mCVs. The IP data were downloaded from Koji Mukai’s IP catalog; blue markers represent the IPs assessed by Mukai to be either “confirmed” and “ironclad,” while red markers are “probable” IPs. We use Mukai’s compilation of spin periods, except for Swift J0503.7-2819 and Paloma, whose spin periods are from Rawat et al. (2022) and Littlefield et al. (2023), respectively. The AP data are from Table 1 in Littlefield et al. (2023), and the periods of the polars are from the AAVSO International Variable Star Index catalog. We have labeled J1344 as well as individual mCVs with 0.25 ≤ P spin/P orb ≤ 0.9.
Paper: SDSS J134441.83+204408.3: A Highly Asynchronous Short-period Magnetic Cataclysmic Variable with a 56 MG Field Strength
Authors: Colin Littlefield, Paul A. Mason, Peter Garnavich, Paula Szkody, John Thorstensen, Simone Scaringi, Krystian Iłkiewicz, Mark R. Kennedy, Natalie Wells
Figure caption: Spectral energy distribution of J1344 compared to selected Koester (2010) WD spectral templates for M = ∼0.8 M ⊙, scaled to the Gaia eDR3 distance of J1344. The SED therefore cannot be explained solely by the WD’s photospheric contribution; while a hot WD could explain the optical continuum, it significantly overestimates the Galex NUV/FUV measurements. Furthermore, while the SED does not pinpoint a unique WD effective temperature, it suggests that the WD is not particularly hot, providing evidence against a recent nova.
Paper: SDSS J134441.83+204408.3: A Highly Asynchronous Short-period Magnetic Cataclysmic Variable with a 56 MG Field Strength
Authors: Colin Littlefield, Paul A. Mason, Peter Garnavich, Paula Szkody, John Thorstensen, Simone Scaringi, Krystian Iłkiewicz, Mark R. Kennedy, Natalie Wells
Figure caption: Top: SDSS spectrum of J1344, with the best-fit cyclotron model spectrum. Bottom: median-smoothed spectrum from the top panel after subtraction of the continuum. Cyclotron harmonics near 4100, 5200, and 6600 Å are visible. The expected positions of the nth cyclotron harmonics are labeled for three different field strengths: the original estimate of 65 MG (shown in red) from Szkody et al. (2011), 56 MG (blue), and 42 MG (cyan). The 65 MG field cannot account for the hump near 650 nm, while a 42 MG field would produce a hump near 860 nm. The 56 MG model (green line), in contrast, successfully predicts the three humps that are visible.
Paper: SDSS J134441.83+204408.3: A Highly Asynchronous Short-period Magnetic Cataclysmic Variable with a 56 MG Field Strength
Authors: Colin Littlefield, Paul A. Mason, Peter Garnavich, Paula Szkody, John Thorstensen, Simone Scaringi, Krystian Iłkiewicz, Mark R. Kennedy, Natalie Wells
Figure caption: High-speed photometry of J1344 obtained on four consecutive nights in 2018 June. Each panel indicates the UT date at the start of the light curve and the beat cycles covered by each light curve. Spin phase 0.0 was arbitrarily chosen to correspond with the strongest peak in the light curve from 2018 June 13, while beat phase 0.0 corresponds with the first point in the June 12 light curve.
Paper: High-eccentricity Migration with Disk-induced Spin–Orbit Misalignment: A Preference for Perpendicular Hot Jupiters
Authors: Michelle Vick, Yubo Su, Dong Lai
Figure caption: The distribution of stellar obliquities from the four sets of population syntheses described in Section 3. Panels (a)–(d) correspond to sets A–D. In all cases, the initial semimajor axis of the planet is a p,0 = 5 au. In sets A–C a b = 300 au, while in set D, a b = 150 au. In set A, the stellar spin and orbital angular momentum begin aligned. In sets B, C, and D, θ sb,i and θ lb,i are determined by interpolation between the results of the integrations described in Section 2. In sets B and D, ϕ sl,i is also found by interpolation, while in set C, ϕ sl,i is randomly selected from [0, 2π). The distributions of θ sl,f for systems that are initially prograde, with mutual inclinations θ lb,0 < 90°, are shown in dark blue.
Paper: High-eccentricity Migration with Disk-induced Spin–Orbit Misalignment: A Preference for Perpendicular Hot Jupiters
Authors: Michelle Vick, Yubo Su, Dong Lai
Figure caption: The distribution of θ jb,f, the angle between  J  =  S  ⋆ +  L  and  L   b  (top row) and the distribution of θ lb,f, the angle between  L  and  L   b  (bottom row). The columns are the same as in Figure 4.
Paper: A JWST NIRSpec Phase Curve for WASP-121b: Dayside Emission Strongest Eastward of the Substellar Point and Nightside Conditions Conducive to Cloud Formation
Authors: Thomas Mikal-Evans, David K. Sing, Jiayin Dong, Daniel Foreman-Mackey, Tiffany Kataria, Joanna K. Barstow, Jayesh M. Goyal, Nikole K. Lewis, Joshua D. Lothringer, Nathan J. Mayne, Hannah R. Wakeford, Duncan A. Christie, Zafar Rustamkulov
Figure caption: Pointing jitter along the x- and y-axes of the NRS1 (top panel) and NRS2 (bottom panel) detectors, as measured by the FIREFly code.
Paper: A JWST NIRSpec Phase Curve for WASP-121b: Dayside Emission Strongest Eastward of the Substellar Point and Nightside Conditions Conducive to Cloud Formation
Authors: Thomas Mikal-Evans, David K. Sing, Jiayin Dong, Daniel Foreman-Mackey, Tiffany Kataria, Joanna K. Barstow, Jayesh M. Goyal, Nikole K. Lewis, Joshua D. Lothringer, Nathan J. Mayne, Hannah R. Wakeford, Duncan A. Christie, Zafar Rustamkulov
Figure caption: Dark blue histograms show posterior distributions for model parameters that were varied in the light-curve fitting. Light blue histograms show corresponding distributions for other parameters that were subsequently derived. Posterior medians and ±34% credible intervals are listed in black font. Red dashed lines show the priors. For the normal priors, the mean μ and standard deviation σ are listed in red font. Half-normal priors were adopted for the σ syst parameters, allowing only positive values and with scale σ listed in red font. Vertical axes are not labeled, as arbitrary normalizations have been applied to all plotted distributions.
Paper: A JWST NIRSpec Phase Curve for WASP-121b: Dayside Emission Strongest Eastward of the Substellar Point and Nightside Conditions Conducive to Cloud Formation
Authors: Thomas Mikal-Evans, David K. Sing, Jiayin Dong, Daniel Foreman-Mackey, Tiffany Kataria, Joanna K. Barstow, Jayesh M. Goyal, Nikole K. Lewis, Joshua D. Lothringer, Nathan J. Mayne, Hannah R. Wakeford, Duncan A. Christie, Zafar Rustamkulov
Figure caption: Panels (a) and (b): raw broadband light curves for the NRS1 and NRS2 detectors, respectively. Orange lines show the best-fit light-curve models. Blue lines show the corresponding instrument baseline trends. Gray horizontal lines are calibrated to the bottom of the first eclipse, to highlight the instrumental drift over the course of the observation. Panels (c) and (d): the same light curves focusing on the planetary emission signal and after correcting for the instrument baseline trends shown by the blue lines in panels (a) and (b). Panels (e) and (f): black points show the residuals between the data and best-fit models for the NRS1 and NRS2 detectors, respectively. Orange lines show the residuals after applying a Gaussian filter to smooth the random noise. Green and purple shading show the times of transit and eclipse, respectively, with darker ranges corresponding to ingress and egress times.
Paper: A JWST NIRSpec Phase Curve for WASP-121b: Dayside Emission Strongest Eastward of the Substellar Point and Nightside Conditions Conducive to Cloud Formation
Authors: Thomas Mikal-Evans, David K. Sing, Jiayin Dong, Daniel Foreman-Mackey, Tiffany Kataria, Joanna K. Barstow, Jayesh M. Goyal, Nikole K. Lewis, Joshua D. Lothringer, Nathan J. Mayne, Hannah R. Wakeford, Duncan A. Christie, Zafar Rustamkulov
Figure caption: Black diamonds show the measured dayside (top panel) and nightside (bottom panel) planet-to-star emission levels. Note that the measurement uncertainties are smaller than the diamond symbols. Predictions from the cloud-free 3D GCM simulations of Parmentier et al. (2018) are also shown for heavy element enrichments of 1×  solar (blue lines) and 5×  solar (orange lines). Circle and square symbols show, respectively, the 1×  and 5×  solar GCM predictions binned to the light-curve passbands, which are shown as green lines in the top panel.
Paper: Excitation of Multiperiodic Kink Motions in Solar Flare Loops: Possible Application to Quasiperiodic Pulsations
Authors: Mijie Shi, Bo Li, Shao-Xia Chen, Mingzhe Guo, Shengju Yuan
Figure caption: Initial density distributions in the z = L 0/2 and x = 0 cuts. The yellow volume shows the region where the nonthermal electrons occupy the volume at t = 0. The white line marks the line of sight (LOS) for the case x 0 = 0.
Paper: Excitation of Multiperiodic Kink Motions in Solar Flare Loops: Possible Application to Quasiperiodic Pulsations
Authors: Mijie Shi, Bo Li, Shao-Xia Chen, Mingzhe Guo, Shengju Yuan
Figure caption: (a) Intensity variations of the 17 GHz emission for three LOS beams. (b) Low-pass and (c) high-pass components of the intensity variations for x 0 = ±1 Mm.
Paper: Excitation of Multiperiodic Kink Motions in Solar Flare Loops: Possible Application to Quasiperiodic Pulsations
Authors: Mijie Shi, Bo Li, Shao-Xia Chen, Mingzhe Guo, Shengju Yuan
Figure caption: Temporal evolution of v  x  sampled at (x, y, z) = (0, 0, L 0/2) (blue), together with its low-pass (red) and high-pass (green) components.
Paper: Excitation of Multiperiodic Kink Motions in Solar Flare Loops: Possible Application to Quasiperiodic Pulsations
Authors: Mijie Shi, Bo Li, Shao-Xia Chen, Mingzhe Guo, Shengju Yuan
Figure caption: Left column: temporal evolution of v  x  sampled in the apex plane at (a) (x, y) = (0, 0)Mm, (b) (x, y) = (1, 0)Mm, and (c) (x, y) = (2, 0)Mm for the case σ = R. Any blue curve represents the original signal, while the red and green curves give the low-pass and high-pass components, respectively. The black dotted lines display the fitting curves of the high-(low-) pass components by an exponentially damping sinusoid, with the best-fit periods and damping times shown in each panel. Middle column: same as the left but for σ = 0.5R. Right column: same as the left but for σ = 2R.
Paper: Excitation of Multiperiodic Kink Motions in Solar Flare Loops: Possible Application to Quasiperiodic Pulsations
Authors: Mijie Shi, Bo Li, Shao-Xia Chen, Mingzhe Guo, Shengju Yuan
Figure caption: Velocity fields in the apex plane of (a) the simulated short-period component at some representative instant and (b) the EVP expectation for the first leaky kink mode.
Paper: Excitation of Multiperiodic Kink Motions in Solar Flare Loops: Possible Application to Quasiperiodic Pulsations
Authors: Mijie Shi, Bo Li, Shao-Xia Chen, Mingzhe Guo, Shengju Yuan
Figure caption: (a) Intensity variations of the 17 GHz emission for different beam sizes for the case x 0 = 1 Mm. (b) Low-pass and (c) high-pass components of (a).
Paper: Radiative Reconnection-powered TeV Flares from the Black Hole Magnetosphere in M87
Authors: H. Hakobyan, B. Ripperda, A. A. Philippov
Figure caption: Panel (a): the time-averaged distribution function of leptons after one light-crossing time of the simulation. Runs with varying cooling strength, ﹩{\gamma }_{\mathrm{rad}}^{\mathrm{syn}}/\sigma ﹩, are shown with different colors, while the magnetization, σ, is fixed for all the runs. Panel (b): time-averaged synchrotron and IC spectra based on the simulation particles. The synchrotron spectrum (peaked near ﹩{\hslash }{\omega }_{B}{\left({\gamma }_{\mathrm{rad}}^{\mathrm{syn}}\right)}^{2}﹩) is computed on the fly and includes the self-consistent values for ﹩{\tilde{B}}_{\perp }﹩. The IC spectrum (peaked near TeV) is computed in post-processing, assuming an isotropic soft photon background, with the particle Lorentz factors rescaled to realistic values. Dashed lines on both panels show the fiducial case of ﹩{f}_{{e}^{\pm }}\propto {\gamma }^{-1}{e}^{-\gamma /{\gamma }_{c}}﹩ (the cutoff is fixed at γ  c  = σ), which is expected to be applicable for σ ≈ 107 in the M87 case, and the analytic prediction for the corresponding synchrotron and IC spectrum.
Paper: Radiative Reconnection-powered TeV Flares from the Black Hole Magnetosphere in M87
Authors: H. Hakobyan, B. Ripperda, A. A. Philippov
Figure caption: Two-dimensional histogram of particles from our 2D reconnection simulations with varying cooling strengths, parameterized by the ratio γ rad/σ (smaller ratio means stronger cooling). Particles are extracted from simulation snapshots at a particular time in the steady state and are binned by two parameters: ﹩{\tilde{B}}_{\perp }/{B}_{0}﹩ (defined in Equation (4)), and γ. At the bottom of each panel where the synchrotron cooling is present, we calculate the χ-parameter we used in Equation (3) to estimate the total synchrotron luminosity. The dashed line roughly shows the strong-to-weak cooling transition (compensated by χ 2). Particles above this line experience synchrotron cooling with strength, ﹩{\sigma }_{T}{\gamma }^{2}{\tilde{B}}_{\perp }^{2}/(4\pi )﹩, which is stronger than the characteristic accelerating force from the parallel electric field ∣e∣E rec.
Paper: Early Insights for Atmospheric Retrievals of Exoplanets Using JWST Transit Spectroscopy
Authors: Savvas Constantinou, Nikku Madhusudhan, Siddharth Gandhi
Figure caption: Initial constraints on the elemental abundances in the atmosphere of WASP-39 b. The O/H (blue), C/H (red), and S/H (yellow) ratios are derived from the molecular abundances retrieved from JWST data in the 3–5 μm range combined with HST/WFC3 data (0.8–1.7 μm). The elemental abundances are shown relative to solar values (Asplund et al. 2021). The dashed vertical line denotes the planet mass (0.28 M J). Closed and open circles within the gray shaded region refer to retrievals using JWST data from the Tiberius and Eureka pipelines, respectively, offset horizontally for clarity. The C/H abundances for solar system giant planets (Atreya et al. 2022) along with a linear fit (in brown) and the O/H in Jupiter from Juno (Li et al. 2020) are shown for reference.
Paper: Early Insights for Atmospheric Retrievals of Exoplanets Using JWST Transit Spectroscopy
Authors: Savvas Constantinou, Nikku Madhusudhan, Siddharth Gandhi
Figure caption: The spectral contributions from H2O, CO, CO2, SO2, and H2S to the best-fit spectrum obtained from the retrieval on JWST observations reduced by the Tiberius pipeline combined with HST/WFC3 data. Also shown is the resulting spectrum from all molecular spectral contributions, corresponding to the aerosol-free model shown in Figure 1. Spectral contributions from MgSiO3 aerosols as shown in Figure 1 are not included here, for visual clarity.
Paper: Early Insights for Atmospheric Retrievals of Exoplanets Using JWST Transit Spectroscopy
Authors: Savvas Constantinou, Nikku Madhusudhan, Siddharth Gandhi
Figure caption: Full posterior distribution from the retrieval using the JWST/NIRSpec PRISM 3–5 μm spectrum, reduced with the Tiberius pipeline, combined with HST/WFC3 data (0.8–1.7 μm). The model parameters correspond to the canonical atmospheric model described in Section 3. Horizontal error bars denote the median and 1σ interval for each retrieved parameter. Also shown is the retrieved P-T profile, with the black line denoting the median retrieved profile, while darker and lighter orange contours indicate the 1σ and 2σ intervals.
Paper: Early Insights for Atmospheric Retrievals of Exoplanets Using JWST Transit Spectroscopy
Authors: Savvas Constantinou, Nikku Madhusudhan, Siddharth Gandhi
Figure caption: Posterior distributions of retrieved molecular abundances. Top: posteriors obtained with JWST NIRSpec PRISM 3–5 μm data reduced by the Tiberius and Eureka pipelines (The JWST Transiting Exoplanet Community Early Release Science Team et al. 2022). Bottom: posteriors with the same two JWST spectra combined with HST/WFC3 data (Wakeford et al. 2018). From left to right, the panels show the posteriors for log-mixing ratios of H2O, CO2, SO2, CO, and H2S. Horizontal error bars denote the retrieved median and 1σ interval for the posterior of corresponding color.
Paper: Radiative Reconnection-powered TeV Flares from the Black Hole Magnetosphere in M87
Authors: H. Hakobyan, B. Ripperda, A. A. Philippov
Figure caption: Snapshots taken at the same exact time step from three different 2D simulations of the magnetic reconnection with varying synchrotron cooling strengths. Panels from top to bottom show: ((a1)–(a3)) the pair-plasma density overplotted with magnetic field lines, ((b1)–(b3)) the mean Lorentz factors of particles, ((c1)–(c3)) synchrotron emissivity, ﹩\int d\gamma {f}_{{e}^{\pm }}{\gamma }^{2}{\tilde{B}}_{\perp }^{2}﹩, for particles with γ > σ/4. In all three simulations, the upstream plasma magnetization is σ = 103. The ratio ﹩{\gamma }_{\mathrm{rad}}^{\mathrm{syn}}/\sigma ﹩ quantifies the strength of synchrotron cooling with smaller values corresponding to stronger cooling. As the cooling strength increases, plasma inside the plasmoids efficiently radiates away the excess momentum perpendicular to the magnetic field. As a result, plasmoids in the strongly cooled case become more compressed (see ((a1)–(a3)), while the mean energy of the particles inside plasmoids corresponds to the radiation limit, ﹩\langle \gamma \rangle \approx {\gamma }_{\mathrm{rad}}^{\mathrm{syn}}/4﹩. When the cooling is weak, high-energy particles inside plasmoids contribute the most to the synchrotron emission ((c1)–(c2)), while in the strong cooling case, only the smallest plasmoids and the relativistic outflows in the current sheet are visible. The x coordinate in these snapshots is measured in units of the Larmor radius, ρ  L , of particles with energies ∼σ m  e  c 2, i.e., ρ  L  ≈ σ ρ 0, where ρ 0 = m  e  c 2/(∣e∣B 0), with B 0 being the magnetic field strength in the far upstream.
Paper: Radiative Reconnection-powered TeV Flares from the Black Hole Magnetosphere in M87
Authors: H. Hakobyan, B. Ripperda, A. A. Philippov
Figure caption: Predicted photon spectra from the reconnecting current sheet during the flaring state of M87. The blue line indicates the main synchrotron component, produced by particles having a power-law distribution with an index p and cutoff γ  c . The pink line is the synchrotron emission from the secondary pairs produced outside the current sheet. The dashed gray line corresponds to the soft quiescent background emission. Compton-scattered photons dominate at energies 10–100 GeV and above; the dark gray line corresponds to the upscattering of soft background photons (IC), the orange line corresponds to the synchrotron self-Compton (SSC) component, and the green line is the spectrum of upscattered secondary synchrotron photons (SSC2). In our calculations, we fix the luminosity of the synchrotron emission and vary the effective magnetic field, 10 < B [G] < 103, the power-law index, 1 < p < 1.5, and the cutoff energy of the accelerated pairs, 107 < γ  c  < 108.
Paper: Radiative Reconnection-powered TeV Flares from the Black Hole Magnetosphere in M87
Authors: H. Hakobyan, B. Ripperda, A. A. Philippov
Figure caption: Schematic illustration of the black hole accretion flow during a reconnection-mediated flare. During the flare, the accretion flow is repelled outwards by the magnetic field to about ∼10r  g . A transient current layer is formed in the equatorial plane, where magnetic reconnection takes place. Leptons are accelerated to large energies in the current sheet, producing high-energy synchrotron emission (shown in blue). Synchrotron photons interact with each other producing e ± pairs, which are fed back to the current layer. These secondary pairs in turn radiate much lower-energy synchrotron radiation (shown in pink). The TeV signal is produced by the upscattering of soft photons of different origins by the accelerated pairs in the current layer. All the colors used in this figure correspond to the ones in Figure 2. The snapshot of plasma β is taken from the high-resolution GRMHD simulation of the magnetically arrested accretion state by Ripperda et al. (2022).