adsabs/AstroCLIMB huggingface dataset:
Paper: Investigation on the Predictive Potentiality of Photospheric Magnetic Parameters for Distinguishing Confined from Eruptive Solar Flares
Authors: Jinhui Pan, Rui Liu
Figure caption: Distribution of the physical parameters for a subset of flares with high-gradient PILs. The red bars represent eruptive flares and the blue bars the confined flares. The overlapping portion is shown in deep brownish red. The dotted lines indicate the medians of the parameters for eruptive flares (red) and confined flares (blue).
Paper: Ionization Rate of Interstellar Neutral Helium from New Horizons/SWAP Observations
Authors: Małgorzata Antonik, Paweł Swaczyna, David J. McComas, Heather A. Elliott, Maciej Bzowski
Figure caption: Left panel: the time variations of the alpha-to-proton density ratios from SWAP (orange) and from the OMNI 2 database (green). The alpha-to-proton density ratios determined from the SWAP data are larger than those obtained from the OMNI 2 database by the ζ scaling factor. Right panel: the relation between the alpha-to-proton density ratio from SWAP and the OMNI 2 database. The gray dashed line represents ζ = 1. The red line shows the fit of the scaling factor ζ.
Paper: Ionization Rate of Interstellar Neutral Helium from New Horizons/SWAP Observations
Authors: Małgorzata Antonik, Paweł Swaczyna, David J. McComas, Heather A. Elliott, Maciej Bzowski
Figure caption: Left panel: the averaged energy-angle response function RE,θ(E/Estep, θ) obtained based on data from H. A. Elliott et al. (2016). Right panel: the energy-angle response function RE,η(E/Estep, η) for the rotation-averaged FOV used in our analysis. Using this new energy-angle response function simplifies the numerical calculations by eliminating one integration dimension. Instead of integrating over the SWAP θ and ϕ coordinates, it is sufficient to integrate over η.
Paper: Ionization Rate of Interstellar Neutral Helium from New Horizons/SWAP Observations
Authors: Małgorzata Antonik, Paweł Swaczyna, David J. McComas, Heather A. Elliott, Maciej Bzowski
Figure caption: Mapping of the angular distance from the center of the FOV η and rotation angles ψ + ω onto the elevation angle θ (left panel) and azimuthal angle ϕ (right panel). During a full rotation of the spacecraft around its axis, a given angular distance from the SWAP FOV center, η, corresponds to different values of the θ and ϕ coordinates, which can then be averaged. The SWAP FOV (hatched in red) limits the regions of the sphere that are observed by SWAP.
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Image comparison of the intensity differential dI/da for each pixel generated by Jipole. Panel (a): dI/da computed using the FD method, shown in symmetric logarithmic scale. Panel (b): dI/da computed using AD, shown in symmetric logarithmic scale. Panel (c): absolute difference between the FD and AD results, in logarithmic scale; the NMSE (Equation (26)) is indicated in the top-right corner. Panel (d): relative difference between the FD and AD results, in logarithmic scale. These intensity differentials display the characteristic lensing behavior of black holes: nested rings that are successively rotated and demagnified.
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Image intensity map generated by Jipole (left column) and ipole (middle column) for the thin disk model described in Section 4.1. The right column illustrates the absolute difference between the two images. Total flux density values (see Equation (25)) are overlaid as text on the intensity maps in the left and middle columns, and the NMSE (Equation (26)) is overlaid on the absolute difference map in the right column.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Selection efficiency (left panel) and completeness (right panel) of giants as a function of g − i color and [Fe/H]LAMOST for the giant dwarf loci method. The contour profile represented the number density of giants.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Top left: histogram distribution of the residuals Δ[Fe/H] for the giant dwarf loci method, with the Gaussian fitting profile overplotted in black. Top right: comparison of [Fe/H]phot with [Fe/H]LAMOST. Bottom panels: the residuals Δ[Fe/H], as a function of g − i color and [Fe/H]LAMOST. The points are color coded by their number density.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Left panel: the H-R diagram of the sample with g − i > 0.6. The red and blue dots represent giants and dwarfs, respectively. The boundary of dwarfs (blue dots) and giants (red dots) is defined by Equation (5). Right panel: values of ﹩{\chi }_{\min ,\mathrm{dwarf}}^{2}﹩ against ﹩{\chi }_{\min ,\mathrm{giant}}^{2}﹩.
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Intensity images generated by Jipole (left column) and ipole (middle column), alongside their absolute difference (right column), for the analytical Model 5 presented in R. Gold et al. (2020). The total flux density (Ftot) for each image is annotated in the top-left corner of the Jipole and ipole panels, while the NMSE (Equation (26)) is on the top-left corner of the right panel.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Comparison of stellar loci for NUV − g (left panel) and u − g (right panel) versus g − i at different [Fe/H] values for dwarfs and giants.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Distribution of the residuals Δ[Fe/H] in the H-R diagram. The color bar represents Δ[Fe/H].
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: The r-band effective radius size–mass distribution for SAGA satellite galaxies (purple, top left), SAGAbg environmentally averaged galaxies (orange, middle left), and SDSS/NSA isolated galaxies (green, bottom left). Middle panel: weighted binned medians and size–mass relation fits for all three samples. The binned 16th–84th percentile scatter for each sample is indicated by the thin colored lines. The mass ranges outside of ﹩7.5\lt {\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })\lt 10.0﹩ are shaded gray in the left column and middle panel, as these represent regions of parameter space where the samples are significantly incomplete. Only data within that mass range is considered. Bootstrapped samples of summary statistics of the normalized-to-average sizes are plotted in the right column. The median distributions are shown for normalized-to-average size fit to all data (top right), and the standard deviation distributions are shown for normalized-to-average size fit to each sample separately (bottom right).
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Size–mass relations and wavelength dependence of sizes for all three samples. Left: size–mass relations using both Reff (solid lines) and R80 (dashed lines), measured in the g (thickest), r, and z bands (thinnest). The colors correspond to the three samples: SAGA satellites (purple), SAGAbg galaxies (orange), and isolated galaxies (green). The offset between R80 and Reff is ∼0.25 dex and consistent across samples, reflecting the similarity in Sérsic indices. Right: median galaxy size in each band, normalized to the average size across g, r, and z for each sample, shown for R80 (top) and Reff (bottom). Sizes in the g and r bands are nearly identical, while z-band sizes are systematically smaller. These trends are consistent with previous work showing that galaxy sizes decrease in redder bands (e.g., R. Lange et al. 2015).
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: We test the effects of incompleteness on our results by measuring the observed offsets using surface brightness thresholds. Top: cumulative distributions of the normalized-to-average size for the SAGA satellite galaxies (purple), SAGAbg environmentally agnostic galaxies (orange), and SDSS/NSA isolated galaxies (green) in the mass range of ﹩7.5\lt {\mathrm{log}}_{10}({M}_{\star }/{M}_{{\odot }})\lt 10.0﹩, as shown in Figure 7. Two additional cumulative distribution functions ​are included per sample, where surface brightness cuts of ﹩{\mu }_{r,{\rm{eff}}}\lt 23\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩ (dotted lines) and ﹩{\mu }_{r,{\rm{eff}}}\lt 24\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩ (dashed lines) are applied. Bottom: bootstrapped samples of the median normalized-to-average size for each subset shown in the top panel. The solid lines in the right panel are equivalent to the distributions shown in the top right panel of Figure 6. Even when restricting the samples to the lower surface brightness sources where completeness is highest, the median size difference between the isolated and satellite samples persists.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Comparison of remeasured sizes with Legacy Tractor catalog sizes. We compare the circularized effective radius (﹩{\mathrm{log}}_{10}({R}_{\mathrm{eff}}\,{\mathrm{kpc}}^{-1})﹩), plotting the residuals between our measurements and the Tractor catalog values against the Tractor values. The left panel shows residuals colored by sample, while the right panel shows residuals colored by morphological model used in the Tractor fit (DEV, EXP, PSF, REX, and SER). The gray shaded region indicates ±0.1 dex. The residuals are small for the majority of the data, demonstrating the consistency between our measurements and the Tractor catalog. While there are some systematic differences in size measurements, particularly at the extremes of the size distribution, they do not affect the samples differently.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: The completeness-corrected size–mass relation for the SAGA Gold sample (Equation (3)) compared to literature observations. Overall, our relation is largely consistent with the ELVES survey (olive dotted line; S. G. Carlsten et al. 2021), GAMA (teal dashed line; R. Lange et al. 2015), and SDSS (sienna dot dashed line; S. Shen et al. 2003), although these relations are determined from different methods and data. ELVES covers a lower-mass range, and GAMA and SDSS are both fit to data at higher masses. Shaded regions around the fits represent the reported 1σ uncertainties.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Top: cumulative normalized size distributions for star-forming galaxies only, across the SAGA satellites (dark blue), SAGAbg galaxies (muted orange), and isolated galaxies (muted green). Bottom left: ellipticity (e) distributions for star-forming galaxies in each sample. Bottom right: Sérsic index (n) distributions for the same samples.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Cumulative distributions of the normalized-to-average size for the SAGA satellite galaxies (purple), SAGAbg environmentally agnostic galaxies (orange), and SDSS/NSA isolated galaxies (green) in the mass range of ﹩7.5\lt {\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })\lt 10.0﹩. Data is normalized to the “all data combined” fit shown by the dotted–dashed line in Figure 6 and in Table 1. We also include the cumulative distribution function for the SAGAbg isolated (dashed, brown) subset.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Left: comparison of the M. Capaccioli (1989) and L. Ciotti & G. Bertin (1999) approximations, and the adjusted approximation presented in this work. The new approximation provides a much better fit to the true values for n < 0.36, while still maintaining high accuracy everywhere else in the domain. Right: percentage error (systematic offset) between input re and actual profile re for different approximation schemes for bn. These results align with general heuristics known in the field; the L. Ciotti & G. Bertin (1999) approximation begins producing offset effective radii at around n ∼ 0.36, while the M. Capaccioli (1989) profile introduces considerable error at low n.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Completeness-corrected ellipticity (e, top) and Sérsic index (n, bottom) distributions of SAGA satellites (purple), SAGAbg galaxies (orange), and isolated galaxies (green) in the mass range of ﹩7.5\lt {\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })\lt 10.0﹩. Gaussian KDE density functions are included to illustrate the overall shape of each distribution, and distributions are normalized to density for direct comparison between populations despite sample size differences. There is no evidence for the ellipticity and Sérsic index distributions differing as a function of environment, with the exception of the quenched satellite population.
Paper: Abundances of Rarely Detected s-process Elements Derived from the Ultraviolet Spectrum of the s-process-enhanced Metal-poor Star HD 196944 
Authors: Ian U. Roederer, Vinicius M. Placco, Amanda I. Karakas, Elizabeth A. Den Hartog, Timothy C. Beers
Figure caption: Sections of the STIS/E230H spectra of HD 196944 around lines of interest. Symbols are the same as in Figure 1.
Paper: Abundances of Rarely Detected s-process Elements Derived from the Ultraviolet Spectrum of the s-process-enhanced Metal-poor Star HD 196944 
Authors: Ian U. Roederer, Vinicius M. Placco, Amanda I. Karakas, Elizabeth A. Den Hartog, Timothy C. Beers
Figure caption: Comparison between the HD 196944 abundance pattern and model predictions for the s-process operating in an AGB star with initial mass = 3.0 M⊙, Z = 0.0001, and partial mixing zone (PMZ) = 0.001 M⊙ (A. I. Karakas 2010; M. Lugaro et al. 2012). The solar s-process pattern from S. Bisterzo et al. (2011; for Ga–Br) and S. Bisterzo et al. (2014; for Rb–Bi) are shown in orange studded lines for comparison. The comparison is shown in terms of ﹩\mathrm{log}\varepsilon ﹩ abundances (top panel), [X/Fe] ratios (middle panel), and differences between the HD 196944 pattern and the predicted s-process pattern (bottom panel).
Paper: Abundances of Rarely Detected s-process Elements Derived from the Ultraviolet Spectrum of the s-process-enhanced Metal-poor Star HD 196944 
Authors: Ian U. Roederer, Vinicius M. Placco, Amanda I. Karakas, Elizabeth A. Den Hartog, Timothy C. Beers
Figure caption: Sections of the STIS/E230H spectra of HD 196944 around lines of interest. The filled squares represent the observed spectrum. The solid blue line represents a synthetic spectrum with the best-fit abundance for each line of interest, and the light-blue bands represent a change in this abundance by a factor of ±2 (0.3 dex). Blue lines without this light-blue band denote upper limits. The solid black line represents a synthetic spectrum with no contributions from the species of interest.
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Gas and radiation temperature profiles, denoted by Tgas and Trad, for the subcritical (left) and supercritical (right) radiative shock tests. The profiles are shown at times t = 3.8 × 104 s and t = 7.5 × 103 s, respectively, as a function of the comoving coordinate s = x − ut. The reduced radiation flux f is overplotted to illustrate the transition between the free-streaming and diffusion regimes across the shock structure.
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Convergence of ∣δEr∣ yielding various resolutions of the radiation wave propagation test. The yellow line represents tests with piecewise linear reconstruction, and the purple line represents tests with piecewise constant reconstruction. Additionally, a dotted black line indicating ﹩{{ \mathcal N }}^{-1}﹩ scaling and a dashed–dotted black line indicating ﹩{{ \mathcal N }}^{-2}﹩ scaling are overplotted for reference.
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Radiation temperature Trad measured at the right edge of the box after 10 light-crossing times across the horizontal extent of the box. Lines of different colors indicate results for different runs, namely HLL-PL (black), HLL-PC (golden yellow), GLF-PL (purple), and GLF-PC (green).
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Face-on view of the gas surface density projection at 1 kyr for the fiducial run (left), the quadruple-resolution run (middle), and the quadruple-﹩\tilde{c}﹩ run (right).
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Temporal evolution of the clump mass mclump within 1 kyr in the fiducial run (black dotted), the quadruple-resolution run (purple solid), and the quadruple-﹩\tilde{c}﹩ run (yellow solid).
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Gas internal energy density as a function of time in two simulations and the corresponding analytical solution.
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Two-dimensional distribution of the radiation temperature ﹩{T}_{{\rm{rad}}}={({E}_{r}/{a}_{r})}^{1/4}﹩ in the HLL-PL run after 10 light-crossing times across the horizontal extent of the box.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Best-fit models created using KinMS for dual-AGN systems. Each row of panels refers to a single system. The left-hand column of panels refers to the zeroth moment (integrated intensity) of the 12CO data cube, whereas the right-hand column refers to the first moment (velocity profile). From left to right, each column shows the data, model, and residual map. Primarily for visual purposes, the data, model, and residual maps have been masked to spatial regions that had pixels with ≥3σ 12CO detections in the ALMA cube. For Mrk 739E and ESO 253-G003 SW, however, we lower this threshold to ≥2σ to account for the faintness of the emission. The best-fit position angle of the rotating disk is shown as a dashed black line. For systems with resolved SoIs, we show the lower and upper bounds of the SoIs as black circles. If only the SoI upper bound is resolved, we only show the upper bound. For systems with unresolved SoIs at both bounds, we mark the AGN position as a star.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: AGN bolometric luminosity (LBol/erg s−1) with respect to the ratio of H2 surface densities at r < 50 pc and r < 200 pc (﹩{{\rm{\Sigma }}}_{{H}_{2}}^{\,\rm{50 pc}\,}﹩/﹩{{\rm{\Sigma }}}_{{H}_{2}}^{\,\rm{200 pc}\,}﹩). The color scale shows the Eddington ratio on a logarithmic scale. This figure was adapted from S. García-Burillo et al. (2021). For the surface density ratios, we measure uncertainties assuming αCO = 0.6 M⊙ (K km s−1 pc−2)−1. The mergers generally show an inverse correlation between gas concentration and AGN activity. Due to the small sample size and outlier, however, the potential trend is not statistically significant (τ = −0.2, p-value = 0.4).