adsabs/AstroCLIMB huggingface dataset:
Paper: The Combined Effects of Two-body Relaxation Processes and the Eccentric Kozai–Lidov Mechanism on the Extreme-mass-ratio Inspirals Rate
Authors: Smadar Naoz, Sanaea C. Rose, Erez Michaely, Denyz Melchor, Enrico Ramirez-Ruiz, Brenna Mockler, Jeremy D. Schnittman
Figure caption: An example of the characteristic strain for 150 (chosen randomly) of the runs that reached P • ≤ 10 yr and a •(1 − e •) < 1 au. We consider the case that includes EKL (+GR) + two-body relaxation + GW.
Paper: Dust Resurgence in Protoplanetary Disks Due to Planetesimal–Planet Interactions
Authors: Lia Marta Bernabò, Diego Turrini, Leonardo Testi, Francesco Marzari, Danai Polychroni
Figure caption: Dust mass vs. age of the star-forming region for disks around solar-type stars (top panel) and red dwarf stars (bottom panel). For each star-forming region, the thin vertical lines highlight the 25th and 75th percentiles, while the horizontal line marks the median value. The thick vertical bars, where present, show the possible range of median values (see Testi et al. 2022 for a detailed explanation of how the range is computed). The red dotted line shows the expected dust decrease due to the formation of planetesimals when no dust rejuvenation is included.
Paper: Luminosities and Masses of Single Galactic Post-asymptotic Giant Branch Stars with Distances from Gaia EDR3: The Revelation of an s-process Diversity
Authors: Devika Kamath, Hans Van Winckel, Paolo Ventura, Maksym Mohorian, Bruce J. Hrivnak, Flavia Dell'Agli, Amanda Karakas
Figure caption: Positions of the Q1 post-AGB stars in the HR diagram. The red filled circles represent the s-process enriched objects and the blue filled squares represent the non-s-process enriched objects. The numbers represent the individual object numbers as listed in Table 1. Also shown are the available post-AGB evolutionary tracks of Miller Bertolami (2016) with Z = 0.001 (left panel) and Z = 0.01 (right panel). See text for more details.
Paper: Luminosities and Masses of Single Galactic Post-asymptotic Giant Branch Stars with Distances from Gaia EDR3: The Revelation of an s-process Diversity
Authors: Devika Kamath, Hans Van Winckel, Paolo Ventura, Maksym Mohorian, Bruce J. Hrivnak, Flavia Dell'Agli, Amanda Karakas
Figure caption: SED of the s-process enriched post-AGB object, IRAS Z02229+6208 (see Table 1). The colored symbols represent the photometry of different passband filters, with the appropriate photometric catalog mentioned in the legend of the plot. The black solid line denotes the appropriate unreddened atmospheric model. The red line is the reddened model with E(B − V) = 1.9, fitted to the observed data. See text for more details.
Paper: Luminosities and Masses of Single Galactic Post-asymptotic Giant Branch Stars with Distances from Gaia EDR3: The Revelation of an s-process Diversity
Authors: Devika Kamath, Hans Van Winckel, Paolo Ventura, Maksym Mohorian, Bruce J. Hrivnak, Flavia Dell'Agli, Amanda Karakas
Figure caption: The [Fe/H] (top left), [O/Fe] (top right), [C/Fe] (bottom left), and [N/Fe] (bottom right) ratios as a function of [s/Fe] for the sample of post-AGB stars. The red circles represent the s-process enriched objects and the blue squares represent the non-s-process enriched objects. Filled symbols denote the Q1 objects, and the open symbols denote the Q2 objects. The numbers represent the individual object numbers as listed in Table 1. The derived abundances and errors are presented in Table 3. See Section 5 for more details.
Paper: Luminosities and Masses of Single Galactic Post-asymptotic Giant Branch Stars with Distances from Gaia EDR3: The Revelation of an s-process Diversity
Authors: Devika Kamath, Hans Van Winckel, Paolo Ventura, Maksym Mohorian, Bruce J. Hrivnak, Flavia Dell'Agli, Amanda Karakas
Figure caption: List of all SEDs of the post-AGB stars in our target sample. The order of the objects is the same as that in Table 1. The black curve represents the atmospheric model. Details of the atmosphere model (e.g., T eff, and E(B − V) are listed in Table 1. The red solid curve is the reddened atmospheric model (see Section 3 for more details). The various symbols correspond to the observed photometric data points where different colors denote the different surveys mentioned on the plot.
Paper: Luminosities and Masses of Single Galactic Post-asymptotic Giant Branch Stars with Distances from Gaia EDR3: The Revelation of an s-process Diversity
Authors: Devika Kamath, Hans Van Winckel, Paolo Ventura, Maksym Mohorian, Bruce J. Hrivnak, Flavia Dell'Agli, Amanda Karakas
Figure caption: An edge-on Milky Way map with the positions of the sample stars marked. The filled-circle symbols represent the s-process enriched rich sources. The filled-square symbols represent the non-s-process enriched sources. The color bar represents the metallicity ([Fe/H]) of the objects.
Paper: Luminosities and Masses of Single Galactic Post-asymptotic Giant Branch Stars with Distances from Gaia EDR3: The Revelation of an s-process Diversity
Authors: Devika Kamath, Hans Van Winckel, Paolo Ventura, Maksym Mohorian, Bruce J. Hrivnak, Flavia Dell'Agli, Amanda Karakas
Figure caption: Figure 5 continued.
Paper: Milliarcsecond Localization of the Repeating FRB 20201124A
Authors: K. Nimmo, D. M. Hewitt, J. W. T. Hessels, F. Kirsten, B. Marcote, U. Bach, R. Blaauw, M. Burgay, A. Corongiu, R. Feiler, M. P. Gawroński, M. Giroletti, R. Karuppusamy, A. Keimpema, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, A. Mikhailov, O. S. Ould-Boukattine, Z. Paragi, M. Pilia, A. Possenti, M. P. Snelders, G. Surcis, M. Trudu, T. Venturi, W. Vlemmings, N. Wang, J. Yang, J. Yuan
Figure caption: Dynamic spectra, temporal profiles, and time-averaged spectra for all 18 bursts presented in this work. For each subfigure, the burst name and time/frequency resolution are shown in the top left and top right, respectively. The colored bars represent the 1σ (dark) and 2σ (light) regions of the temporal width and spectral extent of each burst. Purple is used for bursts detected during Epoch 1, and cyan for those detected during Epoch 2. Data that have been masked due to radio frequency interference is not plotted and indicated with the red ticks. Each burst has been dedispersed using a dispersion measure of 412 pc cm−3.
Paper: Milliarcsecond Localization of the Repeating FRB 20201124A
Authors: K. Nimmo, D. M. Hewitt, J. W. T. Hessels, F. Kirsten, B. Marcote, U. Bach, R. Blaauw, M. Burgay, A. Corongiu, R. Feiler, M. P. Gawroński, M. Giroletti, R. Karuppusamy, A. Keimpema, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, A. Mikhailov, O. S. Ould-Boukattine, Z. Paragi, M. Pilia, A. Possenti, M. P. Snelders, G. Surcis, M. Trudu, T. Venturi, W. Vlemmings, N. Wang, J. Yang, J. Yuan
Figure caption: Left panel: clean EVN 1.4 GHz map of the combined visibilities of all 18 bursts detected during both epochs (i.e., the inverse Fourier transform of the visibilities after deconvolving the telescope response). The white ticks indicate the position of FRB 20201124A. The localization regions of FRB 20201124A as reported by VLA (Ravi et al. 2021), ASKAP (Fong et al. 2021), and uGMRT (Wharton et al. 2021a) are overplotted using pink, green, and orange lines, respectively. Right panel: dirty EVN map (before deconvolution of the interferometer response) of all continuum target data from both epochs to search for persistent radio emission. The position of FRB 20201124A is indicated by the black ticks. Overplotted are the 3σ, 4σ, and 5σ contours of the resolved radio emission detected by the VLA at 22 GHz (Piro et al. 2021). In both panels, the optical center of the host galaxy is indicated by the yellow cross (Fong et al. 2021). The synthesized beam is shown at the bottom left of each panel. Both maps are made using a natural weighting scheme.
Paper: Milliarcsecond Localization of the Repeating FRB 20201124A
Authors: K. Nimmo, D. M. Hewitt, J. W. T. Hessels, F. Kirsten, B. Marcote, U. Bach, R. Blaauw, M. Burgay, A. Corongiu, R. Feiler, M. P. Gawroński, M. Giroletti, R. Karuppusamy, A. Keimpema, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, A. Mikhailov, O. S. Ould-Boukattine, Z. Paragi, M. Pilia, A. Possenti, M. P. Snelders, G. Surcis, M. Trudu, T. Venturi, W. Vlemmings, N. Wang, J. Yang, J. Yuan
Figure caption: Top row: dirty maps (i.e., the inverse Fourier transform of the visibilities) of the combined visibilities of the 13 bursts discovered during Epoch 1 (left), the 5 bursts during Epoch 2 (middle), and all bursts from both epochs (right). Bottom row: same as the top row except showing clean maps (i.e., the Fourier transform of the visibilities after deconvolving the telescope response). The zoom-in panel on the bottom-right subplot shows the best-fit two-epoch position in black, with the positions from Epochs 1 and 2 independently represented by the red cross and plus, respectively. All images are made using a natural weighting scheme, and the scaling of each radio map goes from 5% to 85% of the peak value. The synthesized beam is shown at the bottom left of each panel.
Paper: Milliarcsecond Localization of the Repeating FRB 20201124A
Authors: K. Nimmo, D. M. Hewitt, J. W. T. Hessels, F. Kirsten, B. Marcote, U. Bach, R. Blaauw, M. Burgay, A. Corongiu, R. Feiler, M. P. Gawroński, M. Giroletti, R. Karuppusamy, A. Keimpema, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, A. Mikhailov, O. S. Ould-Boukattine, Z. Paragi, M. Pilia, A. Possenti, M. P. Snelders, G. Surcis, M. Trudu, T. Venturi, W. Vlemmings, N. Wang, J. Yang, J. Yuan
Figure caption: Dirty maps of the individual bursts, with the burst name shown at the top-right corner of each panel. The orange contours represent the two two-dimensional Gaussian fit (1σ region) to the cross-fringe pattern. The white contours represent the 1σ and 2σ Gaussian fits to the intersection of the double Gaussian, normalized by the S/N of the double Gaussian peak. Note: B12, B13, and B18 do not have a constraining Gaussian fit due to the lack of a cross pattern in the dirty map. The best-fit FRB 20201124A position using all 18 bursts is shown by the red cross on each panel, and the phase center used for correlation is indicated by the yellow point.
Paper: Milliarcsecond Localization of the Repeating FRB 20201124A
Authors: K. Nimmo, D. M. Hewitt, J. W. T. Hessels, F. Kirsten, B. Marcote, U. Bach, R. Blaauw, M. Burgay, A. Corongiu, R. Feiler, M. P. Gawroński, M. Giroletti, R. Karuppusamy, A. Keimpema, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, A. Mikhailov, O. S. Ould-Boukattine, Z. Paragi, M. Pilia, A. Possenti, M. P. Snelders, G. Surcis, M. Trudu, T. Venturi, W. Vlemmings, N. Wang, J. Yang, J. Yuan
Figure caption:  uv coverage per observing epoch (left panels) and uv coverage for representative individual bursts with (middle panels) and without (right panels) the cross-fringe pattern in the dirty map. The different colors represent individual bursts. There are multiple points plotted per baseline, representing the different frequency subbands. The points highlighted with the black outline represent baselines involving the Effelsberg telescope (the telescope with the highest sensitivity in our array), which dominates the structure seen in the dirty maps (Figure 4). For the representative individual bursts, the burst name is shown in the top left of the panel.
Paper: Milliarcsecond Localization of the Repeating FRB 20201124A
Authors: K. Nimmo, D. M. Hewitt, J. W. T. Hessels, F. Kirsten, B. Marcote, U. Bach, R. Blaauw, M. Burgay, A. Corongiu, R. Feiler, M. P. Gawroński, M. Giroletti, R. Karuppusamy, A. Keimpema, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, A. Mikhailov, O. S. Ould-Boukattine, Z. Paragi, M. Pilia, A. Possenti, M. P. Snelders, G. Surcis, M. Trudu, T. Venturi, W. Vlemmings, N. Wang, J. Yang, J. Yuan
Figure caption: Individual burst positions determined using the intensity peak on the dirty maps (left) and a Gaussian fit to the dirty maps, which exhibit a clear cross-fringe pattern (right; see also Figure 4). Circles indicate bursts from Epoch 1 and diamonds bursts from Epoch 2. The color bar represents the burst fluence divided by the square root of the burst width and is used as a measure of the burst detectability (a proxy for S/N; Marcote et al. 2017). The black bars represent a 100 mas angular scale, while the red bars in the zoom-in panel represent a 10 mas angular scale. The black ellipse on the left-bottom plot represents the synthesized beam centered on the best-fit FRB 20201124A position, while the cross on the right plots represents the best-fit FRB 20201124A position (in both cases, using all 18 bursts). The points on the left plot outlined in red indicate the bursts that were detected with only six baselines, highlighting the impact of the low number of baselines on the scatter of individual burst positions.
Paper: Milliarcsecond Localization of the Repeating FRB 20201124A
Authors: K. Nimmo, D. M. Hewitt, J. W. T. Hessels, F. Kirsten, B. Marcote, U. Bach, R. Blaauw, M. Burgay, A. Corongiu, R. Feiler, M. P. Gawroński, M. Giroletti, R. Karuppusamy, A. Keimpema, M. A. Kharinov, M. Lindqvist, G. Maccaferri, A. Melnikov, A. Mikhailov, O. S. Ould-Boukattine, Z. Paragi, M. Pilia, A. Possenti, M. P. Snelders, G. Surcis, M. Trudu, T. Venturi, W. Vlemmings, N. Wang, J. Yang, J. Yuan
Figure caption: Separation of the peak (top) and Gaussian-fit (middle) positions of the individual bursts as presented in Figure 6, from the best-fit FRB 20201124A position (using all 18 bursts)—as a function of the effective number of baselines (defined in the text) and the detectability parameter Fluence/√Width. The bottom panel shows the separation of the peak individual burst positions from the best-fit FRB 20201124A position as a function of the burst peak flux density measured in the Effelsberg single-dish data (S Eff                      ) divided by that measured in the interferometric data (S                          I                      ). On all panels, the markers with the cyan circles indicate the bursts from Epoch 2.
Paper: Rotational Modulation of Spectroscopic Zeeman Signatures in Low-mass Stars
Authors: Ryan C Terrien, Allison Keen, Katy Oda, Winter Parts(they/them), Guðmundur Stefánsson, Suvrath Mahadevan, Paul Robertson, Joe P. Ninan, Corey Beard, Chad F. Bender, William D. Cochran, Katia Cunha, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Fred Hearty, Adam Ickler, Shubham Kanodia, Jessica E. Libby-Roberts, Jack Lubin, Andrew J. Metcalf, Freja Olsen, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Verne V. Smith, Ben Turner
Figure caption: The K I line in multiple stellar spectra, with dashed lines representing the estimated continuum level. The left panel shows comparisons between the solar photosphere (Livingston & Wallace 1991; Wallace et al. 1993) and sunspot spectra (Wallace & Livingston 1992; Wallace et al. 1999), and the highly active M dwarf AD Leonis (with ∼kG magnetic fields), and shows the clear presence of Zeeman splitting for this line. The right panel shows all spectra for each of our target stars overlaid in the vicinity of the K I line, as well as the boundaries used for the equivalent width calculation.
Paper: Rotational Modulation of Spectroscopic Zeeman Signatures in Low-mass Stars
Authors: Ryan C Terrien, Allison Keen, Katy Oda, Winter Parts(they/them), Guðmundur Stefánsson, Suvrath Mahadevan, Paul Robertson, Joe P. Ninan, Corey Beard, Chad F. Bender, William D. Cochran, Katia Cunha, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Fred Hearty, Adam Ickler, Shubham Kanodia, Jessica E. Libby-Roberts, Jack Lubin, Andrew J. Metcalf, Freja Olsen, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Verne V. Smith, Ben Turner
Figure caption: EW K  (top), FWHM K  (middle), and dLW (bottom) as measured for Teegarden’s Star (left) and GJ 699 (right) with HPF. Individual measurements are shown as points, while boxes show binned averages (daily for GJ 699, 5 days for the more sparsely sampled Teegarden’s Star) with error bars corresponding to either (1) the measured scatter within that day if multiple spectra are obtained, or (2) the baseline single-measurement precision estimate if only one spectrum was taken during the relevant bin. Significant periodic variations are present in all measurements and are largely in-phase across these separate measurements.
Paper: Rotational Modulation of Spectroscopic Zeeman Signatures in Low-mass Stars
Authors: Ryan C Terrien, Allison Keen, Katy Oda, Winter Parts(they/them), Guðmundur Stefánsson, Suvrath Mahadevan, Paul Robertson, Joe P. Ninan, Corey Beard, Chad F. Bender, William D. Cochran, Katia Cunha, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Fred Hearty, Adam Ickler, Shubham Kanodia, Jessica E. Libby-Roberts, Jack Lubin, Andrew J. Metcalf, Freja Olsen, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Verne V. Smith, Ben Turner
Figure caption: (a) Time-series dLW measurements for Teegarden’s Star from HPF and CARMENES visible (VIS) and infrared (NIR) channels (Zechmeister et al. 2019). Periodic modulations are detected by both instruments, and are larger in amplitude at infrared wavelengths (HPF, CARMENES-NIR) than at visible wavelengths (CARMENES-VIS). (b) The HPF time-series dLW measurements for Teegarden’s Star, separated and color-coded by spectrograph order. Redder (bluer) wavelengths are longer (shorter). Overplotted are the best-fit sinusoids for each wavelength region as determined by the GLS package (Zechmeister & Kürster 2009). (c) The same as (b), but for GJ 699. A consistent oscillatory pattern is clear at each wavelength, and longer wavelengths tend to correspond to higher amplitudes of variation. (d) The amplitudes of the best-fit sinusoids to the order-by-order dLW measurements for Teegarden’s Star (circles) and GJ 699 (stars) as a function of wavelength, showing increasing amplitude with wavelength as expected for the Zeeman effect. The black circles for Teegarden’s Star are calculated from CARMENES data: the left point (CARMENES-VIS) is taken from a best-fit sinusoid; the amplitude from the noisier CARMENES-NIR data is simply estimated as half of the difference between the 2nd and 98th percentiles. Error bars for all best-fit amplitudes represent the residual rms after the removal of the best-fit sinuosid.
Paper: Rotational Modulation of Spectroscopic Zeeman Signatures in Low-mass Stars
Authors: Ryan C Terrien, Allison Keen, Katy Oda, Winter Parts(they/them), Guðmundur Stefánsson, Suvrath Mahadevan, Paul Robertson, Joe P. Ninan, Corey Beard, Chad F. Bender, William D. Cochran, Katia Cunha, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Fred Hearty, Adam Ickler, Shubham Kanodia, Jessica E. Libby-Roberts, Jack Lubin, Andrew J. Metcalf, Freja Olsen, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Verne V. Smith, Ben Turner
Figure caption: (a) The detailed line profile of the K I line in GJ 699 and Teegarden’s Star, showing the change between epochs of low and high EW K . In each case, epoch 1 (2) corresponds to a period of low (high) EW K , FWHM K , and dLW. The difference, shown in the bottom panels, reveals a line-shape change (from first to second epochs) that is consistent with a line that is strengthening and broadening under the Zeeman effect (simulated difference overlaid). (b, c) Measured (orange) and simulated (blue) variations over time of K I line EW K  and FWHM K  for (b) GJ 699 and (c) Teegarden’s Star. Simulations were generated using NICOLE (Socas-Navarro et al. 2015), as described in Section 2.6, varying the magnetic field strength and filling factor. In both stars, the approximate range of variation observed for EW K  and FWHM K  can be reproduced in the simulated spectra. Gray ovals represent the approximate error ellipse, accounting for typical pipeline-reported variances in the measured HPF spectra for each star.
Paper: Rotational Modulation of Spectroscopic Zeeman Signatures in Low-mass Stars
Authors: Ryan C Terrien, Allison Keen, Katy Oda, Winter Parts(they/them), Guðmundur Stefánsson, Suvrath Mahadevan, Paul Robertson, Joe P. Ninan, Corey Beard, Chad F. Bender, William D. Cochran, Katia Cunha, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Fred Hearty, Adam Ickler, Shubham Kanodia, Jessica E. Libby-Roberts, Jack Lubin, Andrew J. Metcalf, Freja Olsen, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Verne V. Smith, Ben Turner
Figure caption: GLS periodograms for Teegarden’s Star and GJ 699. In each case, the false-alarm probability estimates for 10% (solid line), 1% (dashed line), and 0.1% (dashed–dotted line) are indicated. For Teegarden’s Star, a 99.6 ± 1.5 days periodicity (highlighted) is strong in each of the dLW measurements (HPF, and CARMENES-VIS and -NIR), as well as in the EW K  and FWHM K  measurements. For GJ 699, each indicator has a strong peak at the 145 ± 15 days rotation period (highlighted; Toledo-Padrón et al. 2019).
Paper: Evidence for X-Ray Emission in Excess to the Jet-afterglow Decay 3.5 yr after the Binary Neutron Star Merger GW 170817: A New Emission Component
Authors: A. Hajela, R. Margutti, J. S. Bright, K. D. Alexander, B. D. Metzger, V. Nedora, A. Kathirgamaraju, B. Margalit, D. Radice, C. Guidorzi, E. Berger, A. MacFadyen, D. Giannios, R. Chornock, I. Heywood, L. Sironi, O. Gottlieb, D. Coppejans, T. Laskar, Y. Cendes, R. Barniol Duran, T. Eftekhari, W. Fong, A. McDowell, M. Nicholl, X. Xie, J. Zrake, S. Bernuzzi, F. S. Broekgaarden, C. D. Kilpatrick, G. Terreran, V. A. Villar, P. K. Blanchard, S. Gomez, G. Hosseinzadeh, D. J. Matthews, J. C. Rastinejad
Figure caption: Left panel: combined X-ray image consisting of CXO observations spanning δt = 1209–1258 days in the 0.5–8 keV energy range. An X-ray source is clearly detected at the location of GW 170817 with statistical significance of 7.2σ (Table 1). Right panel: combined radio image comprising VLA 3 GHz observations acquired in the time range δt = 1216–1265 days. No radio emission is detected at the location of GW 170817. The rms noise around the location of the BNS merger is ∼1.7 μJy (Section 3.1). In both panels, the orange and light-blue regions have a 1″ and 2.″5 radius, respectively, and mark the location of the BNS merger and its host galaxy.
Paper: Evidence for X-Ray Emission in Excess to the Jet-afterglow Decay 3.5 yr after the Binary Neutron Star Merger GW 170817: A New Emission Component
Authors: A. Hajela, R. Margutti, J. S. Bright, K. D. Alexander, B. D. Metzger, V. Nedora, A. Kathirgamaraju, B. Margalit, D. Radice, C. Guidorzi, E. Berger, A. MacFadyen, D. Giannios, R. Chornock, I. Heywood, L. Sironi, O. Gottlieb, D. Coppejans, T. Laskar, Y. Cendes, R. Barniol Duran, T. Eftekhari, W. Fong, A. McDowell, M. Nicholl, X. Xie, J. Zrake, S. Bernuzzi, F. S. Broekgaarden, C. D. Kilpatrick, G. Terreran, V. A. Villar, P. K. Blanchard, S. Gomez, G. Hosseinzadeh, D. J. Matthews, J. C. Rastinejad
Figure caption: X-ray (upper panel) and radio (3 GHz, lower panel) evolution of the emission from GW 170817 as detected by the CXO and the VLA (light-blue circles). Open circle: peak pixel flux value within one synthesized beam at the location of GW 170817 from Balasubramanian et al. (2021). At δ t > 900 days, the X-ray emission shows an excess compared to the off-axis jet-afterglow model (solid blue line; Sections 4 and 6) that indicates the emergence of a new emission component. Red-to-orange dashed lines: synchrotron radiation from the kilonova afterglow calculated using semi-analytical models (Kathirgamaraju et al. 2019) where we parameterized the kilonova kinetic energy distribution as E k ∝ (Γβ)−α  for β ≥ 0.35, and we used a total kilonova kinetic energy of 1051 erg. These models require p < 2.15 to avoid violating our radio upper limit. Here we use p = 2.05, and we emphasize with a solid thick line the α = 5 model. Other kilonova afterglow parameters assumed: ϵ B = 0.001, ϵ  e  = 0.1, and n = 0.001 cm−3. The gray shaded area shows synchrotron emission calculated from kilonova kinetic ejecta profiles derived from ab initio numerical relativity simulations using a NS mass ratio q = 1 and the LS220 equation of state (EoS; Section 7). These simulations emphasize the contribution from the merger’s dynamical ejecta. The shaded area corresponds to values p KN = 2.05–2.15, n = 6 × 10−3 cm−3, ϵ  e  = 0.1, and ϵ B = 0.01.