adsabs/AstroCLIMB huggingface dataset:
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Simulations at the magma ocean–atmosphere interface of K2-18b assuming real versus ideal gas behavior for different C/H by mass. C/H by mass varies from solar (∼3E-3) to that of the BSE (∼1.3), while other input parameters are fixed, with Tsurface = 3000 K, a total hydrogen mass fraction of 1% of the planet mass, and oxygen fugacity (fO2) at ΔIW = −3. The x-axis corresponds to C/H by mass on a log10-scale. The solid lines correspond to the cases assuming real gases, and the dashed lines assume ideal gas behavior. (a) Pressures of volatile species in the atmosphere (GPa) and the total atmospheric pressure (gray). (b) C/H (purple, left y-axis) and C/O (teal, right y-axis) in the atmosphere. (c) Solubility of each volatile species (wt%, i.e., fraction of the planet’s mantle mass). (d) Fugacity coefficient (ϕ) for each volatile species. The coefficient for ideal behavior (gray dashed line) is unity for all volatiles.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Three-color composite HST image of NGC 6302, created by M. Matsuura et al. (2025, MNRAS, submitted) utilizing images from J. H. Kastner et al. (2022) and B. Balick et al. (2023). This image presents a color overlay of WFC3 observations of NGC 6302, featuring F164N filter in blue, which traces [Fe II] emission, F656N filter in green, which traces Hα emission, and F658N in red, which traces [N II] emission. The white box at the center represents the MIRI field of view for observations described in Section 2.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: CH﹩{}_{3}^{+}﹩ excitation temperature derived for the 25 selected apertures. Teal points represent the I(7.15 μm)/I(7.2 μm) band found in the observed extracted spectra. The corresponding temperatures (as described by Equation (1)) are shown on the y-axis on the right. Purple points represent the best-fit temperature derived from fitting models to the observations.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Intensity ratio I(7.15 μm)/I(7.2 μm) as a function of excitation temperature of CH﹩{}_{3}^{+}﹩. Black points represent the I(7.15 μm)/I(7.2 μm) found in the model spectra for a given excitation temperature. A five-degree polynomial fit to those points is represented by the red curve. The polynomial is given by Equation (1).
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: The image represents a color overlay of HST/WFC3 observations featuring filter F656N in blue (J. H. Kastner et al. 2022), which traces emission from Hα, and the CH﹩{}_{3}^{+}﹩ map in red.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: The continuum-subtracted JWST/MIRI spectrum of NGC 6302 at aperture 1, shown in Figure 2 (black, offset vertically for clarity), compared to a CH﹩{}_{3}^{+}﹩ model (red) by P. B. Changala et al. (2023) at an excitation temperature of 600 K. The H I recombination line at 7.0928 μm and the He II line at 7.2036 μm are labeled at the top.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Model spectra of CH﹩{}_{3}^{+}﹩ at 500, 1000, 1500, and 2000 K. Bands at 7.15 and 7.2 μm are highlighted in blue and red, respectively.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Mass accretion rate evolution in our hydrodynamic simulations. We compare three different models with the same orbital parameters but different feedback methods: no feedback (model M05e05n; green), thermal feedback (model M05e05t; light green) and bipolar feedback (M05e05b; dark gray). Dashed vertical lines mark the periastron passage timings. For the no-feedback model, we overplot the Bondi–Hoyle–Lyttleton accretion rate computed from Equation (13) (dotted).
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: B-DECIGO: joint dependence of ﹩{M}_{p}^{{\rm{\min }}}﹩ on the binary chirp mass Mc and luminosity distance DL. At fixed DL, increasing Mc (hence the intrinsic GW amplitude) lowers ﹩{M}_{p}^{{\rm{\min }}}﹩; at fixed Mc, increasing DL degrades sensitivity. The combination highlights massive, nearby binaries as prime targets for sub-Jovian and even sub-Neptune planets.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: DECIGO: same as Figure 9. Relative to B-DECIGO, DECIGO achieves uniformly lower ﹩{M}_{p}^{{\rm{\min }}}﹩ across the (Mc, DL) plane—extending Earth-mass sensitivity to nearby sources and maintaining sub-Jovian reach to distances orders of magnitude larger.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: Minimum detectable planetary mass ﹩{M}_{p}^{{\rm{\min }}}﹩ versus the source’s initial GW frequency f0 for the reference BNS systems. Sensitivity improves steeply with f0, since the Doppler sidebands scale with the carrier frequency and the SNR. DECIGO can reach Earth-mass scales for high-f0 BNSs in the Milky Way, while B-DECIGO remains sensitive to super-Earth/Neptune analogs under the same assumptions.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Same as Figure 4 but comparing models with different companion masses: M2 = 3 M⊙ (model M03e05b; sky blue), 5 M⊙ (model M05e05b; dark gray), and 10 M⊙ (model M10e05b; blue). All models were simulated with bipolar feedback.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Allowed eccentricities as a function of companion mass. The neutron star mass is fixed to MNS = 1.4 M⊙ and the orbital period to Porb = 12.5 days. Black curves show the minimum eccentricity above which the companion star will overflow its effective Roche lobe at periastron, whereas the red curves show the minimum eccentricity above which the NS will plunge into the companion at periastron. We use the J. R. Hurley et al. (2000) formulae to estimate the stellar radius R2 at zero-age main sequence (dashed) and at t = 10 Myr (solid).
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Schematic diagram of the emission from SN2022jli at ∼200 days.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Undulation light curve folded over undulation phase for the M05e07b model. Gray points are the observed data of SN2022jli (P. Chen et al. 2024). Red solid curves are the folded light curves of the +x model in Figure 9. Both are shifted so that the minima are located at the phase origin.
Paper: Supernova-induced Binary-interaction-powered Supernovae: A Model for SN2022jli
Authors: Ryosuke Hirai, 井遼介 平, Philipp Podsiadlowski, Peter Hoeflich, Maxim V. Barkov, Conrad Chan, David Liptai, Shigehiro Nagataki, 瀧重博 長
Figure caption: Opacity as a function of density and temperature computed from Equation (A1) with κfloor = 0. Overplotted are the density and temperature of each cell in our simulations from the two snapshots used in Figures 13 and 14.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Field of view for narrowband imaging with SWIMS NB1244 (magenta rectangle) and HSC NB921 (blue circle). The J-band imaging (the corresponding broadband of SWIMS NB1244) was conducted with MOIRCS, except for field C1, which was observed using SWIMS (dashed rectangle). The area with archival IRAC coverage is indicated by the red rectangle (see Section 3.4.1). The background green contours represent galaxy surface density derived from sources within the redshift slice z = 0.88–0.91, including both spectroscopically confirmed galaxies (Section 3.4.2) and the dual emitters identified in this study. Galaxy density is computed using Gaussian kernel density estimation. We note that Hβ emitters selected solely based on HSC NB921 imaging are not included in the density estimation.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: (Left) Spatial distribution of emission-line galaxies within our narrowband redshift coverage, color coded according to their r − J colors. The quiescent galaxies are defined by the rest-frame UVJ diagram and selected from the subsample with IRAC coverage (Section 3.4.1). The yellow crosses mark the cluster/group centers as defined by B. C. Lemaux et al. (2012). (Right) Spectroscopically confirmed galaxies from the ORELSE survey (B. C. Lemaux et al. 2012) and M. Hayashi et al. (2019). The shaded regions correspond to the filter effective width coverage for NB1244 (orange) and NB921 (blue).
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Redshift distribution of spectroscopically confirmed galaxies (see Section 3.4.2) within the filter coverage of six Subaru pointings, overlaid with the transmission curves of the NB921 and NB1244 narrowband filters (arbitrarily scaled). The corresponding velocity distribution, centered at z = 0.895, is also shown. The narrowband filters effectively capture the redshift peak at z = 0.895 over a considerable velocity range.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: (Left) Predicted color tracks at z = 0.9 and z = 1.5 based on the T. Kodama et al. (1999) model, illustrating variations in the bulge-to-total ratio from 1 to 0 along the curves. The final sample of 94 galaxies is shown as filled circles, with orange circles representing narrowband selected emitters and gray circles representing narrowband selected emitters confirmed with spectroscopically redshifts. Error bars indicate magnitude uncertainties. (Right) Photometric redshift distribution of the final sample.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Narrowband–broadband color–magnitude diagram used to select Hα emitters. The color excess is calculated using MAG_APER. The gray dashed lines represent the 5σ limiting magnitudes in the J and NB1244 bands. The gray solid curve and the line indicate the 3σ excess in J − NB1244 colors and the J − NB1244 = 0.2 cut, respectively. Orange crosses represent galaxies brighter than the narrowband limiting magnitude. Galaxies meeting our selection criteria (see Section 4.2) are shown as blue points with error bars representing magnitude/color uncertainties.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: Validated QRaFT features of the studied 2017 August 21 TSE image reprojected to the rectangular coordinate system. The background TSE image is courtesy of M. Druckmüller, P. Aniol, and S. Habbal.
Paper: Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrowband Imaging: Degree-scale Balmer Decrement Mapping Across a z = 0.9 Supercluster
Authors: Zhaoran Liu, Tadayuki Kodama, Brian C. Lemaux, Mariko Kubo, Jose Manuel Pérez-Martínez, Yusei Koyama, Ichi Tanaka, Kazuki Daikuhara, Roy R. Gal, Denise Hung, Masahiro Konishi, Kosuke Kushibiki, Ronaldo Laishram, Lori M. Lubin, Kentaro Motohara, Hidenori Takahashi
Figure caption: Redshift distribution of 37 spectroscopically confirmed emitters among 94 photometrically selected emitters. The transmission curves of the NB921 and NB1244 narrowband filters are also shown.
Paper: The Quasi-radial Field-line Tracing (QRaFT): An Adaptive Segmentation of the Open-flux Solar Corona
Authors: Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
Figure caption: QRaFT segmentation of a ground-based TSE image (courtesy of M. Druckmüller, P. Aniol, and S. Habbal) acquired on 2017-08-21. See Figure 5 for notations.
Paper: Electron Instabilities Driven by Beaming Electrons with Anisotropic Temperatures in High-beta Plasmas
Authors: Ye Yu, Jinsong Zhao, Chen Shi, Huasheng Xie
Figure caption: Instabilities in the case of a fast-streaming electron beam with Veb = 150VA: (a1)–(a4) for Aeb = 1 and (b1)–(b4) for Aeb = 2. Panels (c1)–(c4) show instabilities induced by a hot electron component, corresponding to the beam component with Veb = 0VA and Aeb = 2. (a1), (b1), and (c1): normalized growth rate γ/ωce. (a2), (b2), and (c2): normalized real frequency ωr/ωce. (a3), (b3), and (c3): polarization P. (a4), (b4), and (c4): ratio between parallel and perpendicular magnetic perturbations, B∥/B⊥. The five types of instability regimes induced by the fast-streaming electron beam are labeled as “FEI-I,” “FEI-II,” “FEI-III,” “FEI-IV,” and “FEI-V” in panels (a1) and (b1).
Paper: Electron Instabilities Driven by Beaming Electrons with Anisotropic Temperatures in High-beta Plasmas
Authors: Ye Yu, Jinsong Zhao, Chen Shi, Huasheng Xie
Figure caption: Dependence of the quasi-perpendicular instabilities at θ = 89﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and oblique whistler instabilities at θ = 40° on the temperature anisotropy of the electron beam with Veb = 150VA. Panels (a1)–(a2), (b1)–(b2), and (c1)–(c2) show the normalized growth rate γ/ωce and normalized real frequency ωr/ωce of the quasi-perpendicular instabilities for Aeb = 1, 1.5, and 2, respectively. Panels (d1)–(d2), (e1)–(e2), and (f1)–(f2) show γ/ωce and ωr/ωce for the oblique whistler instabilities at the same anisotropy values. The polarization P is overlaid in panels (d1)–(d2), (e1)–(e2), and (f1)–(f2).
Paper: Electron Instabilities Driven by Beaming Electrons with Anisotropic Temperatures in High-beta Plasmas
Authors: Ye Yu, Jinsong Zhao, Chen Shi, Huasheng Xie
Figure caption: Instabilities in the case of a slow-streaming electron beam with Veb = 50VA. The electron beam with Aeb = 1: (a1) the normalized maximum growth rate γ/ωce and (a2) the normalized real frequency ωr/ωce. The electron beam with Aeb = 2: (b1) γ/ωce and (b2) ωr/ωce. The dependence of the instabilities on the Aeb: (c1) γ/ωce and (c2) ωr/ωce.
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Top: cosmic ionizing emissivity as a function of the redshift, ﹩{\dot{n}}_{{\rm{ion}}}(z)﹩, for the hybrid model and inferred fesc =  12% for the stars and fesc =  63% for the AGN. The black hatched corresponds to the combined contribution from stars and AGN, the blue corresponds to the contribution from stars, and the red corresponds to the contribution from AGN. The spread of the hatched regions reflects the spread in the fitted CSFH and CAGNH. We show observational constraints and their 1σ uncertainties from G. D. Becker & J. S. Bolton (2013). Bottom: neutral fraction as a function of the redshift as per Equation (3). The hatched regions have the same meaning as the top panels. We show results and 1σ uncertainties from C. A. Mason et al. (2018), F. B. Davies et al. (2018), A. Hoag et al. (2019), B. Greig et al. (2019), J. Yang et al. (2020), F. Wang et al. (2020), P. Bolan et al. (2022), M. Tang et al. (2024), M. Nakane et al. (2024), H. Umeda et al. (2025) as indicated in the legend. Upper/lower-limit observations from I. D. McGreer et al. (2015), C. A. Mason et al. (2019a), P. Bolan et al. (2022), X. Jin et al. (2023) are shown with arrows as indicated. The gold star with the horizontal error bar shows the midpoint and 1σ uncertainty of reionization redshift inferred from Planck Collaboration (2020a).