adsabs/AstroCLIMB huggingface dataset:
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different schemes for calculating boundaries of convective regions (line style and color).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different schemes for calculating boundaries of convective regions (line style and color) with convective core overshooting.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different solar mixtures of heavy elements (line style and color) with convective core overshooting.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different nuclear reaction rates and nuclear net settings (line style and color) with convective core overshooting.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different methods for interpolating opacity tables (line style and color) with convective core overshooting.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different atmosphere settings (line style and color) with convective core overshooting.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and atomic diffusion included or not (line style and color) with convective core overshooting.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different MLT settings (line style and color) with convective core overshooting.
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: The relative sizes of the proposal distributions of four model parameters (planetary masses and orbital periods) and the resulting acceptance rates for each of the 2000 batches in four neighboring parallel tempering chains with β values equal to 0.05, 0.1. 0.4, and 1.0. Note that, for the chain with a β of 1.0, the mass and period of the first planet have similar relative proposal sizes, while the relative proposal sizes of the mass and period of the second planet differ by a factor of 1000. Nii-C can efficiently determine the optimal proposal sizes for all model parameters. The end of the tuning stage is indicated by the vertical dashed lines.
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: Nii-C fits a linear regression relationship to the simulated data points. The left panel shows the corner plots of the fit. The posterior means and 1σ locations of the parameters a, b, and σ  y  are consistent with the original model that generated the data. The right panel shows the simulated data as blue points and the linear relationship given by the posterior means of the fitted parameters as a red line. The red dashed lines indicate the locations of a standard deviation according to the fitted σ  y .
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: Corner plot of the marginal distributions of the fitted parameters in the hierarchical radius relationship model. The distribution of hot Jupiters in the planetary radius vs. incoming flux space is shown in the top right panel, along with the fitted power-law relationship (red line) and the locations corresponding to one standard deviation (red dashed lines).
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: Corner plot of the marginal distributions of all 15 parameters in the orbit fitting of a two-planet system. The top right panel shows the comparison between the simulated observation and the theoretical signals generated using the fitted parameters.
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: The left panel shows the corner plots of the sampling results of the curved likelihood obtained by Nii-C, while the right panel shows the results obtained by PTMCMCSampler.
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: The left panel displays the theoretical distribution given by Equation (9). The right panel shows the number of effective sampling points obtained by 15 walkers using Nii-C, configured as a basic parallel MCMC code, in each of the 250 grids in the X–Y plane.
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: The workflow of Nii-C code.
Paper: New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9
Authors: C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel
Figure caption: Ten of the 1512 new strong lens candidates discovered in this work. The naming convention is R.A. and decl. in decimal format. For all images, north is up, and east to the left. The top right corner of each image indicates the grade; bottom left corner, the region/The Tractor type, and the photometric redshift of the putative lens (z  d ). First column: doubly lensed systems. Second column: quadruply lensed systems. Third column: arc–counterarc systems, each of which has a large arc with a smaller counterarc on the opposite side of the lens. Fourth column: high-redshift lensing systems, each of which has quadruple images. The image locations of DESI-030.4758-45.3282 suggests a fold configuration where DESI-022.0258+09.2466 shows a cross or cusp configuration (see Gu et al. 2022). These eight systems all have a single galaxy as the lens. Fifth column: group/cluster lensing systems. Putative arcs are indicated with white arrows. For DESI-031.1951+15.4749, the large lensed arc due to the galaxy group potential is also lensed by a group member, forming two small arcs to its left and right (for another example, see Huang et al. 2009). This would enable a lensing-mass measurement of the substructure. Note that this system also has a high z  d  of 0.755. DESI-030.7884-20.2881 is a cluster lensing system with a faint but spectacularly large blue arc to the lower left (marked by two yellow arrows to indicate its extent). There are hints of even fainter arcs around the cluster center. High-resolution imaging will almost certainly reveal more arcs.
Paper: New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9
Authors: C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel
Figure caption: Left: the cross-entropy loss for the training and validation sets for the full 180 epochs of training. The vertical dashed black line at epoch 145 indicates the epoch of the trained model that achieved the highest area under the ROC curve (AUC). We used the trained model at this epoch in the deployment. Right: the ROC curve for the validation set using the best-performing model (epoch 145).
Paper: New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9
Authors: C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel
Figure caption: The DESI Legacy Imaging Surveys DR9 footprint in an equal-area Aitoff projection in equatorial coordinates. The blue border approximately outlines the MzLS/BASS region and the rest is DECaLS. The gray shading indicates the z-band 5σ magnitude limit for a galaxy (0.″45 round exponential profile) at randomly sampled points across the entirety of the DESI Legacy Surveys footprint. The contiguous region with a magnitude limit of ∼23.6 represents the original DES footprint. Note that, prior to DR9, the DES region of DECaLS at δ ≲ −32° was not entirely reprocessed by the Legacy Surveys imaging team. The footprint of the Legacy Surveys DR9 now covers ∼19,000 deg2.
Paper: New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9
Authors: C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel
Figure caption: The PRC for the validation set from the fully trained neural network. The black dots from right to left on the curve indicate probability thresholds from 0.1 to 0.9 with a step of 0.1. The red star indicates the selected probability threshold of 0.4 with red dashed lines showing the precision and recall at that point.
Paper: New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9
Authors: C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel
Figure caption: The 1512 new candidate lensing systems discovered in this work by grades over the depth map of the Legacy Surveys DR9 shown in Figure 1.
Paper: New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9
Authors: C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel
Figure caption: All 3057 candidate lensing systems discovered in the Legacy Surveys reported in Papers I (pink), II (purple), and this work (green), over the depth map of the Legacy Surveys DR9 shown in Figure 1.
Paper: New Strong Gravitational Lenses from the DESI Legacy Imaging Surveys Data Release 9
Authors: C. Storfer, X. Huang, A. Gu, W. Sheu, S. Banka, A. Dey, J. Inchausti Reyes, A. Jain, K. J. Kwon, D. Lang, V. Lee, A. Meisner, J. Moustakas, A. D. Myers, S. Tabares-Tarquinio, E. F. Schlafly, D. J. Schlegel
Figure caption: The 1961 lenses included in the training sample over the depth map of the Legacy Surveys DR9 shown in Figure 1.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: Left: the distribution of pulse-rise time is fitted with a log-Gaussian function (the solid red line), with the mean ﹩{12.87}_{-2.24}^{+2.33}﹩ ms (the red dashed line) and standard deviation ﹩{1.44}_{-0.15}^{+0.20}﹩. Right: the distribution of pulse-decay time is also fitted with a log-Gaussian function with the mean (red dashed line) and standard deviation being ﹩{18.16}_{-3.07}^{+3.57}﹩ ms and ﹩{1.58}_{-0.15}^{+0.17}﹩, respectively.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: The distribution of pulse widths, the solid red line represents the fitting curve using a log-Gaussian function with mean ﹩{39.36}_{-4.98}^{+5.60}﹩ ms (the red dashed line) and standard deviation ﹩{1.24}_{-0.12}^{+0.15}﹩.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: Comparison of MVT results obtained using different methods for 27 XRBs. Left: comparison of the pulse-fitting method Δt mvt,24 (this work) with the variance analysis method Δt mvt,13 (P. N. Bhat 2013). Middle: comparison of the Bayesian block method Δt mvt,BB (S. Xiao et al. 2023) with the variance analysis method. Right: comparison of the pulse-fitting method with the Bayesian block method. The red dashed line represents the equivalence line.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: The correlations between the different pulse parameters (i.e., pulse amplitude, pulse width, skewness, rise time, decay time, and pulse peakedness). The red lines represent the fitting lines, while “a” and “b” correspond to the index and constant of the power-law relationship (i.e., y = bx  a ), respectively.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: The distribution of pulse-waiting times between neighboring pulses, the solid red line represents the fitting curve using a log-Gaussian function with the mean of ﹩{34.44}_{-10.10}^{+15.99}﹩ ms (dashed red line) and standard deviation of ﹩{1.97}_{-0.42}^{+0.50}﹩.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: The distribution of skewness; the solid red line represents the fitting curve using a log-Gaussian function with a mean of ﹩{1.66}_{-0.25}^{+0.32}﹩ (the red dashed line) and a standard deviation of ﹩{1.49}_{-0.12}^{+0.13}﹩.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: The distribution of pulse peakedness ν, the solid red line represents the fitting curve using a log-Gaussian function with a mean of ﹩{0.99}_{-0.06}^{+0.06}﹩ (the red dashed line) and a standard deviation of ﹩{0.55}_{-0.05}^{+0.06}﹩.
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: The correlation between left (right) waiting time and pulse parameters (i.e., pulse amplitude, pulse width, skewness, rise time, decay time, and pulse peakedness).
Paper: A Comprehensive Timing Analysis of Individual Pulses in X-Ray Bursts from SGR J0501+4516
Authors: Jiao-Jiao Yang, Shuo Xiao, Zheng-Huo Jiang, Tong-Lei Liao, Mei-Xin Hong, Xi-Hong Luo
Figure caption: Left: distribution of the number of pulses in XRBs, and the vertical dashed line represents the peak of 2. Right: the relationship between burst duration and the number of pulses.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Median (solid line) along with 25th and 75th percentiles (colored regions) for the maximum recorded relative difference distributions for log age (top panels), ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ (middle panels), and ﹩\mathrm{log}\,L﹩ (bottom panels) at progressing evolutionary phases (horizontal axis). The three colors correspond to three metallicities. The left panels correspond to models computed without convective core overshooting, while in the right panels we show results for models computed with convective core overshooting. At each benchmark point statistics are drawn from a set of 23 evolutionary models computed under different assumptions for seven mass values (2–8 M ⊙).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Similar to Figure 8, but here we present the median along with the 25th and 75th percentiles for 2–8 M ⊙ models and three metallicities. The two colors correspond to models with (orange right-slanted lines) and without convective core overshooting (blue left-slanted lines). Numerical data are collected in Table 6.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different methods for interpolating opacity tables (line style and color).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different nuclear reaction rates and nuclear net settings (line style and color).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different solar mixtures of heavy elements (line style and color).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different atmosphere settings (line style and color).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Location of the 2–15 M ⊙ components of the detached eclipsing binaries from DEBCat in the H-R diagram. Overplotted are the reference evolutionary tracks with Z = 0.004 for 2, 5, and 8 M ⊙. The vertical line marks ﹩\mathrm{log}{T}_{\mathrm{eff}}/{\rm{K}}=3.85﹩.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and atomic diffusion included or not (line style and color).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different MLT settings (line style and color).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 9–15 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different resolution settings (line style and color) as in Table 2.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 9–15 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different resolution settings (line style and color) as in Table 2 with convective core overshooting.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different resolution settings (line style and color) as in Table 2 with convective core overshooting.
Paper: The Impact of Positive AGN Feedback on the Properties of Galaxies in a Semianalytic Model of Galaxy Formation
Authors: Emanuele Contini, Sukyoung K. Yi, Seyoung Jeon, Jinsu Rhee
Figure caption: Evolution of the SMF from z = 3 to z = 1, as predicted by ModA (represented by red stars) and ModB (represented by green squares), compared with the set of observations on which FEGA has been calibrated (illustrated by black lines) and described in Section 3.2. Additionally, we compare our predictions with those of two SAMs that feature the same SN feedback as FEGA: the model by M. Hirschmann et al. (2016; depicted by an orange line), which aligns closely with ModA, and the model by B. M. B. Henriques et al. (2020; depicted by a brown line), which aligns closely with ModB. Both ModA and ModB reasonably describe the evolution of the SMF down to z = 1. The effectiveness of the stellar feedback in ModB is evident even at high redshifts. Although ModA exhibits redshift-dependent stellar feedback (stronger at higher redshifts), the two models show differences for stellar masses below ﹩\mathrm{log}{M}_{* }\sim 9﹩.
Paper: The Impact of Positive AGN Feedback on the Properties of Galaxies in a Semianalytic Model of Galaxy Formation
Authors: Emanuele Contini, Sukyoung K. Yi, Seyoung Jeon, Jinsu Rhee
Figure caption: SMF at the present time, as predicted by ModA and ModB, depicted using the same styles and colors as shown in Figure 1. We compare the predictions of these two models with the set of observations used for calibration, as well as with the predictions of M. Hirschmann et al. (2016) and B. M. B. Henriques et al. (2020) (represented by the same colors as in the previous figure). Additionally, we consider another set of observations from different authors: C. Li & S. D. M. White (2009; represented by a cyan line), R. D’Souza et al. (2015; represented by a purple line), and M. Bernardi et al. (2018; represented by magenta lines indicating the ±σ region). It should be noted (see the text for further details) that at z = 0 the calibration encompasses the region of the SMFs by M. Bernardi et al. (2018) for stellar masses ﹩\mathrm{log}{M}_{* }\gtrsim 11﹩. Both ModA and ModB predict the observed SMF accurately, with both models favoring the high-mass end of the M. Bernardi et al. (2018) SMF. This has important consequences for the stellar-to-halo-mass relation.