adsabs/AstroCLIMB huggingface dataset:
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: Gemini/GMOS and Keck/LRIS spectra of the host galaxy of FRB 20240209A, where we arbitrarily scale the Gemini/GMOS spectrum on the y-axis for easier visualization. The locations of several observed spectral features that enabled a redshift determination are denoted. Telluric features are marked with  ⊕.
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: Effective radius as a function of the Sérsic index for a sample of FRB hosts from the literature (K. E. Heintz et al. 2020; A. G. Mannings et al. 2021; S. Bhandari et al. 2022; Y. Dong et al. 2024) compared to the values that we derive for FRB 20240209A in Section 4. Also shown for comparison are the values derived from HST observations of long GRBs (C. Wainwright et al. 2007) and short GRBs (W. Fong et al. 2010), where we supplement the short GRB sample with GW170817 (P. K. Blanchard et al. 2017).
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: WISE mid-IR colors for the host of FRB 20240209A compared to the hosts of repeating (yellow stars) and nonrepeating (teal squares) FRBs with WISE detections. Shown for comparison are the kernel density estimation distributions for the galaxy subsamples from the MIXR catalog (B. Mingo et al. 2016). The horizontal dashed line at W1 − W2 = 0.8 mag denotes the minimum threshold for AGN-dominated galaxies (D. Stern et al. 2012), while vertical lines mark the division between spheroidal/early-type galaxies, intermediate disks/spiral galaxies, and star-forming/late-type disks (T. H. Jarrett et al. 2017).
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: Observed SED of the host galaxy of FRB 20240209A including Gemini/GMOS spectroscopy (blue curve) and broadband photometry (blue circles) with the best-fit spectrum (gray curve) and photometry (black squares) from Prospector. The agreement between the observed and modeled spectrum is demonstrated in the zoomed-in inset panels. The bottom panel depicts the transmission filters for each of the photometric points (see also Table 1). Limits correspond to 3σ.
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: Mass-assembly history as a function of the lookback time for the host galaxy of FRB 20240209A as inferred from the star formation history, where tlookback = 0 corresponds to the redshift of the host.
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: Top: slices of rest-mass density, ρ, in the co-orbiting frame at representative times in our four simulations. Here ﹩x^{\prime} ﹩ and ﹩z^{\prime} ﹩ are the coordinates in the co-orbiting frame. Bottom: equatorial slices of plasma β at representative times in our four simulations. Only the fiducial simulation shows a clear structure of an accreting midplane and poloidal jet. The other simulations show more unstructured accretion flows, with occasional weak and intermittent jets in the tilted and rB = 500rg simulations. In the midplane, regions of low β are seen propagating outward from the near-horizon flow and mixing with the gas at larger radii. These include both “flux tubes” like those seen in MAD accretion flows and bubbles blown out by weak jets (in the case of the tilted simulation). The low-β regions are particularly large and mix to particularly large radii in the tilted and rB = 500rg simulations. Such mixing likely inhibits the accumulation of net magnetic flux on the event horizon, required for sustained jet launching. Animations of this figure are available for the fiducial (https://youtu.be/XQbifuBWjw8), χ = 0 (https://youtu.be/yoiAEejPz2Q), tilted (https://youtu.be/I5UnUlYVHag), and rB = 500rg (https://youtu.be/YrTxBuysitk) simulations.
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: Time series of accretion- and jet-related quantities. Top left: total accretion rate, ﹩\dot{M}﹩, onto both black holes normalized to the Bondi rate, ﹩{\dot{M}}_{{\rm{B}}}﹩. Top right: total dimensionless magnetic flux threading both black holes, ϕBH (calculated from Equation (2)). Bottom left: total electromagnetic energy outflow efficiency, ηEM. Bottom right: maximum distance from the origin reached by the jets, rjet, measured as the maximum distance at which gas with σ > 1 is found. In calculating ϕBH and ηEM, the accretion rates in the denominator have been averaged over one orbital time. All simulations show approximate saturation of magnetic flux at some mean value. The fiducial and χ = 0 simulations saturate at higher horizon-penetrating magnetic fluxes (ϕBH ∼ 30–50) and display strong variability. The tilted and rB = 500rg simulations, on the other hand, saturate at ϕBH ≈ 20–30, with less variability. Correspondingly, the jet efficiencies in the fiducial simulation are the largest, with ηEM ∼ 20%–50% on average, while the efficiencies in the tilted and rB = 500rg simulations only occasionally rise above a few percent. This shows that both larger Bondi radii and tilted accretion flows can inhibit the formation of strong jets in equal-mass black hole binaries.
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: Three-dimensional volume renderings of our fiducial (top row), tilted (middle row), and rB = 500rg (bottom row) simulations at four different representative times, highlighting regions of high magnetization, σ, in orange/yellow and regions of high ρ in blue. Each panel is on a scale of ﹩{(75{r}_{g})}^{2}﹩. Jets in the fiducial simulation are much more sustained and propagate more effectively than in both the tilted and rB = 500rg simulations. In the last two simulations the jets are sporadic and intermittent. This result may imply that sustained jets are more difficult to form in SMBH binary systems when the spins are misaligned with the orbital plane. Whether or not this result holds for different types of large-scale accretion flows (e.g., circumbinary disks) requires future study. Animations of this figure are available for the fiducial (https://youtu.be/rMieXN7HFvg), tilted (https://youtu.be/U6pGvOZ83Zo), and rB = 500rg (https://youtu.be/-l8sEZXR2zg) simulations.
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: Evidence of magnetic reconnection between two jets in our fiducial simulation. Left: three-dimensional rendering of the jets at a representative time. Right: slices of plasma parameter β through the z = 50rg (bottom panel), z = 100rg (middle panel), and z = 150rg (top panel) planes. Since the spins of the black holes have the same polarity, the in-plane magnetic fields in the jet cores are usually oriented in clockwise loops. Because of this, “X”-points are formed when the jets initially touch, with oppositely directed field lines driven to reconnect and dissipate. This is seen as the jet propagates to larger radii and the cores merge into one. This reconnection layer can accelerate electrons to nonthermal energies, which could radiate at high electromagnetic frequencies (as estimated in the main text and Section B.1). An animated version of this figure is available here (https://youtu.be/KI5tQbRJ9k4).
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: Binary separation distance, dBH, vs. time for our four orbital configurations. The freefall times at the two choices for Bondi radii, tff, are also shown on the x-axis. The time that it takes for the binaries to merge is a strong function of the initial separation distance, dBH,0, with the dBH,0 = 27rg orbit taking an extra  ∼  2 × 104M than dBH,0 = 25rg orbits. Orbits with nonzero black hole spin aligned with the orbital angular momentum generally take longer to merge owing to the additional net angular momentum.
Paper: Structure Functions of Rotation Measures Revealing the Origin of Fast Radio Bursts
Authors: Rui-Nan Li, Zhen-Yin Zhao, Qin Wu, Shuang-Xi Yi, Fa-Yin Wang
Figure caption: The SFs for PSR B1744–24A and FRB 20201124A. Panel (a): SF of RM for PSR B1744–24A. Orange plus symbols represent the nonbinned data after performing correction, and blue circles indicate binned data with uncertainties estimated as the standard error on the mean. The red solid line is the fit using Equation (10) with RM0 = 157 ± 40 rad m−2, and the orbital period is ∼1.8 hr. The dot solid line corresponds to the statistical component Ds = 2927.14 rad2 m−4. The black dashed line corresponds to the orbital period of 1.8 hr derived in previous research (D. Li et al. 2023). Panel (b) SF of DM for PSR B1744–24A. The red solid line corresponds to the linear fit with power-law index −0.004 ± 0.021. Panel (c): SF of RM for FRB 20201124A. RM0 = 136 ± 24 rad m−2, and the orbital period P = 37 ± 1 days. The statistical component is Ds = 221.88 rad2 m−4. Panel (d): SF of DM for FRB 20201124A. The power-law index is −0.04 ± 0.02.
Paper: Structure Functions of Rotation Measures Revealing the Origin of Fast Radio Bursts
Authors: Rui-Nan Li, Zhen-Yin Zhao, Qin Wu, Shuang-Xi Yi, Fa-Yin Wang
Figure caption: The SFs for FRB 20180916B, FRB 20190520B, and FRB 20121102A. Panel (a): SF of the RM for FRB 20180916B. Orange plus symbols represent the nonbinned data after doing correction, and blue circles indicate binned data with uncertainties estimated as the standard error on the mean. The red solid line is the fit using Equation (10) with RM0 > 33 rad m−2 and the orbital period P > 2094 days. The dotted solid line corresponds to the statistic component Ds = 4.75 rad2 m−4. The black dashed line corresponds to the active period of 16.35 days. Panel (b): SF of the DM for FRB 20180916B. The red solid line corresponds to linear fit with power-law index −0.09 ± 0.03. Panel (c): SF of the RM for FRB 20190520B. RM0 > 2 × 104 rad m−2, orbital period P > 524 days, and Ds = 7.6 × 105 rad2 m−4. Panel (d): SF of the DM for FRB 20190520B. The power-law index is 0.03 ± 0.03. Panel (e): SF of the RM for FRB 20121102A. RM0 > 1.7 × 104 rad m−2, orbital period P > 785 days, and Ds = 1.2 × 104 rad2 m−4. Panel (f): SF of the DM for FRB 20121102A. The power-law index −0.07 ± 0.02.
Paper: Structure Functions of Rotation Measures Revealing the Origin of Fast Radio Bursts
Authors: Rui-Nan Li, Zhen-Yin Zhao, Qin Wu, Shuang-Xi Yi, Fa-Yin Wang
Figure caption: The schematic diagram of binary systems. Panel (a): the top-down view of binary systems. The black solid lines with arrows correspond to the toroidal magnetic field line in the decretion disk or winds. The yellow line is the LOS. The changes in the angle between the LOS and the magnetic field contribute to the geometric component in the RM SF. Panel (b): the 3D schematic diagram of binary systems. The gray shaded area indicates the decretion disk of the companion star. The blue shaded area indicates the stellar wind of the companion star.
Paper: Structure Functions of Rotation Measures Revealing the Origin of Fast Radio Bursts
Authors: Rui-Nan Li, Zhen-Yin Zhao, Qin Wu, Shuang-Xi Yi, Fa-Yin Wang
Figure caption: Test of the geometric component using simulations. Panel (a): simulated RM of FRB 20190520B. The red line represents the RM data simulated by the binary model. The model parameters are the same as those used for the observed RM fit (F. Y. Wang et al. 2022). The period is taken as 600 days. Panel (b): SF of simulated RM for FRB 20190520B. Orange plus symbols represent the nonbinned data after doing correction, and blue circles indicate binned data with uncertainties estimated as the standard error on the mean. The red solid line is the fit using Equation (10) with RM0 = 16612 ± 651 rad m−2, and the orbital period P = 605 ± 3 days, which is consistent the one used in simulations (F. Y. Wang et al. 2022).
Paper: Structure Functions of Rotation Measures Revealing the Origin of Fast Radio Bursts
Authors: Rui-Nan Li, Zhen-Yin Zhao, Qin Wu, Shuang-Xi Yi, Fa-Yin Wang
Figure caption: The SFs for FRB 20180301A, FRB 20190303A, and FRB 20220912A. Panel (a): SF of the RM for FRB 20180301A. Orange plus symbols represent the nonbinned data after doing correction, and blue circles indicate binned data with uncertainties estimated as the standard error on the mean. The red solid line corresponds to linear fit with power-law index 0.70 ± 0.09. Panel (b): SF of the DM for FRB 20180301A. The red solid line corresponds to the linear fit with power-law index 0.02 ± 0.04. Panel (c): SF of the RM for FRB 20190303A. The red solid line corresponds to the linear fit with power-law index 0.78 ± 0.41. Panel (d): SF of the DM for FRB 20190303A. The red solid line corresponds to the linear fit with power-law index −0.06 ± 0.09. Panel (e): SF of the RM for FRB 20220912A. The red solid line corresponds to the linear fit with power-law index −0.02 ± 0.01. Panel (f): SF of the DM for FRB 20220912A. The red solid line corresponds to the linear fit with power-law index 0.00 ± 0.01.
Paper: Uncorrelated Estimations of H0 Redshift Evolution from DESI Baryon Acoustic Oscillation Observations
Authors: X. D. Jia, J. P. Hu, S. X. Yi, F. Y. Wang
Figure caption: Fitting results of H0,z for Bayesian block methodology. Panel (a) shows the value of H0,z as a function of redshift. There is a clear decreasing trend with 4.9σ significance between z = 0 and z = 1.5. The green line gives H0 = 73.04 ± 1.04 km s−1 Mpc−1 from the local distance ladder and its 1σ uncertainty (A. G. Riess et al. 2022). The yellow line is the value of H0 = 67.4 ± 0.5 km s−1 Mpc−1 from the CMB measurements and its 1σ uncertainty (Planck Collaboration et al. 2020). Panel (b) shows the probability density of H0,z.
Paper: Uncorrelated Estimations of H0 Redshift Evolution from DESI Baryon Acoustic Oscillation Observations
Authors: X. D. Jia, J. P. Hu, S. X. Yi, F. Y. Wang
Figure caption: Corner plot of H0,z values in units of km s−1 Mpc−1. The panels on the diagonal show the 1D posterior probability distribution for each parameter obtained by marginalizing over the other parameters. The off-diagonal panels show 2D projections of the posterior probability distributions for each pair of parameters, with contours to indicate 1σ to 3σ confidence levels.
Paper: Uncorrelated Estimations of H0 Redshift Evolution from DESI Baryon Acoustic Oscillation Observations
Authors: X. D. Jia, J. P. Hu, S. X. Yi, F. Y. Wang
Figure caption: Fitting results of H0,z for Model 1 and Model 2. Panel (a) shows the value of H0,z as a function of redshift for Model 1, while panel (b) presents the value for Model 2. The green line gives H0 = 73.04 ± 1.04 km s−1 Mpc−1 from the local distance ladder and its 1σ uncertainty (A. G. Riess et al. 2022). The yellow line is the value of H0 = 67.4 ± 0.5 km s−1 Mpc−1 from the CMB measurements and its 1σ uncertainty (Planck Collaboration et al. 2020).
Paper: Uncorrelated Estimations of H0 Redshift Evolution from DESI Baryon Acoustic Oscillation Observations
Authors: X. D. Jia, J. P. Hu, S. X. Yi, F. Y. Wang
Figure caption: Fitting results of H0,z in eight redshift bins. Panel (a) shows the value of H0,z as a function of redshift. There is a clear decreasing trend with 7.2σ significance between z = 0 and z = 1.5. The green line gives H0 = 73.04 ± 1.04 km s−1 Mpc−1 from the local distance ladder and its 1σ uncertainty (A. G. Riess et al. 2022). The yellow line is the value of H0 = 67.4 ± 0.5 km s−1 Mpc−1 from the CMB measurements and its 1σ uncertainty (Planck Collaboration et al. 2020). Panel (b) shows the probability density of H0,z.
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: An example of a “magnetic bridge” flaring event in our tilted simulation. Shown in panels 1–6 is a time series of three-dimensional representations of magnetic field lines in the corotating frame on top of a two-dimensional contour of entropy per unit mass, ﹩s=1/(\gamma -1)\mathrm{log}(P/{\rho }^{\gamma })﹩, in the ﹩x^{\prime} ﹩-﹩z^{\prime} ﹩ plane. Only field lines that thread at least one of the black hole event horizons and get closer than 10rg to the other black hole are shown. Yellow (blue) field lines are those that pierce the first (second) black hole's event horizon (the first black hole is always positioned on the left in these plots), while green field lines are those that pierce both event horizons. The gray shaded regions in the entropy contour represent the regions inside the event horizons of the black holes. The second black hole captures initially fairly straight field lines connected to the first black hole and, through a combination of orbital and black hole spin motion, twists them into a tangled tube. Finally, the field lines reconnect close to the second black hole, releasing magnetic energy and causing an eruption of high-entropy gas that gets expelled to larger radii. This mechanism is a promising candidate for unique electromagnetically powered high-energy flaring signatures of SMBH binary AGN. An animation of this figure is available here (https://youtu.be/6xs0QUaJX5s).
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: Properties of the magnetic reconnection layer formed just before the eruption event in the tilted simulation plotted in Figure 6. Top left: two-dimensional slice centered on the second black hole of magnetic energy density normalized to the time-averaged accretion rate, ﹩{u}_{b}{r}_{g}^{2}/(| \langle \dot{M}\rangle | c)﹩, with the reconnection layer indicated by yellow arrows. Top right: two-dimensional slice of σ = b2/ρ. Bottom left: same as the top left panel, but on a  ∼4 times smaller scale. Bottom right: one-dimensional profiles through the reconnection layer (along the line indicated in the bottom left panel) of the three spatial components of the comoving magnetic field, bμ. The available energy for reconnection is highest near the horizon, with ﹩{u}_{b}{r}_{g}^{2}/(| \langle \dot{M}\rangle | c)﹩ ∼  0.075, where the layer is surrounded by plasma with σ ∼  a few. Furthermore, there is a negligible guide field, with all three spatial components of bμ changing sign across the layer.
Paper: Dual Jet Interaction, Magnetically Arrested Flows, and Flares in Accreting Binary Black Holes
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Elias R. Most
Figure caption: Properties of the magnetic reconnection layer formed by the two interacting jets at the time shown in Figure 5. Top: two-dimensional slice of σ through the z = 50rg plane. Middle: same as the top panel, but for magnetic energy density normalized to the time-averaged accretion rate, ﹩{u}_{b}{r}_{g}^{2}/(| \langle \dot{M}\rangle | c)﹩, with magnetic field lines overplotted. Bottom: one-dimensional profiles through the reconnection layer (along the line indicated in the middle panel) of the three spatial components of the comoving magnetic field boosted into the jet frame, ﹩\left({b}^{\mu }\right)^{\prime} ﹩. The upstream flow is characterized by σ ≈ 100, the imposed numerical limit (meaning that in reality it would be much larger), and a guide field of comparable strength to the reconnecting field.
Paper: Uncorrelated Estimations of H0 Redshift Evolution from DESI Baryon Acoustic Oscillation Observations
Authors: X. D. Jia, J. P. Hu, S. X. Yi, F. Y. Wang
Figure caption: Fitting results of H0,z in eight redshift bins. Panel (a) shows the value of H0,z as a function of redshift. There is a clear decreasing trend with 6.4σ significance between z = 0 and z = 1.5. The green line gives H0 = 73.04 ± 1.04 km s−1 Mpc−1 from the local distance ladder and its 1σ uncertainty (A. G. Riess et al. 2022). The yellow line is the value of H0 = 67.4 ± 0.5 km s−1 Mpc−1 from the CMB measurements and its 1σ uncertainty (Planck Collaboration et al. 2020). Panel (b) shows the probability density of H0,z.