adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Masses of the three observed HMXB BHs (red error bars), compared to the mass function of field BBHs (left-hand panel) and dynamical BBHs (right-hand panel) from GW population inference. Left-hand panel: The green dashed region shows the 90% credible interval of the inferred primary-mass function of the 1st subpopulation; the blue lines and dashed regions show the median and 90% credible intervals of the CDF curves of three random draws from the 1st subpopulation. Right-hand panel: The pale-green regions are the inferred mass function of the low-spin BHs in the 2nd subpopulation, while the sandy-brown regions are the modified mass function with α = α 2nd,LS + 2, indicating the initial mass function of BHs in the environment for dynamical channels (R. M. O’Leary et al. 2016).
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Reconstructed primary-mass, spin-magnitude, and cosine-tilt-angle distributions of the low-spin BBHs for each subpopulation inferred with MAIN MODEL; the upper panel shows the differential local-universe merger rate as a function of primary mass. The solid curves are the mean values and the colored bands are the 90% credible intervals; the insets are for the mass-ratio distributions of the two subpopulations.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Posterior distributions of the power-law slopes of (underlying) component-mass distributions and pairing function of the two subpopulations; the dashed and solid contours mark the central 50% and 90% posterior credible regions, respectively. The black curves are for the inference using the MAIN MODEL with hierarchical mergers, while the orange curves are for the inference using the EXTEND DEFAULT model without high-spin events.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Reconstructed (underlying) component-mass distributions (before paired). The solid curves are the mean values and the colored bands are the 90% credible intervals; the inset is for the spin-magnitude distributions.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Reconstructed primary-mass, spin-magnitude, and cosine-tilt-angle distributions of BBHs for each population, inferred with the EXTEND DEFAULT model. The upper panel shows the differential local-universe merger rate as a function of primary mass. The solid curves are the mean values and the colored bands are the 90% credible intervals; the insets are for the mass-ratio distributions of the two subpopulations.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Posterior distribution of main parameters describing the full BBH population, inferred with the MAIN MODEL; the dashed lines in the marginal distribution represent the 90% credible intervals.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7 but for the restriction of σ t < 0.5.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Posterior distributions of all the hyperparameters describing the two subpopulations, inferred with the EXTEND DEFAULT model; the dashed lines in the marginal distribution represent the 90% credible intervals.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7, but for the case with variable μ t.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Posterior distributions of the μ t and σ t describing the ﹩\cos {\theta }_{\mathrm{1,2}}﹩ distribution of the nearly aligned subpopulation; the dashed lines in the marginal distribution represent the 90% credible intervals.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The mass of 99th percentile and the maximum mass of the field BBHs, inferred with the MAIN MODEL.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Posterior distribution of the main hyperparameter describing the two subpopulations, inferred without ﹩\cos {\theta }_{2}﹩ information.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7, but for the inference with only ﹩\cos {\theta }_{1}﹩ distribution.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7, but for the inference with the full catalog.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7, but for the inference with nonparametric ﹩\cos \theta ﹩-distribution in [0, 1]. The mass distributions of the two subpopulations are rather similar to those inferred using the EXTEND DEFAULT model with σ t < 0.5.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7, but for the inference with nonparametric ﹩\cos \theta ﹩-distribution in [−1, 1]. The mass distributions of the two subpopulations are similar to those inferred using the EXTEND DEFAULT model.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7, but for the inference without selection effects.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 7, but for the analysis with mock data where the injections having features found in this work.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 20, but for injections that do not have features found in this work.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: Spin-magnitude distributions of BBHs in the nearly aligned and isotropic-spin subpopulation. The solid curves are the medians and the colored bands are the 90% credible intervals.
Paper: Exploring Field-evolution and Dynamical-capture Coalescing Binary Black Holes in GWTC-3
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Shi-Jie Gao, 世杰 高, Dao-Cheng Wu, 道成 伍, Yuan-Zhu Wang, 远瞩 王
Figure caption: The same as Figure 18, but for the inference with constraint σ t < 0.5.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The face-on (xy-projected) view of different AGN jet simulations with high-energy flux. Each row represents a different AGN jet simulation. From top to bottom, rows present the precessing kinetic jet, thermal jet, cosmic-ray jet, and the fiducial simulation with no jet for comparison purposes. Each column represents a different parameter constraint applied during the post-processing. In each column, from left to right, we present the logarithm of the overall gas mass density, the O VIII surface mass density, the O VI surface mass density, the Mg II surface mass density, and gas temperature, respectively. The color bars depicted at the bottom of the figure show the intensity of each projection map. All snapshots shown occur at the t = 1 Gyr point in the simulations.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The edge-on (yz-projected) view of different AGN jet simulations with low-energy flux. Each row represents a different AGN jet simulation. From top to bottom, the rows present the precessing kinetic jet, thermal jet, cosmic-ray jet, and the fiducial simulation with no jet for comparison purposes. Each column represents a different parameter constraint applied during the post-processing. In each column, from left to right, we present the logarithm of the overall gas mass density, the O VIII surface mass density, the O VI surface mass density, the Mg II surface mass density, and gas temperature, respectively. The color bars depicted at the bottom of the figure show the intensity of each projection map. All snapshots shown occur at the t = 1 Gyr point in the simulations.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The face-on (xy-projected) view of different AGN jet simulations with low-energy flux. Each row represents a different AGN jet simulation. From top to bottom, the rows present the precessing kinetic jet, thermal jet, cosmic-ray jet, and the fiducial simulation with no jet for comparison purposes. Each column represents a different parameter constraint applied during the post-processing. In each column, from left to right, we present the logarithm of the overall gas mass density, the O VIII surface mass density, the O VI surface mass density, the Mg II surface mass density, and gas temperature, respectively. The color bars depicted at the bottom of the figure show the intensity of each projection map. All snapshots shown occur at the t = 1 Gyr point in the simulations.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The radial distribution of the median of the mass density (top row) and the ion-to-element mass ratio (bottom row) from all snapshots for Mg II (left panel), O VI (middle panel), and O VIII (right panel), respectively. These plots are indicative of the MSA method, where we pick the time median of the profile obtained from each snapshot. The radius of 101 kpc indicates the approximate edge of the galactic disk in each simulation.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: Left panel: median gas mass density in the galaxy to distance from the center of the galaxy along the x-axis. Middle panel: the median temperature vs. the radial profile. Right panel: the median temperature vs. the distance from the z-axis. Overlaid in each panel, we present different simulations using different colored lines. The panels show a grouping of behavioral patterns between jets of similar energy fluxes, where low-energy jets display lower overall temperatures but higher median gas mass density across all runs, while high-energy jets have a higher overall temperature but a lower median mass density. These plots are indicative of the MSA method, where we pick the time median of the profile obtained from each snapshot. The radius of 101 kpc indicates the approximate edge of the galactic disk in each simulation.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The edge-on (yz-projected) view of different AGN jet simulations with high-energy flux. Each row represents a different AGN jet simulation. From top to bottom, the rows present the precessing kinetic jet, thermal jet, cosmic-ray jet, and the fiducial simulation with no jet for comparison purposes. Each column represents a different parameter constraint applied during the post-processing. In each column, from left to right, we present the logarithm of the overall gas mass density, the O VIII surface mass density, the O VI surface mass density, the Mg II surface mass density, and gas temperature, respectively. The color bars depicted at the bottom of the figure show the intensity of each projection map. All snapshots shown occur at the t = 1 Gyr point in the simulations.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The depiction of the mass ratio for the disk (top panel) and the jet (bottom panel). From the left to right, we present Mg II, O VI, and O VIII, respectively. Plots are indicative of the MSA method, where we pick the time median of the profile obtained from each snapshot.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: A cartoon picture of the criteria for successful jet models.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The thermal jet propagation at several distinct snapshots. Each panel displays the mass-weighted temperature map in the y–z projection. The t value corresponds to the time in the simulation of each snapshot.
Paper: Strong Chemical Tagging in FIRE: Intra- and Intercluster Chemical Homogeneity in Open Clusters in Milky Way–like Galaxy Simulations
Authors: Binod Bhattarai, Sarah R. Loebman, Melissa K. Ness, Andrew Wetzel, Emily C. Cunningham, Hanna Parul, Alessa Ibrahim Wiggins
Figure caption: Scatter plot of the mean [Fe/H] vs. birth radius of OCs from three simulations: m12i (top panel), m12f (middle panel), and m12m (bottom panel). The blue dots indicate the mean [Fe/H] of each cluster and the solid black curve represents the median trend for data in 0.5 kpc radial bins. The gray shaded area represents the ±1σ range within 0.5 kpc bins. The blue horizontal line represents the average of all OCs in the sample, and the blue horizontal shaded region represents the typical ±1σ scatter of [Fe/H] within any given cluster. It can be seen that the metallicity distribution varies differently in the inner disk than the outer, and many clusters have a similar mean [Fe/H], despite being found at varying locations across the disk.
Paper: Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies
Authors: Nadia Qutob, Razieh Emami, Kung-Yi Su, Randall Smith, Lars Hernquist, Dian P. Triani, Cameron Hummels, Drummond Fielding, Philip F. Hopkins, Rachel S. Somerville, David R. Ballantyne, Mark Vogelsberger, Grant Tremblay, James F. Steiner, Douglas Finkbeiner, Ramesh Narayan, Minjung Park, Josh Grindlay, Priyamvada Natarajan, Christopher C. Hayward, Dušan Kereš, Sam B. Ponnada, Sirio Belli, Rebecca Davies, Gabriel Maheson, Letizia Bugiani, Yijia Li
Figure caption: The depiction of the mass density for the disk (top panel) and the jet (bottom panel). From the left to right, we present Mg II, O VI, and O VIII, respectively. These plots are indicative of the MSA method, where we pick the time median of the profile obtained from each snapshot.
Paper: Strong Chemical Tagging in FIRE: Intra- and Intercluster Chemical Homogeneity in Open Clusters in Milky Way–like Galaxy Simulations
Authors: Binod Bhattarai, Sarah R. Loebman, Melissa K. Ness, Andrew Wetzel, Emily C. Cunningham, Hanna Parul, Alessa Ibrahim Wiggins
Figure caption: Number of young (<3 Myr) massive OCs identified in the last ∼100 Myr of the simulations. OC selection has been run at a 3 Myr interval to avoid double counting. m12i is indicated by the dashed lines colored in indigo, m12f is indicated by the dashed–dotted lines colored in red, and m12m is indicated by the solid blue lines. A varying rate of star cluster formation is observed in all three simulations, with m12m having the lowest number of clusters produced throughout the 100 Myr period. This reflects a globally suppressed SFR for m12m at the present day. See Section 2.2 for further discussion.
Paper: Strong Chemical Tagging in FIRE: Intra- and Intercluster Chemical Homogeneity in Open Clusters in Milky Way–like Galaxy Simulations
Authors: Binod Bhattarai, Sarah R. Loebman, Melissa K. Ness, Andrew Wetzel, Emily C. Cunningham, Hanna Parul, Alessa Ibrahim Wiggins
Figure caption: Snapshots from three Latte simulations of m12i, m12f, and m12m. Background: mean [Fe/H] for gas in the disk of each simulation. The corresponding values are shown by the color bar on the left. Contours: density of stars < 50 Myr old that highlight the spiral arms. Circles: mean [Fe/H] of OCs and associations identified at 13.693 Gyr. Note that the mean [Fe/H] of the clustered star formation reflects the global metallicity distribution of the gas in the disk.
Paper: Strong Chemical Tagging in FIRE: Intra- and Intercluster Chemical Homogeneity in Open Clusters in Milky Way–like Galaxy Simulations
Authors: Binod Bhattarai, Sarah R. Loebman, Melissa K. Ness, Andrew Wetzel, Emily C. Cunningham, Hanna Parul, Alessa Ibrahim Wiggins
Figure caption: The [Fe/H] distribution for a subset of OCs from the subsample highlighted in blue from Figure 5 for each simulation. Each smoothed histogram represents the metallicity distribution for a single OC and was generated using Gaussian kernel smoothing. The shaded region indicates the ±1σ from the overall mean of the distribution of all clusters from that simulation. Despite their locations in the disk, it is possible to find OCs that have similar abundance distributions at different R.
Paper: Strong Chemical Tagging in FIRE: Intra- and Intercluster Chemical Homogeneity in Open Clusters in Milky Way–like Galaxy Simulations
Authors: Binod Bhattarai, Sarah R. Loebman, Melissa K. Ness, Andrew Wetzel, Emily C. Cunningham, Hanna Parul, Alessa Ibrahim Wiggins
Figure caption: Mass distribution of the OCs from all three simulations. m12i is indicated by the dashed lines colored in indigo, m12f is indicated by the dashed–dotted lines colored in red, and m12m is indicated by the solid blue lines. The slope of the cluster-mass function is similar for all three simulations, with m12i having a shallower slope with a few high-mass outliers.