adsabs/AstroCLIMB huggingface dataset:
Paper: What Can We Learn about Reionization Astrophysical Parameters Using Gaussian Process Regression?
Authors: Purba Mukherjee, Antara Dey, Supratik Pal
Figure caption: Forecasting the reionization power spectrum of six ΛCDM parameters with two astrophysical parameters, ionization efficiency and clumping factor, using the Planck+SKA+Lyα+UV17(A) data sets and the Planck+SKA+Lyα+UV17(B) data sets. Here, for this forecast and MCMC analysis, we have used fake Planck realistic data. The analysis is undertaken using the mean reconstructed QH II function without incorporating the errors.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: The evolution of a noisy start realization of the baseline model from SC23 with force terms 1 ≤ m ≤ 8 all active. The color scale indicates the logarithm of the disk surface density. Notice that no strong bar forms, though a short, weak bar is visible from time to time.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: Top: the mean amplitudes of the bar-like A(2, 0, t) (Equation (3)) in 10 noisy start realizations of model A for four different values in N with unrestricted forces. Middle: the same as for the top panel but for m = 3. Bottom: the evolution of the bar amplitude in identical noisy start simulations when nonaxisymmetric forces are restricted to m = 2. Results from the individual simulations were shifted in time in the bottom panel only so that A = 0.06 at t = 100 for each before averaging.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: Three example rotation curves (black curves) of disk + compressed halo. The disk contribution, which is the same in all three, is shown in red and the compressed halo in green, with V0 = 0.6 in the left panel, V0 = 0.7 in the middle panel, and V0 = 0.8 in the right panel. In all three panels the contribution of the halo before compression, for which rc = Rd/2, is shown by the dotted curve.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: The radial variation of Q at intervals of 50 dynamical times in the simulation illustrated in Figure 1. The lines are not labeled because increases in Q are mostly monotonic.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: The evolution of one comparison simulation of model A having N = 60K particles. The initial disk extends to R = 5Rd, and times are given in dynamical times.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: The later part of the evolution of the disk component in the V0 = 0.6 3D simulation, whose rotation curve is given in the left panel of Figure 5. Notice that a strong bar forms.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: The model parameter posterior sample distribution found via NESSAI using a REDBACK refreshed shock afterglow model, and the absorption/extinction corrected data shown in Figure 3. Top-right panel: spectral energy distribution for 200 randomly selected posterior sample outputs at given times vs. the data. Note the radio excess at 0.07 day.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: Top panel: the radio lightcurve of GRB 231117A at 5–6 GHz (yellow) and 9–10 GHz (green) obtained with ATCA, e-MERLIN, and VLA (the latter data points are taken from G. Schroeder et al. 2025). A nearby check source detected at both frequencies in the ATCA images is also plotted in gray to demonstrate the observed variability of GRB 231117A is real. The solid data points show ATCA detections (>3σ). In contrast, the open data points are force-fitted flux densities at the known position of the source in the ATCA images when there was no significant detection. e-MERLIN and VLA nondetections are plotted as 3σ upper limits. Bottom panel: spectral index evolution (where the flux density is Sν ∝ ν−β) between the ATCA 5.5 and 9 GHz detections of the GRB (black) and check source (gray). An open data point is plotted when at least one of the flux densities used to calculate the spectral index was force-fitted in the ATCA image. The spectral evolution from the VLA 6 and 10 GHz detections are also plotted as black diamonds.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: Estimating afterglow emission characteristics using closure relations vs. the observed absorption/extinction corrected data. Our best reproduction requires a forward shock afterglow with p < 2, and a period of significant energy injection, between ∼0.02 and 1.0 day post-burst. Temporal indices for the various components are listed, as are the key timescales—the t−α labels correspond to the line immediately below the label. The solid gray lines are our lightcurve estimates (labeled “lightcurve est.”), and the dashed blue lines give possible radio lightcurve behaviors for before the jet break (labeled “lightcurve pos.”) dependent on the spectral regime at radio wavelengths, before or after the passage of the synchrotron self-absorption frequency.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: The required dynamical parameters from the refreshed shock model fit to the data indicate that the shell collision required by the model fit may have been “violent.” Solving the shock jump conditions and the requirement for a supersonic shock system, we can determine the duration of any violent collision and estimate the additional afterglow emission due to a reverse and forward shock system within the colliding shells. We adopt the labeling index from B. Zhang & P. Mészáros (2002; see their Figure 2) for the various shell zones: A subscript “1” indicates the unshocked external medium, “2” is the shocked swept-up external medium (forward shock), “3” is the hot impulsive shell, “4” is the collision shocked hot impulsive shell, “5” is the shocked injection shell (reverse shock), and “6” is the unshocked injection shell. See also Figure 10 for our setup and Equation (A17) for the definition od γb.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: (a) Average outflow mass flux ﹩\langle {\dot{M}}_{{\rm{ou}}}\rangle ﹩ vs. θ in units of ﹩{\dot{M}}_{{\rm{Edd}}}﹩; (b) 〈vp〉 (in unit of c) of the outflow measured at r = 500rg for the model L1, α values as mentioned in panel (a); (c) ﹩\langle {\dot{M}}_{{\rm{ou}}}\rangle ﹩ vs. θ; and (d) 〈vp〉 vs. θ for α = 0.05 of different models.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Variation of bolometric luminosity (shown in the upper panel) in the unit of erg s−1 and corresponding PDS (shown in the lower panel) with the different α case for the model L2. We consider a BH mass of MBH = 10M⊙.
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: Discovery of the GRB 231117A optical afterglow. Top panels: 40 cm SLT r-band discovery image taken 7.39 hr after the Swift trigger (left), subtracted from the SDSS template (middle), and afterglow identification (right). Bottom panel: Lulin One-meter Telescope (LOT) gri-color combined image of the afterglow and field.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Space–time diagrams showing (a) the angle-averaged angular momentum (〈λ〉) and (b) the accretion rate (﹩\dot{M}﹩ in the units of ﹩{\dot{M}}_{{\rm{Edd}}}﹩) for viscosity α = 0.025 for model L2.
Paper: Exploring the Signature of Assembly Bias and Modified Gravity Using Small-scale Clusterings of Galaxies
Authors: Yirong Wang, 艺蓉 王, Zhongxu Zhai, 忠旭 翟, Xiaohu Yang, 小虎 杨, Jeremy L. Tinker
Figure caption: Bias in the measurement of fσ8 when the model of galaxy clustering at the nonlinear scale has assembly bias or not. The mocks are produced by the Aemulus test simulations with different HOD models and assembly bias parameters. In order to denote the strength of assembly bias, for each HOD model, we compute the residual of ξi compared with the result when fenv is set to 0, i.e., the assembly bias effect is turned off. We arbitrarily choose the value at 10h−1 Mpc as a proxy and plot on the x-axis, which is equivalent to the y-axis in Figure A1. Then for the test model we run recovery tests with (black squares) and without (red squares) assembly bias parameters in the model. The result shows that the ignorance of assembly bias in the model can lead to biased cosmological measurements when the universe has assembly bias in it, and the deviation is proportional to the strength of the assembly bias. The upper panel shows the offset of fσ8 as the signal, while the bottom panel shows the Bayesian evidence for the corresponding tests. It shows that an incomplete model for assembly bias is not favored by the data, consistent with the biased measurement in the upper panel.
Paper: Exploring the Signature of Assembly Bias and Modified Gravity Using Small-scale Clusterings of Galaxies
Authors: Yirong Wang, 艺蓉 王, Zhongxu Zhai, 忠旭 翟, Xiaohu Yang, 小虎 杨, Jeremy L. Tinker
Figure caption: Two examples of the constraints on Ωm, σ8, and γf for two different cosmologies and different HOD models. The “C1, C2, C3, C4” for different colors stand for different cases, which are listed in Table 2. The first three fit perfectly, but there is the largest deviation for “C4” within blue regions, indicating that ignoring assembly bias can yield biased constraints on cosmological parameters. The deviation between cases with and without assembly bias in these two panels can be quantified by Δξi/ξi(s = 10 h−1 Mpc) as explained in the text. Specifically, the deviations are –0.0941 for the left panel and –0.3577 for the right panel, i.e., the strength of assembly is roughly proportional to the bias in the final constraints.
Paper: The b3Π–a3Δ and b3Π–X1Σ+ Band Systems of ZrO
Authors: Manish Bhusal, Peter F Bernath, Jacques Liévin, Léo Lavy
Figure caption: Ab initio TDM curve in real form for the b3Π–a3Δ transition of ZrO calculated in this work by S. R. Langhoff & C. W. Bauschlicher (1990), and by A. N. Perri et al. (2023). The y-axis is in atomic units (a.u.) with 1 a.u. = 2.542 D.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The b3Π–a3Δ and b3Π–X1Σ+ Band Systems of ZrO
Authors: Manish Bhusal, Peter F Bernath, Jacques Liévin, Léo Lavy
Figure caption: This figure provides a comparison of the line positions for the 0–0 band with those reported in A. N. Perri et al. (2023). Figure (a) illustrates the differences in line positions observed in this analysis compared to those reported in A. N. Perri et al. (2023) for the P, Q, and R branches in the 3Π2–3Δ3 and 3Π1–3Δ2 subbands. Figures (b) and (c) show the differences in line positions for the P, Q, and R branches in the 3Π0–3Δ1 subband. It is to be noted that the parities of the lines from A. N. Perri et al. (2023) were reversed before making the comparison (see text for details).
Paper: The b3Π–a3Δ and b3Π–X1Σ+ Band Systems of ZrO
Authors: Manish Bhusal, Peter F Bernath, Jacques Liévin, Léo Lavy
Figure caption: The spectrum of ZrO (above) and simulation (below) for the 3Π2−3Δ3 subband of the 0–0 band of b3Π–a3Δ transition. Note that the lambda doubling in the 3Π2−3Δ3 subband appears only for high J transitions (e.g., R3f(92) and R2e(92) in the figure) and is not well resolved for the low J transitions in the figure.
Paper: The b3Π–a3Δ and b3Π–X1Σ+ Band Systems of ZrO
Authors: Manish Bhusal, Peter F Bernath, Jacques Liévin, Léo Lavy
Figure caption: The above figure compares the Einstein A values for the 0–0 band of the b3Π–a3Δ transition from this analysis with those from A. N. Perri et al. (2023). Figure (a) shows the plot of the ratio of Einstein A from this analysis and that from A. N. Perri et al. (2023) versus rotational quantum number (J) for the P, Q, and R branches in the 3Π2–3Δ3 and 3Π1–3Δ2 subbands, whereas Figure (b) illustrates it for the 3Π0 –3Δ1 subband.
Paper: The b3Π–a3Δ and b3Π–X1Σ+ Band Systems of ZrO
Authors: Manish Bhusal, Peter F Bernath, Jacques Liévin, Léo Lavy
Figure caption: The line positions and Einstein A values from this analysis are compared to those from J. Zhang et al. (2025) in the figure above. Figure (a) illustrates the comparison of line positions for the P, Q, and R branches of the 0–0 band of the b3Π–a3Δ transition, and Figure (b) shows the comparison of the Einstein A values for the same branches.
Paper: The b3Π–a3Δ and b3Π–X1Σ+ Band Systems of ZrO
Authors: Manish Bhusal, Peter F Bernath, Jacques Liévin, Léo Lavy
Figure caption: The spectrum of ZrO and the simulation for the 0–0 band of the b3Π1–X﹩{}^{1}{{\rm{\Sigma }}}_{0}^{+}﹩ transition is presented in the figure above. The brown color represents the experimental spectrum, while the blue color indicates the simulated spectrum.
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: [O/Fe] as a function of [Fe/H] (left) and ﹩12+{\mathrm{log}}({\rm{O}}/{\rm{H}})﹩ (right). The star symbols, cross symbols, and magenta-shaded region are the same as in Figure 5. The cyan and orange squares represent measurements for the composite spectra of star-forming galaxies at z ∼ 2–3 (C. C. Steidel et al. 2016; F. Cullen et al. 2021; D. Kashino et al. 2022) and z ~ 6 (Y. Harikane et al. 2020), respectively. The orange circle and diamond indicate measurements for the z ∼ 6 galaxies, GS_3073 (X. Ji et al. 2024) and GS9422 (S. Tacchella et al. 2025), respectively. The yellow, green, blue, and gray circles denote measurements for MW stars (J. Meléndez et al. 2003; E. Carretta et al. 2005, 2010; D. Yong et al. 2005, 2008; A. Lecureur et al. 2007; L. Pasquini et al. 2008; E. Valenti et al. 2011; T. Bensby et al. 2013; G. Zhao et al. 2016; A. M. Amarsi et al. 2019) in the bulge, thick disk, thin disk, and halo, respectively. The white circles present measurements of metal-poor stars in the Sculptor galaxy (V. Hill et al. 2019; B. Tang et al. 2023). The gray dashed lines denote the solar abundance ratios.
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: Fe/H ratio as a function of absolute UV magnitude. The magenta (red) star symbols represent well-constrained stellar abundance ratios for GN-z11 (GS-z11-0 and GS-z9-0). The cross symbols indicate the stellar abundance ratios, whose posterior distributions are either bimodal or truncated near the lower bound. The magenta-shaded region represents our measurement of GN-z11 with the AGN models.
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: Overview of the construction processes for the PISN and SN Ia models. Top left: initial mass function. The purple, black, green, and orange lines show the top-heavy, E. E. Salpeter (1955), P. Kroupa et al. (1993), and top-light IMFs, respectively. Top right: stellar lifetime as a function of stellar mass. The black line is derived with stellar evolution models (P. Padovani & F. Matteucci 1993; K. Takahashi et al. 2018). Bottom left: DTD for SNe Ia. The distributions are approximated by power-law functions of ∝ t−1 (e.g., S. A. Rodney et al. 2014). The solid, dashed, and dotted lines correspond to minimum delay times of ﹩{t}_{{\rm{\min }}}=100﹩, 50, and 30 Myr, respectively. Bottom right: [O/Fe] ratio as a function of stellar age. The black line represents an example SN Ia model with a delay time of ﹩{t}_{{\rm{\min }}}=100\,{\rm{Myr}}﹩, assuming a constant star formation history.
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: Results of fitting for GN-z11 with AGN models. The black and red solid lines present the observed grating spectrum and best-fit model spectrum, respectively. The green, blue, yellow, and purple dashed lines indicate the best-fit power-law continuum, Balmer continuum, Fe II emission, and Mg II emission, respectively.
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: Abundance diagnostic diagram. The grid lines show the calculated EW(Mg II) and EW(Fe II) as functions of Mg/Fe (=10[Mg/Fe]) and [Fe/H] (H. Sameshima et al. 2017; see Section 3.2). The red-shaded region denotes the measurements of GN-z11 with the AGN models.
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption:                         Posterior PDF of the fitting parameters obtained for the grating spectrum of GN-z11 with the AGN models. The symbols are the same as in Figure 4.