adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: H2 gas fraction versus redshift for our sample and literature QGs, with detectability (CO- or dust-based) noted in the legend. The points include QGs at z ∼ 1 (S. Belli et al. 2021; R. Bezanson et al. 2022; C. Woodrum et al. 2022), z ∼ 2–3 (K. E. Whitaker et al. 2021b; C. C. Williams et al. 2021; T. Morishita et al. 2022; T. L. Suzuki et al. 2022; H. Umehata et al. 2025), and stacks (G. E. Magdis et al. 2021, D. Blánquez-Sesé et al. 2023). Colored symbols show δDGR, directly estimated only for our sample, two QGs at z ∼ 0.7 (J. S. Spilker et al. 2025) and a QG at z ∼ 1.5 (M. Hayashi et al. 2018), with others showing limits. The main-sequence H2-scaling relation (L. J. Tacconi et al. 2018) is shown in blue. The shaded area shows the new parameter space of ﹩{f}_{{{\rm{H}}}_{2}}﹩ opened for individual detections. The right panel zooms in on our QGs relative to the main-sequence relation at their z and M⋆. The typical error on ﹩{f}_{{{\rm{H}}}_{2}}﹩ for our QGs is shown in the upper right subpanel.
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: Relation between fdust and mass-weighted stellar age, color-coded by H2 fraction. As in Figure 1, circles and triangles mark ALMA-detected and nondetected QGs, respectively, with arrows denoting upper limits. The single triangle with an fdust constraint corresponds to a PACS-detected but ALMA-undetected QG. The gray square shows the stacked nondetections in Band 6 dust continuum. Curves trace exponential tracks for fast and slow dust removal from G. Lorenzon et al. (2025). White symbols indicate literature QGs at z ∼ 2. The shaded region highlights the previously unexplored fdust–age space of old QGs.
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: Per-galaxy variation of δDGR and time since quenching, adopting a delayed-tau (tq,customSFH) and a delayed+exp (tq,fiducialSFH) SFH model. Nondetections are shown as empty triangles.
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: Results of our mock CIGALE analysis quantifying the offset between the mock input (“true”) and SED-fitting output (“observed”) parameters, as a function of M⋆ and independently measured Dn4000. Dark violet lines show binned means, indicating good constraints with no systematic offsets.
Paper: Velocity-space Turbulent Cascade in the Near-Sun Solar Wind: First Insights from the Parker Solar Probe Mission
Authors: A. Larosa, O. Pezzi, T. Bowen, L. Sorriso-Valvo, N. Sioulas, F. Pucci, D. Trotta, J. L. Verniero, R. Livi, S. Bharati Das, A. Chasapis, D. Perrone, F. Valentini, S. Servidio
Figure caption: Top to bottom: power-spectral density of the magnetic field (top), kurtosis of the magnetic field (middle), and average Hermite spectrum (bottom) for the wave stream (black) and turbulent stream (red). In gray are typical reference slopes (these are not fits) to aid the eye. The slopes for the Hermite spectra are the ones from the S. Servidio et al. (2017) phenomenological model.
Paper: Velocity-space Turbulent Cascade in the Near-Sun Solar Wind: First Insights from the Parker Solar Probe Mission
Authors: A. Larosa, O. Pezzi, T. Bowen, L. Sorriso-Valvo, N. Sioulas, F. Pucci, D. Trotta, J. L. Verniero, R. Livi, S. Bharati Das, A. Chasapis, D. Perrone, F. Valentini, S. Servidio
Figure caption: Representative VDFs for the wave stream (top) and turbulent stream (bottom). The VDFs are integrated along ϕ and plotted in the Energy-θ plane (see J. L. Verniero et al. 2020) in field-aligned coordinates. These are the original nongyrotropic PSP VDFs for which the procedure described in Section 2 has not been applied yet.
Paper: Velocity-space Turbulent Cascade in the Near-Sun Solar Wind: First Insights from the Parker Solar Probe Mission
Authors: A. Larosa, O. Pezzi, T. Bowen, L. Sorriso-Valvo, N. Sioulas, F. Pucci, D. Trotta, J. L. Verniero, R. Livi, S. Bharati Das, A. Chasapis, D. Perrone, F. Valentini, S. Servidio
Figure caption: From top to bottom in each panel: Kaufmann–Paterson measure and normalized enstrophy, PVI, LET, and Hermite spectrogram for the wave stream (top) and the turbulent stream (bottom). The shaded areas highlight regions of interest described in the main text. The Hermite spectrograms are represented through the scientifically derived color map batlow (F. Crameri et al. 2020).
Paper: Velocity-space Turbulent Cascade in the Near-Sun Solar Wind: First Insights from the Parker Solar Probe Mission
Authors: A. Larosa, O. Pezzi, T. Bowen, L. Sorriso-Valvo, N. Sioulas, F. Pucci, D. Trotta, J. L. Verniero, R. Livi, S. Bharati Das, A. Chasapis, D. Perrone, F. Valentini, S. Servidio
Figure caption: Magnetic field, velocity field, density, parallel and perpendicular temperatures, and magnetic helicity in the wave stream (top) and turbulent stream (bottom).
Paper: Velocity-space Turbulent Cascade in the Near-Sun Solar Wind: First Insights from the Parker Solar Probe Mission
Authors: A. Larosa, O. Pezzi, T. Bowen, L. Sorriso-Valvo, N. Sioulas, F. Pucci, D. Trotta, J. L. Verniero, R. Livi, S. Bharati Das, A. Chasapis, D. Perrone, F. Valentini, S. Servidio
Figure caption: VDF processing for the wave stream. VDF averaged over ϕ and plotted in the energy-θ plane (left), VDF averaged over θ and plotted in the energy-ϕ plane (center), and VDF after the procedure described in Section 2, before the interpolation into the Hermite grid (right).
Paper: Velocity-space Turbulent Cascade in the Near-Sun Solar Wind: First Insights from the Parker Solar Probe Mission
Authors: A. Larosa, O. Pezzi, T. Bowen, L. Sorriso-Valvo, N. Sioulas, F. Pucci, D. Trotta, J. L. Verniero, R. Livi, S. Bharati Das, A. Chasapis, D. Perrone, F. Valentini, S. Servidio
Figure caption: Original Hermite spectrum for the wave stream (left) and turbulent stream (right) in black, compared with the Hermite spectrum of the underlying bi-Maxwellian in gray.
Paper: Understanding the Origin and Dynamical Evolution of the Unique Open Star Cluster Berkeley 20 Using FIRE Simulations
Authors: Alessa I. Wiggins, Jamie R. Quinn, Micah Oeur, Sarah R. Loebman, Peter M. Frinchaboy, Kathryne J. Daniel, Fiona McCluskey, Jonah M. Otto, Hannah R. Woodward, Elena D'Onghia, Andrew Wetzel, Hanna Parul, Binod Bhattarai, Maximilian Cozzi
Figure caption: BOB’s vertical height changes significantly in response to the satellite’s passage. Top-down and side-on visualization of in situ and ex situ stars in m12f during and after the satellite interaction. BOB is marked in green in each panel, with a 4 kpc2 zoom centered on BOB. In situ stars are shown in the background, and ex situ stars are highlighted in blue. Arrows indicate the satellite’s center of velocity vectors, originating from its center of mass, computed via an iterative zoom-in method. Left: satellite appears on the lower right edge-on. The region surrounding BOB is well populated with satellite stars, and BOB is near the midplane of the disk. Middle: satellite passes through the disk, and the bulk of its stars pass near BOB. Right: satellite is at the outskirts of the disk, above the midplane. There are few ex situ stars near BOB, but the impact of the satellite interaction can be seen by the drastic change in Z.
Paper: Understanding the Origin and Dynamical Evolution of the Unique Open Star Cluster Berkeley 20 Using FIRE Simulations
Authors: Alessa I. Wiggins, Jamie R. Quinn, Micah Oeur, Sarah R. Loebman, Peter M. Frinchaboy, Kathryne J. Daniel, Fiona McCluskey, Jonah M. Otto, Hannah R. Woodward, Elena D'Onghia, Andrew Wetzel, Hanna Parul, Binod Bhattarai, Maximilian Cozzi
Figure caption: The satellite’s passage induces significant asymmetry in the stellar mass distribution, ρ(Z), about the midplane. We measure the asymmetry within a cylindrical volume centered on BOB with a radius of 1.4 kpc and height of ± 3 kpc. The stellar disk near BOB is twice as asymmetric as anti-BOB, which corresponds to the same cylindrical region but on the opposite side of the disk azimuthally immediately following the satellite passage (marked by the dashed gray line). This spike is evidence of a strong, localized vertical mass redistribution in the disk surrounding BOB, a direct response to the satellite encounter.
Paper: Surprisingly Large Doppler Shifts in Hinode EUV Imaging Spectrometer (EIS) Solar Spectra Resulting from an Inconspicuous Small-scale Jet in Extreme-ultraviolet Images
Authors: Alphonse C. Sterling, Louise K. Harra, Navdeep K. Panesar, Ronald L. Moore
Figure caption: (a) GOES soft X-ray fluxes with time in the 1–8 Å (red) and 0.5–4 Å (green) channels. (b) Variation of AIA 94 Å intensity with time integrated over the red box of Figure 2(d) through the time of the AIA images in Figure 2. (c) Variation of positive magnetic flux with time in the positive-polarity flux patch in the yellow box of Figure 4(g). The red dashed line in (b) and (c) shows the time of the strong EIS Doppler shift. (d) A time–distance plot from AIA 171 Å images from the green rectangle in Figure 2(b), where the ordinate of that rectangle is the y-axis here, where we integrated over the width of that green rectangle to increase the signal in this time–distance plot. The resulting southward-directed flows in the Figure 2(b) green rectangle show up as bright tracks moving southward in time that are pointed out by the arrows; the red arrow is at the time of the strong Doppler feature of Figure 1, and the green arrows show other south-flowing events. Each of the arrowed south-flowing events can be identified in the animation accompanying Figure 2, near the times indicated by the arrows. (e)–(g) A sequence of images from the Figure 2(b) AIA 171 Å animation, showing a faint south-directed flow corresponding to the feature pointed to by the red arrow in (d). The blue arrows track a location near the front of the moving feature, which is used in estimating the flow speed given in the text.
Paper: Surprisingly Large Doppler Shifts in Hinode EUV Imaging Spectrometer (EIS) Solar Spectra Resulting from an Inconspicuous Small-scale Jet in Extreme-ultraviolet Images
Authors: Alphonse C. Sterling, Louise K. Harra, Navdeep K. Panesar, Ronald L. Moore
Figure caption: (a) Hinode/EIS raster image showing the observed active region, NOAA AR 12824. The raster started on the west edge of the FOV at 20:32:10 UT on 2021 May 21 and finished at the east edge at 21:32:55 UT, and the arrow points to the source of the strong-Doppler-blueshifted spectral line shown in (b). Blue lines show the FOV of panels (c)–(e). (b) The EIS 195.12 Å spectrum from 20:39:51 UT on the same day (histogram) with a two-Gaussian fit. The peak on the left is strongly blueshifted compared to the peak on the right near the rest wavelength. Panels (c)–(f) show images from SDO/AIA and a magnetogram from HMI of the region of the EIS strong-Doppler-shifted nonflare event at the times given in the tops of the respective panels: (c) AIA 1600 Å, (d) HMI line-of-sight magnetogram, (e) AIA 304 Å, and (f) AIA 193 Å. The blue boxes show the FOV of Figure 2. To within 1 minute, all four images in (c)–(f) are at the same time, and at the same time as the spectrum in (b). Solar images in all figures have north upward and west to the right. AIA and HMI images in all figures are displayed rotated to 20:40 UT on 2021 May 21.
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Properties of the leading fast magnetosonic wave in the nonlinear regime. Meridional x–z-plane slice at time t = 75 r*/c, illustrating the rescaled magnetosonic and Alfvén wave energy densities ﹩{r}^{2}\delta {U}_{f}/{r}_{* }^{2}{B}_{* }^{2}﹩ and ﹩{r}^{2}\delta {U}_{A}/{r}_{* }^{2}{B}_{* }^{2}﹩, the relativistic drift speed amplitude γv/c, and the radial drift speed vr/c. The wave is in a strong nonlinear regime, vr ≃ c, and the geometry of the nonlinear zone resembles that of a monster shock (A. M. Beloborodov 2023; D. Bernardi et al. 2025c).
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Time evolution of different energy components, ﹩{ \mathcal E }﹩, within r < 100 r*. Here r* and B* are the stellar radius and magnetic field strength, respectively. The left panel shows the various energy components, while the right panel presents their proportions relative to the injected energy. From t = 100 r*/c, the first perturbations escape the integration domain. At this stage the magnetosphere partially transitions into a split-monopole configuration, making it more difficult to define (linear) wave perturbations as done here.
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Angular distribution of the radial energy flux associated with the first nonlinear fast pulse and nonlinear Alfvén ejecta, shown in a Mollweide projection. The Poynting flux on a spherical surface of radius r = 56 r* was integrated over the time interval ct/r* ∈ [57, 77].
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: Top: the bilby.fits sky map from The LIGO Scientific Collaboration et al. (2025a), with our targeted PS tiling observations performed within 7 days postburst overlaid. Bottom: the same as above but with the ATLAS observation footprints within 7 days postburst overlaid.
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: Light curve of SN2025ulz. We include the discovery gr-band data from ZTF (R. Stein et al. 2025) in addition to our multicolor PS, ATLAS, SLT, and LOT data. The hollow symbols correspond to 3σ upper limits.
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: Comparison of the GW signal properties of S250818k to those from the LVK GWTC-3 catalog (R. Abbott et al. 2023), following M. Nicholl & I. Andreoni (2025).
Paper: Capture into Apsidal Resonance and the Decimation of Planets around Inspiraling Binaries
Authors: Mohammad Farhat, Jihad Touma
Figure caption: Phase portraits in (ζp, ηp)-space corresponding to the Hamiltonian of Equation (2), which governs the planar dynamics of a circumbinary test-particle planet around a stellar binary precessing under GR. The phase portraits are restricted to the region around the resonance of interest. Moving from left to right, level curves of the Hamiltonian are plotted in different panels for decreasing values of the drift parameter α = aAB/ap, i.e., showing the phase space of the CBP as the binary’s orbit shrinks. Beyond a critical value of α, the secular precession resonance under study is encountered, giving rise to the libration island around apse alignment (ϖp = ϖAB; ηp = 0), with the latter growing in eccentricity as α decreases further. At the center of the libration island lies the equilibrium point, shown in red, at which ﹩{\dot{\varpi }}_{p}={\dot{\varpi }}_{\mathrm{AB}}﹩, located by solving the equilibrium condition of Equation (4). Here we adopted mA = 2 M⊙, mB = 1 M⊙, and eAB = 0.35.
Paper: Capture into Apsidal Resonance and the Decimation of Planets around Inspiraling Binaries
Authors: Mohammad Farhat, Jihad Touma
Figure caption: Sample simulations representing the outcome regimes of the population synthesis study of Figure 4. For each regime, the first panel plots the evolution of the orbital periods of the binary, the planet, and the boundary of the circumbinary instability zone (estimated following N. Georgakarakos et al. 2024); the second panel plots the eccentricity evolution of the binary and the planet; the third panel plots the evolution of the rate of change of the longitude of the periaspse for both the binary and the planet; and the fourth panel plots the resonant angle ϖp – ϖAB. From left to right, mAB = 2.28, 1.58, 2.33,  and 1.95 M⊙. The first regime corresponds to CBPs that do not encounter the sweeping resonance in the course of the binary’s tidal decay. Regime B showcases the resonant capture and subsequent ejection of the planet from the system. The third column shows resonance capture that leaves the planet on a stable eccentric orbit, saved by the binary stopping its orbital decay upon circularization. The fourth column shows the richer dynamics of Regime D, where the planet is first captured by and later escapes the resonance. We elaborate further on the dynamical pathways of these regimes in the main text.
Paper: Capture into Apsidal Resonance and the Decimation of Planets around Inspiraling Binaries
Authors: Mohammad Farhat, Jihad Touma
Figure caption: Resonant decimation of CBPs. From our population study of Figure 4, we plot the planetary eccentricity as a function of the binary’s orbital period at the end of our simulations. All CBPs were initiated on circular orbits. Three distinct families are identified in the plot: (i) in green, a family of planets that avoid the sweeping resonance and thus maintain stable near-circular orbits; (ii) in red, a family of planets captured in resonance and consequently excited to extreme eccentricity values, to be destabilized and ejected, as their host binaries reach tight orbits; and (iii) in yellow, a family of planets that are resonantly excited but end up on stable eccentric orbits, saved from destabilization by the binary reaching its tidal equilibrium early enough, or by occupying wide orbits. The orbital period of the tightest binary observed to host a transiting planet, Kepler-47, is marked by the vertical line.
Paper: Capture into Apsidal Resonance and the Decimation of Planets around Inspiraling Binaries
Authors: Mohammad Farhat, Jihad Touma
Figure caption: Distributions of the initial and end states of the dynamical evolution of 1630 triple systems of binaries and CBPs. The population synthesis is described in the main text, and the secular evolution follows the equations of motion in the Appendix. Shown, in order, are the population’s initial and final binary orbital period Porb;AB, binary eccentricity eAB, planetary eccentricity ep, and the system’s prescribed ages compared to the times at which unstable planets are destabilized. The binaries’ orbital decay and eccentricity decrease are driven by the binary tides, while the planets’ eccentricity growth and probable destabilization are driven by capture into the secular apsidal precession resonance.
Paper: Capture into Apsidal Resonance and the Decimation of Planets around Inspiraling Binaries
Authors: Mohammad Farhat, Jihad Touma
Figure caption: Profiles of CBP equilibrium eccentricity when apse aligned with the binary: at different locations for the binary and the planet with eAB = 0.2 (top), and for different binary location and eccentricity with ap = 1.5 au (bottom). The realistic dynamical behavior of a CBP is expected to develop around this equilibrium structure if the system is captured in resonance and evolves in time while maintaining adiabaticity. Here we have adopted mA = 2 M⊙ and mB = 1 M⊙, while the CBP is treated as a test particle.
Paper: Capture into Apsidal Resonance and the Decimation of Planets around Inspiraling Binaries
Authors: Mohammad Farhat, Jihad Touma
Figure caption: Locating the resonance in orbital period parameter space. Plotted is a contour surface of the function ﹩\,\rm{sgn}\,({\dot{\varpi }}_{p}-{\dot{\varpi }}_{\mathrm{AB}})\times {\mathrm{log}}_{10}(1+| {\dot{\varpi }}_{p}-{\dot{\varpi }}_{\mathrm{AB}}| ).﹩ The precession rates of the host binary and the CBP equate at the dashed black curve, identifying the resonance. We adopt the test-particle approximation for the planet here; therefore, ﹩{\dot{\varpi }}_{{\rm{AB}}}﹩ is driven by GR, while ﹩{\dot{\varpi }}_{p}﹩ is driven by the binary’s torque. We use mA = 2 M⊙, mB = 1 M⊙, and eAB = 0.2. The instability zone on the upper left follows the criterion of M. J. Holman & P. A. Wiegert (1999).
Paper: Machine Learning Confirms GW231123 is a “Lite” Intermediate Mass Black Hole Merger
Authors: Chayan Chatterjee, Kaylah McGowan, Suyash Deshmukh, Nicholas Tyler-Howard, Karan Jani
Figure caption: (a) Receiver operating characteristic (ROC) and precision–recall (PR) curves obtained on the IMBH test set, after fine-tuning the original GW-WHISPER model, initially trained for evaluation of the MLGWSC-1 dataset. (b) Distribution of false-alarm rates (FARs) per month, derived from background triggers obtained by applying the fine-tuned GW-WHISPER to dataset 4 of MLGWSC-1.
Paper: Machine Learning Confirms GW231123 is a “Lite” Intermediate Mass Black Hole Merger
Authors: Chayan Chatterjee, Kaylah McGowan, Suyash Deshmukh, Nicholas Tyler-Howard, Karan Jani
Figure caption: (a) Overlap distributions between GW231123-like waveforms in Hanford and Livingston generated from posterior samples of various approximants and their AWARE reconstructions. (b) Overlap distributions between AWARE reconstructions and GW231123-like injections in O3 noise contaminated by different glitches.