adsabs/AstroCLIMB huggingface dataset:
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Effective temperature of the sphere model with L = LEdd(106 M⊙). The horizontal axis is the reference density, ρref, a proxy for the Eddington ratio (Equation (11)) and the photosphere density (ρref ∼ ρph if Teff ∼ 5000 K). Curves show analytical estimates using the effective opacity at 5000 Å (solid) or the Rosseland mean opacity (dotted). These estimates depend on the dimensionless photosphere scale height, Hph/Rph, as a free parameter. Plus signs mark measurements of the gas temperature at Teff (5000 Å) = 1/2 from the gray simulations, where the photosphere scale height is determined self-consistently by radiation energy transport. The analytical effective temperature is very insensitive to the reference density for a given luminosity and Hph/Rph, although numerical measurements suggest a somewhat steeper Teff–ρref relation.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: The ratio of two continuum effective opacities (accounting for absorption and scattering), κeff(4000 Å)/κeff(3600 Å), for different temperature and density. A ratio significantly below 1 tends to produce a Balmer break. Star symbols mark the parameters corresponding to the star Vega and the Sun. The optimal temperature to produce a Balmer break increases with density.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Cartoon showing the two scenarios considered in this work. Straight or curved arrows indicate the direction of gas flow. Dashed lines represent the photosphere. Wiggle arrows indicate photons. Left: a standard thin disk in super-Eddington accretion, which we investigate in Section 4. It reproduces the red optical color and Balmer break of LRDs if the disk has an inner truncation radius where the effective temperature is ∼5000 K, which is fine-tuned. Right: a spherical gas profile undergoing turbulent accretion, which we investigate in Section 5. This model gives rise to a red optical continuum and the Balmer break over a large range of gas densities (a proxy for a wide range of accretion rates). Components with question marks, i.e., truncation in the disk scenario and outflow and clumps in the sphere scenario, are discussed in Section 6.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Workflow in this paper. Methods are outlined in yellow blocks, and results are outlined in blue blocks. “Sec.,” “app.,” and “cond.” stand for “section,” “appendix,” and “condition.”
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Critical halo mass Mcrit of Pop III-forming halos as a function of redshift employed in our semianalytic model (Equation (4)). Solid, dashed, and dotted–dashed curves indicate examples for various combinations of (JLW, vbc). Upper thick-dotted and lower thin-dotted curves represent the critical mass of atomic cooling halos (Equation (3)) and the critical mass of the HD cooling (Equation (7)), respectively.
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Number density of Pop III stars as a function of the Lyman–Werner flux radiated on their halos at z = 23.9 (left) and z = 13.0 (right) for the vbc = 0 model. Histograms show JLW from Pop III and Pop II sources in the fiducial (self-consistent) model. We divide a single-digit JLW range into four logarithmic bins and calculate the number density in each bin. Vertical dashed lines show results from the spatially uniform JLW model.
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Left: number density of Pop III stars formed at all redshifts as a function of the Pop III mass in a halo. We divide a single-digit mass range into four logarithmic bins and calculate the number density in each bin. Four model results with the different values of streaming velocity, vbc = 0, 1σvbc, 2σvbc, and 3σvbc, are shown. Right: cumulative probability distribution of the number of Pop III stars as a function of the Pop III mass in a halo.
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Left: star formation rate density of Pop III (solid curves) and Pop II (dashed) stars. Four model results with the different values of streaming velocity, vbc = 0, 1σvbc, 2σvbc, and 3σvbc, are shown. Filled and open symbols show other semianalytic results for Pop III and Pop II, respectively (S. Hegde & S. R. Furlanetto 2023; C. R. Feathers et al. 2024; A. Trinca et al. 2024). Right: formation rate density of Pop III-forming halos per Mpc3 and year.
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Comparison of different implementations of the LW feedback on the Phi-4096 simulation for the vbc = 1σvbc case. Blue and green curves show results of the fiducial (self-consistent) model and spatially uniform JLW model, respectively. Top: number density of Pop III stars formed at all redshifts as a function of the Pop III mass in a halo (same as Figure 3). Middle: star formation rate density (same as Figure 5). Bottom: formation rate density of Pop III-forming halos (same as Figure 5).
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Average number of supermassive stars per halo (﹩{\overline{N}}_{{\rm{SMS}}}﹩) as a function of halo virial mass at z = 7.5. Blue and green curves show the results for MIII > 104 and 105 M⊙, respectively. Thin and thick curves show the results for 0σvbc and the combination of four models, respectively (details are provided in the text and tha caption to Table 2).
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Comparison of model results calculated on simulations with different box sizes (16h−1, 8h−1, and 3h−1 Mpc for Phi-4096, M8, and M3, respectively). Left and right panels show results of the model with vbc = 0 and 1σvbc, respectively. Top: number density of Pop III stars formed at all redshifts as a function of the Pop III mass in a halo (same as Figure 3). Middle: star formation rate density (same as Figure 5). Bottom: formation rate density of Pop III-forming halos (same as Figure 5).
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Comparison of critical halo mass Mcrit of Pop III-forming halos as a function of redshift employed in our semianalytic model (Equation (4); solid green curve) and one originally proposed by M. Kulkarni et al. (2021; three blue curves). Blue solid, dashed, and dotted–dashed curves indicate the results for JLW = 0, 10, and 100, respectively. Upper thick curves represent the critical mass of atomic cooling halos (Equation (3)). Left and right panels show the results with streaming velocities of 1σvbc and 3σvbc, respectively.
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Dependence of Pop III mass on virial mass (left), redshift (middle), and Lyman–Werner flux (right) of host halos. From top to bottom, model results with vbc = 0, 1σvbc, 2σvbc, and 3σvbc are presented. Color bars show the number of Pop III stars at each pixel.
Paper: Emission-line Diagnostics at z > 4: [O III]λ4364/Hγ versus [Ne III]λ3870/[O II]λ3730
Authors: Bren E. Backhaus, Nikko J. Cleri, Jonathan R. Trump, Allison Kirkpatrick, Raymond C. Simons, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Madisyn Brooks, Antonello Calabrò, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Mario Llerena, Fabio Pacucci, Nor Pirzkal, Casey Papovich, Stephen M. Wilkins
Figure caption: Top: stacked spectra for 15 BLAGN galaxies above z > 4. The broad Hα feature can be seen in the bottom spectra. We also note that even when stacked, a broad Hβ component does not appear. Bottom: stacked Spectra of 269 galaxies above z > 4 without any broad-line features. These stacks are missing
Paper: Magnetic Activities of GJ 1151: Flares in TESS Data and Radio Observation in uGMRT
Authors: Diya Ram, Soumen Mondal, Anandmayee Tej, Tapas Baug, Ramkrishna Das, Dusmanta Patra, Samrat Ghosh, Rajib Kumbhakar
Figure caption: TESS PDCSAP light curve (pink) and detrended light curve (blue) of GJ 1151 in Sector 22 (upper left), Sector 48 (upper right), and Sector 75 (bottom). The detrending procedure is described in Section 3.1.
Paper: Magnetic Activities of GJ 1151: Flares in TESS Data and Radio Observation in uGMRT
Authors: Diya Ram, Soumen Mondal, Anandmayee Tej, Tapas Baug, Ramkrishna Das, Dusmanta Patra, Samrat Ghosh, Rajib Kumbhakar
Figure caption: The phased light curve of GJ 1151 from combined sectors of the TESS observations (blue dots); the red dots indicate the binned light curve, and the dashed-dotted line indicates estimated maximal amplitude 1.00023 of GJ 1151.
Paper: Magnetic Activities of GJ 1151: Flares in TESS Data and Radio Observation in uGMRT
Authors: Diya Ram, Soumen Mondal, Anandmayee Tej, Tapas Baug, Ramkrishna Das, Dusmanta Patra, Samrat Ghosh, Rajib Kumbhakar
Figure caption: Flare events of GJ 1151 in TESS light curve.
Paper: Magnetic Activities of GJ 1151: Flares in TESS Data and Radio Observation in uGMRT
Authors: Diya Ram, Soumen Mondal, Anandmayee Tej, Tapas Baug, Ramkrishna Das, Dusmanta Patra, Samrat Ghosh, Rajib Kumbhakar
Figure caption: Radio image of GJ 1151 on 2022 December 12 at an observing frequency of 1.36 GHz from the legacy uGMRT. The position of the object is marked with the plus sign. The source is not detected at band 5. The rms of the image is 35 μJy beam−1. The contour of the image is drawn with a 3σ limit, where σ is the local rms noise.
Paper: Emission-line Diagnostics at z > 4: [O III]λ4364/Hγ versus [Ne III]λ3870/[O II]λ3730
Authors: Bren E. Backhaus, Nikko J. Cleri, Jonathan R. Trump, Allison Kirkpatrick, Raymond C. Simons, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Madisyn Brooks, Antonello Calabrò, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Mario Llerena, Fabio Pacucci, Nor Pirzkal, Casey Papovich, Stephen M. Wilkins
Figure caption: Distribution of Hβ SFR and redshift for samples from JADES, CEERS, and GLASS NIRSpec observations. The galaxies hosting a BLAGN are denoted by a star. The average uncertainty is shown in the top left corner.
Paper: Emission-line Diagnostics at z > 4: [O III]λ4364/Hγ versus [Ne III]λ3870/[O II]λ3730
Authors: Bren E. Backhaus, Nikko J. Cleri, Jonathan R. Trump, Allison Kirkpatrick, Raymond C. Simons, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Madisyn Brooks, Antonello Calabrò, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Mario Llerena, Fabio Pacucci, Nor Pirzkal, Casey Papovich, Stephen M. Wilkins
Figure caption: [O III]λ4364/Hγ  versus [Ne III]/[O II] diagram of z ∼ 0 galaxies with a SNR > 5 for one emission line in each ratio. A galaxy is marked as an AGN (blue point) if it resides in the AGN region of the VO87 diagram. Additionally, if the galaxies have a broad Hα feature, it is marked as a star. The AGN faction in each region is noted under its label. We define the SF region such that it has a low 5% AGN contamination, which is shown as the black dashed line. We then improve our AGN region by defining the solid black dashed line so that the region to the left has an AGN fraction of 0.31. This leads to our final AGN region having an AGN fraction of 0.82. Galaxies noted as AGN in the VO87 diagram have higher [O III]λ4364/Hγ  and [Ne III]/[O II].
Paper: Emission-line Diagnostics at z > 4: [O III]λ4364/Hγ versus [Ne III]λ3870/[O II]λ3730
Authors: Bren E. Backhaus, Nikko J. Cleri, Jonathan R. Trump, Allison Kirkpatrick, Raymond C. Simons, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Madisyn Brooks, Antonello Calabrò, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Mario Llerena, Fabio Pacucci, Nor Pirzkal, Casey Papovich, Stephen M. Wilkins
Figure caption: [O III]λ4364/Hγ  versus [Ne III]/[O II] for z > 4 galaxies. BLAGN are colored gold, whereas other galaxies are gray. The average error bar for BLAGN and other galaxies is shown in the top right corner. The histogram on either axis shows the distribution between these two samples. We redshift correct the SF/AGN lines defined in Figure 4 using the evolution of the emission lines shown in Figure 3. High-redshift BLAGN appear to prefer higher [Ne III]/[O II]. The AGN region defined by Equations (2) and 3 for z ∼ 0 galaxies contains most of the z > 4 BLAGN.
Paper: Emission-line Diagnostics at z > 4: [O III]λ4364/Hγ versus [Ne III]λ3870/[O II]λ3730
Authors: Bren E. Backhaus, Nikko J. Cleri, Jonathan R. Trump, Allison Kirkpatrick, Raymond C. Simons, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Madisyn Brooks, Antonello Calabrò, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Mario Llerena, Fabio Pacucci, Nor Pirzkal, Casey Papovich, Stephen M. Wilkins
Figure caption: [O III]λ4364/Hγ  versus [Ne III]/[O II] with AGN and SF photoionization models from Cleri 2025, in preparation. The inset vectors in the lower right corner indicate the direction of increasing metallicity for the SF models in the left panel and AGN models in the right panel. Left: z ∼ 0 SDSS galaxies with SNR > 3 in all emission lines, where gray contours represent SF galaxies and red contours represent AGN. The SF galaxies are best represented by SF models with low to moderate ionization and low to moderate metallicity. Meanwhile, the AGN are best represented by AGN models with moderate ionization and 0.2 < Z/Z⊙ < 0.5. Right: z > 4 galaxies are best represented by AGN models. The BLAGN are best represented by AGN models with high ionization and moderate to high metallicity, while galaxies without a broad-line feature are best represented by AGN models with low to moderate ionization and moderate to high metallicity.
Paper: Emission-line Diagnostics at z > 4: [O III]λ4364/Hγ versus [Ne III]λ3870/[O II]λ3730
Authors: Bren E. Backhaus, Nikko J. Cleri, Jonathan R. Trump, Allison Kirkpatrick, Raymond C. Simons, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Madisyn Brooks, Antonello Calabrò, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Mario Llerena, Fabio Pacucci, Nor Pirzkal, Casey Papovich, Stephen M. Wilkins
Figure caption: Left: evolution of the [O III]λ4364/Hγ emission line over redshift. Right: evolution of the [Ne III]/[O II] emission line over redshift. The arrows in these figures represent upper and lower limits in the emission-line ratio. The red line represents the best fit applied to the non-BLAGN galaxies (shown as gray points and arrows). The black point is the median ratio of the SDSS sample requiring SNR > 5 in Hγ and [O II]. The average error bar for the emission-line ratios is shown in the top left corner.
Paper: Emission-line Diagnostics at z > 4: [O III]λ4364/Hγ versus [Ne III]λ3870/[O II]λ3730
Authors: Bren E. Backhaus, Nikko J. Cleri, Jonathan R. Trump, Allison Kirkpatrick, Raymond C. Simons, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Madisyn Brooks, Antonello Calabrò, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Mario Llerena, Fabio Pacucci, Nor Pirzkal, Casey Papovich, Stephen M. Wilkins
Figure caption: Stacked spectra of galaxies that do not have a broad emission-line feature based on the region of the [O III]λ4364/Hγ  versus [Ne III]/[O II] diagram they occupy. Top: 14 stacked galaxies in the BLAGN region of the [O III]λ4364/Hγ  versus [Ne III]/[O II] diagram. Middle: 7 stacked galaxies in the composite region of the [O III]λ4364/Hγ  versus [Ne III]/[O II] diagram. Bottom: 18 stacked galaxies in the SF region of the [O III]λ4364/Hγ  versus [Ne III]/[O II] diagram. The emission-line flux for these stacked spectra is shown in Table 2.
Paper: Luminous Late-time Radio Emission from Supernovae Interacting with Circumbinary Material
Authors: Samantha C. Wu, Daichi Tsuna
Figure caption: Light curves of radio emission at 3 GHz for the models listed in the legend of the second panel from the top. Each is calculated using the values of fΩ, ϵB, and ϵE listed in the upper right of each panel. The solid lines represent the light curves for models assuming a kinetic energy of Eej = 1051 erg. The shaded regions represent the range of emitted flux between Eej = 5 × 1050 erg and Eej = 1.5 × 1051 erg, with lower luminosities for smaller Eej. Scatter points represent observed late-time radio emission from a sample of events listed in the legend of the top panel, taken from M. C. Stroh et al. (2021).
Paper: Luminous Late-time Radio Emission from Supernovae Interacting with Circumbinary Material
Authors: Samantha C. Wu, Daichi Tsuna
Figure caption: Top row: light curves of radio emission at 3 GHz for the models listed in the legend. Each is calculated with Eej = 1051 erg and the parameters listed in the upper right of each panel. The solid lines show an estimate of the light curve for a face-on viewing angle, which is the sum of contributions from the low-density stellar wind in the polar regions and from the dense CSM in the torus. The early peaks appear due to the low-density stellar wind (dotted line), and the second bright peak is set by SSA for the CSM. The dashed lines show the light curve from an edge-on viewing angle along the direction of the CSM, as in Figure 2, which represents the maximum absorption due to both FFA and SSA. The shaded region encompasses the range of emission between the face-on and edge-on viewing angles. The scatter points represent the same events as listed in the legend of Figure 2. Bottom row: light curves of radio emission at 15 GHz for the same models as in the top row. The scatter points represent the same events as listed in the top right legend of Figure 3.
Paper: Luminous Late-time Radio Emission from Supernovae Interacting with Circumbinary Material
Authors: Samantha C. Wu, Daichi Tsuna
Figure caption: Top row: light curves of radio emission at 3 GHz for the models listed in the legend. Each is calculated with Eej = 1051 erg and the parameters listed in the upper right of each panel. The solid lines show the light curve for a CSM velocity of 0.3 vorb,c, as in Figure 2. The dotted lines show the light curve for a fast CSM of 103 km s−1, assuming the CSM has been accelerated by some mechanism upon ejection from the binary system. The scatter points represent the same events as listed in the legend of Figure 2. Bottom row: light curves of radio emission at 15 GHz for the same models as in the top row. The scatter points represent the same events as listed in the top right legend of Figure 3.
Paper: Luminous Late-time Radio Emission from Supernovae Interacting with Circumbinary Material
Authors: Samantha C. Wu, Daichi Tsuna
Figure caption: Light curves of radio emission at 15 GHz for the same models as in Figure 2. Scatter points show observed radio emission at ≈15 GHz for the events listed.
Paper: Optical Strong Line Ratios Cannot Distinguish between Stellar Populations and Accreting Black Holes at High Ionization Parameters and Low Metallicities
Authors: Nikko J. Cleri, Grace M. Olivier, Bren E. Backhaus, Joel Leja, Casey Papovich, Jonathan R. Trump, Pablo Arrabal Haro, Véronique Buat, Denis Burgarella, Emilie Burnham, Antonello Calabrò, Jonathan H. Cohn, Justin W. Cole, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Ray Garner, Michaela Hirschmann, Weida Hu, Taylor A. Hutchison, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Zach J. Lewis, Michael V. Maseda, Lise-Marie Seillé, Raymond C. Simons
Figure caption: The ratios of ionizing photon production Q in each of the D. A. Berg et al. (2021) zones of ionization shown in Figure 1 for all of the BPASS stellar populations and black hole accretion disk ionizing spectra used in this work. We show here the stellar models of log age/yr < 8, excluding the ages for which there is no significant production of photons at the energies traced by the [N II]-BPT, VO87, and OHNO diagrams.
Paper: Optical Strong Line Ratios Cannot Distinguish between Stellar Populations and Accreting Black Holes at High Ionization Parameters and Low Metallicities
Authors: Nikko J. Cleri, Grace M. Olivier, Bren E. Backhaus, Joel Leja, Casey Papovich, Jonathan R. Trump, Pablo Arrabal Haro, Véronique Buat, Denis Burgarella, Emilie Burnham, Antonello Calabrò, Jonathan H. Cohn, Justin W. Cole, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Ray Garner, Michaela Hirschmann, Weida Hu, Taylor A. Hutchison, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Zach J. Lewis, Michael V. Maseda, Lise-Marie Seillé, Raymond C. Simons
Figure caption: The [N II]-BPT (left), VO87 (center), and OHNO (right) diagrams with our suite of Cloudy models for BPASS stellar populations (gold circles) and black hole accretion disks (blue crosses). The lines show the demarcations for star formation and AGN (below and above the lines, respectively) for the [N II]-BPT (L. J. Kewley et al. 2001; G. Kauffmann et al. 2003), VO87 (J. R. Trump et al. 2015), and OHNO (B. E. Backhaus et al. 2022) diagrams, respectively. The full model parameters are described in Section 2.
Paper: Optical Strong Line Ratios Cannot Distinguish between Stellar Populations and Accreting Black Holes at High Ionization Parameters and Low Metallicities
Authors: Nikko J. Cleri, Grace M. Olivier, Bren E. Backhaus, Joel Leja, Casey Papovich, Jonathan R. Trump, Pablo Arrabal Haro, Véronique Buat, Denis Burgarella, Emilie Burnham, Antonello Calabrò, Jonathan H. Cohn, Justin W. Cole, Kelcey Davis, Mark Dickinson, Steven L. Finkelstein, Ray Garner, Michaela Hirschmann, Weida Hu, Taylor A. Hutchison, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Zach J. Lewis, Michael V. Maseda, Lise-Marie Seillé, Raymond C. Simons
Figure caption: Example ionizing spectra of the four stellar population (gold) and three accreting black hole (blue) models used in this work. The annotations mark the four “zones” of ionization from D. A. Berg et al. (2021). The stellar populations are shown with constant IMF and metallicity with varying age, and the black hole accretion disk models are shown with constant Lbol/LEdd and spins and varying black hole masses. The full details of the models are discussed in Section 2.