adsabs/AstroCLIMB huggingface dataset:
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for H2O. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The results of applying the SYSREM algorithm to five orders of the data. The panels are as described in the caption of Figure 25. One order at the blue end of this plot was excluded from our analysis. Note that the y-axis scale in the bottom plot differs from that in Figure 25.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Ca I. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Fe II. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Ti II. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The results of applying the SYSREM algorithm to five orders of the data at the red end of the spectrum. The panels are as described in the caption of Figure 25. Note that the y-axis scale in the bottom plot differs from that in Figure 25. Note as well the rise in the standard deviation around 940 nm due to greater telluric contamination.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The 2D K  p –RV maps for species that were not detected in this analysis. All plots were made using the 2000 K template; higher-temperature templates also resulted in nondetections. The species is indicated in the top right corner. The white lines indicate the expected K  p  and RV of the signal.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The results of applying the SYSREM algorithm to five orders of the data. The panels are as described in the caption of Figure 25. Note that the y-axis scale in the bottom plot differs from that in Figure 25. Note as well the rise in the standard deviation around 760 nm due to greater telluric contamination.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The 2D K  p –RV maps for species that were not detected in this analysis. The figures are as described in the caption of Figure 30.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The results of applying the SYSREM algorithm to five orders of the data. The panels are as described in the caption of Figure 25. Note that the y-axis scale in the bottom plot differs from that in Figure 25.
Paper: Rovibrational Spectroscopy of CI Tau—Evidence of a Multicomponent Eccentric Disk Induced by a Planet
Authors: Janus Kozdon, Sean D. Brittain, Jeffrey Fung, Josh Kern, Stanley Jensen, John S. Carr, Joan R. Najita, Andrea Banzatti
Figure caption: The top row is the final snapshot of the hydrodynamic simulation (Section 3.3) with a hypothetical 1 M J planet that may reproduce the disk eccentricities we observed (0.05; Figure 4). The color scale is logarithmic and in units of CO molecules cm−2. The left and right panels are the same picture in Cartesian and polar coordinates, respectively. The white dashed line traces the orbit of the simulated planet. In this case, the outer disk develops an eccentricity similar to the planet’s, while the eccentricity of the inner disk is more subtle. The bottom row plots the azimuthally averaged CO column density profile. The orange solid curve is taken from the same simulation and time-averaged over the last orbit; the orange dashed curve represents the unperturbed disk; and the green solid curve is the emission we detected (Table 4; Section 3.2.1). A τ = 1 region was calculated for the P(20)–P(40) transitions and plotted as the red region (Section 3.3). The simulated profile (orange) is normalized so that, even at the bottom of the planetary gap, it lies above our detected CO column, illustrating that even though the gap is depleted by a factor of ∼100, its 12CO emission can remain optically thick (Section 3.3).
Paper: Rovibrational Spectroscopy of CI Tau—Evidence of a Multicomponent Eccentric Disk Induced by a Planet
Authors: Janus Kozdon, Sean D. Brittain, Jeffrey Fung, Josh Kern, Stanley Jensen, John S. Carr, Joan R. Najita, Andrea Banzatti
Figure caption: The 2022 average stacked emission line profile of the high-J 12CO lines is plotted with best-fit synthetic data alongside residuals (Section 3.2). The top left panel is a circular disk (Section 3.2.1) fit that fails to replicate certain asymmetric features (see Table 4 for the best-fit parameters). The bottom left panel is the multicomponent disk fit (Section 3.2.2), which allowed for the inner and outer components of the disk to contribute independently and provide a much better fit (see Table 4 for the best-fit parameters). The right panel is a visual of the best-fit multicomponent disk where the inner and outer components are eccentric and antiparallel.
Paper: Rovibrational Spectroscopy of CI Tau—Evidence of a Multicomponent Eccentric Disk Induced by a Planet
Authors: Janus Kozdon, Sean D. Brittain, Jeffrey Fung, Josh Kern, Stanley Jensen, John S. Carr, Joan R. Najita, Andrea Banzatti
Figure caption: 2022 average M-band spectrum of CI Tau (described in Section 3). Captured are the 12CO emissions originating from the disk’s surface. The low-J transitions (﹩\tilde{\nu }\geqslant 2058﹩ cm−1) have a superimposed narrow absorption feature indicative of lower-temperature gas of the same species being present in the foreground. The most prominent feature is the hydrogen Pfβ line at 2147.8 cm−1, which is used to infer stellar accretion rates (Section 3.1).
Paper: Rovibrational Spectroscopy of CI Tau—Evidence of a Multicomponent Eccentric Disk Induced by a Planet
Authors: Janus Kozdon, Sean D. Brittain, Jeffrey Fung, Josh Kern, Stanley Jensen, John S. Carr, Joan R. Najita, Andrea Banzatti
Figure caption: The normalized line profiles of CI Tau (described in Section 3) with the 2022 average (red). The two left panels display the 12CO low-J and high-J lines where the 2022 epochs (#4–12) remained consistent but a clear variation is present when compared to the earlier epochs #1–3. The right panel displays the hydrogen Pfβ line where variation was observed between each epoch and the next.
Paper: Rovibrational Spectroscopy of CI Tau—Evidence of a Multicomponent Eccentric Disk Induced by a Planet
Authors: Janus Kozdon, Sean D. Brittain, Jeffrey Fung, Josh Kern, Stanley Jensen, John S. Carr, Joan R. Najita, Andrea Banzatti
Figure caption: The equivalent widths (Section 3.1) of the average 12CO lines and the hydrogen line (see Table 3) with the 2022 averages plotted as the horizontal dashed lines (12COavg = 21.8 km s−1 and Havg = 73.7 km s−1). In the 2022 epochs (#4–12) we see the hydrogen vary with a possible nine-day period whereas the 12CO stayed consistent. The 2022 epochs are noticeably different from the earlier ones.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Sample results of running the simulation-based calibration procedure on a model consisting of a single planet parameterized with Thiele-Innes elements (A, B, F, G, etc.) and position angle θ. Each count represents a model fit to a different simulated system. The horizontal band gives a 99% range around the expected value for a perfect sampling procedure. The observation epochs and uncertainties are taken from Table 1.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Corner plot of key orbital parameters for the case shown in Figure 4 compared between three packages: orvara, orbitize!, and Octofitter. The semimajor axis is plotted on a log scale to reveal how the sampler behavior differs in the long tail. Though we expect all packages to eventually converge to near-identical results, we find that there are small differences in the ω, a, and e marginal posteriors that persist even after running for multiple days.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Comparison between packages of the average time until chains converged to a stationary distribution and the rate at which independent posterior samples are generated. The effective sample size (ESS) rate was measured separately using the bulk and tail methods of MCMCDiagnostics.jl. Note that the ﹩\hat{R}﹩ and ESS of the slowest variable for a given sampler are used as this is what ultimately limits sampling performance. These results are based on the astrometry presented in Table 1 and are expected to depend strongly on hardware, input data, and choice of priors.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Posterior density of photometry vs. semimajor axis for a simulated detection and nondetection. The solid lines mark the mean of the marginal photometry posterior, and the dashed lines mark ±1σ. We consider a planet detected when the S/N based on the photometry marginalized over all other parameters is greater than some chosen threshold, e.g., 5σ.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Conceptual schematic of three different ways to use Octofitter. Other possibilities, like combining images with Doppler or astrometric velocimetry or using a mix of relative astrometry and images without detections to constrain orbits, are also possible.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Orbit fitting posteriors visualized in the plane of the sky, compared between three packages: orvara, orbitize!, and Octofitter.
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Amplitude per radial mode for stars observed by Kepler (blue circles; Huber et al. 2011) compared to the upper amplitude limits derived from TESS for stars with 20 s cadence data that fall along evolutionary sequences for our spectropolarimetric targets (orange triangles). Note that the upper limit for ϵ Eri is off scale at 30.5, far above the markers in the legend.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: Plots of the positional uncertainties for the solution S7 from 2010 to 2030 in the heliocentric RTN directions, in which the horizontal axis is taken as the month and the color gradient from dark to light indicates the evolution of the year. The dashed line arrow shows the evolution direction for σ  T .
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: The panels show the uncertainty in the semimajor axis, eccentricity, inclination, and mean longitude, respectively, from 2000 to 2200. The results in blue are computed using the full planetary gravitational perturbation model, and the red ones exclude the Earth perturbation.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: The time evolution of ﹩\tfrac{\partial \lambda \left(t\right)}{\partial {a}_{0}}﹩ and ﹩\tfrac{\partial \lambda \left(t\right)}{\partial {A}_{2}}﹩ for the two force models from 2000 to 2200, in which the initial epoch is 2023 February 25 00:00:00 TDB.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption: The ring model for a rotational temperature of 1500 K and a density of 1.6 × 1018 cm−2 plotted with solid lines on the data points plotted in Figure 3. The model matches the 1–0 data quite well except at the highest energies, where it underestimates the line strength. It also underestimates the line strength at the higher vibrational states, suggesting that the excitation of these lines is dominated by fluorescence. The model overestimates the 2–1 data, most likely because its emitting area is smaller than that of 1–0. The model calculations show that the 13CO abundance needs to be increased by a factor of 6–7 compared to normal interstellar abundances.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption: Median line profiles of 12CO υ = 1–0 and 2–1 and 13CO 1–0 and 12CO 2–0 emission lines. The dashed blue line is the 12CO 2–1 profile scaled by 2.25, the dashed red line is the 13CO 1–0 profile scaled by 3, and the dashed orange line is the scaled 12CO 2–0. The scaled profiles demonstrate the differences in widths compared to the 12CO 1–0 profile.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption: Rotational diagram with the observed data points plotted with large filled circles. The line bands are identified by their colors in the lower left corner of the plot. For almost all of the data, the error bars are smaller than the circle size.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption: The CO overtone bands observed with iSHELL in K band showing a large number of double-peaked lines. The 2–0 bandhead at 2.29 μm is very weak.
Paper: A Crater Chronology for the Jupiter’s Trojan Asteroids
Authors: S. Marchi, D. Nesvorný, D. Vokrouhlický, W. F. Bottke, H. Levison
Figure caption: Trojans–Trojans MPFs for 4.4 Ga, compared with Mathilde cratering (see text). We report the results for three different scaling laws. The CS scaling with Y = 10 kPa strength comes closer to Mathilde cratering. Crater saturation is indicated by shaded area (black line corresponds to 10% of geometric saturation; see Marchi et al. 2015).
Paper: A Crater Chronology for the Jupiter’s Trojan Asteroids
Authors: S. Marchi, D. Nesvorný, D. Vokrouhlický, W. F. Bottke, H. Levison
Figure caption: Comets–Trojans MPFs for 4.4 Ga, compared with Mathilde cratering (see text). Compare to Figure 6 for Trojans–Trojans cratering for the same crater scaling laws. Crater saturation is indicated by shaded area (black line corresponds to 10% of geometric saturation; see Marchi et al. 2015).
Paper: A Crater Chronology for the Jupiter’s Trojan Asteroids
Authors: S. Marchi, D. Nesvorný, D. Vokrouhlický, W. F. Bottke, H. Levison
Figure caption: Trojan model production functions (MPFs) for cratering from Trojans and comets. Solid and dashed curves are for 4 and 1 Ga, respectively. This is for scaling law CS, Y = 10 kPa (see Figure 4).
Paper: An Exploration of AGN and Stellar Feedback Effects in the Intergalactic Medium via the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Sultan Hassan, Rachel S. Somerville, Romeel Davé, Federico Marinacci, Lars Hernquist, Mark Vogelsberger
Figure caption: Same as Figure 4 but fitting the results of each parameter variation to the observational data by allowing the strength of the UVB to vary. A table including the UVB correction value and reduced χ 2 values for the fit can be found in Table 2 in Appendix B.
Paper: An Exploration of AGN and Stellar Feedback Effects in the Intergalactic Medium via the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Sultan Hassan, Rachel S. Somerville, Romeel Davé, Federico Marinacci, Lars Hernquist, Mark Vogelsberger
Figure caption: The CDD for all the CAMELS CV set simulations for both the SIMBA and IllustrisTNG suites. The solid black lines are the median of the CAMELS CV CDDs, the shaded region is the 90th percentile range of the CV CDDs, and the dashed red lines are the original Simba and TNG300-1 simulations. Variations in the CDDF due to varying initial conditions result in a maximum shift in the overall normalization by 0.25 dex. Both the original Simba and TNG300-1 simulations are largely contained within the allowed variation of the CDD due to cosmic variance.
Paper: An Exploration of AGN and Stellar Feedback Effects in the Intergalactic Medium via the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Sultan Hassan, Rachel S. Somerville, Romeel Davé, Federico Marinacci, Lars Hernquist, Mark Vogelsberger
Figure caption: The redshift evolution of the SIMBA (black solid line) and TNG (red dashed lines) simulation column density distributions. The TNG CDD has been adjusted so as to use the same Haardt & Madau (2012) UVB model as used in Simba. This has been done to more accurately determine what differences are caused by either feedback or large-scale environment as opposed to the ionizing background.
Paper: An Exploration of AGN and Stellar Feedback Effects in the Intergalactic Medium via the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Sultan Hassan, Rachel S. Somerville, Romeel Davé, Federico Marinacci, Lars Hernquist, Mark Vogelsberger
Figure caption: Similar to Figure 6 but instead for the CAMELS-TNG simulations. The top row displays the SMBH accretion rate density for the thermal feedback mode. The bottom row displays the total number of SMBHs (solid lines) along with the number of SMBHs in the thermal mode (dashed lines). The results for variations in the AGN feedback parameters are not shown, since those statistics are largely unaffected.
Paper: An Exploration of AGN and Stellar Feedback Effects in the Intergalactic Medium via the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Sultan Hassan, Rachel S. Somerville, Romeel Davé, Federico Marinacci, Lars Hernquist, Mark Vogelsberger
Figure caption: Same as Figure 11, but instead for the b-value distribution. The blue points are observational data from Danforth et al. (2016). The b-value distributions are calculated only for absorbers in the column density range corresponding to the observational data as written in the figure panels. The x-axis range ends at 100 km s −1, to avoid blends of multiple lines and continuum-fitting errors.
Paper: An Exploration of AGN and Stellar Feedback Effects in the Intergalactic Medium via the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Sultan Hassan, Rachel S. Somerville, Romeel Davé, Federico Marinacci, Lars Hernquist, Mark Vogelsberger
Figure caption: The redshift evolution of the total number of absorbers per redshift distance for CD bins of 1012 < N HI < 1014 cm−2 and 1014 < N HI < 1017 cm−2. Results from CAMELS-Simba and CAMELS-TNG are shown. The dotted gray line marks z = 0.7, the threshold at which the shape of the CDDs diverge significantly between Simba and TNG. Like in Figure 9, the CAMELS-TNG data are corrected in post-processing to utilize the Haardt & Madau (2012) UVB for comparison to the CAMELS-Simba data.