adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies
Authors: Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer, Ezequiel Treister
Figure caption: The relationship between the kinetic pressure of the ISM (P ISM) and the weight of the ISM (﹩{ \mathcal W }﹩) for inactive galaxies (panel (a)) and for quasar host galaxies (panels (b)–(d)). Each data point represents a specific pixel. The blue circles illustrate the mean values of P ISM for normal star-forming galaxies within 0.3 dex ﹩{ \mathcal W }﹩ bins, while red circles denote that for PG quasars. Error bars indicate the standard deviation of P ISM within each ﹩{ \mathcal W }﹩ bin. The black dashed line represents the line of equality, with an associated scatter of 0.3 dex by the dotted lines. The blue dashed–dotted line represents the fitting result obtained through the usage of linmix, with uncertainties represented by the blue-shaded region.
Paper: Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies
Authors: Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer, Ezequiel Treister
Figure caption: An illustrative example of our analysis. Panels (a) and (b) show the velocity-dispersion map generated from the deconvolved 3D BAROLO model and the corresponding mock observation, respectively. Panel (c) displays the σ map obtained by applying our correction method to the map in panel (b). Panel (d) presents a comparison between the pixel-wise velocity dispersions derived from the two methods. The x-axis represents the pixel-wise velocity dispersion directly extracted from the second-moment map generated by the 3D BAROLO model (panel a), while the y-axis represents the velocity dispersion obtained using our beam-smearing-correction method. The blue dotted lines indicate the input value of σ, and the black dashed line denotes the 1:1 relation. In panels (a) through (c), the black contours start at 30 km s−1 and increase in increments of 10 km s−1.
Paper: Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies
Authors: Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer, Ezequiel Treister
Figure caption: Comparison between the stellar masses obtained through our dynamical methodology and those documented in the literature. The black solid line corresponds to the equality line, while the dotted lines represent the extent of the associated 0.3 dex uncertainties. The best-fit outcome of the linmix fitting procedure is represented by the dashed–dotted line, while the associated uncertainties inherent in the linmix results are shown as the shaded gray region. The mass of I Zw 1 is also included in this figure (Q. Fei et al. 2023).
Paper: Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies
Authors: Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer, Ezequiel Treister
Figure caption: The scale height of the molecular gas disk in quasar host galaxies (orange boxes) and in the control sample (light blue). Each box represents the range between the 25th and 75th percentile of the scale height, with the median value indicated by a thick vertical line. The extended caps on the boxes represent the range between the 16th and 84th percentile of the scale height, which are used to estimate the uncertainty. The values and uncertainties of the scale height for each galaxy are labeled on the right side of the figure. The vertical dashed lines represent the range of gas disk scale height given by previous studies for normal star-forming galaxies and starburst galaxies (C. Bacchini et al. 2019; C. D. Wilson et al. 2019).
Paper: Multi-Observatory Research of Young Stellar Energetic Flares (MORYSEF): X-Ray-flare-related Phenomena and Multi-epoch Behavior
Authors: Konstantin V. Getman, Eric D. Feigelson, Abygail R. Waggoner, L. Ilsedore Cleeves, Jan Forbrich, Joe P. Ninan, Oleg Kochukhov, Vladimir S. Airapetian, Sergio A. Dzib, Charles J. Law, Christian Rab
Figure caption: Low-resolution, smoothed Chandra ACIS-I images of the Orion Nebula region presented for each of the four distinct epochs of observations: 2003 January, 2012 October, 2016 November, and 2023 December. The images are given for the 0.5−8 keV energy band. Each panel represents the combined view of multiple observations conducted during the corresponding epoch, with ﹩17^{\prime} \times 17^{\prime} ﹩ fields of view for each observation outlined in blue. Due to variations in roll angles among observations within each epoch, the merged images sometimes display polygonal shapes rather than perfect squares.
Paper: Model-independent Calibration for Sound Horizon: Combining Observations of Supernovae and Baryon Acoustic Oscillation Measurements
Authors: Tonghua Liu, Xinyi Zhong, Marek Biesiada, Jieci Wang
Figure caption: Left panel: the GPR reconstructed unanchored distances H 0 D  L /c using the Pantheon SN Ia data set. Right panel: the same as the left figure but for Pantheon+ data set. The lines are from the GPR reconstruction and are made up of 1000 curves. The points and error bars come from observed samples of SNe Ia.
Paper: Thermal Evolution of the Intergalactic Medium due to Lyα Photons during the Cosmic Dawn
Authors: Janakee Raste, Anjan Kumar Sarkar, Shiv K. Sethi
Figure caption: In the left panel, we show the evolution of intensity profile J(x, t) for photons injected at x = 0 with Voigt profile. The x-axis is in units x 0 = x(T = 10 K). The left and the middle panel share the same y-axis (ticks on left panel) and the color scheme for time evolution of profiles (inset of middle panel). The source switches on at redshift z = 20 with an initial temperature T = 10 K and source intensity ﹩C={10}^{-10}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}\,{\mathrm{sr}}^{-1}﹩. In the middle panel, we start with quasi-static profile (with the same redshift and initial temperature as the left panel) and follow the intensity profile after switching off the source at t = 0. In the right panel, we show the evolution of temperature for the following cases: (a) the curves “source switched on” are for sources switching on at t = 0 (J(x) evolution is shown in the left panel). These plots correspond to two different values of C (red and blue curves) and redshifts z = 20 (solid curves) and z = 15 (dashed curves), (b) for the case “source continues,” the initial profile at t = 0 is assumed to be the quasi-static solution at T = 10 K, and it evolves with thermal feedback, with ﹩C={10}^{-10}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}\,{\mathrm{sr}}^{-1}﹩ and z = 20 (J(x) evolution for this case is not shown in the plot), and (c) for the case “source switched off,” the initial profile is again the quasi-static solution with T = 10 K, but the source is switched off at t = 0, and the profile is allowed to evolve (J(x) evolution is shown in the middle panel).
Paper: Thermal Evolution of the Intergalactic Medium due to Lyα Photons during the Cosmic Dawn
Authors: Janakee Raste, Anjan Kumar Sarkar, Shiv K. Sethi
Figure caption: This figure shows all the three branches the intensity profile J(x, t) for continuum energy injection, including the approach to quasi-static intensity profile (Equation (13)). In all the panels, ﹩{x}_{\max }=250﹩, the initial temperature T = 10 K, and z = 20. The left and the middle panels correspond, respectively, to ﹩C={10}^{-15}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}\,{\mathrm{sr}}^{-1}﹩ and ﹩C={10}^{-12}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}\,{\mathrm{sr}}^{-1}﹩. In the right panel, we show the temperature evolution for a range of photon injection rates, C (solid curves), which includes the two cases for which the intensity profiles are shown in the left and the middle panel. We also show the temperature evolution for the flat profiles displayed in Figure 2 (dashed curves) and the tilted profile with ﹩{x}_{\max }=500﹩ (dotted curves) for comparison. J(x) evolution for ﹩{x}_{\max }=500﹩ case is not shown here. We see that the final equilibrium temperature is a function of ﹩{x}_{\max }﹩, with larger ﹩{x}_{\max }﹩ resulting in higher final temperature.
Paper: Thermal Evolution of the Intergalactic Medium due to Lyα Photons during the Cosmic Dawn
Authors: Janakee Raste, Anjan Kumar Sarkar, Shiv K. Sethi
Figure caption: In the left and middle panels, we show the evolution of Lyα continuum photons intensity J(x, t) at redshift z = 20 and initial temperature T = 10 K when the source switches on (left panel) and switches off (middle panel). The energy injection rate ﹩C={10}^{-12}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}\,{\mathrm{sr}}^{-1}﹩. In the right panel, we show the evolution of temperature for the same cases as in Figure 1.
Paper: The Excess of JWST Bright Galaxies: A Possible Origin in the Ground State of Dynamical Dark Energy in the Light of DESI 2024 Data
Authors: N. Menci, A. A. Sen, M. Castellano
Figure caption: The ratio of the characteristic mass M  c (t) for different nCC models to that in the ΛCDM case, for our fiducial combination w 0 = −0.9, w  a  = 0.1. The color code corresponds to different values of ΩΛ as shown in the color bar.
Paper: The Excess of JWST Bright Galaxies: A Possible Origin in the Ground State of Dynamical Dark Energy in the Light of DESI 2024 Data
Authors: N. Menci, A. A. Sen, M. Castellano
Figure caption: The evolution of galaxy LFs for the different values of ΩΛ shown in the legend. We assumed our fiducial choice of the combination w 0 = −0.9 and w  a  = 0.1. The data are from R. J. Bouwens et al. (2015, 2021, 2022) (filled triangles), S. L. Finkelstein et al. (2023) (filled squares), M. Stefanon et al. (2021) (open circles), C. T. Donnan et al. (2023) (filled circles), D. J. McLeod et al. (2024) (filled pentagons), C. M. Casey et al. (2024) (empty squares), Y. Harikane et al. (2023) (empty triangles), N. J. Adams et al. (2024) (empty pentagons), and B. Robertson et al. (2024) (filled hexagons).
Paper: The Excess of JWST Bright Galaxies: A Possible Origin in the Ground State of Dynamical Dark Energy in the Light of DESI 2024 Data
Authors: N. Menci, A. A. Sen, M. Castellano
Figure caption: The evolution of UV luminosity density for the values of ΩΛ shown in the color bar, and for our fiducial combination w 0 = −0.9 and w  a  = 0.1. The data are from S. L. Finkelstein et al. (2023) (downward triangles), C. T. Donnan et al. (2024) (circles), D. J. McLeod et al. (2024) (filled pentagons), Y. Harikane et al. (2023) (squares), N. J. Adams et al. (2024) (hexagons), and P. G. Pérez-González et al. (2023) (upward triangles).
Paper: The Excess of JWST Bright Galaxies: A Possible Origin in the Ground State of Dynamical Dark Energy in the Light of DESI 2024 Data
Authors: N. Menci, A. A. Sen, M. Castellano
Figure caption: The DM halo mass function corresponding at redshift z = 7 (red lines) and z = 13 (black lines) in nCC models with different, negative values of ΩΛ are shown as continuous lines. For reference, we also show as dashed lines the halo mass function corresponding to the standard ΛCMD cosmology.
Paper: The Excess of JWST Bright Galaxies: A Possible Origin in the Ground State of Dynamical Dark Energy in the Light of DESI 2024 Data
Authors: N. Menci, A. A. Sen, M. Castellano
Figure caption: For each (w 0, w  a ) we show as colored contours the values of ΩΛ leading to the same boost (to within 5%) in the peak value of the characteristic mass shown in Figure 1. The red contour shows the 2σ confidence region consistent with CMB+DESI+Pantheon Plus data sets (H. Wang et al. 2024).
Paper: The Mass and Redshift Dependence of Halo Star Clustering
Authors: Zhenlin Tan, Wenting Wang, Jiaxin He, Yike Zhang, Vicente Rodriguez-Gomez, Jiaxin Han, Zhaozhou Li, Xiaohu Yang
Figure caption: This Figure, together with Figure 2 below, shows the median 2PCF signals for halo stars in galaxies with different halo mass, redshift, and formation redshift from TNG50, TNG100, or TNG300. For panels in the same row, they refer to galaxies with the same host halo mass, and the number in brackets of the left panel in each row corresponds to the log halo mass range. The leftmost panels also indicate the source of the results, specifying whether they come from the TNG50, TNG100, or TNG300 simulation. For panels in the same column, there are 2PCF signals at the same redshift, as indicated by the text on top of each column. In each panel, galaxies are divided into three different ranges according to their formation redshifts (z 3/4, see the legend), and their median 2PCFs are plotted in different colors and symbols. Here z 3/4 is defined as the redshift at which one galaxy has accreted three-fourths of its total ex situ stellar mass at the corresponding redshift. r in the x-axis is the galactocentric distance. When calculating the 2PCFs, we choose a fixed pair separation of Δx = 2.5−5 kpc. The error bars are based on the 1σ scatters of 100 bootstrapped subsamples.
Paper: The Mass and Redshift Dependence of Halo Star Clustering
Authors: Zhenlin Tan, Wenting Wang, Jiaxin He, Yike Zhang, Vicente Rodriguez-Gomez, Jiaxin Han, Zhaozhou Li, Xiaohu Yang
Figure caption: A continuation of Figure 1 above.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: Differentials of the BBH merger rate in the redshift ranges [0, 1], [1, z peak], [z peak, z peak + 1], and [z peak + 1, 9] as well as z peak and the local rate ﹩{{ \mathcal R }}_{0}﹩ plotted as a function of model parameters while keeping the second grid parameter fixed.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: The differential BBH merger rate in the interval z = 0 to z = 1 as a function of α CE values for different fixed values of β in our simulation grid A.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: The delay time distribution of BBHs, BHNSs, and BNSs for the model with α CE = 2.0 and β = 0.5. The left, middle, and right panels are the delay times for binaries formed at z = 0.2, 2.0, and 6.0, respectively.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: Same as Figure 2 but for the formation rates of BBH, BHNS, and BNS systems instead of merger rates. We define the formation time as directly after the second SN when both compact objects have formed.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: The same as Figure 7 but for BHNSs instead of BBHs.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: The same as Figure 7 but for BNSs instead of BBHs.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption:  S(T) of three different methods used to remove the trend of NE5. The cyan line corresponds to a power spectrum S(f) ∝ 1/f  β  with β equal to 8 and describes how the sum of the HHT trend, IMF5, and IMF4 varies (such power spectrum exponents usually arise in sums of IMFs and trend in HHT; see, e.g., Figure 7 of N. V. Sarlis et al. 2018). The Fourier transform power spectra have been normalized to unity so that ﹩{\int }_{0}^{{f}_{s}/2}S(f){df}=1﹩, where f  s  is the sampling frequency 14.61 yr−1.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: The scaling exponents H, a DFA, h CMA, and 1 + χ  H  for each of the five IBEX energy channels when analyzing the spikeless D14 flux time series. When examining whether the four scaling exponents exhibit a statistically significant result that shows a difference (anisotropy) between north and south, we obtain the corresponding p-values written in green. The method to estimate these p-values, which correspond to the probability to obtain such a result by chance, is presented in Appendix B.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption:  V  r  at 2h from the midplane in a simulation with a planet mass of 5M th and a numerical resolution of CPH = 20 at 100 (left) and 100.35 (middle) planetary orbits. The right panel shows the midplane density. The planet location is marked with a cyan dot in the first two panels. The dashed circle marks a region in between primary and secondary spiral arms in the inner disk. Color bars are in units of m s−1 and planetary Keplerian velocity V p,Kep. See Sections 3.1.1 and 3.1.2 for discussions.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: How the various detrending methods affect the fluctuation measure F DFA of DFA in the case of the energy channel NE5. Only F DFA for the original, the Hilbert–Huang, and the Wiener detrended data are not vertically displaced. The other three F DFA have been vertically displaced for reasons of clarity.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Surface density at 100 (upper) and 1000 orbits (middle) and the corresponding azimuthal average (excluding azimuth within ﹩\arcsin \left(3{R}_{{\rm{H}}}/{r}_{{\rm{p}}}\right)﹩ to the planet) surface-density profiles (lower). Cyan lines mark gap edges of r p ± 2R H (r p = 100 au and R H ∼ 9.4 au) in all panels. The surface-density peak along the primary inner and outer spirals is traced by green open circles.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Short-term variations in V  r  within five orbits at five locations at 2h above the midplane from point a to e in the disk and at t 0 = 100, 300, and 1000 orbits. The locations of points a, b, c, d, and e are shown in the midplane density map at 1000 orbits in the lower right panel. See Section 3.1.1 for details.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: Three-dimensional representation of the four scaling exponents H, a DFA, h CMA, and 1 + χ  H  vs. energy in which the standard error of each exponent is depicted by the color bar. The data concerning the north pole are shown by circles, while those of the south pole are shown by diamonds.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: 2D standard deviation map of V  r  at 100, 300, and 1000 orbits (left to right). The standard deviations are obtained within five orbits (see details in Section 3.1.1).
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: The maximum-likelihood geometry configuration for the joint NICER and XMM-Newton analysis using the PDT-U H R eq ∈ [10, 14] km model. The viewing angle represents the Earth’s inclination to the spin axis. The maximum-likelihood geometry is very similar for the PDT-U H R eq R21 and PDT-U He R eq R21 models, except that the primary superseding component is located at the equator for the latter.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: Posterior distributions for radius, mass, compactness, the logarithm of the surface gravity, and the cosine of the inclination for the ST-U runs. See the caption of Figure 5 for additional details.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption:  PDT-U posterior distributions for radius and the secondary hot region parameters. See the caption of Figure 5 for additional details.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption:  PDT-U posterior distributions for radius and the primary hot region parameters. See the caption of Figure 5 for additional details.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption:  PDT-U posterior distributions for radius and the other parameters. See the caption of Figure 5 for additional details.
Paper: Mildly Super-Eddington Accretion onto Slowly Spinning Black Holes Explains the X-Ray Weakness of the Little Red Dots
Authors: Fabio Pacucci, Ramesh Narayan
Figure caption: Top Row: comparison (at z = 0) between typical X-ray weak (left, mildly super-Eddington with zero spin) and X-ray strong (right, mildly super-Eddington with high spin) SEDs. Bottom Row: same as in the top row, but at z = 6. The eight gray lines represent the spectrum for lines of sight ranging from 80° (bottom) to 10° (top) from the pole. The red line indicates the spectrum averaged over 4π steradians. In the bottom panel, the arrows indicate typical flux limits for deep-field X-ray surveys with Chandra (2–10 keV) and AXIS (0.2–10 keV). Some of these SEDs extend up to ∼1 MeV.
Paper: Mildly Super-Eddington Accretion onto Slowly Spinning Black Holes Explains the X-Ray Weakness of the Little Red Dots
Authors: Fabio Pacucci, Ramesh Narayan
Figure caption: Comparison of the 2–10 keV bolometric correction as a function of the logarithm of the Eddington ratio in the rest frame (left panel) and in the observed 2–10 keV band when the source is placed at the median redshift of z = 6 (right panel). Different colors indicate varying inclination angles from the pole (degrees), and different markers represent different spin values: triangles for a = 0.9, circles for a = 0.68, and stars for a = 0. Mildly super-Eddington accretion rates (1.4 <  f Edd < 4) onto slowly spinning black holes, if observed at large inclination angles from the pole, lead to extremely large values of the bolometric correction, especially if the SMBH is highly redshifted.