adsabs/AstroCLIMB huggingface dataset:
Paper: The Rotation Dip in the Envelope–Disk Transition of HH 111: Evidence for Magnetic Braking
Authors: Jyun-Heng Lin, Chin-Fei Lee, Zhi-Yun Li, Yueh-Ning Lee, Ya-Lin Wu, J. A. López-Vázquez
Figure caption: The C18O PV diagrams are cut along the major axis of the disk. The x-axis represents the velocity relative to the Vsys = 8.85 km s−1, while the y-axis shows the positional offset from the source center. The top panel shows the PV diagram obtained from the channel maps with a robust parameter of 0.5, while the bottom panel from the channel maps with a robust parameter of -2. The corresponding angular resolutions are 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩73 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩61 and 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩16 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩13, respectively.
Paper: Projections of Earth’s Technosphere: Strategies for Observing Technosignatures on Terrestrial Exoplanets
Authors: Jacob Haqq-Misra, Ravi K. Kopparapu, George Profitiliotis
Figure caption: Total observation time required for a solar gravitational lens with a 1 m diameter optical telescope to resolve images of an Earth-sized planet at a distance of 10 pc (following Equation (3)). An image with 128 × 128 pixel resolution could be obtained in a few days, but higher resolutions of 256 × 256 would require half a year of observation time. Even higher resolutions would extend observation times to decades or even centuries.
Paper: The Rotation Dip in the Envelope–Disk Transition of HH 111: Evidence for Magnetic Braking
Authors: Jyun-Heng Lin, Chin-Fei Lee, Zhi-Yun Li, Yueh-Ning Lee, Ya-Lin Wu, J. A. López-Vázquez
Figure caption: In the top panel, the infall velocity vr from the best-fit model (as in Figure 3(g)) is shown as a green solid line, while the green dotted line represents the freefall velocity vff and the green dashed line corresponds to the infall velocity derived from both angular momentum and energy conservation vr,ℓ,e. In the bottom panel, the rotation velocity vϕ used in the best-fit model is shown as a blue solid line. The pink dashed–dotted line represents the rotation velocity derived from Keplerian motion vKep the purple dashed line indicates the rotation velocity derived from specific angular momentum conservation vϕ,ℓ, and the black line represents the sound speed.
Paper: Numerical Nonadiabatic Tidal Calculations with GYRE-tides: The WASP-12 Test Case
Authors: Meng Sun, 萌 孙, R. H. D. Townsend, Hongbo Xia, 宏博 夏, Jifeng Liu
Figure caption: Synchronization timescale tsync (top panel) and orbital decay timescale ta (bottom panel) as functions of orbital period, computed for the WASP-12 system considering only radiative damping of the dynamical tide. The results are based on linear tidal response functions calculated with GYRE-tides. Sharp decreases in the timescales arise from resonance with g-modes; the labels beneath the plot identify the resonant mode, and additionally indicate (in parentheses) the orbital harmonic k involved in the resonance, and the propagation direction (“p”: prograde; “r”: retrograde) of the mode. The horizontal dashed lines in both panels denote the age of the Universe. Outside the resonances, the predicted timescales generally exceed the observed decay timescale by approximately 3 orders of magnitude, indicating that radiative damping alone cannot explain the rapid inspiral of WASP-12b. The red star marks the observed value of the orbital decay timescale, ∣ta∣ ∼ 2.2 Myr.
Paper: Numerical Nonadiabatic Tidal Calculations with GYRE-tides: The WASP-12 Test Case
Authors: Meng Sun, 萌 孙, R. H. D. Townsend, Hongbo Xia, 宏博 夏, Jifeng Liu
Figure caption: As in Figure 1, the same binary configuration and stellar structure are used, but here both with convective damping and radiative damping are included. The inclusion of convective damping enhances tidal dissipation across a broader range of orbital periods. The red star denotes the observed decay timescale.
Paper: Numerical Nonadiabatic Tidal Calculations with GYRE-tides: The WASP-12 Test Case
Authors: Meng Sun, 萌 孙, R. H. D. Townsend, Hongbo Xia, 宏博 夏, Jifeng Liu
Figure caption: Characteristic frequencies, viscosity prescriptions, radial displacement amplitudes, and the gravitational potential perturbation response for a 1.3 M⊙ main-sequence stellar model, as a function of pressure. Top: the plotted quantities include the Brunt–Väisälä frequency N/2π (blue), the Lamb frequency S2/2π for ℓ = 2 (orange), the inverse thermal timescale 1/tth (orange dashed line), the inverse eddy turnover timescale 1/ted (green dashed line), the dynamical frequency 1/tdyn (horizontal black dashed line), and the tidal forcing frequency 1/Pf (horizontal black dotted line). Horizontal royal blue and coral lines mark the propagation regions of multiple g-modes and p-modes, respectively. Bottom: viscosity profiles standard mixing-length formulation (labeled STD; blue solid line), eddy viscosity implemented in GYRE (orange solid line), and Zahn’s reduced viscosity (labeled Z; green solid line).
Paper: Handy Relation between Binary Black Hole Merger Times and Host Galaxy Properties
Authors: Kelly Holley-Bockelmann, Fazeel Mahmood Khan, Isaiah Williams, Jaelyn Roth, Michael Rizzo Smith, Kaitlin Porter, Jillian Bellovary, Andrea Derdzinski, Andrea V. Macciò
Figure caption: Left: stellar density of the host galaxy at the binary radius of influence, ρinfl,b, versus s, the binary hardening parameter. We measure s several time units after the binary hardens to prevent an overestimate of the hardening rate. The colored dots indicate the orientation of the binary BH orbital angular momentum with respect to that of the host galaxy—buff: no rotation; pink: retrograde; and green: prograde. Over 6 orders of magnitude in stellar density, there is a tight relation between the stellar density and binary BH hardening, with only minor differences due to the orbit, kinematics, or shape. Note the best fits for the pro- and retrograde are both plotted in pink and green, respectively; they are just indistinguishable in this figure. This indicates that the simulations are properly resolving the few-body scattering phase and is consistent with the finding that the energy extraction from a binary orbit depends on the stellar density in the loss cone (e.g., G. D. Quinlan 1996). Right: binary hardening parameter, s, versus coalescence time, log(Tcoal). For a given hardening parameter, there is a difference in the coalescence time of between 1 and 2 orders of magnitude, broadly separated by binary orbit, with prograde configurations taking longer to merge than their retrograde counterparts.
Paper: Numerical Nonadiabatic Tidal Calculations with GYRE-tides: The WASP-12 Test Case
Authors: Meng Sun, 萌 孙, R. H. D. Townsend, Hongbo Xia, 宏博 夏, Jifeng Liu
Figure caption: Mode analysis of the ℓ = m = k = 2 tidal response in our fiducial 1.3 M⊙ main-sequence stellar model. Top: radial displacement amplitude ξr (real and imaginary parts), including results from the full nonadiabatic forced oscillation calculation, the case with radiative diffusion damping only, and the analytical equilibrium tide (green solid); the dimensionless nonlinearity parameter krξr is also shown as red solid line. Middle: horizontal displacement amplitude ξh (real and imaginary parts), compared with the case with radiative diffusion damping only; the corresponding khξh is indicated as a red solid line. Bottom: Eulerian gravitational potential perturbation Φℓm (real and imaginary parts), with both full and radiative-only solutions. All quantities are plotted as a function of radius.
Paper: Handy Relation between Binary Black Hole Merger Times and Host Galaxy Properties
Authors: Kelly Holley-Bockelmann, Fazeel Mahmood Khan, Isaiah Williams, Jaelyn Roth, Michael Rizzo Smith, Kaitlin Porter, Jillian Bellovary, Andrea Derdzinski, Andrea V. Macciò
Figure caption: MBH binary coalescence time as a function of selected features. In each panel, the dots are colored according to the orientation of the binary orbital angular momentum vector with respect to that of the host galaxy—green: prograde; buff: nonrotating host; and pink: retrograde orbits. Left: we select a host-galaxy-related feature, the galaxy stellar mass. Middle: here, we feature the coalescence time as a function of a BH-related feature, the binary BH mass, MBBH. Right: we show how the coalescence time depends on the eccentricity in the hardening radius, ﹩{e}_{{r}_{h}}﹩. Note the large degree of scatter in the coalescence time in each panel, as well as the strong clustering of coalescence time with binary orbit; these are indications that these features are a projection of a higher-dimension manifold, and that the orbit is one of the key predictors of the coalescence time.
Paper: Handy Relation between Binary Black Hole Merger Times and Host Galaxy Properties
Authors: Kelly Holley-Bockelmann, Fazeel Mahmood Khan, Isaiah Williams, Jaelyn Roth, Michael Rizzo Smith, Kaitlin Porter, Jillian Bellovary, Andrea Derdzinski, Andrea V. Macciò
Figure caption: Measured versus predicted coalescence time. The colored points represent the predicted coalescence times for the three-term model (left, see Equation (4)) and the four-term model (right, see Equation (5)), for a given measured coalescence time, with the least-squares fits to these data plotted in matching colors (left: purple; and right: yellow). The black line represents a perfect prediction. Using a coalescence model with Reff, v/σ∣proj, log MNSC, and log MBBH, we can reduce the variance in the merger time predictions from 2 orders of magnitude to less than a factor of roughly 2.
Paper: Handy Relation between Binary Black Hole Merger Times and Host Galaxy Properties
Authors: Kelly Holley-Bockelmann, Fazeel Mahmood Khan, Isaiah Williams, Jaelyn Roth, Michael Rizzo Smith, Kaitlin Porter, Jillian Bellovary, Andrea Derdzinski, Andrea V. Macciò
Figure caption: Fractional differences in coalescence time predictions for the galaxy runs described in Table 2, using the four-term model (Equation (5)). A typical coalescence time prediction will under- or overestimate the true coalescence time by ∼20%. There is a slight hint that the predicted coalescence timescales for retrograde orbits have a larger scatter and a small bias toward overestimating the true coalescence timescale.
Paper: Numerical Nonadiabatic Tidal Calculations with GYRE-tides: The WASP-12 Test Case
Authors: Meng Sun, 萌 孙, R. H. D. Townsend, Hongbo Xia, 宏博 夏, Jifeng Liu
Figure caption: Same as Figure 4, but for a 1.2 M⊙ subgiant stellar model whose core is dominated by a radiative zone.
Paper: Handy Relation between Binary Black Hole Merger Times and Host Galaxy Properties
Authors: Kelly Holley-Bockelmann, Fazeel Mahmood Khan, Isaiah Williams, Jaelyn Roth, Michael Rizzo Smith, Kaitlin Porter, Jillian Bellovary, Andrea Derdzinski, Andrea V. Macciò
Figure caption: Correlation matrix for selected features used in this study. The intensity of the hue represents the correlation strength, with green indicating a positive correlation and purple representing an anticorrelation. It is clear that there are very few features that are uncorrelated, indicating that care must be taken to address multicollinearity in potential models.
Paper: Multimessengers from the Radioactive Decay of r-process Nuclei
Authors: Axel Gross, Samuel Cupp, Matthew R. Mumpower
Figure caption: (a) Neutrino flux at different times as a function energy assuming an ejecta mass of 0.01M⊙ at a source distance of 15 kpc. (b) γ-ray flux at different times as a function of energy assuming an ejecta mass of 0.01M⊙ at a source distance of 15 kpc. This spectrum was broadened as described in Equation (A6) with an assumed expansion velocity of 0.1c. The gray lines show the detection limits of next-generation γ-ray detectors for a 1 Ms (106 s) duration exposure.
Paper: Handy Relation between Binary Black Hole Merger Times and Host Galaxy Properties
Authors: Kelly Holley-Bockelmann, Fazeel Mahmood Khan, Isaiah Williams, Jaelyn Roth, Michael Rizzo Smith, Kaitlin Porter, Jillian Bellovary, Andrea Derdzinski, Andrea V. Macciò
Figure caption: Fractional error in coalescence time for our test suite. The simulations are taken from M. A. Mirza et al. (2017), where the A models explore the effect of binary orbital inclination with respect to the galaxy plane and the B models investigate the effect of counterrotating galaxy cores. The subscript corresponds to Θ, the angle between the angular momentum axis of the binary BH orbit and the angular momentum axis of the galaxy, where 0∘ < Θ < 90∘ corresponds to corotation of the binary with the stellar material of the galaxy and 90∘ < Θ < 180∘ corresponds to counterrotation.
Paper: Multimessengers from the Radioactive Decay of r-process Nuclei
Authors: Axel Gross, Samuel Cupp, Matthew R. Mumpower
Figure caption: (a) Average particle energy as a function of time. The solid curves give the result from the calculation, while the dotted curves give the expected value assuming thermal equilibrium. (b) Spectral energy distribution at 10 s (solid curves) as compared to the expected distribution assuming thermal equilibrium (dotted curves). The colored ticks on the upper x-axis give the average energy of the emitted particles (solid) and that expected from a thermal distribution (dotted).
Paper: Multimessengers from the Radioactive Decay of r-process Nuclei
Authors: Axel Gross, Samuel Cupp, Matthew R. Mumpower
Figure caption: Each panel gives the calculated β-decay spectra for electrons (solid blue), γ-rays (dashed green), neutrinos (dotted purple), and neutrons (dashed–dotted orange) at the corresponding time, in units of number s–1 MeV–1, per unit abundance (left axis). The right axis characterizes these spectra scaled to the emission per gram of emitted material. The colored ticks above the plot region give the average energy per particle of the corresponding species at the given time. Note the axis bounds change between rows.
Paper: Multimessengers from the Radioactive Decay of r-process Nuclei
Authors: Axel Gross, Samuel Cupp, Matthew R. Mumpower
Figure caption: (a) Total energy (flux) of emitted particles in units of MeV s–1 per unit abundance (left axis) as a function of time. The right axis gives the emission scaled to the conventional units of erg s–1 g–1. (b) The relative contributions of each channel to the total emission energy.
Paper: Multimessengers from the Radioactive Decay of r-process Nuclei
Authors: Axel Gross, Samuel Cupp, Matthew R. Mumpower
Figure caption: Final abundance pattern (at 100 Myr ) of our nucleosynthesis calculation (red) as compared to the solar r-process residuals (black). The two patterns are normalized to be identical at A = 150.
Paper: Very Large Telescope Observations of Interstellar Comet 3I/ATLAS. II. From Quiescence to Glow: Dramatic Rise of Ni I Emission and Incipient CN Outgassing at Large Heliocentric Distances 
Authors: Rohan Rahatgaonkar, Juan Pablo Carvajal, Thomas H. Puzia, Baltasar Luco, Emmanuel Jehin, Damien Hutsemékers, Cyrielle Opitom, Jean Manfroid, K. Aravind, Michaël Marsset, Bin Yang, Laura Buchanan, Wesley C. Fraser, John Forbes, Michele Bannister, Dennis Bodewits, Bryce T. Bolin, Matthew Belyakov, Matthew M. Knight, Colin Snodgrass, Erica Bufanda, Rosemary Dorsey, Léa Ferellec, Fiorangela La Forgia, Manuela Lippi, Brian Murphy, Prasanta K. Nayak, Mathieu Vander Donckt
Figure caption: Nickel production versus heliocentric distance: measurements from VLT/X-Shooter (blue circles) and VLT/UVES (teal hexagons) obtained in this work are shown for comet 3I/ATLAS—the black solid and gray dashed curves are power-law fits to the 3I data only, giving ﹩Q({\rm{Ni}})\propto {r}_{h}^{-7.7\pm 1.0}﹩ (weighted) and ﹩Q({\rm{Ni}})\propto {r}_{h}^{-8.8\pm 1.0}﹩ (unweighted), respectively. The colored symbols compare with solar system comets compiled from the literature, grouped by dynamical class as in the legend; the green squares mark measurements for 2I. The left axis gives ﹩{\mathrm{log}}_{10}[Q({\rm{Ni}})/{\rm{atoms}}\,{{\rm{s}}}^{-1}]﹩ and the bottom axis gives in log scale the heliocentric distance rh (au). The right axis shows an approximate equilibrium surface temperature T(rh)—orange line, scaled to 200 K at rh  =  3 au—to guide the eye (see the text for details). The horizontal dashed lines indicate sublimation thresholds for CO, NH3, CO2, and H2O. Other comet references: P. Guzik & M. Drahus (2021), D. Hutsemékers et al. (2021), J. Manfroid et al. (2021), and C. Opitom et al. (2021).
Paper: Very Large Telescope Observations of Interstellar Comet 3I/ATLAS. II. From Quiescence to Glow: Dramatic Rise of Ni I Emission and Incipient CN Outgassing at Large Heliocentric Distances 
Authors: Rohan Rahatgaonkar, Juan Pablo Carvajal, Thomas H. Puzia, Baltasar Luco, Emmanuel Jehin, Damien Hutsemékers, Cyrielle Opitom, Jean Manfroid, K. Aravind, Michaël Marsset, Bin Yang, Laura Buchanan, Wesley C. Fraser, John Forbes, Michele Bannister, Dennis Bodewits, Bryce T. Bolin, Matthew Belyakov, Matthew M. Knight, Colin Snodgrass, Erica Bufanda, Rosemary Dorsey, Léa Ferellec, Fiorangela La Forgia, Manuela Lippi, Brian Murphy, Prasanta K. Nayak, Mathieu Vander Donckt
Figure caption: CN production versus heliocentric distance: measurements from VLT/X-Shooter (blue circles) and VLT/UVES (teal hexagons) obtained in this work are shown for 3I/ATLAS—the black solid and gray dashed curves are power-law fits to the 3I data only, giving ﹩Q({\rm{CN}})\propto {r}_{h}^{-6.7\pm 0.2}﹩ (weighted) and ﹩Q({\rm{CN}})\propto {r}_{h}^{-6.6\pm 0.2}﹩ (unweighted), respectively. The colored symbols compare with solar system comets compiled from the literature, grouped by dynamical class as in the legend; the green squares mark measurements for 2I. The left axis gives ﹩{\mathrm{log}}_{10}[Q({\rm{CN}})/{\rm{molecules}}\,{{\rm{s}}}^{-1}]﹩ and the bottom axis gives in log scale the heliocentric distance rh (au). The right axis shows an approximate equilibrium surface temperature T(rh). The horizontal dashed lines indicate sublimation thresholds for CO, NH3, CO2, and H2O. Other comet references: H. Rauer et al. (2003), R. Schulz et al. (2004), C. Opitom et al. (2016), C. Opitom et al. (2017), A. Fitzsimmons et al. (2019), C. Opitom et al. (2019), and J. Manfroid et al. (2021).
Paper: Very Large Telescope Observations of Interstellar Comet 3I/ATLAS. II. From Quiescence to Glow: Dramatic Rise of Ni I Emission and Incipient CN Outgassing at Large Heliocentric Distances 
Authors: Rohan Rahatgaonkar, Juan Pablo Carvajal, Thomas H. Puzia, Baltasar Luco, Emmanuel Jehin, Damien Hutsemékers, Cyrielle Opitom, Jean Manfroid, K. Aravind, Michaël Marsset, Bin Yang, Laura Buchanan, Wesley C. Fraser, John Forbes, Michele Bannister, Dennis Bodewits, Bryce T. Bolin, Matthew Belyakov, Matthew M. Knight, Colin Snodgrass, Erica Bufanda, Rosemary Dorsey, Léa Ferellec, Fiorangela La Forgia, Manuela Lippi, Brian Murphy, Prasanta K. Nayak, Mathieu Vander Donckt
Figure caption: Continuum-subtracted UV/blue spectra of 3I/ATLAS showing Ni I emission over 11 VLT/X-Shooter (blue) and two VLT/UVES (cyan) visits. The spectra are vertically offset for clarity, with visit labels and dates indicated. The UVES data are scaled to match X-Shooter continuum noise levels (using visits 9–11 as references) for visualization. Left panel: 3210–3255 Å region showing selected Ni I lines. Right panel: 3350–3630 Å region displaying the full forest of Ni I transitions. The dotted vertical lines mark the laboratory wavelengths of the detected Ni I lines (in angstroms). The emission strengthens toward later epochs, with the first significant detection at rh = 3.78 au in visit X5 (2025 July 23).
Paper: Very Large Telescope Observations of Interstellar Comet 3I/ATLAS. II. From Quiescence to Glow: Dramatic Rise of Ni I Emission and Incipient CN Outgassing at Large Heliocentric Distances 
Authors: Rohan Rahatgaonkar, Juan Pablo Carvajal, Thomas H. Puzia, Baltasar Luco, Emmanuel Jehin, Damien Hutsemékers, Cyrielle Opitom, Jean Manfroid, K. Aravind, Michaël Marsset, Bin Yang, Laura Buchanan, Wesley C. Fraser, John Forbes, Michele Bannister, Dennis Bodewits, Bryce T. Bolin, Matthew Belyakov, Matthew M. Knight, Colin Snodgrass, Erica Bufanda, Rosemary Dorsey, Léa Ferellec, Fiorangela La Forgia, Manuela Lippi, Brian Murphy, Prasanta K. Nayak, Mathieu Vander Donckt
Figure caption: Continuum-subtracted spectra of 3I/ATLAS in the CN B2Σ+–X2Σ+(0–0) violet band region (3860–3890 Å) from a monitoring campaign spanning 2025 July 4–August 21. The grid displays 11 X-Shooter spectra (X1–X11) and two high-resolution UVES observations (U1 and U2), arranged by decreasing heliocentric distance, from top left to bottom right. Each panel indicates the observation date and heliocentric distance rh (in astronomical units). CN emission is first detected in visit X6 (2025 July 27, rh = 3.65 au) and increases in strength as the comet approaches the Sun. The green shaded region marks the CN-band feature. UVES spectra show finer spectral structure compared to the lower-resolution X-Shooter observations. The shaded regions represent 1σ uncertainties.
Paper: AT2025ulz and S250818k: Deep X-Ray and Radio Limits on Off-axis Afterglow Emission and Prospects for Future Discovery
Authors: Brendan O'Connor, Roberto Ricci, Eleonora Troja, Antonella Palmese, Yu-Han Yang, Geoffrey Ryan, Hendrik van Eerten, Muskan Yadav, Xander J. Hall, Ariel Amsellem, R. L. Becerra, Malte Busmann, Tomás Cabrera, Simone Dichiara, Lei Hu, Ravjit Kaur, Keerthi Kunnumkai, Ignacio Magaña Hernandez
Figure caption: Allowed parameter space (shaded regions) for afterglow nondetection, assuming a Gaussian structured jet, at 400 Mpc (z = 0.08484) based on our deep radio and X-ray upper limits. The darker shaded regions show a range of parameters that produce late-peaking afterglows that are detectable to our observational limits (if extended in time to ∼150 days) but not ruled out by the current data (<50 days). Left: allowed values of the magnetic energy fraction εB versus circumburst density n for different viewing angles θv/θc. We have fixed Ekin = 1052 erg, θc = 0.056 rad (3.2°), εe = 0.1, and p = 2.2. Right: allowed viewing angles θv/θc as a function of core kinetic energy Ekin for different circumburst density n. We have fixed θc = 0.056 rad (3.2°), εB = 10−2, εe = 0.1, and p = 2.2.
Paper: AT2025ulz and S250818k: Deep X-Ray and Radio Limits on Off-axis Afterglow Emission and Prospects for Future Discovery
Authors: Brendan O'Connor, Roberto Ricci, Eleonora Troja, Antonella Palmese, Yu-Han Yang, Geoffrey Ryan, Hendrik van Eerten, Muskan Yadav, Xander J. Hall, Ariel Amsellem, R. L. Becerra, Malte Busmann, Tomás Cabrera, Simone Dichiara, Lei Hu, Ravjit Kaur, Keerthi Kunnumkai, Ignacio Magaña Hernandez
Figure caption: Afterglow lightcurves for different viewing angles θv/θc generated using afterglowpy (G. Ryan et al. 2020), using the afterglow fit parameters derived for GW170817 (G. Ryan et al. 2024) for a distance of 400 Mpc. The viewing angle of θv/θc = 6 corresponds to the observed value for GW170817. X-ray lightcurves at 1 keV are shown as solid lines, and radio lightcurves at 6 GHz are shown as dashed lines. X-ray upper limits are shown as black triangles, and radio upper limits as gray triangles. All radio observations are from the VLA, and X-ray observations are ordered from left to right as: Swift, EP/FXT, Swift, XMM-Newton, Chandra, and Chandra. The parameters used to plot the lightcurves are (G. Ryan et al. 2024) Ekin = 4.8 × 1053 erg, θc = 3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2, θw = 4.9θc, n = 2.4 × 10−3 cm−3, p = 2.13, εe = 1.9 × 10−3, εB = 5.75 × 10−4, ξN = 1.0, dL = 400 Mpc, and z = 0.08484.