adsabs/AstroCLIMB huggingface dataset:
Paper: The Day-long, Repeating GRB 250702B: A Unique Extragalactic Transient
Authors: Andrew J. Levan, Antonio Martin-Carrillo, Tanmoy Laskar, Rob A. J. Eyles-Ferris, Albert Sneppen, Maria Edvige Ravasio, Jillian C. Rastinejad, Joe S. Bright, Francesco Carotenuto, Ashley A. Chrimes, Gregory Corcoran, Benjamin P. Gompertz, Peter G. Jonker, Gavin P. Lamb, Daniele B. Malesani, Andrea Saccardi, Javier Sánchez-Sierras, Benjamin Schneider, Steve Schulze, Nial R. Tanvir, Susanna D. Vergani, Darach Watson, Jie An, Franz E. Bauer, Sergio Campana, Laura Cotter, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Dimple, Dieter H. Hartmann, Jens Hjorth, Luca Izzo, Páll Jakobsson, Amit Kumar, Andrea Melandri, Paul O'Brien, Silvia Piranomonte, Giovanna Pugliese, Jonathan Quirola-Vásquez, Rhaana Starling, Gianpiero Tagliaferri, Dong Xu, Makenzie E. Wortley
Figure caption: The Fermi-GBM (8 keV –900 keV energy range; observer frame) count-rate light curve spanning from −2 × 103 to 1.2 × 104 s after the GRB 250702D trigger (main panel, gray lines; with data from each burst highlighted in color), along with zoom ins around the time of the individual triggers (upper row). EP-WXT observations revealed an X-ray counterpart a day earlier (blue arrow; H. Q. Cheng et al. 2025), indicating transient high-energy emission preceding the GBM trigger. The dashed vertical lines indicate periods of 2825 s (the measured gap between GRB 250702D and GRB 250702B).
Paper: The Day-long, Repeating GRB 250702B: A Unique Extragalactic Transient
Authors: Andrew J. Levan, Antonio Martin-Carrillo, Tanmoy Laskar, Rob A. J. Eyles-Ferris, Albert Sneppen, Maria Edvige Ravasio, Jillian C. Rastinejad, Joe S. Bright, Francesco Carotenuto, Ashley A. Chrimes, Gregory Corcoran, Benjamin P. Gompertz, Peter G. Jonker, Gavin P. Lamb, Daniele B. Malesani, Andrea Saccardi, Javier Sánchez-Sierras, Benjamin Schneider, Steve Schulze, Nial R. Tanvir, Susanna D. Vergani, Darach Watson, Jie An, Franz E. Bauer, Sergio Campana, Laura Cotter, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Dimple, Dieter H. Hartmann, Jens Hjorth, Luca Izzo, Páll Jakobsson, Amit Kumar, Andrea Melandri, Paul O'Brien, Silvia Piranomonte, Giovanna Pugliese, Jonathan Quirola-Vásquez, Rhaana Starling, Gianpiero Tagliaferri, Dong Xu, Makenzie E. Wortley
Figure caption: The effective radius (top) and absolute magnitude of the host galaxy of GRB 250702B at various redshifts from 0.1 < z < 3. The top panel shows how the physical radius would evolve across the redshift range (black line), while the shaded blue region is the galaxy size–redshift relation from K. Ormerod et al. (2024), and the green points a set of direct measurements of high-z (z > 1) galaxy sizes (and masses) from the Hubble Frontier Fields (L. Yang et al. 2021). The GRB host population from J. D. Lyman et al. (2017) is also shown. The lower panel shows the absolute magnitude of the host galaxy in the F140W filter, as well as a crude conversion to stellar mass. Both the sizes and luminosities of the host of GRB 250702B would be consistent with the GRB host and field galaxy population at low z, matching particularly well at z < 0.5. At higher redshift large, luminous galaxies do occur, but as the intrinsic luminosity of the GRB 250702B host increases with redshift, they become increasingly rare. The host would be unusually luminous beyond z ∼ 1.
Paper: The Day-long, Repeating GRB 250702B: A Unique Extragalactic Transient
Authors: Andrew J. Levan, Antonio Martin-Carrillo, Tanmoy Laskar, Rob A. J. Eyles-Ferris, Albert Sneppen, Maria Edvige Ravasio, Jillian C. Rastinejad, Joe S. Bright, Francesco Carotenuto, Ashley A. Chrimes, Gregory Corcoran, Benjamin P. Gompertz, Peter G. Jonker, Gavin P. Lamb, Daniele B. Malesani, Andrea Saccardi, Javier Sánchez-Sierras, Benjamin Schneider, Steve Schulze, Nial R. Tanvir, Susanna D. Vergani, Darach Watson, Jie An, Franz E. Bauer, Sergio Campana, Laura Cotter, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Dimple, Dieter H. Hartmann, Jens Hjorth, Luca Izzo, Páll Jakobsson, Amit Kumar, Andrea Melandri, Paul O'Brien, Silvia Piranomonte, Giovanna Pugliese, Jonathan Quirola-Vásquez, Rhaana Starling, Gianpiero Tagliaferri, Dong Xu, Makenzie E. Wortley
Figure caption: Left: discovery image of the counterpart of GRB 250702B obtained with the VLT/HAWK-I. The false-color composite is constructed from the H- and K-band observations and demonstrates the transient’s extremely red color. Middle: zoomed-in region (corresponding to the white box in the left panel) around GRB 250702B’s counterpart at δt = 5.737 days as observed with HAWK-I in excellent seeing conditions. The transient appears to be offset from a likely extended source. Right: HST imaging clearly resolves the extended source, revealing a complex, asymmetric morphology, as well as the possible presence of a strong dust lane through the disk of the galaxy.
Paper: The Day-long, Repeating GRB 250702B: A Unique Extragalactic Transient
Authors: Andrew J. Levan, Antonio Martin-Carrillo, Tanmoy Laskar, Rob A. J. Eyles-Ferris, Albert Sneppen, Maria Edvige Ravasio, Jillian C. Rastinejad, Joe S. Bright, Francesco Carotenuto, Ashley A. Chrimes, Gregory Corcoran, Benjamin P. Gompertz, Peter G. Jonker, Gavin P. Lamb, Daniele B. Malesani, Andrea Saccardi, Javier Sánchez-Sierras, Benjamin Schneider, Steve Schulze, Nial R. Tanvir, Susanna D. Vergani, Darach Watson, Jie An, Franz E. Bauer, Sergio Campana, Laura Cotter, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Dimple, Dieter H. Hartmann, Jens Hjorth, Luca Izzo, Páll Jakobsson, Amit Kumar, Andrea Melandri, Paul O'Brien, Silvia Piranomonte, Giovanna Pugliese, Jonathan Quirola-Vásquez, Rhaana Starling, Gianpiero Tagliaferri, Dong Xu, Makenzie E. Wortley
Figure caption: Light curves (left) and spectral energy distributions (right) for the afterglow of GRB 250702B spanning from ≈0.5 to 20 days at radio to X-ray wavelengths. The observations can be well explained by a standard synchrotron model comprising radiation (solid lines) from forward (dashed) and reverse (dotted) shocks at z ≈ 0.16 and high host attenuation, AV ≈ 12 mag (see Section 5 for details and Appendix A for model parameters).
Paper: The Day-long, Repeating GRB 250702B: A Unique Extragalactic Transient
Authors: Andrew J. Levan, Antonio Martin-Carrillo, Tanmoy Laskar, Rob A. J. Eyles-Ferris, Albert Sneppen, Maria Edvige Ravasio, Jillian C. Rastinejad, Joe S. Bright, Francesco Carotenuto, Ashley A. Chrimes, Gregory Corcoran, Benjamin P. Gompertz, Peter G. Jonker, Gavin P. Lamb, Daniele B. Malesani, Andrea Saccardi, Javier Sánchez-Sierras, Benjamin Schneider, Steve Schulze, Nial R. Tanvir, Susanna D. Vergani, Darach Watson, Jie An, Franz E. Bauer, Sergio Campana, Laura Cotter, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Dimple, Dieter H. Hartmann, Jens Hjorth, Luca Izzo, Páll Jakobsson, Amit Kumar, Andrea Melandri, Paul O'Brien, Silvia Piranomonte, Giovanna Pugliese, Jonathan Quirola-Vásquez, Rhaana Starling, Gianpiero Tagliaferri, Dong Xu, Makenzie E. Wortley
Figure caption: Correlation plots and marginalized posterior density functions for four key free parameters in the afterglow model (Section 5 and Appendix A), demonstrating that low-redshift z ≲ 0.3 and high-extinction (AV ≳ 10 mag) models are favored by the data under the modeling constraints employed here.
Paper: The Day-long, Repeating GRB 250702B: A Unique Extragalactic Transient
Authors: Andrew J. Levan, Antonio Martin-Carrillo, Tanmoy Laskar, Rob A. J. Eyles-Ferris, Albert Sneppen, Maria Edvige Ravasio, Jillian C. Rastinejad, Joe S. Bright, Francesco Carotenuto, Ashley A. Chrimes, Gregory Corcoran, Benjamin P. Gompertz, Peter G. Jonker, Gavin P. Lamb, Daniele B. Malesani, Andrea Saccardi, Javier Sánchez-Sierras, Benjamin Schneider, Steve Schulze, Nial R. Tanvir, Susanna D. Vergani, Darach Watson, Jie An, Franz E. Bauer, Sergio Campana, Laura Cotter, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Dimple, Dieter H. Hartmann, Jens Hjorth, Luca Izzo, Páll Jakobsson, Amit Kumar, Andrea Melandri, Paul O'Brien, Silvia Piranomonte, Giovanna Pugliese, Jonathan Quirola-Vásquez, Rhaana Starling, Gianpiero Tagliaferri, Dong Xu, Makenzie E. Wortley
Figure caption: X-shooter spectroscopy in 2D (top) and 1D (bottom) of the counterpart of GRB 250702B obtained on 2025 July 4, rebinned in the 1D to 50 Å per bin. Signal is only recovered in the infrared arm (shown) at low signal to noise. The gray bands indicate regions of high telluric absorption that are not corrected for. The source shows brightening through the H and K regions of the spectrum consistent with photometry. Given the low signal to noise no significant absorption or emission features are visible in the counterpart spectrum. The slit was also oriented to cover the location of the host galaxy, but no redshift could be derived.
Paper: The Day-long, Repeating GRB 250702B: A Unique Extragalactic Transient
Authors: Andrew J. Levan, Antonio Martin-Carrillo, Tanmoy Laskar, Rob A. J. Eyles-Ferris, Albert Sneppen, Maria Edvige Ravasio, Jillian C. Rastinejad, Joe S. Bright, Francesco Carotenuto, Ashley A. Chrimes, Gregory Corcoran, Benjamin P. Gompertz, Peter G. Jonker, Gavin P. Lamb, Daniele B. Malesani, Andrea Saccardi, Javier Sánchez-Sierras, Benjamin Schneider, Steve Schulze, Nial R. Tanvir, Susanna D. Vergani, Darach Watson, Jie An, Franz E. Bauer, Sergio Campana, Laura Cotter, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Antonio de Ugarte Postigo, Dimple, Dieter H. Hartmann, Jens Hjorth, Luca Izzo, Páll Jakobsson, Amit Kumar, Andrea Melandri, Paul O'Brien, Silvia Piranomonte, Giovanna Pugliese, Jonathan Quirola-Vásquez, Rhaana Starling, Gianpiero Tagliaferri, Dong Xu, Makenzie E. Wortley
Figure caption: Comparison of the X-ray light curve of GRB 250702B with those of Swift GRBs (grayscale background) and relativistic TDE candidates, downloaded from the Swift Burst Analyser (P. A. Evans et al. 2007, 2009, 2010) and the Living Swift-XRT Point Source Catalogue (P. A. Evans et al. 2023) and processed as described in S. Schulze et al. (2014). At any reasonable redshift the luminosity of the event is comparable to those of GRBs, and GRB 250702B is clearly faster and less luminous than the relativistic TDE candidates. This would be consistent with a lower-mass black hole involved in a disruption, or with a more normal GRB interpretation.
Paper: Further Evidence for a Direct-collapse Origin of the Supermassive Black Hole at the Center of the ∞ Galaxy
Authors: Pieter van Dokkum, Gabriel Brammer, Connor Jennings, Imad Pasha, Josephine F. W. Baggen
Figure caption: NIRSpec IFU observations of the ∞ galaxy. Top left: broadband image of the galaxy created from the NIRCAM F090W (blue), F115W + F150W (green), and F200W (red) data, sampled at ﹩0\mathop{.}\limits{^{\prime\prime} }02﹩ resolution with north up and east to the left. Top right: example spectra from three different regions, highlighting the diversity of spectra in the data cube. Bottom: maps of [O III], Hα, and [N II] emission, sampled with ﹩0\mathop{.}\limits{^{\prime\prime} }05﹩ pixels. There is a cloud of ionized gas in between the nuclei. Both nuclei and the SE ring are detected in Hα.
Paper: Further Evidence for a Direct-collapse Origin of the Supermassive Black Hole at the Center of the ∞ Galaxy
Authors: Pieter van Dokkum, Gabriel Brammer, Connor Jennings, Imad Pasha, Josephine F. W. Baggen
Figure caption: Line ratios. Left: map of the [O III]/Hα ratio, multiplied by a factor of 4 so values can be more easily compared to [O III]/Hβ measurements. Middle: map of the [N II]/Hα ratio. Right: individual ﹩0\mathop{.}\limits{^{\prime\prime} }05\times 0\mathop{.}\limits{^{\prime\prime} }05﹩ spaxels in the BPT diagram. The cloud shows very high 4 ×  [O III]/Hα ratios of ∼10 and is in the Seyfert regime. The nuclei are in the LINER part of the BPT diagram, and the ring is consistent with star formation.
Paper: Further Evidence for a Direct-collapse Origin of the Supermassive Black Hole at the Center of the ∞ Galaxy
Authors: Pieter van Dokkum, Gabriel Brammer, Connor Jennings, Imad Pasha, Josephine F. W. Baggen
Figure caption: Radial average surface brightness profile of the [O III] emission in the cloud. The profile has a clear peak and falls off monotonically. The red line shows the expectation for photoionization, with the gas having a constant density core with a radius of ﹩{r}_{{\rm{core}}}=2.5﹩ kpc and a power-law distribution with n ∝ r−0.75 at ﹩r\gt {r}_{{\rm{core}}}﹩.
Paper: The Link between Athor and EL Meteorites Does Not Constrain the Timing of the Giant Planet Instability
Authors: André Izidoro, Rogerio Deienno, Sean N. Raymond, Matthew S. Clement
Figure caption: Implantation of a planetesimal from the terrestrial region into the asteroid belt during the final accretion phase of terrestrial planets in our Athor-1 simulation. The planetesimal is implanted in the inner main belt, in the Athor region. The x-axes show time, and the y-axes show, from top to bottom, semimajor axis, orbital eccentricity, and inclination. Dashed lines delimit the Athor region, defined as 2.3 au < a < 2.48 au, e < 1–2/a, and i ≤ 15°. This simulation corresponds to an example where the instability takes place at the time of the disk dispersal, i.e., tinst = 5 Myr after the solar system formation. At 5 Myr, the gray-line planetesimal is at about 1.4 au, and it finally enters the asteroid belt at ∼100 Myr (a ≳ 1.8 au). Its effective implantation occurs at ∼120 Myr, when a planetary embryo (which will be later referred to as Krios; light brown) is ejected from the system.
Paper: The Link between Athor and EL Meteorites Does Not Constrain the Timing of the Giant Planet Instability
Authors: André Izidoro, Rogerio Deienno, Sean N. Raymond, Matthew S. Clement
Figure caption: Temporal evolution of the ratio of the average number of planetesimals in the terrestrial scattered disk in simulations where the instability takes place at 5 Myr (giant planets are in their current orbits) after solar system formation and simulations where the giant planets are kept in preinstability orbits. Planetesimals in the terrestrial scattered disk are defined as those in the terrestrial region (1 au < a < 1.8 au) and those in the belt region but with very high orbital eccentricities and inclinations (1.8 au < a < 3.5 au, e > 0.4, and i > 35°). We have tested several different cutoffs for the definition of planetesimals in the terrestrial scattered disk, and the results were similar to the presented case. For instance, accounting only for planetesimals in the terrestrial region (1 au < a < 1.8 au) leads to broadly similar results. The number of planetesimals in the terrestrial scattered disk for each giant planet configuration is averaged over 50 simulations modeling the accretion of terrestrial planets. The gray lines show 1σ standard deviation.
Paper: The Link between Athor and EL Meteorites Does Not Constrain the Timing of the Giant Planet Instability
Authors: André Izidoro, Rogerio Deienno, Sean N. Raymond, Matthew S. Clement
Figure caption: Implantation of a planetesimal from the terrestrial region into the asteroid belt during the final accretion phase of terrestrial planets in our Athor-2 simulation. The planetesimal is implanted in the inner main belt, in the Athor region. The x-axes show time, and the y-axes show, from top to bottom, semimajor axis, orbital eccentricity, and inclination. Dashed lines delimit the Athor region, defined as 2.3 au < a < 2.48 au, e < 1–2/a, and i ≤ 15°. Like Figure 1, this simulation corresponds to another example where the instability takes place at the time of the disk dispersal, i.e., tinst = 5 Myr after the solar system formation. At 5 Myr, the gray-line planetesimal is at about 1.6 au, and it finally enters the asteroid belt at ∼100 Myr (a ≳ 1.8 au). Its effective implantation occurs at ∼290 Myr, when Krios (orange) is ejected from the system.
Paper: The Link between Athor and EL Meteorites Does Not Constrain the Timing of the Giant Planet Instability
Authors: André Izidoro, Rogerio Deienno, Sean N. Raymond, Matthew S. Clement
Figure caption: Evolution of semimajor axis, pericenter, and apocenter of all planetary bodies shown in Figure 1, using the same color-coding in both figures. The implantation of the planetesimal in the belt (gray lines) at about 120 Myr occurs due to its gravitational interaction with Krios and Mars. The high eccentricity and inclination phases of Krios before its ejection induce secular effects on the planetesimal that reduce its orbital inclination and eccentricity, ultimately implanting it in the belt around Athor’s modern orbit.
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: The transmission spectra of TRAPPIST-1 e interpreted with GPs and atmospheric/atmosphereless models. (Top) Transmission spectra on our four visits (black points with error bars) modeled with a GP times either an atmospheric model (blue) or a flat-line spectrum (i.e., with no atmosphere or with a high-altitude cloud deck; orange); a GP (offset; dashed lines) acts multiplicatively to distort those signals. Bands represent the 1σ and 3σ credibility bands. (Bottom) Visit-combined transmission spectrum by (weighted) averaging the four visits after correcting for the modeled GP component (using the flat-line model-derived GP; black points with error bars). The atmospheric model and the flat-line model are indistinguishable according to the Bayesian evidence—more data are needed to distinguish between those. Bands represent the 1σ and 3σ credibility bands. Note how, within the error bars, an Earth-like model (gray; with the locations of the main active spectroscopic features) is still consistent with our data. Also note that the blue and orange models are shared but fitted to each individual visit.
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: White-light TRAPPIST-1 e JWST/NIRSpec PRISM transit light curves. (Top) Data points of the transit event (gray; binned at a cadence of 14 s) along with the best-fit transit plus systematics model (black; which includes a visit-long slope and a GP; see text for details). The date at which each observation was obtained is indicated at the top of each panel. (Middle) Residuals of the data minus the best-fit light-curve model in parts per million; the rms of the data at this 14 s cadence is indicated for each observation. (Bottom) Light curves at the Hα line (0.656 ± 0.02 μm, in parts per thousand) at the same cadence as the white-light curves (small light blue) and binned at 5 minutes (large dark blue); note how a flare is revealed at about −0.25 hr in this light curve as the most likely explanation for the bump in the 2023 July 23 transit event.
Paper: JWST-TST DREAMS: NIRSpec/PRISM Transmission Spectroscopy of the Habitable Zone Planet TRAPPIST-1 e
Authors: Néstor Espinoza, Natalie H. Allen, Ana Glidden, Nikole K. Lewis, Sara Seager, Caleb I. Cañas, David Grant, Amélie Gressier, Shelby Courreges, Kevin B. Stevenson, Sukrit Ranjan, Knicole Colón, Brett M. Morris, Ryan J. MacDonald, Douglas Long, Hannah R. Wakeford, Jeff A. Valenti, Lili Alderson, Natasha E. Batalha, Ryan C. Challener, Jingcheng Huang, Zifan Lin, Dana R. Louie, Elijah Mullens, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Andrea Bellini, Jens Kammerer, Mattia Libralato, Isabel Rebollido, Emily Rickman, Sangmo Tony Sohn, Roeland P. van der Marel
Figure caption: H2 abundance constraints for TRAPPIST-1 e from HST and JWST as a function of surface pressure. Posterior distribution showcasing the improvement on constraints on possible H2-dominated atmospheres on TRAPPIST-1 e between HST (left in gray; obtained by applying our GP retrieval methodology to the HST/WFC3 data in Z. Zhang et al. 2018) and JWST (right in blue; obtained by applying it to the four NIRSpec/PRISM transits presented in this work). The distribution for HST mainly follows the centered log-ratio prior allowing the H2-dominated solution at virtually all pressures ≳1 bar; the JWST one disfavors the H2-dominated solution.
Paper: The Link between Athor and EL Meteorites Does Not Constrain the Timing of the Giant Planet Instability
Authors: André Izidoro, Rogerio Deienno, Sean N. Raymond, Matthew S. Clement
Figure caption: Representative example of implantation of a planetesimal that arrives relatively early in the belt, at about ∼40 Myr. The early arrival of this object in the asteroid belt makes it most likely inconsistent with Athor. As in Figure 1, the x-axes show time, and the y-axes show, from top to bottom, semimajor axis, orbital eccentricity, and inclination. Dashed lines delimit the Athor region, defined as 2.3 au < a < 2.48 au, e < 1–2/a, and i < 15°. This simulation corresponds to an example where the instability also takes place at the time of the disk dispersal, tinst = 5 Myr, relative to the solar system formation time. The final implantation of this planetesimal happens at about 85 Myr, when Krios is ejected from the system.
Paper: The Link between Athor and EL Meteorites Does Not Constrain the Timing of the Giant Planet Instability
Authors: André Izidoro, Rogerio Deienno, Sean N. Raymond, Matthew S. Clement
Figure caption: Evolution of the semimajor axis, pericenter, and apocenter of all planetary bodies shown in Figure A1, using the same color-coding for both figures. The implantation of the planetesimal in the belt (gray lines) at about 85 Myr occurs due to its gravitational interaction with Krios and Mars, but note that it enters the asteroid belt region (a ≳ 1.8 au) between 30 and 40 Myr. As in Figure 3, the high eccentricity and inclination phases of Krios before its ejection induce secular effects on the planetesimal, reducing its orbital inclination and eccentricity and ultimately implanting it in the belt and Athor’s region.