adsabs/AstroCLIMB huggingface dataset:
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: Coefficients of the LR model trained on all features. Bias is the constant term in the model. The plot shows the mean value of the coefficient for each feature across all models, with the error bars for 95% confidence intervals.
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: Yearly training, validation, and test splits for the five ensemble members for both evaluation test cases.
Paper: Beyond Ultra-diffuse Galaxies. I. Mass–Size Outliers among the Satellites of Milky Way Analogs
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Johnny P. Greco, Song Huang, 崧 黄, Peter Melchior, Rachael Beaton, Kirsten Casey, Shany Danieli, Andy Goulding, Remy Joseph, Erin Kado-Fong, Ji Hoon Kim, Lauren A. MacArthur
Figure caption: Abundance of UDGs as a function of the host halo mass. Left: We compile the UDG abundance measurements from the literature covering a wide range of host mass. The UDG abundance from our work N UDG = 0.44 ± 0.05 is shown as a red square, and the power-law relations from van der Burg et al. (2017) and Mancera Piña et al. (2018) are shown in gray and blue respectively. Our fitting result is shown in pink. Our UDG abundance is consistent with ELVES but significantly higher than that in SAGA. After including more measurements at the lower halo-mass end, the power law is shallower than the relation reported in van der Burg et al. (2017). Right: We split the UDG sample into bins based on the host halo mass (circles) and g − i color (diamonds). The UDG abundance is higher for more massive hosts and redder hosts.
Paper: Beyond Ultra-diffuse Galaxies. I. Mass–Size Outliers among the Satellites of Milky Way Analogs
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Johnny P. Greco, Song Huang, 崧 黄, Peter Melchior, Rachael Beaton, Kirsten Casey, Shany Danieli, Andy Goulding, Remy Joseph, Erin Kado-Fong, Ji Hoon Kim, Lauren A. MacArthur
Figure caption: Correspondence between the Sérsic profile (Equation (C3)) and the Spergel profile (Equation (C1)). We fit a Spergel profile to each Sérsic while fixing the total luminosity and half-light radius. The black line in the left panel shows the best-fit Spergel index ν as a function of the Sérsic index n. We also provide a symbolic approximation to this relation in Equation (C5), shown as the gray dashed–dotted line. In the right panel, two Sérsic profiles (solid) and their best-fit Spergel profiles (dashed–dotted) are shown. The Spergel profile approximates the Sérsic profile well at a small Sérsic index.
Paper: Beyond Ultra-diffuse Galaxies. I. Mass–Size Outliers among the Satellites of Milky Way Analogs
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Johnny P. Greco, Song Huang, 崧 黄, Peter Melchior, Rachael Beaton, Kirsten Casey, Shany Danieli, Andy Goulding, Remy Joseph, Erin Kado-Fong, Ji Hoon Kim, Lauren A. MacArthur
Figure caption: Distribution of UPGs (blue) and mock galaxies (red) in g − i color, ellipticity, and Sérsic index n. We translate the Spergel index to the Sérsic index using Equation (C5). The mock galaxy population represents the real UDG/UPG population well.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Average frequency depolarization ratios in bins of 2.″5 along R.A. or decl. axis. Top: ratios as a function of decl. for all R.A. Bottom: ratios as a function R.A. for all decl. The southern tail is to the left of R.A./decl. = 0″, and the northern tail to the right. Red: ratio of 6 and 10 GHz denoted as FDR2. Green: ratio of 2 and 10 GHz (FDR1). Only pixels with fractional error <80% were used for computing the averages and dispersions. The spread shown corresponds to the standard deviation of the depolarization ratios within bins along decl./R.A. The tails depolarize to a similar value for FDR1 ranging between 0.01–0.1. The distribution of FDR2 shows radial dependence particularly along R.A., with a large spread suggesting varying levels of depolarization in this higher frequency ratio.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Example lines of sight showing fractional polarization versus λ 2 (left column), the observed polarization angle versus λ 2 in black and the residual angles in blue (middle column), and Faraday spectra superimposed with the Gaussian RMTF in red (right) all at 1.″50 × 1″. The residual polarization angles were obtained by removing the dominant peak in the Faraday spectrum (subtracting RMpeak λ 2). The top two rows are from the ‘smoothly decaying’ class, the middle two rows are from the “sinc-like” class, and the bottom two are from the “complex class.”
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Depolarization ratio maps across the tails at 1.″5 × 1.″0 resolution. Top panel: FDR1, the ratio of the 2 GHz polarization image to the 10 GHz polarization image. Bottom panel: FDR2, the ratio of the 6 GHz polarization image to the 10 GHz polarization image. Left panel: northern tail. Right panel: southern tail. Only pixels with fractional error of less than 80% are shown. Note the range of color scales in the upper and lower panels are different, due to the stronger depolarization at 2 GHz. Attempting to match the color scales hides the important variations.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: The fractional polarization p across the tails of Hydra A at selected frequencies at a resolution of 1.″5 × 1″. The pixels shown have signal-to-noise in p/σ  p  > 60%, where σ  p  is the estimated rms noise in the polarization. Left: northern tail. Right: southern tail. Both tails depolarize significantly with decreasing frequency. The northern tail is relatively less depolarized compared to the southern tail. The physical scale shown in the top panel is the same for the rest of the panels.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Fractional polarization at 6 GHz at four resolutions. Left: northern tail. Right: southern tail. Resolution from top to bottom: 0.″5, 0.″75, 1.″5, and 3″. Only pixels with signal-to-noise p/σ  p  > 60% are shown. In nearly all locations, the higher-resolution images are more highly polarized. The physical scale shown in the top panel is the same for the rest of the panels.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Resolution-dependent depolarization ratio. RDR1 is 3″/0.″30 at 10 GHz. RDR2 is 3″/0.″50 at 6 GHz. The left side of decl. zero is the southern tail, and the right side is the northern tail. The pixels shown have fractional error <80%. The general depolarization ratio behavior is similar at the two frequencies. The depolarization is stronger across the southern tail. The two tails depolarize differently with distance from the center: the depolarization across the northern tail decreases with distance from the AGN, while the depolarization is strongest away from the center across the southern tail. We find the same behavior for RDR binned along R.A.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Line-of-sight fractional polarization as a function of resolution. Green: 10 GHz. Red: 8 GHz. Cyan: 6 GHz. Black: 4 GHz. Magenta: 2 GHz. Plot titles: lines of sight position coordinates and the RDR value at 3″/0.3″ (10 GHz). Some lines of sight (top row) show the “expected” increase in fractional polarization with increasing resolution (these make up roughly 59% of the lines of sight). In some cases, we find lines of sight with fractional polarization changing unexpectedly with increasing resolution (two bottom rows, roughly 41% of the lines of sight behave this way).
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Example of fitting a simple random depolarization screen defined in Equation (1) to the high-resolution 6-12 GHz data. The left column shows fractional Q and U, the middle column shows fractional polarization, p, and the right column shows the polarization angle for all three as a function of λ 2.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Depolarization ratio maps across the tails. Top panel: RDR1, the ratio of the 3″ resolution fractional polarization image to the 0.″3 image at 10 GHz. Bottom panel: RDR2 –the ratio of the 3″ fractional polarization to the 0.″5 polarization image at 6 GHz. Only pixels with fractional error of less than 80% are shown.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Predictions of low-frequency, low-resolution depolarization using high-resolution polarization and RM maps derived from high-resolution, high-frequency data. Left column: fractional polarization vs. λ 2. Middle column: polarization angle vs λ 2. Right column: Faraday spectra. Black: observed data. Red: predictions. Two top rows: reasonably good predictions (roughly 4% of the lines of sight). Last three rows: partially reproduced (71%).
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: The RM profile as a function of distance from the image center along decl., in bins of 50 pixels (2.5″). The mean of RMs computed across R.A. is shown in red data points, and a standard deviation is in a red shade. The median is shown in blue data points, and the first and third quartiles are in the blue shade. The RM profile is consistent with that of Taylor & Perley (1993).
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: A histogram of RM dispersions distribution across both tails (in bins of 600). We find a mean of 234 rad m−2 and a standard deviation of 200 rad m−2 for the northern tail and a mean of 380 rad m−2 and a standard deviation of 226 rad m−2 across the southern tail. The σ range roughly between 0 and 800 rad m−2 for the northern tail, and 0 and 1000 rad m−2 for the southern tail.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Parameters derived from fitting Equation (1) to high-frequency (6–12 GHz) high-resolution 0.″50 × 0.″35 polarization data. The left column shows the northern tail, and the right column shows the southern tail. The top row shows the intrinsic fractional polarization (extrapolated to zero λ), the middle row shows the rotation measure maps, and the third row is the RM dispersion. Shown are pixels with errors in fractional polarization <0.1. The physical scale shown in the top panel is true for the rest of the panels.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: A histogram of RM distribution across both tails (in bins of 600). We find a mean of 313 rad m−2 and a standard deviation of 1298 rad m−2 for the northern tail, and a mean of −2049 rad m−2 and a standard deviation of 3396 rad m−2 across the southern tail.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Magnetic field orientations superimposed on a 2 GHz total intensity map. The vector lengths are proportional to the fractional polarization (magnified by a factor of 30). Showing only pixels with fitting error in p 0 < 0.1.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: The “V”-shaped structure in brightness and magnetic fields in the northern tail of Hydra A. The orientation vectors correspond to the magnetic field orientation and the lengths are proportional to the fractional polarization. The magnetic field orientation traces the “V,” while the fractional polarization has a minimal effect.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: RM dispersion profile as a function of distance from the image center along decl., in bins of 50 pixels (2.5″). The mean of dispersions computed across R.A. is shown in red data points, and the standard deviation is in a red shade. The median is shown in blue data points, and the first and third quartiles are in a blue shade.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: LCs for the 2D 5122 AMR run with κ = 0.1, 0.2, and 0.4. Each graded color plot contains LCs from ten viewing angles: θ = 0°–90° in 10° increments. The LCs peak at 1.1–2.8 × 1043 erg s−1 for 70–130 days and then plateau at 3–5 × 1042 erg s−1 for 150–200 days.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Gas densities, velocities, radiation energy densities, and radiation fluxes for the κ = 0.1, 8192-zone model from 0 to 350 days after the ejection of P3. P2 and P3 mark the positions of the shocks in the corresponding shells. At t = 0, the gas at r > 1015 cm is the tail of P1. The collision between P3 and P2 can be seen in the merger of the two velocity peaks over time. Collisional heating produces a large radiation flux at the shock front P2.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Density structure of the 2D κ = 0.1, 0.2, and 0.4 runs at two different resolutions at 270 days. The colored arrows mark the direction of radiation flux. The thickness and deformation of the shell decrease as the opacity increases.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Zoom-in of the density spike in the 1D κ = 0.1, 8192-zone run at 300 days. The red dashed line marks the position of the shock in P2+P3. The spike is ∼1.4 × 1014 cm across and is resolved by about 50 zones. The density of the spike peaks at ∼10−12 g cm−3, which is about 1000 times higher than its surroundings. The spike also exhibits abrupt changes in velocity and radiation flux.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: The 2D density images for the κ = 0.2, 5122 AMR run (left), and the hydro-only HD model (right) from Chen et al. (2014) at 50 and 256 days. The 2D RHD and HD simulations have resolutions of 4.88 × 1012 cm and 1.22 × 1012 cm, respectively. Mixing during the collision is stronger in HD than in RHD.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Evolution of the gas density and radiation flux in 2D for the κ = 0.2, 5122 AMR run at 77, 157, 212, and 268 days, respectively. Initially, two dense shells form in P2 and P3 and later merge. The off-axis corrugations in the merged shell are due to radiative cooling.
Paper: Ion Loss within a Reconnection Exhaust near Mars: MAVEN Observations
Authors: Xiaojun Xu, 军 徐晓, Xing Wang, 星 王, Zilu Zhou, 露 周梓, Qing Chang, 清 常, Lei Luo, 磊 罗, Peishan He, 珊 何佩, Siqi Yi, 琦 易思, Hui Li, 晖 李
Figure caption: Schematic illustration of the MAVEN encounter with the reconnection exhaust. Dense heavy ions from the Martian ionosphere are observed within the reconnection exhaust, with the reconnection jet moving mainly downstream. The magnetic field lines have been detached from the ionosphere, suggesting that these ionospheric ions have escaped. These heavy ions are affected by other processes, such as the pickup, after their detachment from the ionosphere.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: LCs for the 1D runs. Left: 1024, 4096, and 8192 zones with κ = 0.2. The second peak is smeared out in the 1024-zone run because the thin shells are underresolved. Right: LCs for the 8192-zone run for κ = 0.1–0.4.
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: The top panel compares the frequency measured for the 8 GTIs without significant period drift. The middle panel shows the periodogram measured for these 8 GTIs, yielding a period of 35.87 s (see text). The bottom panel shows the phased light curves, with a 1 s bin, of the drifting-period “red” GTIs on the left, and that of the eight stable-period “blue” GTIs on the right. The data points were folded in the bottom panel with the 35.08 s period and with the 35.87 s periods, respectively. The count rate was normalized by the highest measured, and below, we binned the data in bins of 0.1 times the phase (10 per cycle) and plotted the average count rate in each bin.
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: The spectrum observed with the Chandra LETG grating and the HRC-S camera on 2006 June 6, and a fit with two components at thermal plasma at 240 and 630 eV, with N(H) = 2.2 × 1021 cm−2 and moderately enhanced abundances except for iron (which is only 15% the solar abundance).
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: The gray rectangles represent the frequency coverage of each SPW, and the numbers correspond to the setup number in Table 2. The background spectrum was obtained in NGC 1068 with the Nobeyama 45 m telescope in a previous observation (Takano et al. 2019).
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: The average spectrum observed on 2021 October 28, and the fit with two composite model: a stellar atmosphere and a BVAPEC thermal component (left), and two BVAPEC thermal components (left). Both fits yield χ 2/d.o.f.=1.4, and are virtually indistinguishable.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: The rotational diagram of each molecule (a) HNCO, (b) HC3N, (c) CH3CN, (d) CS, (e) C18O, and (f) 13CO in the CND (circle symbols) and the SBR (square symbols). The calculated rotational temperatures are shown beside a fitting line. The error bars are based on the ± 1σ noise level of integrated flux.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption:  L X against F XO (left) for galaxies and (right) QSOs from the SDSS spectroscopic sample. The red diagonal line is a near-linear relation (a slope of 1.02), which fits the galaxy sample. The vertical and horizontal lines identify the parameter spaces of XBONGs (galaxies with L X > 1042 erg s−1 and F XO > 0.1) and possible diluted AGNs (L X > 1042 erg s−1, F XO < 0.1)—see text for details. Also drawn are two additional lines (1) at L X = 1037 erg s−1 below which stars dominate, and (2) at F XO = 0.01 below which galaxies dominate with almost no QSO.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Left: the HR(ms) distribution of the normal galaxy sample. Right: the normal galaxy sample is divided into three L X bins. The vertical green dashed lines correspond to those in Figure 4. The number next to the object type in the legend box indicates the scaling factor of each distribution (see text).
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Left: the HR(ms) distribution of the XBONG sample in red. The black (blue) points for the normal galaxy (QSO) sample are the same as in Figure 6. The shaded regions indicate the two HR(ms) bins where the statistical significance is calculated in Table 3. Right: the XBONG sample is divided into three L X bins. The vertical green dashed lines correspond to those in Figure 4. The number next to the object type in the legend box indicates the scaling factor of each distribution.