adsabs/AstroCLIMB huggingface dataset:
Paper: Shadow Geometry of Kerr Naked Singularities
Authors: Bao Nguyen, Pierre Christian, Chi-kwan Chan
Figure caption: Shadows of KNSs with different spins a and observational inclination angles i. From left to right, the plots correspond to a = 1.37, 1.63, and 1.96, respectively. In each plot, the shadow shifts from left to right as the inclination angles range from i = 15°, 30°, and 45° for the left, center, and right plots, respectively, to i = 75°, with increments of 15°. The colors represent the effective angular momentum Φ of each spherical photon orbit projected on the image plane and range from Φ = −9 (more retrograde) to Φ = −1 (less retrograde). Redder and bluer colors represent higher and lower effective angular momenta, respectively. The plots show that for a fixed spin a ≳ 1.18, as ﹩{{\rm{\Phi }}}_{\max }\lt 0﹩, retrograde photon orbits at lower inclination might exceed ﹩{{\rm{\Phi }}}_{\max }﹩, so the shadow vanishes. As the inclination increases, the retrograde photon orbits become more retrograde, and their effective angular momentum falls below ﹩{{\rm{\Phi }}}_{\max }﹩, so the shadow reemerges again.
Paper: Shadow Geometry of Kerr Naked Singularities
Authors: Bao Nguyen, Pierre Christian, Chi-kwan Chan
Figure caption: Shadows of KNSs with different spins a and observational inclination angles i. From left to right, the plots correspond to i = 15°, 45°, and 90°, respectively. In each plot, different colors correspond to different spins, ranging from purple being a = 1 to dark red being a = 1.403 for i = 15° and a = 2 for i = 45° and 90°. The plots demonstrate that for smaller inclination angles (closer to face-on), the shadow of KNS opens its gap at a greater spin and vanishes at a smaller spin in comparison to greater inclination angles (closer to edge-on). These features are consistent with the a − i phase space classification in Figure 2. In general, the KNS shadows shift rightward like KBH shadows; however, for low inclination angles like i = 15°, the shadow vanishes faster than its rightward shifting, so it appears to shift leftward.
Paper: Shadow Geometry of Kerr Naked Singularities
Authors: Bao Nguyen, Pierre Christian, Chi-kwan Chan
Figure caption: Shadows of KNSs with different spins a and observational inclination angles i. From left to right, the plots correspond to a = 1.01, 1.18, and 1.38, respectively. In each plot, different colors correspond to different inclination angles, ranging from purple being i = 0° (face-on) for the left and central plots and i = 14° for the right plot to dark red being i = 90° (edge-on). The plots show that a closed shadow is only possible for lower inclination angles and small spins 1 < a ≲ 1.18. For a ≈ 1.18, the shadow is open with a gap for all inclination angles. For a ≳ 1.18, the shadow vanishes for small inclination angles. These features are consistent with the a − i phase space classification in Figure 2.
Paper: Shadow Geometry of Kerr Naked Singularities
Authors: Bao Nguyen, Pierre Christian, Chi-kwan Chan
Figure caption: Deflection angle plots on the image plane for spins a = 1.01 and 1.38 and observational inclination angle i = 30° for the numerical ray-tracing calculations described in Section 3.1. Redder colors represent higher deflection angles for light rays that return to the vicinity of the image plane. Bluer colors represent lower deflection angles for light rays that travel to the other side of the KNS. The yellow curve represents the analytical shadow computed by Equations 8(a)–9(b) in Section 2.1. On the deflection angle plot, the numerical shadow corresponds to the region where light rapidly oscillates between high deflection angles and low deflection angles because the shadow is defined as the projection of unstable spherical photon orbits. Our numerical ray-tracing calculations reproduce the analytical predictions of the KNS shadow in Section 2.2.
Paper: Shadow Geometry of Kerr Naked Singularities
Authors: Bao Nguyen, Pierre Christian, Chi-kwan Chan
Figure caption: Schematic diagram of the numerical setup. The orange ring represents the KNS centered at the origin of the Cartesian Kerr–Schild coordinate system. The blue square grid represents the image plane, which is located at a distance 10,000  M away from the KNS at a polar inclination angle i with respect to the normal of the ring singularity. The image plane is effectively at infinity with respect to the KNS, so its orthogonal coordinates α and β are related to the conserved quantities of photons by Equation (9). The brown circles represent the photons, which are spaced 0.125 M from each other on a grid of 128 × 160.
Paper: Shadow Geometry of Kerr Naked Singularities
Authors: Bao Nguyen, Pierre Christian, Chi-kwan Chan
Figure caption: The blue solid line demonstrates maximum Φ for unstable photon orbits as a function of spin a. The red and black dotted lines correspond to spins of interest a = 1 and a ≈ 1.18, respectively.
Paper: Evidence of Extended Dust and Feedback around z ≈ 1 Quiescent Galaxies via Millimeter Observations
Authors: Jeremy Meinke, Seth Cohen, Jenna Moore, Kathrin Böckmann, Philip Mauskopf, Evan Scannapieco
Figure caption: Overlap (black, circles) and Wide-Area (blue, triangles) galaxy energies in 0.1 dex stellar mass bins with the associated energy–mass fit as described in Table 6 after forward-modeling our stellar mass uncertainties (Section 4.12.1). The shaded fit regions correspond to forward-modeled 2σ levels. Inset: 1 and 2σ bounds of the (non–forward-modeled) fit parameters E th(μ = 11.36 dex) and slope α. We show E th(μ = 11.36 dex) instead of E pk here as the samples contain different peak masses.
Paper: Evidence of Extended Dust and Feedback around z ≈ 1 Quiescent Galaxies via Millimeter Observations
Authors: Jeremy Meinke, Seth Cohen, Jenna Moore, Kathrin Böckmann, Philip Mauskopf, Evan Scannapieco
Figure caption: Overlap (black, circles) and Wide-Area (blue, triangles) galaxy dust masses in 0.1 dex stellar mass bins with the associated dust–stellar mass fit as in Table 6 after forward-modeling our stellar mass uncertainties (Section 4.12.1). The shaded fit regions correspond to forward-modeled 2σ levels. Inset: 1 and 2σ bounds of the non–forward-modeled fit parameters M d(μ = 11.36 dex) and α d. We show M d(μ = 11.36 dex) instead of M d,pk here as the samples contain different peak stellar masses.
Paper: Evidence of Extended Dust and Feedback around z ≈ 1 Quiescent Galaxies via Millimeter Observations
Authors: Jeremy Meinke, Seth Cohen, Jenna Moore, Kathrin Böckmann, Philip Mauskopf, Evan Scannapieco
Figure caption: Posterior corner plot of the dust profile fit for our Overlap (blue) and Wide-Area (black) galaxy catalogs. From dark to light, the three shaded contour regions correspond to the 1σ, 2σ, and 3σ levels.
Paper: Evidence of Extended Dust and Feedback around z ≈ 1 Quiescent Galaxies via Millimeter Observations
Authors: Jeremy Meinke, Seth Cohen, Jenna Moore, Kathrin Böckmann, Philip Mauskopf, Evan Scannapieco
Figure caption: Radial bin (﹩0^{\prime} \mbox{--}15^{\prime} ﹩) correlation matrices for the dust (left) and tSZ (right) two-component fit (Section 4.7) of 4000 bootstrap resamples outlined in Section 4.4 for the Overlap (top) and Wide-Area (bottom) galaxy catalogs.
Paper: Evidence of Extended Dust and Feedback around z ≈ 1 Quiescent Galaxies via Millimeter Observations
Authors: Jeremy Meinke, Seth Cohen, Jenna Moore, Kathrin Böckmann, Philip Mauskopf, Evan Scannapieco
Figure caption: Posterior corner plot of the tSZ profile fit for our Overlap (blue) and Wide-Area (black) galaxy catalogs. From dark to light, the three shaded contour regions correspond to the 1σ, 2σ, and 3σ levels.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Maps of the median metallicity in the disk in polar coordinates, to highlight any nonaxisymmetric features in the disk. The spatial bins are sized ΔR = 1 kpc and Δθ = 10°. The rows are different slices in Z, moving from closest to the Galactic plane (top row, ∣Z∣ ≤ 0.5 kpc), to farther above (bottom row, 1 ≤ ∣Z∣ ≤ 2.0 kpc). The left column shows the median [Fe/H] for each bin as a function of θ (point color), compared to the ±1σ expected spread from uncertainty in the measurement of the median (gray shaded region). The right column shows the median metallicity maps as a function of radius R and azimuthal angle θ. The black line is the approximate location of the Galactic Bar, defined as an ellipse with major axis length 10 kpc, a 0.4 axis ratio, and rotated 25°. The black square in the top panel highlights the region shown in more detail in Figure 12.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Same as Figure 8, but colored by stellar age. Points with [Fe/H] ≤ −0.7 have been excluded for potentially unreliable age estimates with the cuts described in Section 2.4. The percentage of stars (f distmass) in each bin that pass the distmass quality criterion is shown in parentheses in the upper-right corner of each panel.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Variation in the [Mg/Fe]–[Fe/H] plane as a function of Galactic radius (color) for stars within ∣Z∣ < 0.5 kpc of the plane. Top panel: the contour containing 75% of points for both the low-α and high-α samples, calculated separately. Bottom panel: the median [Mg/Fe] as a function of [Fe/H] for both sequences. The shaded regions denotes the ±1σ uncertainty in the median. In both panels, the black line is our defined boundary between the low-α and high-α described in Equation (1).
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Azimuthal variation in metallicity restricted to a window near the solar neighborhood, outlined by the black rectangle in Figure 11. The metallicity value is calculated as a running median for bin size ΔR = 0.5 kpc and Δθ = 5°, evaluated every ΔR = 0.1 kpc and Δθ = 1° for smoothing. The approximate locations of the nearby spiral arms from Reid et al. (2019) are plotted as colored lines.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Top panel: the radial R median metallicity profile of the low-α disk, split into different samples of stellar age (line color). Bottom panel: the vertical (Z) median metallicity profile of the low-α disk, split into different samples of stellar age (line color).
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The best-fit slope for each vertical metallicity profile in Figure 15, fit with a single line for stars beyond R > 7 kpc for the total sample (black line), and the low-α (blue line) and high-α (red line) samples independently. The shaded region indicates the ±1σ uncertainty in the slope measurement.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The best-fit slope for each radial metallicity profile in Figure 13 in units of dex kpc−1, fit with a single line for stars beyond R > 7 kpc for the total sample (black line), and the low-α (blue line) and high-α (red line) samples independently. The shaded region indicates the ±1σ uncertainty in the slope measurement.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Radial median metallicity profile as a function of height out of the plane (line color), for the total stellar population (top panel), the low-α disk (middle panel), and the high-α disk (bottom panel).
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Vertical median metallicity profile as a function of Galactocentric radius (line color) for the total stellar population (top panel), the low-α disk (middle panel), and the high-α disk (bottom panel).
Paper: Rapid Formation of Gas-giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores. II. Dependence on Pebble Bulk Density and Disk Temperature
Authors: Hiroshi Kobayashi, Hidekazu Tanaka
Figure caption: Results of DTPS with ρ m = 10−3 g cm−3 and T 1 = 100 K. Left: (a) solid surface density, ﹩{\rm{\Delta }}{{\rm{\Sigma }}}_{{\rm{s}}}/{\rm{\Delta }}\mathrm{ln}m﹩ at t = 2.3 × 105 yr, as a function of the mass of bodies and the distance from the host star. The values of the solid surface density are shown in the color bar. Right: protoplanet mass (b) and total solid surface density (c), as a function of the distance from the host star.
Paper: Rapid Formation of Gas-giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores. II. Dependence on Pebble Bulk Density and Disk Temperature
Authors: Hiroshi Kobayashi, Hidekazu Tanaka
Figure caption: Same as Figure 1, but for ρ m = 0.1 g cm−3. (a) is at 1.5 × 105 yr.
Paper: Rapid Formation of Gas-giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores. II. Dependence on Pebble Bulk Density and Disk Temperature
Authors: Hiroshi Kobayashi, Hidekazu Tanaka
Figure caption: Same as Figures 1(a), 2(a), and 3(a), but at 1.4 × 105 yr for T 1 = 300 K and ρ m = 0.1 g cm−3. The snowline is at ≈4  au.
Paper: Rapid Formation of Gas-giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores. II. Dependence on Pebble Bulk Density and Disk Temperature
Authors: Hiroshi Kobayashi, Hidekazu Tanaka
Figure caption: Same as Figures 1 and 2, but for T 1 = 200 K and ρ m = 0.1 g cm−3. (a) is at 6.7 × 104 yr.
Paper: Can Cuspy Dark-matter-dominated Halos Hold Cored Stellar Mass Distributions?
Authors: Jorge Sánchez Almeida, Angel R. Plastino, Ignacio Trujillo
Figure caption: Summary of the allowed (blue bullet symbols) and forbidden (red plus symbols) regions of the parameter space when both the baryon density profile and the density defining the underlying potential follow a profile described by Equation (32) and illustrated in Figure 2. The symbols c and c  p  represent the inner slope of the density profile and the density generating the potential, respectively. The ordinate axis is split into two (logarithmic scale on the top and linear scale at the bottom ) to show the whole range of values of interest. The lines x = 0 and y = 0 are shown in light gray. Left panel: r  s /r  sp  = 1/4, with the baryons more centrally concentrated that the potential. Right panel: r  s /r  sp  = 2, with the baryons more spread out than the potential. Baryons do not contribute to the overall potential and their velocity distribution is assumed to be isotropic (β = 0) at all radii. In both cases, the sampling in c  p  is Δc  p  = 0.02 whereas the sampling in c is Δc = 10−4 in the linear scale and ﹩{\rm{\Delta }}\mathrm{log}c=0.05﹩ in the logarithmic scale.
Paper: Can Cuspy Dark-matter-dominated Halos Hold Cored Stellar Mass Distributions?
Authors: Jorge Sánchez Almeida, Angel R. Plastino, Ignacio Trujillo
Figure caption: Top panels: similar to Figure 1 but with a hint of cusp in the density: c = 0.005 and c  p  = 1. The DF f < 0 but not at the largest ϵ. This combination of the baryon soft core and NFW potential is still inconsistent. However, the inconsistency goes away as soon as the inner slope of the stellar density profile increases, as shown in the bottom panels, where c = 0.1 and c  p  = 1. The global picture of compatibility–incompatibility is summarized in Figure 4. The shape of the profiles defining the baryon distribution and the potential is given by Equation (32).
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVIII. The Dark Matter Halo Mass of Quasars at z ∼ 6
Authors: Junya Arita, Nobunari Kashikawa, Yoshiki Matsuoka, Wanqiu He, Kei Ito, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Yoshihiro Takeda, Kazushi Iwasawa, Masafusa Onoue, Yoshiki Toba, Masatoshi Imanishi
Figure caption: Top: red and blue histograms show 1450 Å absolute magnitude distribution for SHELLQs quasars and other quasars respectively. Bottom: red and blue histograms show the redshift distribution for SHELLQs quasars and other quasars respectively. The black line represents N(z), the redshift distribution of SHELLQs quasars estimated by kernel density estimation, which is used in Section 3.1.
Paper: Can Cuspy Dark-matter-dominated Halos Hold Cored Stellar Mass Distributions?
Authors: Jorge Sánchez Almeida, Angel R. Plastino, Ignacio Trujillo
Figure caption: Diagnostic plot similar to that in Figure 4, except that this time we represent simulations where both c and r  s /r  sp  are varied. Note how r  s  cannot be larger than ∼2 r  sp  for f to remain positive, a constraint that may be used in real galaxies to set a lower limit to the size of the DM halo. In these simulations the abc profile shapes of density and potential are identical, explicitly, a = a  p , b = b  p , and c = c  p , the three of them varying as for Equation (32). The sampling in c is Δc = 10−4 in the linear scale and ﹩{\rm{\Delta }}\mathrm{log}c=0.1﹩ in the logarithmic scale. The relative radii are shown in a logarithmic scale with a sampling of ﹩{\rm{\Delta }}\mathrm{log}({r}_{s}/{r}_{{sp}})=0.1﹩.
Paper: Can Cuspy Dark-matter-dominated Halos Hold Cored Stellar Mass Distributions?
Authors: Jorge Sánchez Almeida, Angel R. Plastino, Ignacio Trujillo
Figure caption: Similar to Figure 4 but using a = 2.5 − c, so that Equation (38) (or Equation (E4)) can be tested. Note that c = c  p  = 0 is unphysical even though ρ and the density profile producing the potential are identical.
Paper: Can Cuspy Dark-matter-dominated Halos Hold Cored Stellar Mass Distributions?
Authors: Jorge Sánchez Almeida, Angel R. Plastino, Ignacio Trujillo
Figure caption: Similar to Figure 5 with c = c  p  = 0 and a = a  p  = 2.1. Even if the two density profiles have the same shape, f < 0 somewhere (the dashed line). This behavior for a > 2 is predicted analytically in Appendix E and discussed further in Section 4.2, item 6.
Paper: Can Cuspy Dark-matter-dominated Halos Hold Cored Stellar Mass Distributions?
Authors: Jorge Sánchez Almeida, Angel R. Plastino, Ignacio Trujillo
Figure caption: Similar to Figure 1 but this time only with a hint of cusp in the density that generates the potential: c = 0 and c  p  = 0.05. Note that f < 0 at large ϵ, implying that density and potential are inconsistent with each other.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVIII. The Dark Matter Halo Mass of Quasars at z ∼ 6
Authors: Junya Arita, Nobunari Kashikawa, Yoshiki Matsuoka, Wanqiu He, Kei Ito, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Yoshihiro Takeda, Kazushi Iwasawa, Masafusa Onoue, Yoshiki Toba, Masatoshi Imanishi
Figure caption: Comparison of M 1450, the absolute magnitudes at 1450 Å of SHELLQs quasars (red circles) and those of known quasars. We refer to the M 1450 from the quasar sample in Jiang et al. (2016; black triangle) and that of newly identified quasars in Bañados et al. (2016), Bañados et al. (2023; black open square).