adsabs/AstroCLIMB huggingface dataset:
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Evolution of a GMC of mass 106 M⊙ and metallicity of 0.002 (SM6_sZ002). The top panels depict projected distributions of the density, and the middle panels show composite images of the gas density (dark blue being denser), the fraction of ionized hydrogen (blue means fully ionized), and H I-ionizing photon flux (brighter means more luminous) in the central region (158 pc on a side) of the simulation. The intrinsic (dotted) and emergent (solid) spectra of Lyα photons are shown in the bottom panels. The emergent velocity profile of the leftmost column is magnified by a factor of 100 to improve readability. The simulation epoch is displayed in the upper-right corner of the figures in the top row. The two values in the middle-row panels indicate the logarithmic total mass of stars and the escape fraction at λ = 900 Å. In the bottom panels, we also include the escape fraction, the velocity separation of the two peaks, and the flux ratio of the blue part to the red part of the Lyα spectrum.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Star formation histories of the simulated GMCs. Different color codes and line styles correspond to runs with different initial conditions and input physics, as indicated in the legend. In most of the clouds, star formation ends within about 3 Myr, except for the homogeneous spherical clouds in which gas collapses slowly because of its lower surface density.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Escape fraction of LyC photons (fLyC) in GMCs simulated with different input physics and parameters. The solid and dashed lines indicate instantaneous and luminosity-weighted escape fractions, respectively, and the dotted–dashed lines show the intrinsic number of LyC photons (NLyC). Note that the maximum NLyC is normalized to 0.1 in each panel for better readability. The different panels compare the escape fraction from different runs, which are indicated in the legend. The escape fraction generally increases with time since the GMC gets disrupted.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Same as Figure 5, but for Lyα photons. Intrinsic Lyα luminosities are computed from recombinative and collisional processes by taking the gas density and ionized fraction from each computational cell in the simulation. The maximum luminosity is normalized to 0.1 for better readability. Note that Lyα luminosities drop more rapidly than LyC luminosities (Figure 5) because recombinative radiation (L ∝ nenH II) weakens as the GMCs get dispersed.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Luminosity-weighted escape fractions of LyC (filled squares) and Lyα photons (empty squares). The escape fractions are averaged over the simulation duration (≈8.4 Myr). Different color codes correspond to runs with various physical properties or resolutions, as indicated in the legend.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Projected density distributions of GMCs when the escaping Lyα luminosity is the maximum. The time of each snapshot (in megayears) is specified at the top-right corner. Black dots denote stars with > 8 M⊙, and the cyan bar measures 30 pc. The simulated clouds show the brightest Lyα emission before they are completely dispersed. An exception is HM6_sZ002, where gas collapsing at the center contributes significantly to the total Lyα luminosity.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Time-averaged velocity spectra of Lyα photons from simulated GMCs. The abscissa represents the angle-averaged escaping Lyα luminosity summed over each bin in units of 1049 # s−1, where # is the number of Lyα photons. The bin size is 2 km s−1. Different color codes correspond to results from simulations with different physical parameters or resolutions, as indicated in the legend.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Plot of the location of the red peak (vpeak,red) vs. the relative flux ratio between the blue part and red part of the Lyα spectrum (Lblue/Lred). Blue empty circles connected by dotted lines show an example of the time evolution of a metal-poor massive cloud (SM6_sZ002). Colored symbols indicate values obtained from the stacked Lyα spectrum in each simulation, and observational data are marked in gray color with various symbols, as indicated in the legend.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Effects of scattering due to the inner or outer cloud gas in the simulations. The upper panel shows an example of Lyα spectra from the lower-mass metal-poor cloud (SM5_pZ002), while the lower panel exhibits spectra from a massive cloud with high surface density (SM5D_Z002) during the Lyα bright phase (i.e., the same snapshot as in Figure 8). Colored solid lines indicate the spectra in the absence of scattering due to the diffuse ISM region at r > 30 or 50 pc (orange) or the dense GMC region at r < 30 or 50 pc (blue), where r is the three-dimensional radius from the Lyα luminosity center. The black lines correspond to the Lyα spectra processed by the entire gas in the simulated volume. The purple dashed line corresponds to the case in which the radial outflow velocity of the cloud is artificially augmented by a factor of 10.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Relationship between the velocity separation of the Lyα double peak (vsep) and the escape fraction at λ ≈ 900 Å (f900, left panel). Results for our simulated GMCs are shown as colored symbols, as indicated in the legend of the right panel. The gray empty circles indicate earlier results obtained from RHD simulations of GMCs (Kimm et al. 2019). The black star symbols correspond to galactic-scale measurements taken from Vanzella et al. (2015, 2018), Izotov et al. (2016a, 2016b, 2018), and Verhamme et al. (2017). The smaller star symbol with error bars indicates the results obtained from a low-mass galaxy sample by Izotov et al. (2021). The black lines show simple analytic estimates obtained by assuming T = 20,000 K for various turbulent velocities (solid, dashed, and dotted lines: σ = 0, 15, and 30 km s−1, respectively). The right panel shows the comparison between f900 and fLyα on cloud scales. The dashed line indicates a simple fit to our results, ﹩{f}_{\mathrm{Ly}\alpha }\approx {f}_{900}^{0.27}﹩, at f900 > 10−3.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Correlation between the LyC escape fraction and Lyα EW in GMCs. Different symbols show the attenuated Lyα EW in different simulations, as indicated in the legend. The intrinsic Lyα EWs are shown as solid lines, and black empty triangles and filled diamonds represent galactic measurements from Gazagnes et al. (2020) and Izotov et al. (2021), respectively. Note that the attenuated Lyα EWs are often larger than the intrinsic EWs.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Correlation between the luminosity-weighted escape fraction and the total star formation efficiency in the simulated clouds (left). Different symbols indicate the results from the runs with different simulation parameters, as indicated in the legend. Clouds with a smaller mass (105 M⊙) are shown with smaller symbols. Dotted lines correspond to the extrapolated luminosity-weighted escape fraction measured until t = 20 Myr assuming that fLyC is kept the same as the value in the final snapshot. Also included as gray star symbols are the escape fractions from Kimm et al. (2019) with the single (empty) or binary stellar evolution model (filled). Bigger star symbols indicate the results measured from 106 M⊙ clouds, while the small star symbols correspond to those from 105 M⊙ clouds. The gray filled square shows the solar-metallicity case from Kimm et al. (2019). The gray crosses display the 〈fLyC〉 measured from 105 clouds by Kim et al. (2021b). The simulated data for clouds with 105  ≤ Mcloud ≤ 3 × 105 M⊙ from He et al. (2020) are shown as filled gray diamonds. Note that there is a clear correlation between SFEtot and the luminosity-weighted escape fraction of LyC photons. The right panel indicates the correlation between the escape fraction and the destruction timescale of dense gas (τdest). We define τdest as the time between the onset of star formation and the moment at which the amount of gas with nH ≥ 100 cm−3 drops to 0.1 Mcloud.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Differences in the development of ionized bubbles in GMCs with normal (upper panel) and high gas surface density (lower panel). The solid lines indicate the amount of dense gas with nH ≥ 100 cm−3, divided by 106 M⊙. The dashed lines show the neutral fraction of hydrogen within a radius inside which the total gas mass is 106 M⊙. The circle and star symbols correspond to the moment at which the fraction of dense gas and the fraction of neutral hydrogen fall below 0.1, respectively. Note that the destruction timescales are similar for the two GMCs, but a larger portion of the gas is kept neutral for an extended period of time in the run with higher gas surface density (compare the dashed lines at 2–3 Myr).
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: The intrinsic luminosities and escape fractions of photons with various wavelengths from the metal-poor (SM6_sZ002; left) and metal-rich cloud (SM6_sZ014; right). From top to bottom, each row indicates the intrinsic luminosity in units of erg s−1, UV magnitude at 1500 Å, Lyα equivalent width in Å, escape fraction, and escaping luminosity, normalized to 1041 erg s−1. Photons with different wavelengths are shown as different colors.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: The correlation between the escape fraction of various wavelengths. The colored symbols show simulated escape fractions measured at different times from GMCs with different conditions, as indicated in the legend. The dotted line shows one-to-one correspondence. The solid and dashed lines in the bottom panels exhibit the correlation predicted from the uniform media with Small Magellanic Cloud–type or Milky Way–type dust. Note that the simulated GMCs display a steeper correlation than the uniform case, indicating that the UV photons are absorbed by clumpy gas distributions.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Escape fraction of LyC radiation deduced from the number of Lyα photons produced per second (﹩{f}_{\mathrm{LyC}}^{{\prime} }\equiv 1-{N}_{\mathrm{Ly}\alpha }^{\mathrm{int}}/0.68/{N}_{\mathrm{LyC}}^{\mathrm{int}}﹩). The runs with different input parameters are shown as different symbols and color codings, as indicated in the legend. For comparison, we display the one-to-one relation as a dashed line. The inferred escape fractions (﹩{f}_{\mathrm{LyC}}^{{\prime} }﹩) reasonably match the true fLyC in the range ﹩{f}_{\mathrm{LyC}}^{{\prime} }\gtrsim 0.1﹩, albeit with significant scatter (ΔfLyC ∼ 0.2). Note that ﹩{f}_{\mathrm{LyC}}^{{\prime} }﹩ tends to be greater than fLyC at ﹩{f}_{\mathrm{LyC}}^{{\prime} }\gtrsim 0.4﹩ (see the text).
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Impact of the choice of ﹩{f}_{\mathrm{dust}}^{\mathrm{ion}}﹩, the fraction of dust that survives in ionized media, on the luminosity-weighted Lyα profiles in a metal-poor (SM6_sZ002, top) and metal-rich GMCs (SM6_sZ002, bottom). The line profiles are normalized by the bin size of the velocity. Increasing ﹩{f}_{\mathrm{dust}}^{\mathrm{ion}}﹩ suppresses the line fluxes, but the velocity separations of the double peaks are barely changed.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Effect of resolutions on the escape of LyC and Lyα radiation. The results from the runs with varying resolutions are shown as different color codings. The solid and dashed lines show instantaneous and cumulative escape fractions, respectively, while the dotted–dashed lines correspond to the number of LyC photons or intrinsic Lyα luminosity, as indicated in the legend.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Two-color diagrams to select dropout sources. The left, middle, and right panels show two-color diagrams to select g-dropout (z ∼ 4), r-dropout (z ∼ 5), and i-dropout (z ∼ 6) sources, respectively. The red lines indicate color criteria we use to select dropout sources (Equations (1)–(9)), and the red circles are spectroscopically identified sources in the UltraDeep layers (for the left panel) and in all layers (for the middle and right panels). The solid black lines are colors of star-forming galaxies expected from the Bruzual & Charlot (2003) model as a function of redshift. As model parameters, we adopt the Salpeter (1955) IMF, an age of 70 Myr after the initial star formation, metallicity of Z/Z⊙ = 0.2, and the Calzetti et al. (2000) dust extinction law with reddening of E(B − V) = 0.16 (see Section 3.2). The circles on the line show their redshifts with an interval of Δz = 0.1. The blue circles are z = 0–3 sources spectroscopically identified in the UD-COSMOS region. The dotted, dashed, and dotted–dashed lines are, respectively, typical spectra of elliptical, Sbc, and irregular galaxies (Coleman et al. 1980) redshifted from z = 0 to z = 2 (for the left panel) and to z = 3 (for the middle and right panels). The black stars indicate Galactic stars taken from Gunn & Stryker (1983) and L /T dwarfs from Knapp et al. (2004).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Examples of sky distributions of dropout sources. The red squares, orange circles, and black dots are, respectively, the positions of sources whose magnitudes are i < 22.0, 22.0–22.5, and 22.5–25.0 (24.0) mag for z ∼ 4 sources, z < 22.5, 22.5–23.0, and 23.0–25.5 (24.5) mag for z ∼ 5 sources, and y < 23.0, 23.0–23.5, and 23.5–25.5 (25.0) mag for z ∼ 6 and 7 sources, in the UltraDeep (Deep and Wide) layers. The scale on the map is marked in degrees and in the projected distance (comoving Gpc).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Spectra of HSC J160953+532821 at z = 6.923, HSC J161207+555919 at z = 6.788, HSC J020834−021239 at z = 4.088, and HSC J022552−054439 at z = 3.647 from top to bottom, obtained in our spectroscopic follow-up observations. In each figure, the top panel shows the two-dimensional spectrum (black is positive), and the bottom panel shows the one-dimensional spectrum. In the top panel, our dropout galaxy is located at the center in the spatial direction, and the spatial range is ±3″. In the bottom panel, the black line indicates the spectrum of the object, and the blue line shows the sky spectrum with an arbitrary normalization. For the sources with weak Lyα emission, we also plot the averaged spectra over 200 Å bins with red filled circles to show the Lyman break features.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Selection completeness estimates for our z ∼ 4, 5, 6, and 7 samples. The black curves correspond to the results of the Monte Carlo calculations, in Section 3.3, averaged over the Wide, Deep, and UltraDeep layers. Average redshifts of these samples are 3.8, 4.9, 5.9, and 6.9. The histograms show redshift distributions of spectroscopically identified sources in the z ∼ 4 (blue), z ∼ 5 (green), z ∼ 6 (orange), and z ∼ 7 (red) samples.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Each bottom panel shows rest-frame UV luminosity functions of dropout sources (including galaxies and AGNs) at z ∼ 4 and 5. The red circles show our results based on the HSC-SSP survey data. For comparison, we also show previous results for galaxies+AGNs in Ono et al. (2018; cyan circles), Stevans et al. (2018; orange squares), and Adams et al. (2020; orange diamonds), galaxies in Bouwens et al. (2021; magenta squares), Finkelstein et al. (2015b; green circles), van der Burg et al. (2010; blue triangles), and Pelló et al. (2018; orange diamonds), and AGNs in Akiyama et al. (2018; black squares), Parsa et al. (2018; black triangles), Giallongo et al. (2015; black crosses), Glikman et al. (2011; black pluses), Niida et al. (2020; black diamonds), and Kim et al. (2020; black stars). Each top panel shows a fraction of galaxies in our dropout sample based on spectroscopic results. For the denominator of the fraction, the sum of the numbers of galaxies and AGNs is used. Note that this fraction is estimated based on various spectroscopic catalogs, and its uncertainty is discussed in Section 4.2.1.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Same as Figure 5 but at z ∼ 6 and 7. For comparison, we also show previous results for galaxies+AGNs in Ono et al. (2018; cyan circles), galaxies in Bouwens et al. (2021; magenta squares), Pelló et al. (2018; orange diamonds), Ishigaki et al. (2018; orange diamonds), Bowler et al. (2017, 2015; blue triangles), Finkelstein et al. (2015b; green circles), Schenker et al. (2013; brown triangles), and McLure et al. (2013; purple circles), and AGNs in Matsuoka et al. (2018c; black squares), Parsa et al. (2018; black triangles), Onoue et al. (2017; black stars), Jiang et al. (2016; black circles), Giallongo et al. (2015; black crosses), Kashikawa et al. (2015; black triangles), and Willott et al. (2010b; black pluses). In the z ∼ 7 panel, the z ∼ 6 AGN luminosity functions are plotted because there are no results of the AGN luminosity function at z ∼ 7.