adsabs/AstroCLIMB huggingface dataset:
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Stellar mass distribution for our AGN (red), quiescent AGN (pink), and no AGN (teal) galaxy samples.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: (a) B  z /B as the function of z in the rQT region. z is on a scale of R ⊙. (b) f(z) as the function of z near the rQT region center. It gives the region’s characteristic scale of L  θ  ∼ R ⊙. (c) The analytical results obtained based on Equation (29). (d) V f as the function of ν for V i = 1. (e) V f as the function of ν for V i = 0.9. (f) V f as the function of ν for V i = 0. Here the frequency range that we consider is 1–10  GHz, and the red solid line represents the average value of the oscillations, which can be determined by Equation (29). At the center of the rQT region, there are n 0 = 104 cm−3 and B 0 = 100 G, thus, ν T ∼ 3GHz.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: The side view of a binary system involving neutron stars with different companion magnetic field configurations, where the yellow circular denotes the neutron star, which is at the superior conjunction (the neutron star behind the companion star), and the rQT region is likely to be present in both scenarios, as shown in the shaded area of the figure.
Paper: Polarization Evolution of Fast Radio Burst Sources in Binary Systems
Authors: Zhao-Yang Xia, Yuan-Pei Yang, Qiao-Chu Li, Fa-Yin Wang, Bo-Yang Liu, Zi-Gao Dai
Figure caption: A geometric interpretation of the generalized Faraday rotation by the Poincaré sphere. The state of the polarization  P  = (Q, U, V) can be determined by latitude 2χ and longitude 2ψ. The generalized Faraday rotation corresponds to the polarization point  P  rotating around the modal axis  ρ  at constant latitude.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Thermal energy measured within a 2′ radius for stacked galaxies convolved with a 2.′1 beam at a range of redshifts. The black line at z = 1 represents the best-fit power law to observational ACT data from Meinke et al. (2023).
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Radial bin correlation matrices for 37.″5 bins for SZ-y signals convolved with the ACT 2.′1 beam at z = 1. Left: correlation matrix out to radial distances of 20′ for the stacked AGN data, Right: correlation matrix out to a radius of 5′. The radial profiles shown in Figure 4 represent bins of this size.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Radial bin correlation matrices for 12.″5 bins for SZ-y signals convolved with TolTEC’s 9.″5 beam at z = 1. Left: correlation matrix out to radial distances of 20′ for the stacked AGN data, Right: correlation matrix out to a radius of 5′.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Thermal energy measured within a 2′ radius for massive galaxies convolved with a 2.′1 beam plotted against halo mass at a range of redshifts.
Paper: NGC 6302: The Tempestuous Life of a Butterfly
Authors: Bruce Balick, Lars Borchert, Joel H. Kastner, Adam Frank, Eric Blackman, Jason Nordhaus, Paula Moraga Baez
Figure caption: Sundry images of the nebular structure of NGC6302 displayed to facilitate easy comparisons. Images in panels (b)–(f) are aligned 1000 × 2000 portions of HST images displayed at 0.″079/pixel. North is up. Panel (a) shows a deep wide-field Hα + [N II] image (esahubble.org/images/heic0407b/), taken by Romano Corradi (courtesy Albert Zijlstra) on which our image of [Fe II] emission is overlayed in red. Panel (b) is a contrast-enhanced version of the [Fe II] showing its prominent pair of feathers and other more subtle structures. The signals of patterns of proper motions appear in panel (c). Panel (d) presents the residuals after the fits to the ZUEs are removed (red lines border regions where the removal of these residuals was not successful). Panels (e) and (f) show the ratios of image ratios, as described in the text. Colored pointers refer to particular features that are discussed in the text.
Paper: NGC 6302: The Tempestuous Life of a Butterfly
Authors: Bruce Balick, Lars Borchert, Joel H. Kastner, Adam Frank, Eric Blackman, Jason Nordhaus, Paula Moraga Baez
Figure caption: A modified version of Figure 5 in K+22a that identifies morphologically distinct wedges within the bipolar wings of NGC 6302 as seen in contrast-enhanced versions of [Fe II] (red) and [N II]/H (gray) images. Various significant zones beyond the core (gray circle) are identified. A schematic of the main equatorial CO ring from S-G+17 has been aligned to the HST images. North is up.
Paper: NGC 6302: The Tempestuous Life of a Butterfly
Authors: Bruce Balick, Lars Borchert, Joel H. Kastner, Adam Frank, Eric Blackman, Jason Nordhaus, Paula Moraga Baez
Figure caption: Panels (a)–(c) show the residuals in the eastern portions of the 2020 and 2009 F658N image ratios after the latter has been magnified by a factor of M and divided by the former. Those features that share a common magnification (aka expansion age) are nulled if M is successfully chosen; however, no value of M nulls the full set of sinewy features in the red zone. (Faint horizontal waves are artifacts imposed by internal reflections in the filter.) Panel (d) The pattern of the residuals in the red zone after a 4.0 pixel radial translation of the 2009 image relative to that of 2019 (see the text).
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: Difference between the position angles of the 2D major axes obtained by projecting all particles θ and only 3D major axes θ major of galaxies and halos, as a function of the mean axis ratios b/a (left) and c/a (right). Galaxies and halos are binned by F acc at each redshift. Results from different redshifts are displayed by different colors, with dots for halos and triangles for galaxies.
Paper: Centaurus A: Exploring the Nature of the Hard X-Ray/Soft Gamma-Ray Emission with INTEGRAL
Authors: James Rodi, E. Jourdain, M. Molina, J. P. Roques
Figure caption: Cen A SPI (black diamonds) and ISGRI (red triangles) long-term light curves on an INTEGRAL revolution timescale. The date of the NuSTAR observation is shown with a vertical green line. The solid black line denotes a flux of 0 mCrab. The dashed black line denotes the mean flux.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: We demonstrate that the sum of exponential functions with similar exponents τ can also be effectively approximated by a single exponential function. All exponential functions are normalized within the interval [0, π/2]. In cases where n exponential functions are summed up, all the exponential functions being summed are divided by n.
Paper: Centaurus A: Exploring the Nature of the Hard X-Ray/Soft Gamma-Ray Emission with INTEGRAL
Authors: James Rodi, E. Jourdain, M. Molina, J. P. Roques
Figure caption: Plot of photon index vs. 50 keV flux for spectral groups for SPI (top) and ISGRI (bottom). The best-fit photon index for each instrument is shown as a red dashed line.
Paper: Low-mass Quiescent Galaxies Are Small in Isolated Environments: Environmental Dependence of the Mass–Size Relation of Low-mass Quiescent Galaxies
Authors: Yongmin Yoon, Jae-Woo Kim, Jongwan Ko
Figure caption: Left panel: distribution of our sample in the u − r vs. r − z color–color diagram. The filled gray contours indicate the densities of the data points (darker contours mean a higher density of data points). Note that 90% of the galaxies in the sample is located within the outermost gray dashed contour line. The red contour lines denote the densities of the galaxies with EW(Hα) ≥ −1 Å, whereas the blue contour lines represent the densities of the EW(Hα) < −1 Å (an emission line has a negative value of EW(Hα)). The thick black solid line indicates the color cut that distinguishes between quiescent and star-forming galaxies (Equations (1) and (2); galaxies located in the upper region of the line are quiescent). The black dotted–dashed line represents Equation (1), while the black dashed line represents Equation (2). Right panel: histogram of the u − r color distribution of our sample. The vertical dashed line indicates the local minimum between the two peaks in the u − r color distribution, which corresponds to the horizontal cut in the urz diagram (Equation (1)).
Paper: Low-mass Quiescent Galaxies Are Small in Isolated Environments: Environmental Dependence of the Mass–Size Relation of Low-mass Quiescent Galaxies
Authors: Yongmin Yoon, Jae-Woo Kim, Jongwan Ko
Figure caption: Color images of LQGs with ﹩\mathrm{log}({M}_{\mathrm{star}}/{M}_{\odot })\leqslant 9.8﹩ and spatial distribution map for galaxies within ∼1 Mpc of each LQG. By the gray separation lines, this figure is divided into four parts, which represent galaxies in the four environments bins used in this study. For example, the upper left part is for galaxies in the highest-density bin, while the lower right part is for galaxies in the lowest-density bin. The galaxy ID, R  e , Σ10, and stellar mass are shown in the color image. The horizontal bar in the color image indicates the angular scale of the image. The green star in the galaxy map indicates the location of the LQG, while the black filled circles represent other galaxies in the environment. As indicated in the accompanying legend in the bottom right panel, the size of the circle denotes the stellar mass of the galaxy.
Paper: Low-mass Quiescent Galaxies Are Small in Isolated Environments: Environmental Dependence of the Mass–Size Relation of Low-mass Quiescent Galaxies
Authors: Yongmin Yoon, Jae-Woo Kim, Jongwan Ko
Figure caption: Mass–size relation of our quiescent galaxies. The squares of the different colors represent the different environment bins, while the black squares denote all quiescent galaxies. A square indicates the mean ﹩\mathrm{log}{R}_{e}﹩ of the mass bin (with a bin size of 0.2 dex), after excluding outliers beyond 5σ. The error bars denote the standard error of the mean. This figure displays only bins with a minimum of 45 galaxies. The filled gray contours indicate the density of data points (a darker contour means a higher density of data points). Note that 90% of the galaxies in the sample are located within the outermost gray dashed contour line. The units of Σ10 in the legend are Mpc−2.
Paper: Low-mass Quiescent Galaxies Are Small in Isolated Environments: Environmental Dependence of the Mass–Size Relation of Low-mass Quiescent Galaxies
Authors: Yongmin Yoon, Jae-Woo Kim, Jongwan Ko
Figure caption: Comparison between the logarithmic values of Σ10 and Σ M . The filled gray contours indicate the density of data points (darker contours mean a higher density of data points). The black solid line indicates the line fitted to the distribution of data points. The equation of the line is ﹩\mathrm{log}{{\rm{\Sigma }}}_{M}=1.1\mathrm{log}{{\rm{\Sigma }}}_{10}+10.4﹩. In this figure, we only show data points within 5σ from the line, where σ is 0.2 dex in the direction of the y-axis. The two quantities show a nearly perfect correlation with a Spearman’s correlation coefficient of 0.95 and a small scatter of 0.2 dex. Therefore, they are almost interchangeable.
Paper: Low-mass Quiescent Galaxies Are Small in Isolated Environments: Environmental Dependence of the Mass–Size Relation of Low-mass Quiescent Galaxies
Authors: Yongmin Yoon, Jae-Woo Kim, Jongwan Ko
Figure caption: Lower panel: surface number density (﹩\mathrm{log}{{\rm{\Sigma }}}_{10}﹩) distributions for quiescent (the black solid line) and star-forming galaxies (the gray dashed line). The vertical lines in both panels divide the quiescent galaxies into the four environment bins used in this study. Upper panel: quiescent fractions f  q  for galaxies with different stellar masses in the four environment bins.
Paper: Low-mass Quiescent Galaxies Are Small in Isolated Environments: Environmental Dependence of the Mass–Size Relation of Low-mass Quiescent Galaxies
Authors: Yongmin Yoon, Jae-Woo Kim, Jongwan Ko
Figure caption: Quiescent region of the urz diagram from Figure 1, in which the median color of quiescent galaxies with different stellar masses in the four environment bins is plotted on the diagram. The data points are differentiated by shape to indicate the different stellar mass bins and by colors to represent the different environment bins. The error bars denote the standard error of the median. The units of Σ10 in the legend are Mpc−2.
Paper: Low-mass Quiescent Galaxies Are Small in Isolated Environments: Environmental Dependence of the Mass–Size Relation of Low-mass Quiescent Galaxies
Authors: Yongmin Yoon, Jae-Woo Kim, Jongwan Ko
Figure caption: Color images of HQGs with ﹩\mathrm{log}({M}_{\mathrm{star}}/{M}_{\odot })\geqslant 10.5﹩ and spatial distribution map for galaxies within ∼1 Mpc of each HQG. The other details for this figure are the same as those in Figure 5.
Paper: Needle in a Haystack: Finding Supermassive Black Hole-related Flares in the Zwicky Transient Facility Public Survey
Authors: Yael Dgany, Iair Arcavi, Lydia Makrygianni, Craig Pellegrino, D. Andrew Howell
Figure caption: Distribution of the separationArcsec parameter from Criterion 1 (shown in a stacked histogram) for all detections of our five TDEs. There is no significant difference in the separations between the TDEs in the 0.″5 threshold subsample (AT 2020vwl and AT 2021ehb) and the TDEs in the 1″ threshold subsample (AT 2022bdw, AT 2022csn, and AT 2022dbl), meaning that the change of separation threshold does not have a strong effect on the number of TDEs discovered.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: (a) The map illustrates the differences between the first velocity moment (velocity field) of 13CO (J = 2–1) and the systemic velocity of the cloud (V lsr = −37.7 km s−1). The main and branched skeletons are shown as white and black curves, respectively. Magenta ellipses mark the dust clumps. The filled magenta circle in the lower right corner indicates the beam size of the CO observation. (b) Same as the left panel, but for C18O (J = 2–1). (c) Color-coded line-of-sight velocity centroids of C18O (J = 2–1) extracted along filaments overlaid on top of an H2 column density map. The sizes of the symbols indicate the line width of C18O (J = 2–1). The filled magenta circle in the lower right corner indicates the beam size of the Herschel 500 μm wave band.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: (a) Velocity integrated intensity map of 13CO (J = 2–1) with the H2 column density determined from spectral energy distribution fitting overlaid as contours in levels of (0.9, 1.1, 1.3, 1.5, 1.9, 2.4, 3.0, 4.0, and 5.0) × 1022 cm−2. The velocity interval for integration is [−41.5, −33.0] km s−1. The σ levels of the 13CO (J = 2–1) integrated map is σ = 0.08 K km s−1. The main and branched skeletons are shown as white and black curves, respectively. Magenta ellipses mark the dust clumps. The filled magenta circle in the lower right corner indicates the beam size (HPBW) of the CO observation. (b) Same as panel (a), but for C18O (J = 2–1). (c) Same as panel (a), but for dust temperature. The filled magenta circle in the lower right corner indicates the beam size of the Herschel 500 μm wave band.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: Left: maps of the 13CO/C18O abundance ratio obtained from the 13CO and C18O J = 2–1 lines assuming LTE. Contours are the H2 column density in levels of (0.9, 1.1, 1.3, 1.5, 1.9, 2.4, 3.0, 4.0, and 5.0) × 1022 cm−2. Magenta ellipses mark the dust clumps. Part of the black dashed circle indicates the infrared bubble MWP1G326725+007745. The main and branched skeletons are shown as white and black curves, respectively. The beam size of the CO observation is shown in the lower right corner. Magenta ellipses mark the dust clumps. Right: projected local gravitational field (gray arrows) overlaid on the H2 column density contours in levels of (0.9, 1.1, 1.3, 1.5, 1.9, 2.4, 3.0, 4.0, and 5.0) × 1022 cm−2 and the color-coded velocity centroids of C18O (J = 2–1). The sizes of the symbols indicate the line width of C18O (J = 2–1). The gravitational force vectors are displayed with uniform lengths to emphasize their directions.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: Same as Figure 7, but for the absolute gradient of the acceleration at each position over the size of ∼0.15 pc. The units of the acceleration gradient are 1 × 10−12 km s−2 pc−1.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: The absolute velocity gradient along each skeleton, computed over ∼0.19 pc, is plotted as a function of position relative to the centers of the filaments for F3, F4, and F5. The major branch, F1+F2, is plotted from north to southeast. Red vertical solid lines represent the three ATLASGAL clumps. Blue vertical dashed lines indicate the positions of the 11 compact ArTéMiS sources situated in the F1+F2 skeleton. The green vertical solid line indicates the position of the junction between F3 and the major branch of filaments.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: (a) Averaged spectra of 13CO (J = 2–1) (black) and C18O (J = 2–1) (red) over the hub–filament cloud of G326. The intensity of C18O (J = 2–1) has been reduced by a scale factor of 5 for ease of viewing. The vertical dashed lines show the velocity interval −41.5 to −33.0 km s−1 over which the infrared dark hub–filament cloud of G326 extends. (b) Beam-averaged spectra of 13CO (J = 2–1) (black) and C18O (J = 2–1) (red) for C1. (c) Same as panel (b), but for C2. (d) Same as panel (b), but for C3.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: Channel maps of the 13CO (J = 2–1) and C18O (J = 2–1) lines, showing a 13CO (J = 2–1) integrated intensity map (start from 6σ) with C18O (J = 2–1) integrated intensity overlaid as contours. The contours start from 6σ to the peak value with steps of 8σ. The σ of the integrated intensity for both CO isotopologues in the interval velocity range of 0.5 is 0.018 K km s−1. This value is calculated as ﹩{T}_{\mathrm{rms}}\times \sqrt{{N}_{\mathrm{channels}}}\times \delta V﹩, where T rms = 0.08 K represents the typical rms value of the molecular line observations, N channels = 5 denotes the total number of line channels, and δ V = 0.1 km s−1 stands for the velocity resolution. The main and branched skeletons are shown as white and black curves, respectively.
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: The line-of-sight velocity profile of the gas within each filament is plotted as a function of position from the center of the filament. The positions are as follows: position C2 for F1 (black solid line), F4 (cyan dotted line), and F5 (magenta dotted line); position at the junction between F3 and the major branch of filaments for F3 (blue dotted line); and position C3 for F2 (red solid line).
Paper: Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
Authors: Yu-Xin He, Hong-Li Liu, Xin-Di Tang, Sheng-Li Qin, Jian-Jun Zhou, Jarken Esimbek, Si-Rong Pan, Da-Lei Li, Meng-Ke Zhao, Wei-Guang Ji, Toktarkhan Komesh
Figure caption: Left: 13CO position–velocity diagram as a function of the distance along the main skeleton (see Figure 5) from the southern to northern end. The color scale is displayed after taking the square root. The white arrows represent the positions of C1, C2, and C3. Right: same as the left panel, but for C18O.
Paper: Ultra-deep Keck/MOSFIRE Spectroscopic Observations of z ∼ 2 Galaxies: Direct Oxygen Abundances and Nebular Excitation Properties
Authors: Leonardo Clarke, Alice Shapley, Ryan L. Sanders, Michael W. Topping, Tucker Jones, Mariska Kriek, Naveen A. Reddy, Daniel P. Stark, Mengtao Tang
Figure caption: [N II], [S II], and [O I] BPT diagrams showing where the auroral and [O I] galaxy samples from this work lie in relation to SDSS galaxies in the local Universe (grayscale, 2D histogram). We also compare the galaxies and stacks from this work to local H II regions from the literature (compiled by Sanders et al. 2017) and display a running median. The [O III] auroral targets are shown by squares, while the non-[O III]-auroral targets are shown by diamonds. The 1 ≤ z < 2 and 2 ≤ z ≤ 3 targets are displayed in blue and orange, respectively. For comparison, stacks of z ∼ 1.5 and z ∼ 2.3 galaxies from Shapley et al. (2019) are shown as purple and red triangles, respectively. Upper limits on [S II] and [O I] detections are shown in black. In the bottom three panels, the same BPT diagrams are shown with CLOUDY photoionization models overlaid. The curves are color-coded by stellar metallicity, indicated in the color bar.
Paper: Radial and Local Density Dependence of Star Formation Properties in Galaxy Clusters from the Hyper Suprime-Cam Survey
Authors: Hung-Yu Jian, Lihwai Lin, Bau-Ching Hsieh, Keiichi Umetsu, Carlos Lopez-Coba, Masamune Oguri, Connor Bottrell, Yoshiki Toba, Yusei Koyama, Yu-Yen Chang, Tadayuki Kodama, Yutaka Komiyama, Surhud More, Kai-Yang Lin, Atsushi J. Nishizawa, Ichi Tanaka
Figure caption: The quiescent fractions (f  q ) as a function of the normalized cluster-centric radius in three redshift ranges. Five different color lines represent five different mass ranges. The dashed vertical lines denote the cluster boundary. The error bars are estimated using bootstrap resampling. Normalized for mass and redshift, f  q  still exhibits an apparent correlation with r  p /r 200m , i.e., f  q  decreases with the increasing r  p /r 200m , indicating a significant radial effect.