adsabs/AstroCLIMB huggingface dataset:
Paper: The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method
Authors: Wei Zhu, 伟 祝
Figure caption: Surface gravity (﹩\mathrm{log}g﹩) vs. effective temperature (T eff) for stars in the CLS sample. Here, black dots are all CLS stars, red dots are the Sun-like stars according to the selection criteria of Section 3.1, and the blue circles mark the CLS stars with planet detections.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Broadening profiles for the spectra with the most distinguishable contributions from the two stars, with orbital phase given in the upper right corner. The lines show the fits to the primary star profile (green), the secondary star profile (red), the normalized fit (blue), and the summation (orange). The first four panels are from NOT FIES spectra, and the last seven panels are from KPNO spectra.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: MIST isochrones (Choi et al. 2016) for ages 600 (red), 650 (cyan), 700 (yellow), and 750 (orange) Myr. MIST evolutionary tracks are also shown (black) for masses of the primary and secondary star (M  p  = 2.420 M ⊙, M  s  = 2.226 M ⊙). Crosses indicate binary systems. To graph the evolution tracks and isochrones, a distance modulus (m − M)0 = 6.33, initial rotation v/v crit = 0, iron abundance [Fe/H] = +0.16, and reddening E(G BP − G RP) = 0.073 were used.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: PARSEC isochrones (Bressan et al. 2012) for ages 600 (red), 650 (cyan), 700 (yellow), and 750 (orange) Myr. In the graph, distance modulus (m − M)0 = 6.33, iron abundance [Fe/H] = +0.16, and reddening E(G BP − G RP) = 0.073 were used. Crosses indicate binary systems. The colored crosses indicate where our calculated masses in Table 3 land on the isochrone.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: BaSTI-IAC isochrones (Hidalgo et al. 2018) for ages 600 (red), 650 (cyan), 700 (yellow), and 750 (orange) Myr. BaSTI-IAC evolutionary tracks are also shown (black) for masses of the primary and secondary stars (M  p  = 2.420 M ⊙, M  s  = 2.226 M ⊙). Crosses indicate binary systems. In the graph, distance modulus (m − M)0 = 6.33, iron abundance [Fe/H] = +0.16, and reddening E(G BP − G RP) = 0.073 were used. Overshooting and diffusion were also allowed under available grids.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: MIST isochrones (Choi et al. 2016) for ages 630 (green), 635 (light green), 640 (yellow), and 645 (orange) Myr. Distance modulus (m − M)0 = 6.33, iron abundance [Fe/H] = +0.14, and reddening E(G BP − G RP) = 0.073 were used. Colored circles show the model positions of stars with the measured masses of the components of ϵ Cnc, and blue rectangles show the G magnitude and uncertainty of the components as inferred from spectroscopy.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Hyades members in a color–absolute magnitude diagram using Gaia EDR3 photometry and parallaxes. Color-coding for individual stars is based on measured rotational velocity ﹩{v}_{\mathrm{rot}}\sin i﹩, and crosses indicate binary systems. The blue point is the blue straggler δ 3 Tau. MIST isochrones (Choi et al. 2016) for [Fe/H] = +0.14 and zero reddening are shown, with ages 635 (blue), 740 (green), and 850 (red) Myr shown.
Paper: Cupid is not Doomed Yet: On the Stability of the Inner Moons of Uranus
Authors: Matija Ćuk, Robert S. French, Mark R. Showalter, Matthew S. Tiscareno, Maryame El Moutamid
Figure caption: A 50 Myr “nominal” simulation of the Belinda group moons using SWIFT-rmvs4 integrator and orbital elements found by French et al. (2017). Belinda was assumed to have a mass of 1.6 × 1017 kg, and Belinda/Cupid and Belinda/Perdita mass ratios were set to 125 and 27, respectively. The moons are stable over the whole course of the simulation.
Paper: Cupid is not Doomed Yet: On the Stability of the Inner Moons of Uranus
Authors: Matija Ćuk, Robert S. French, Mark R. Showalter, Matthew S. Tiscareno, Maryame El Moutamid
Figure caption: Relative amount of orbital evolution ∣Δa/a∣ over 1 Gyr for the regular moons of Uranus, assuming Love number k 2 = 0.1 and tidal quality factor Q = 15,000 for Uranus. Known masses have been used for the five large satellites (Ćuk et al. 2020), while we used radii from Table 1 and density of 850 kg m−3 for the inner moons. Labeled moons are Juliet (J), Portia (Po), Belinda (B), Puck (Pu), Miranda (M), and Ariel (A). The dashed line plots the distance to the synchronous orbit from the planet’s center; the moons interior to it migrate inward, while the moons exterior to this line migrate outward.
Paper: Cupid is not Doomed Yet: On the Stability of the Inner Moons of Uranus
Authors: Matija Ćuk, Robert S. French, Mark R. Showalter, Matthew S. Tiscareno, Maryame El Moutamid
Figure caption: The resonant argument 44λ  P  − 43λ  B  − ϖ  P  of the Belinda–Perdita 44:43 MMR in the same simulation shown in Figure 1 (variables have the same meaning as in Table 1). The librating argument establishes that the two moons are in the resonance for the whole duration of the simulation.
Paper: Cupid is not Doomed Yet: On the Stability of the Inner Moons of Uranus
Authors: Matija Ćuk, Robert S. French, Mark R. Showalter, Matthew S. Tiscareno, Maryame El Moutamid
Figure caption: Simulation identical to the one shown in Figure 1, except that the masses of all three moons have been increased by a factor of 2. The simulation results in an instability in less than 3 Myr.
Paper: Evaluating the V-band Photometric Metallicity with Fundamental Mode RR Lyrae in the Kepler Field
Authors: Chow-Choong Ngeow
Figure caption: Comparisons of the photometric [Fe/H], either in the V band (left panels) or VT band (right panels), derived from Equation (7) to the [Fe/H]spec. Errors on photometric [Fe/H] include the rms error and propagated errors on ϕ 31 from Equation (7), and we assume errors on P are negligible. The top, middle, and bottom panels are the comparisons for three different cases as discussed in the text (see Section 5). The solid lines represent the 1:1 relation and they are not the fits to the data. The dashed lines show the expected ±0.41 dex rms on the photometric [Fe/H].
Paper: Evaluating the V-band Photometric Metallicity with Fundamental Mode RR Lyrae in the Kepler Field
Authors: Chow-Choong Ngeow
Figure caption: Example light curves for Blazhko RR Lyrae before and after removing the Blazhko modulation. The error bars include errors from the instrumental magnitudes and the calibration processes. Panel (a) shows an example with no clear sign of Blazhko modulation seen in the light curves. Panel (b) and (c) are examples where improvements and no improvements were seen on the light curves after removing the Blazhko modulation, respectively.
Paper: Evaluating the V-band Photometric Metallicity with Fundamental Mode RR Lyrae in the Kepler Field
Authors: Chow-Choong Ngeow
Figure caption: Comparison of the derived V-band ϕ  s  31 Fourier parameters before and after removing the Blazhko modulations from the light curves. The filled color symbols correspond to the three cases as presented in Figure 2. The dashed line represents the 1: 1 relation.
Paper: Evaluating the V-band Photometric Metallicity with Fundamental Mode RR Lyrae in the Kepler Field
Authors: Chow-Choong Ngeow
Figure caption: Calibrated grV-band light curves and the transformed VT-band light curve for a non-Blazhko RR Lyrae. The error bars include errors from the instrumental magnitudes and the calibration processes.
Paper: An ALMA Search for High-albedo Objects Among the Midsized Jupiter Trojan Population
Authors: Anna M. Simpson, Michael E. Brown, Madeline J. Schemel, Bryan J. Butler
Figure caption: Derived albedos and diameters based on WISE observations (Grav et al. 2012). The black points show all Trojans for which the WISE-derived albedo uncertainties are 0.02 or lower. The median and 1σ variation of albedo of these Trojans are shown as red horizontal lines. The nine objects shown in red all have WISE-derived albedos and uncertainties that appear to be 3σ or more above the median Trojan albedo. Also shown, in cyan, are three objects measured by WISE to have typical albedos; these targets are used as emissivity calibrators for the survey.
Paper: An ALMA Search for High-albedo Objects Among the Midsized Jupiter Trojan Population
Authors: Anna M. Simpson, Michael E. Brown, Madeline J. Schemel, Bryan J. Butler
Figure caption: Comparison of albedos obtained using ALMA data to the rescaled albedos of Grav et al. (2012). The gray line is of slope 1, so that if the same result was found for an object in both analyses, it would fall on that line. The three objects used for emissivity calibration are shown in red.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. I. New Discoveries
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, Kaspar von Braun, David R. Ciardi, Jennifer G. Winters, Rocio Kiman
Figure caption: The mass ratio (left) and projected separation (right) distributions for the 26 previously undetected companions discovered throughout the POKEMON survey. These values were estimated using our observed properties, as well as the parallaxes and 2MASS K magnitudes for these objects. The mass ratios follow a relatively flat distribution, while the projected separations follow a roughly Gaussian distribution, as expected. The peak of our projected separation distribution is at 7.8 au, with a standard deviation of ﹩{\sigma }_{\mathrm{log}a}=0.4﹩.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. I. New Discoveries
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, Kaspar von Braun, David R. Ciardi, Jennifer G. Winters, Rocio Kiman
Figure caption: Using the wdwarfdate code, we estimate an age for the white dwarf Wolf 672 A, and thus its companions, the M dwarf Wolf 672 B and the new discovery we detected. The panels (from left to right) show the main-sequence age (the age of the progenitor), the cooling age, the total age, the initial mass (the mass of the progenitor), and the final mass of the white dwarf. We find a cooling age of ﹩{0.30}_{-0.01}^{+0.01}﹩ Gyr, and a final mass of ﹩{0.55}_{-0.01}^{+0.01}\,{M}_{\odot }﹩, which are in complete agreement with the Montreal White Dwarf Database values for Wolf 672 A of 0.29 Gyr and 0.55 M ⊙.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. I. New Discoveries
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, Kaspar von Braun, David R. Ciardi, Jennifer G. Winters, Rocio Kiman
Figure caption: Angular separation (left) and I-band or “red” delta magnitude (right) distributions for the 26 new discoveries revealed by the POKEMON survey. These values were obtained from our DSSI and NESSI speckle observations, and have not been corrected for anisoplanatism.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. I. New Discoveries
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, Kaspar von Braun, David R. Ciardi, Jennifer G. Winters, Rocio Kiman
Figure caption: The newly detected companion to 2MASS J11030845+1517518, shown in the reconstructed image on the left and in the detection plot on the right. These data were taken on UT 2017 April 17. The companion is at a separation of 0.″39 (6.8 au), and its delta magnitude is measured to be 1.5.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. I. New Discoveries
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, Kaspar von Braun, David R. Ciardi, Jennifer G. Winters, Rocio Kiman
Figure caption: Scatter plot of delta magnitude versus angular separation for the 26 new discoveries. Most new discoveries are measured to be within ∼ 0.7″ of their primaries, though they span a range of delta magnitudes.
Paper: The POKEMON Speckle Survey of Nearby M Dwarfs. I. New Discoveries
Authors: Catherine A. Clark, Gerard T. van Belle, Elliott P. Horch, Kaspar von Braun, David R. Ciardi, Jennifer G. Winters, Rocio Kiman
Figure caption: The sky locations of the 1070 stars in the POKEMON sample. 290 of these are known multiples. Single stars are marked with open black circles, known multiples are marked with filled black circles, and the 26 systems with new discoveries are marked with larger, red stars.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Sky orbit for ϵ Cnc B relative to ϵ Cnc A (marked with a cross). Black points mark the model orbital position during the measurements with the CLIMB beam combiner at CHARA. Blue points are position measurements from the MIRC-X beam combiner. Red points are position measurements from the CLIMB beam combiner (triangles are values closest to the predicted position, and not the global best binary fit). Red ellipses show 5σ uncertainties. Secondary star motion is counterclockwise in this diagram. The inset panels are zoom-ins on observations taken near the extremes of the orbit. In the insets, blue dashed lines connect the measured position to the model’s predicted position.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Top: SED for the binary ϵ Cnc from photometry (red points) and for the best-fit main-sequence stars (HD 73819 with blue points and HD 73711 with green points increased in flux by a factor of 1.1). Horizontal error bars represent the effective width of the filter. Bottom: fractional difference between the binary star photometry fluxes and the best-fit sum of main-sequence stars.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Gaia EDR3 CMD for bright Praesepe members. ϵ Cnc is shown with a large red pentagon, the best-fit main-sequence stars (HD 73819 and HD 73711) are outlined in green, the blue straggler candidate HD 73666 is a large blue point, likely single faint main-sequence stars are small blue points, faint binary candidates are small black points, and stars without measured rotational velocities are large black points. Otherwise the bright stars are color-coded by rotational velocity. Crosses indicate binary systems. The green horizontal lines are inferred brightnesses for ϵ Cnc A and B.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Top: SED for HD 73819 from photometry (red points), compared to an ATLAS9 model with T eff = 8060 K and ﹩\mathrm{log}g=3.6﹩ and synthetic photometry calculated from the model (green points). Horizontal error bars represent the effective width of the filter. Bottom: fractional difference between the observed photometry fluxes and best-fit synthetic photometry.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Closure phases (Φ) as a function of the interferometric baseline for CLIMB and MIRC-X data, separated by date of observation. Here the baseline is the sum of the baseline lengths for the first two legs of the triangle of telescopes. Black circles are the predicted values, and colored circles are observed values on different dates (CLIMB) or from different telescope pairs (MIRC-X).
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Top: SED for HD 73711 from photometry (red points), compared to an ATLAS9 model with T eff = 8330 K and ﹩\mathrm{log}g=4.0﹩ and synthetic photometry calculated from the model (green points). Horizontal error bars represent the effective width of the filter. Bottom: fractional difference between the observed photometry fluxes and best-fit synthetic photometry.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Squared visibilities as a function of interferometric baseline for the MIRC-X data, separated by date of observation. Black circles are the predicted values, and the colored circles are the observed values. Different colors in the panels represent measurements from different telescope pairs.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Squared visibilities as a function of interferometric baseline for the CLIMB data, separated by date of observation. Black circles are the predicted values, and the colored circles are the observed values. Different colors in the panels represent measurements from different telescope pairs.
Paper: The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age
Authors: Leslie M. Morales, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, Robert Klement, Luigi R. Bedin, Mattia Libralato, Luca Malavolta, Domenico Nardiello, Jerome A. Orosz, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo ten Brummelaar, Claire L. Davies, Jacob Ennis, Tyler Gardner, Cyprien Lanthermann
Figure caption: Radial velocity vs. orbital phase for the components of ϵ Cnc. Star symbols represent the primary star, and circles represent the secondary star.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: EW and α  P  distributions of the candidates without J-band detection. The gray circles are the color-selected candidates, while the orange circles are the ones satisfying the AICc criterion (w  q  > 0.99). Several candidates matched to the same quasar model were overlaid, so they appear to have low transparency on the diagram. The candidates covered by the HSC survey are marked by teal crosses. The five quasars in this work are shown as red circles. The blue diamond (and blue lines on the histograms) represents the reported normal distribution of z ∼ 6 quasars: ﹩\mathrm{logEW}=1.542\pm 0.391﹩ (Bañados et al. 2016) and α  P  = −1.6 ± 1.0 (Mazzucchelli et al. 2017), in the form of mean ± standard deviation. Note that the correlation between the reported EW and α  P  is not reflected in this figure.