adsabs/AstroCLIMB huggingface dataset:
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: The rms z-scale height for preexisting (old) stars as a function of radius R (in kiloparsecs) for each value of fgas. The left panel is for no halo accretion cases; the right panel is for halo accretion models. In all plots, the color coding indicates the time evolution, as indicated. The scale height of the α-rich thick disk today at R0 = 8.2 kpc is indicated by the cross (J. Bland-Hawthorn & O. Gerhard 2016). Note that the vertical scale has a fourfold stretch compared to the horizontal axis. Gas-rich models are more able to reproduce the α-rich disk within 1.5–2 Gyr.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: (Left) The fgas = 100% accreting halo case is repeated from Figure 11 and highlights the different heating phases due to rapid reversals along the sloshing track. In practice, we allow for 1% of the disk mass to be an existing stellar population so that we can trace the impact of the heating. The z-height is starting to saturate after 1.5 Gyr. (Right) This is a repeat of the LHS plot but for stars forming in the gas rather than preexisting stars. The heating rate is essentially the same. The bottom 10 tracks (100 Myr apart) are removed because of large intrinsic scatter; this is a consequence of small number statistics and early populations being born out of dynamical equilibrium. Note for both plots that the vertical scale has a fourfold stretch compared to the horizontal axis. The cross indicates the vertical scale height of the Milky Way’s α-rich disk at the solar circle today.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: (Left) Where new stars are born in time as a function of vertical height ∣z∣.  The left-hand side (LHS) panels look very similar for all fgas, quite unlike the RHS panels. (Right) The rms z-scale height for newborn stars as a function of radius R (in kiloparsecs) for each value of fgas for the halo accretion cases. In all plots, the color coding indicates the time evolution, as indicated. The bottom 10 tracks (100 Myr apart) are removed because of large intrinsic scatter; this is a consequence of small number statistics and early populations being born out of dynamical equilibrium. The scale height of the α-rich thick disk today at R = 8 kpc are indicated by the blue star (J. Bland-Hawthorn & O. Gerhard 2016). Note that the vertical scale has a fourfold stretch compared to the horizontal axis. The gas-rich models are able to reproduce the thickness of the α-rich disk within 1.5–2 Gyr.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Evolution of wave amplitudes ﹩A(t)={\widetilde{{\rm{\Sigma }}}}_{1}(t)﹩ in the presence of an impulse, obtained by solving the iterative integral in Equation (23), where the tilde indicates a surface density amplitude normalized to evolution without gravity. The horizontal axis shows time evolution in units of κ/π, consistent with shearing-sheet analysis (W. H. Julian & A. Toomre 1966), starting at ﹩\kappa {t}_{i}=-\frac{3\pi }{2}﹩. (Left) The response of a Mestel disk to a sharp impulse for Q = 1.2, 1.3, 1.4, demonstrating the increasing importance of self-gravity to the disk’s response (J. Binney 2025). The red curves illustrate the weak disk response when self-gravity is neglected. (Right) This repeats the left panel but for a longer-wavelength disturbance; only wavelengths shorter than k = kcrit are stabilized by the initial Q value. The range of Q values shown describes the Nexus disks for most of their evolution.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: (Top) The radial scale length for preexisting stars as a function of time (in megayears) for each value of fgas indicated in the key. The left panel is for no halo accretion models; the right panel is for halo accretion models. (Right) The same quantity but for newly formed stars as a function of time (in megayears) for each value of fgas indicated in the key. In all panels, the gray band indicates the radial scale length of the thick disk today, i.e., ﹩{R}_{\mathrm{disk}}^{T}=2.0\,\pm \,0.2﹩ kpc (J. Bland-Hawthorn & O. Gerhard 2016).
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Predicted trends at 2 Gyr (z ≈ 1.5) after disk onset for the halo accreting fgas = 100% model, representative of the high fgas models in general. (Left) Age–metallicity trend in the simulated α-rich disk in the simulated R − z plane, i.e., within a vertical slice that is 100 pc thick along the line of sight. (Top right) Age distribution in the same plane showing a weak trend in radius but a stronger vertical gradient, such that the youngest stars lie near the plane. (Bottom right) Metallicity distribution in the same plane showing a weak trend in radius but a stronger vertical stratification, such that the most metal-rich stars lie near the plane. For the RHS figures, representative stellar density contours within the vertical slice are overlaid.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Two different perspectives of the same Brownian motion track in a moderately flattened, spherical gravitational potential. The slosh coordinates (in kiloparsecs) are equivalent to those presented in Figure 7. The color scheme once again shows the evolution over 2 Gyr (blue → red). The track is similar in character to the baryon sloshing tracks in Figures 7 and 8.
Paper: Turbulent Gas-rich Disks at High Redshift: Origin of Thick Stellar Disks Through 3D “Baryon Sloshing”
Authors: Joss Bland-Hawthorn, Thor Tepper-Garcia, Oscar Agertz, Christoph Federrath, Misha Haywood, Paola di Matteo, Timothy R. Bedding, Takafumi Tsukui, Emily Wisnioski, Melissa Ness, Ken Freeman
Figure caption: Baryon sloshing presented as the change in radius ﹩{R}_{{\rm{slosh}}}=\sqrt{{x}_{{\rm{slosh}}}^{2}+{y}_{{\rm{slosh}}}^{2}+{z}_{{\rm{slosh}}}^{2}}﹩ with cosmic time (upper panels) in the reference frame of the total potential for fgas = 0%, 20%, 40%, 60%, 80%, 100%. The lower panels are the derivative ﹩{\dot{R}}_{{\rm{slosh}}}﹩ of the upper panels. The red lines indicate the changing physical scales between panels, where the overall trend is increasing with fgas. Note also that the sloshing frequency declines with increasing R, as expected from Equation (15).
Paper: UHECRs Propagation and Their Multimessengers: Upper Limits and the Impact of the Extragalactic Magnetic Field
Authors: Rodrigo Sasse, Rubens Costa, Adriel G.B. Mocellin, Carlos H. Coimbra-Araujo, R. C. Dos Anjos
Figure caption: Upper limits (ULs) on the integral gamma-ray flux, ﹩{I}_{\gamma }^{{\rm{UHECR}}}(\gt {E}_{{\rm{th}}})﹩, as a function of the source distance, calculated using the UL on the flux observed by the Pierre Auger Observatory at the 95% confidence level (CL) for a given energy threshold Eth. (a) Dependence on the cutoff energy Ecut, with fixed parameters α = 2.3 and Eth = 0.1 GeV. (b) Dependence on the spectral index α, for fixed parameters Ecut = Z × 1021 eV and Eth = 330 GeV. (c) Dependence on the energy threshold Eth, for fixed parameters Ecut = Z × 1021 eV and α = 2.3.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: Individual elemental abundances support a common formation between the Pleiades core, UPK 303, HSC 1964, and the diffuse GPC-1 region. Top panel: median [X/Fe] and 1σ dispersion for various elements, as measured from LAMOST DR7 medium-resolution spectra for the Pleiades core, UPK 303, and the GPC-1 region. Gray points show a random field sample drawn from stars within 500 pc and T < 16. Bottom panel: same as above but using Milky Way Mapper (SDSS DR19) high-resolution abundances for the Pleiades core, HSC 1964, and the GPC-1 region. We exclude P, V, and Cu because measurements of these elements were marked as having poor quality in S. Mészáros et al. (2025a). We additionally only include stars with 3500 < Teff < 6000 to match the parameter ranges in S. Mészáros et al. (2025a) where measurements are optimal. In both panels, the close agreement of our substructures with the Pleiades core across multiple elements—and their divergence from the broader field distribution (especially in C, Al, Mg, and Si)—suggests a common origin. Note that UPK 545, HSC 1964, and the GPC-2 region lack coverage in LAMOST DR7 (top), and UPK 303, UPK 545, and the GPC-2 region are absent from MWM DR19 (bottom).
Paper: UHECRs Propagation and Their Multimessengers: Upper Limits and the Impact of the Extragalactic Magnetic Field
Authors: Rodrigo Sasse, Rubens Costa, Adriel G.B. Mocellin, Carlos H. Coimbra-Araujo, R. C. Dos Anjos
Figure caption: Cosmogenic multimessenger fluxes simulated using CRPropa3 (R. Alves Batista et al. 2022). The green curve shows the cosmic-ray spectrum injected at the location of NGC 1068, at a comoving distance of 14 Mpc from Earth. The red curves depict the secondary photon fluxes produced during the propagation of UHECRs, whereas the blue curves represent the resulting cosmogenic neutrino flux. The solid lines correspond to a proton composition for the injected particles, and the dashed lines represent an iron composition scenario. Additionally, the plot includes the UL of the flux measured by the PAO, which serves as a reference for normalizing the simulated cosmic-ray spectrum (A. Aab et al. 2020). This normalization was also applied to the gamma-ray and neutrino fluxes to ensure consistency across multimessenger predictions. See the text for details.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: Back integrations for the six regions of interest relative to the Pleiades core using three different Galactic potential models: MilkyWayPotential2022 (solid), MWPotential2014 (dashed), and McMillan17 (dashed and dotted). Each panel shows the median 3D separation between the region and the Pleiades core as a function of time before the present, integrated to 120 Myr in the past. The three regions with convergent behavior (UPK 303, HSC 1964, and UPK 545) display minima in separation across all three potentials, indicating robustness to model choice. For the remaining regions (AB Dor, GPC-1, and GPC-2), the trajectories remain inconclusive regardless of potential.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: Top panel: the original spatial distributions of Orion members from R. Kerr et al. (2023). Gray points are outliers that were not considered in our analysis. Bottom panels: results of our back integration experiment with Orion. The true path the cluster took is shown in black, while the recovered path is shown as a color. The time of closest approach is written on each plot, and is far more precise than the distance at closest approach.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: The time of minimum separation in the past between each star in the Greater Pleiades Complex and the core of the Pleiades, using only stars with a non-null Gaia radial velocity and RUWE <1.2. Stars that do not get closer to the Pleiades core in the past are shown in gray. There is a dynamical age gradient present along the structure, with stars closer to the core appearing lighter and the stars farther away appearing darker. This is especially true for UPK 303 and the combination of the HSC 1964 and UPK 545 regions. Gaps or irregularities in the color gradient may reflect uncertainties in the radial velocities rather than physical substructure.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: Back-integrated 3D separations between each group (UPK 303, HSC 1964, and UPK 545) and the Pleiades core as a function of time before the present. The colored, solid curve in each panel shows the same trajectory as in the diagnostic plots for each region above. Black curves show the same quantity for 100 randomly selected regions at similar present-day separations. The diagnostic value of our back integrations is supported by the fact that few random samples yield similarly close approaches, particularly at comparable times.
Paper: Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Authors: Andrew W. Boyle, Luke G. Bouma, Andrew W. Mann
Figure caption: The full extent of the Greater Pleiades Complex as it would appear on the night sky if all stars from our membership list were visible to the naked eye. The seven brightest stars in the Pleiades are shown in green, while the stars from our membership list are shown in white. The Big Dipper, Orion, and Taurus are overlaid in blue. Of the 3091 stars in our membership catalog, 1603 are above the horizon at the selected observing conditions. The plot is oriented to match what an observer looking to the South would see.
Paper: Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era
Authors: Alessandra Venditti, Julian B. Muñoz, Volker Bromm, Seiji Fujimoto, Steven L. Finkelstein, John Chisholm
Figure caption: Left: SFR per unit halo mass (﹩{\dot{M}}_{\star }/{M}_{{\rm{h}}}﹩) as a function of halo mass (Mh) at z = 6.1 (with Δz = 1), incorporating a UV enhancement of ε⋆,UV/ε⋆. Our reference “BURSTY”/“HEAVY” models (with ﹩{M}_{\mathrm{up}}^{\mathrm{III}}\sim 1{0}^{8}/1{0}^{10}\,{M}_{\odot }﹩ respectively, and ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}\sim 1{0}^{-2.4}﹩) are shown as red/blue, thick, dashed lines. The model of H. A. G. Cruz et al. (2025, dark-red, dotted line, see text for details), and the corresponding Population II model from J. B. Muñoz et al. (2023, black, solid line), are included as a reference. The blue crosses show the average ﹩{\dot{M}}_{\star }/{M}_{{\rm{h}}}﹩ at the two extremes of the considered redshift range (z ≈ 5.6/6.6, in lighter/darker shade respectively) for the dustyGadget simulations (C. Di Cesare et al. 2023; A. Venditti et al. 2023) in bins of Mh, assuming a rescaling of ηIII = 0.3 for the Pop III mass (see Appendix A for more details). Right: UVLFs (ΦUV) as a function of UV magnitude (MUV) resulting from the models in the left panel (with same color and linestyle, assuming ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}=1.5/0.7﹩ for the “BURSTY”/“HEAVY” models, respectively), compared with the data point and upper limits from S. Fujimoto et al. (2025a, dark-red circle and triangles), including the AMORE6 candidate from T. Morishita et al. (2025) in the faintest MUV bin; filled/empty circles distinguish between MUV bins containing spectroscopic/photometric candidates (see text and Appendix B for more details). The gray, shaded area encompasses a range of UVLF fitting functions (from R. J. Bouwens et al. 2021; S. L. Finkelstein & M. B. Bagley 2022; J. B. Muñoz et al. 2023) extrapolated at the faint end, included as a reference together with data points from R. J. Bouwens et al. (2021) and R. J. Bouwens et al. (2022) at z = 5/6/7 (green/golden/brown dots). While the model of H. A. G. Cruz et al. (2025) assuming ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}=0.7﹩ (consistent with the value inferred from galaxy populations at the same redshift, as demonstrated by the agreement with observed data points of the Population II black line when assuming ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}\approx 0.7﹩) is unable to explain the data, models with enhanced stochasticity (“BURSTY” model) or a larger high-mass cutoff (“HEAVY” model) would be marginally consistent with GLIMPSE-16043 and AMORE6.
Paper: Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era
Authors: Alessandra Venditti, Julian B. Muñoz, Volker Bromm, Seiji Fujimoto, Steven L. Finkelstein, John Chisholm
Figure caption: Joint posterior for the effective SFE normalization ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}﹩ (Equation (6)) and the high-mass cutoff ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩ (Equation (5)), resulting from fitting our Pop III UVLF model described in Section 2 against the observed data points from S. Fujimoto et al. (2025a) and T. Morishita et al. (2025) at z ≈ 5.6–6.6, with fixed ﹩{\beta }_{\star }^{{\rm{III}}}=0﹩ and ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}=1.5/0.7﹩ (red/blue curves). The dashed, thick lines show the values adopted for ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}﹩ and ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩ in our reference “BURSTY” and “HEAVY” models (refer to Figure 1): for each chosen value of ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩, these represent the best-fit values of Log﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}﹩ corresponding roughly to the 2.3rd percentile of the Log﹩({M}_{\mathrm{up}}^{\mathrm{III}}/{M}_{\odot })﹩ marginalized posterior. The dotted, dark-red and solid, dark-blue lines further show the values of ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}﹩ and ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩ from the model of H. A. G. Cruz et al. (2025) (as in Figure 1), and the maximum halo mass hosting Pop III stars at z ≈ 5.6–6.6 from the dustyGadget simulation suite (C. Di Cesare et al. 2023; A. Venditti et al. 2023) as a reference. Note that either large stochasticities (﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}\gtrsim 1.5﹩) or large high-mass cutoffs (﹩{M}_{\mathrm{up}}^{\mathrm{III}}\gtrsim 1{0}^{10}\,{M}_{\odot }﹩, still well below the most massive Pop III halo in the dustyGadget simulations) are required to fit the data within 2σ.
Paper: Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era
Authors: Alessandra Venditti, Julian B. Muñoz, Volker Bromm, Seiji Fujimoto, Steven L. Finkelstein, John Chisholm
Figure caption: Top: same as Figure 1, but exploring different values for the stochasticity parameter ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩ (from 0.5 to 2, in rainbow color scale); the top-right inset in the left panel shows the 1D posterior for the Log﹩({M}_{\mathrm{up}}^{\mathrm{III}}/{M}_{\odot })﹩ parameter corresponding to each chosen value of ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩, as in the bottom-left panel of Figure 2. More stringent requirements are imposed on ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩ for lower values of ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩, ranging from ﹩{M}_{\mathrm{up}}^{\mathrm{III}}\gtrsim 1{0}^{8}\,{M}_{\odot }﹩ to ﹩{M}_{\mathrm{up}}^{\mathrm{III}}\gtrsim 1{0}^{11}\,{M}_{\odot }﹩ in order to fit the data within 2σ. The thin, dashed, red line shows a variation of the “BURSTY” model, including the effect of the streaming velocities and LW (JLW and vcb, see text for more details), which produces a slight decrease in the overall UVLF. Bottom: 1D posterior for the ﹩{\beta }_{\star }^{{\rm{III}}}﹩ parameter resulting from fits with fixed ﹩{M}_{\mathrm{up}}^{\mathrm{III}}={M}_{\mathrm{atom}}/1{0}^{10}\,{M}_{\odot }/1{0}^{12}\,{M}_{\odot }﹩ (left/center/right) and free ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}﹩ and ﹩{\beta }_{\star }^{{\rm{III}}}﹩, for different values of ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩ (same color scale as the top panels), showing that our standard assumption of ﹩{\beta }_{\star }^{{\rm{III}}}=0﹩ (“feedback-light” model, as in the top panels) is consistent with these results, albeit slightly disfavored in models with both large ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩ and large ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩.
Paper: UHECRs Propagation and Their Multimessengers: Upper Limits and the Impact of the Extragalactic Magnetic Field
Authors: Rodrigo Sasse, Rubens Costa, Adriel G.B. Mocellin, Carlos H. Coimbra-Araujo, R. C. Dos Anjos
Figure caption: Energy-dependent differential flux sensitivity and spectral energy distribution (SED) for the NGC 1068 region. (a) The black dashed line represents the intrinsic spectral model (Equation (15)), while the black solid line includes attenuation due to extragalactic background light (EBL), modeled using Saldana-Lopez (A. Saldana-Lopez et al. 2021; Equation (16)). Model parameters are in Table 3, with shaded regions indicating errors. Sensitivity curves for CTAO South are shown with different configurations: solid blue (14 MSTs + 37 SSTs), solid red (MSTs only), and solid green (SSTs only) for 50 hr observations; the dashed blue line represents the full array for 200 hr. IRFs are optimized for a 50 hr exposure at a 20° zenith angle with azimuth-averaged pointing. (b) Modeled gamma-ray flux for NGC 1068 overlaid with Fermi-LAT (3FHL, 3FGL, and 4FGL) and MAGIC data (Table 4). The black solid line represents the absorbed spectral model from Saldana-Lopez (A. Saldana-Lopez et al. 2021; Table 3), while lighter green circles show CTAO South flux points for a 50 hr observation. Error bars indicate statistical uncertainties.
Paper: Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era
Authors: Alessandra Venditti, Julian B. Muñoz, Volker Bromm, Seiji Fujimoto, Steven L. Finkelstein, John Chisholm
Figure caption: Same as Figures 1 and 2, but also including the uncertain JOF-21739 Pop III candidate at bright ﹩{M}_{{\rm{UV}}}^{{\rm{III}}}\approx -17.6﹩ in the fit. The “BURSTY”/“HEAVY” models in this case correspond to larger ﹩{M}_{\mathrm{up}}^{\mathrm{III}}\sim 1{0}^{9}/1{0}^{12}\,{M}_{\odot }﹩, and ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}\sim 1{0}^{-2.8}/1{0}^{-3.4}﹩ (with the usual reference ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}=1.5/0.7﹩). An additional ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}=2﹩ scenario is included in pink, which approximately corresponds to the minimum stochasticity allowing to fit the data within 2σ with a cutoff close to the atomic-cooling halo mass threshold; see, e.g., the “BURSTIER” model (﹩{M}_{\mathrm{up}}^{\mathrm{III}}\sim 1{0}^{8}\,{M}_{\odot }﹩, ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}\sim 1{0}^{-3.1}﹩).