adsabs/AstroCLIMB huggingface dataset:
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 evolution of polarization (V, L) and DM with orbital phases in HMCBs.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Cumulative star formation and H I gas mass growth for isolated dwarfs, binned by z = 0.05 stellar mass. Individual growth tracks are shown for quiescent dwarfs (red lines), while the median growth track for star-forming dwarfs (blue line) is shown with interquartile ranges. We show the median value of t 90 for quiescent (red dashed) and star-forming (blue dashed) dwarfs. Left: cumulative star formation history over cosmic time for isolated dwarfs. In all panels, quiescent dwarfs grow stars more rapidly than star-forming dwarfs, and quench earlier. More massive dwarfs tend to quench at earlier times than less massive dwarfs, but all generally quench by redshift z = 0.5. Right: total mass of cool, star-forming H I gas as a function of the cosmic time. On average, star-forming dwarfs grow slowly in H I mass over time. The majority of quiescent dwarfs instead rapidly lose H I gas around the time of t 90, and remain devoid of H I. Six quiescent dwarfs regain small amounts of H I after the initial episode, reigniting low levels of star formation.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Quiescent fraction for isolated dwarf galaxies in ROMULUS25 (blue solid), EAGLE (yellow dashed), ILLUSTRISTNG (red dotted–dashed), SIMBA (purple dotted), and SDSS (Geha et al. 2012, black squares). Each curve represents the median across 25 randomly selected sight lines for galaxies above a limiting apparent magnitude of m  r  = 17.7 and an r-band surface brightness of μ  r  = 23 mag arcsec−2, with the shaded regions representing the 95% binomial uncertainties averaged across all sight lines (see text for details). All simulations except ILLUSTRISTNG tend to reproduce the quiescent fraction for higher-mass dwarfs M star > 2 × 109 M ⊙, but every simulation predicts 5–15× more quiescent low-mass dwarfs than found in observations.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Median quiescent fraction across all 25 randomly selected sight lines (blue solid), highlighting the contribution from dwarfs with central MBH (yellow dashed) vs. dwarf galaxies entirely without MBHs (purple open circle). The median quiescent fraction for dwarfs without MBHs frequently falls below the lower limits of the figure, in which case they are marked by an unfilled arrow with upper limits on the uncertainties. Dwarfs with central MBHs are 2–10× more likely to be quiescent relative to dwarfs without MBHs. Dwarfs with central MBHs elevate the overall quiescent fraction for isolated dwarfs while dwarfs without MBHs exhibit quiescent fractions consistent with those found in SDSS at M star < 109 M ⊙ (Geha et al. 2012, black squares).
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Instantaneous (top) and 100 Myr averaged (bottom) intrinsic SFR vs. stellar mass for isolated dwarfs at z = 0.05. Quiescent dwarfs (red circles) selected through Hα EW and D n4000 exhibit lower SFRs at fixed stellar mass than star-forming dwarfs (blue dots). The SFR–M star relation derived from star-forming dwarfs (blue-shaded interquartile range) approximately agrees with the main sequence found from SDSS (Hahn et al. 2019), though simulation SFRs are slightly overpredicted at the highest masses shown. 64% of isolated, quiescent dwarfs in ROMULUS25 have 100 Myr averaged SFR below 10−4 M ⊙ yr−1.
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: Comparison between our model and observations of FRB 20201124A. (a) The observed oscillating polarization structure of the burst 926 of FRB 20201124A (Xu et al. 2022). The points represent the observation data, and the lines represent the fitting line with ν RM ≃ 11.0 GHz,  ν CM ≃ 0.4 GHz. Here the parameters are fiducial due to the model’s complexity. (b) The outgoing CP as a function of the squared wavelength based on Equation (30). Compared with the black line, the orange line has a smaller amplitude, leading to a smaller oscillation rate.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Similar to Figure 4, median growth tracks for specific star formation rate (sSFR) scaled by the mean sSFR for star-forming dwarfs in the same mass range. For clarity, we show only the median growth tracks for both quiescent dwarfs (red lines) and star-forming dwarfs (blue lines), along with their interquartile ranges. We show the median value of t 90 for quiescent (red dashed) and star-forming (blue dashed) dwarfs. Quiescent dwarfs start with comparable levels of specific star formation at early times, then decrease in sSFR relative to star-forming dwarfs around t 90. By z = 0.05, quiescent dwarfs exhibit ≲1 dex lower sSFR.
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 orbital evolution of the degree of LP/CP and DM. Panel (a) shows the evolution of the degree of LP/CP with different frequencies. The higher the frequency, the narrower the window for the FC. Panel (b) shows the evolution of the degree of LP/CP with different ν  T . The higher ν  T , the wider the window. Panel (c) shows the DM evolution with different wind densities at the companion surface. The larger n w,0, the larger the DM.
Paper: Rest-frame Near-infrared Radial Light Profiles up to z = 3 from JWST/NIRCam: Wavelength Dependence of the Sérsic Index
Authors: Marco Martorano, Arjen van der Wel, Eric F. Bell, Marijn Franx, Katherine E. Whitaker, Angelos Nersesian, Sedona H. Price, Maarten Baes, Katherine A. Suess, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Gabriel Brammer
Figure caption: Median Sérsic index (and 16–84th percentile ranges as shaded areas) of the quiescent and star-forming population as a function of the rest-frame wavelength. Error bars indicate the statistical uncertainty in the median (﹩{\sigma }_{n}/\sqrt{N}﹩) at log-spaced wavelengths. Solid lines show a spline regression to the medians as outlined in the text. Dashed gray horizontal lines represent the overall median, integrated over the wavelength. The dotted lines show the low-z GAMA comparison sample. For both star-forming and quiescent galaxies we see no strong change in n with λ REST from the near-UV to the near-IR.
Paper: Rest-frame Near-infrared Radial Light Profiles up to z = 3 from JWST/NIRCam: Wavelength Dependence of the Sérsic Index
Authors: Marco Martorano, Arjen van der Wel, Eric F. Bell, Marijn Franx, Katherine E. Whitaker, Angelos Nersesian, Sedona H. Price, Maarten Baes, Katherine A. Suess, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Gabriel Brammer
Figure caption: Upper panel: Sérsic index at 0.5 μm against Sérsic index at 1.1 μm color coded with A  V  (from the PROSPECTOR SED fits). Blue and red solid lines show the median for star-forming and quiescent galaxies, respectively, computed as explained in the text. Error bars show the statistical uncertainty (84–16th percentiles ﹩/\sqrt{N}﹩). In the lower right corner is shown the median (and 16–84th percentiles) ratio n 0.5μm/n 1.1μm for the whole sample, the star-forming population and the quiescent population. In the upper left corner in black are shown the median uncertainties. Lower panel: ratio between Sérsic index at 0.5 and 1.1 μm against A  V . Only galaxies with S/N > 100 are included in this figure to highlight the trend with A  V . In the lower right corner in black is shown the median uncertainty propagated to the ratio of Sérsic indices.
Paper: Rest-frame Near-infrared Radial Light Profiles up to z = 3 from JWST/NIRCam: Wavelength Dependence of the Sérsic Index
Authors: Marco Martorano, Arjen van der Wel, Eric F. Bell, Marijn Franx, Katherine E. Whitaker, Angelos Nersesian, Sedona H. Price, Maarten Baes, Katherine A. Suess, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Gabriel Brammer
Figure caption: Sérsic indices at 1.1 μm (top row), 0.5 μm (mid row) and their ratio (bottom row) vs. the stellar mass, color coded as star-forming (blue) and quiescent (red). The left column shows galaxies at 0.5 ≤ z < 1.5; the right column shows galaxies at 1.5 ≤ z ≤ 3. Blue and red lines show the medians for the star-forming and quiescent galaxies, respectively, while the black lines represent the full (combined) sample. Median lines are computed as described in Section 3.1 with a smoothing factor of 0.3 for the quiescent population and 1 for the star-forming and the whole sample. Error bars show the statistical uncertainty (84–16th percentiles ﹩/\sqrt{N}﹩) in bins of width 0.5 dex for the quiescent population and 0.25 dex for the others. In the lower right corner of each panel a black error bar represents the median uncertainty for the whole sample. We see a clear dependence of n on the stellar mass, regardless of the wavelength and redshift, and no significant evidence for a mass- or redshift dependence for n 1.1μm/n 0.5μm.
Paper: Rest-frame Near-infrared Radial Light Profiles up to z = 3 from JWST/NIRCam: Wavelength Dependence of the Sérsic Index
Authors: Marco Martorano, Arjen van der Wel, Eric F. Bell, Marijn Franx, Katherine E. Whitaker, Angelos Nersesian, Sedona H. Price, Maarten Baes, Katherine A. Suess, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Gabriel Brammer
Figure caption: Upper panel: comparison between the HST/F160W Sérsic indices from van der Wel et al. (2012; y-axis) and the HST/F160W Sérsic indices derived in this paper (x-axis) color coded by the ﹩{\mathrm{log}}_{10}({\rm{S}}/{\rm{N}})﹩. Lower panel: comparison of the Sérsic indices from the JWST/NIRCam filter F150W and HST/WFC3 filter F160W (this paper). Filled circles represent F150W estimates with the WebbPSF-based model PSF while open circles show F150W estimates with the empirical PSF. Dark-gray and light-gray solid lines show linear fits, respectively, of the model PSF and empirical PSF data sets after 3σ clipping. In the lower right corner of each panel are reported the median ratios and the 16–84th percentile intervals. Next to the legends we show the median uncertainties. The first panel shows that the agreement with literature results is remarkable, while the second highlights how differences between the empirical and model PSFs arise mostly for high values of n.
Paper: Rest-frame Near-infrared Radial Light Profiles up to z = 3 from JWST/NIRCam: Wavelength Dependence of the Sérsic Index
Authors: Marco Martorano, Arjen van der Wel, Eric F. Bell, Marijn Franx, Katherine E. Whitaker, Angelos Nersesian, Sedona H. Price, Maarten Baes, Katherine A. Suess, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Gabriel Brammer
Figure caption: First panel: Galaxy 5751 in the Leja et al. (2020) catalog with M = 109.84 M ⊙ and redshift z = 0.74; second panel: Galaxy 11438 with M = 109.60 M ⊙ and redshift z = 0.98; third panel: Galaxy 10662 with M = 109.53 M ⊙ and redshift z = 2.49; fourth panel: Galaxy 14128 with M = 109.60 M ⊙ and redshift z = 2.98. For each of the four sets, the first row shows the original image, the second row the model used, and the third row the residuals. Per each galaxy the color of the panels spans the same scale in all the filters. Cutouts have been cropped with respect to those adopted for the fit to enhance galaxy visibility. Together with the model, in the bottom right corner, is shown the measured Sérsic index in each filter. In case that the fit of a filter failed, the value of Sérsic index reported is nan.
Paper: Rest-frame Near-infrared Radial Light Profiles up to z = 3 from JWST/NIRCam: Wavelength Dependence of the Sérsic Index
Authors: Marco Martorano, Arjen van der Wel, Eric F. Bell, Marijn Franx, Katherine E. Whitaker, Angelos Nersesian, Sedona H. Price, Maarten Baes, Katherine A. Suess, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Gabriel Brammer
Figure caption: Sérsic index at 1.1 μm rest frame against the sSFR in two redshift bins, color coded with the ratio between the Sérsic indices at 1.1 μm and at 0.5 μm. The solid line shows the median for the whole sample in sSFR bins while the dashed lines show the 16–84th percentiles. In the upper left corner of each panel a black error bar shows the median uncertainty in n 1.1μm. Low-sSFR galaxies have systematically larger Sérsic indices in the rest-frame near-IR.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The distribution of ∣θ 2D∣ for galaxies binned by M vir (left) and M * (right) at z = 0. Dots show the measurements from TNG300 and lines show the best-fit TSE distribution with two free parameters, A and B.
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 distnr parameter, which quantifies the offset of a source from its host galaxy center (shown in a stacked histogram) for all detections of SNe, TDEs, and the BFF. The vertical lines at the top denote the average value for each class. The number of total detections per class of events is shown in parentheses in the legend. While TDEs show a lower average offset compared to SNe, the difference is not large enough to be used a discriminant.
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: Redshift distribution (shown in a stacked histogram) of the 241 classified candidates of interest with redshifts on the TNS. The number of events in each class is denoted in parentheses in the legend.
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: Numbers and fractions of the classes of candidates of interest from the different Lasair 1.0 queries, as detailed in the text and in Table 1. The numbers in parentheses next to each subplot title denote the total number of events in that query.
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: The same as Figure 2, but for classified events only.
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: Morphology of G326 seen at Spitzer 8 μm and Herschel 70, 160, 250, 350, and 500 μm. The green circles, magenta ellipses, and red rectangles mark the Herschel 70 μm point sources, the dust clumps (Urquhart et al. 2014a), and the compact ArTéMiS sources (Peretto et al. 2020), respectively. In panel (a), part of the black dashed circle indicates the infrared bubble MWP1G326725+007745 (Simpson et al. 2012). The dust clumps are referred to as C1, C2, and C3. In panel (d), two green rectangles show the areas covered by the Millimetre Astronomy Legacy Team 90 GHz (MALT90) Survey (Jackson et al. 2013). The five subfilaments are referred to as F1, F2, F3, F4, and F5. The major branch of filaments, composed of F1 and F2 (longest, and represented as F1+F2 in Table 2), and branched skeletons are shown as blue and yellow curves, respectively. In panel (f), the outlined subregion is the masking area used in the algorithm FilFinder (Koch & Rosolowsky 2015) and is used to trace the major branch of the filaments.
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: Merger rate per galaxy (left y-axes) and merger probability (right y-axes) for simulated galaxies as a function of halo mass M halo (upper panels) and local number density of galaxies ρ 10 (lower panels). The results for major mergers (μ ≥ 0.2) are shown in the left panels, while the results for minor mergers (0.01 ≤ μ < 0.2) are displayed in the right panels. The target galaxies used in this figure are quiescent galaxies at z = 0 from the galaxy formation simulation of Guo et al. (2011) based on the Millennium-II simulation (Boylan-Kolchin et al. 2009). The mergers that occur by z < 0.63 are counted to calculate the merger rates of the target galaxies. The data points are differentiated by shape (and color) to indicate the different stellar mass bins. The bins in which more than 75% of mergers are gas-rich ones are marked by the blue filled circles.
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 relations of quiescent galaxies in different environments with the fitted broken power-law functions of Equation (5) overlaid on the relations. The mass–size relations of the different environment bins are displayed in the separate panels, each with its own color. A square indicates the mean ﹩\mathrm{log}{R}_{e}﹩ of the mass bin (with a bin size of 0.1 dex), after excluding outliers beyond 5σ. The error bars indicate the standard error of the mean. This figure shows only bins with a minimum of 25 galaxies. The colored dashed lines in each panel represent the 25th and 75th percentiles of R  e . The colored solid line in each panel indicates the smoothly broken power-law function fitted to each mass–size relation. The mass–size relation of all quiescent galaxies and its fitting result are shown in all the panels as the black squares and the black solid lines. In the upper left panel, we also display the smoothly broken power-law function (the black dashed line or dotted line) fitted to the mass–size relation of star-forming galaxies with Σ10/Mpc−2 ≥ 1.14 and Σ10/Mpc−2 < 1.14, for the purpose of comparison. The gray dashed (or dotted) lines in the upper left panel represent the 25th and 75th percentiles of R  e  for star-forming galaxies. The units of Σ10 in the legends 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: Mass–size relations of quiescent galaxies in various environments, when using alternative definitions for quiescent galaxies, size, and environment. Panel (a): the case when Σ M  (Equation (4)) is used as the definition of environment instead of Σ10. The units of Σ M  are M ⊙ Mpc−2. Panel (b): the case when the r- band Petrosian 90% light radius (R  p90) is used instead of R  e . Panel (c): the case when the main criterion to select quiescent galaxies is EW(Hα) ≥ −1 Å. Panel (d): the case when quiescent galaxies are selected using the combination of a Sérsic index cut of n ≥ 2.5 and the color cut of Equations (1) and (2). The four environment bins in each panel are set to correspond to percentile ranges of 0%–10%, 10%–40%, 40%–80%, and 80%–100%, respectively, as in the main text. The other details in each panel are the same as those in Figure 7.
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: Best-fit parameters (α, β, and ﹩\mathrm{log}{M}_{p}﹩) for the smoothly broken power-law functions (Equation (5)) for the different environment bins. The circles with different colors represent the parameters of the different environment bins. The black horizontal line with the dark gray area in each panel represent the best-fit parameter with its error for all quiescent galaxies. Similarly, the black dashed line with the light gray area indicates the best-fit parameter with its error for star-forming galaxies with Σ10/Mpc−2 ≥ 1.14. 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: Mean R  e  and Sérsic index (n) as a function of environment, with the exclusion of outliers beyond 5σ in the calculation of the mean value. Low percentiles correspond to low-density environments. The data points are differentiated by shape to indicate the different stellar mass bins. The error bars indicate the standard error of the mean.
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: Correlation between the colors and sizes of our quiescent galaxies in the different environments (the left panel is for u − r and the right panel is for r − z). Each data point (the triangle) represents the mean ﹩\mathrm{log}{R}_{e}﹩ of the color bin, after excluding outliers beyond 5σ. The error bars denote the standard error of the mean. The data points are differentiated by shape to indicate the different stellar mass bins and by colors to represent the different environment bins. The four color bins correspond to percentile ranges of 0%–25%, 25%–50%, 50%–75%, and 75%–100%, respectively, for the colors of LQGs and HQGs. 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: Distribution of ﹩\mathrm{log}{R}_{e}﹩ for LQGs with ﹩9.4\leqslant \mathrm{log}({M}_{\mathrm{star}}/{M}_{\odot })\lt 9.8﹩ (the left panel) and HQGs with ﹩10.5\leqslant \mathrm{log}({M}_{\mathrm{star}}/{M}_{\odot })\lt 10.7﹩ (the right panel). The different colors represent the different environment bins. The units of Σ10 in the legend are Mpc−2.
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 fraction f  q  shown as a function of local overdensity ﹩{{\rm{log}}}_{10}(1+{\delta }_{6})﹩ in the range of 0 < r  p /r 200m  < 0.25, 0.25  < r  p /r 200m  < 0.5, 0.5 < r  p /r 200m  < 0.75, 0.75 < r  p /r 200m  < 1.0, and r  p /r 200m  > 1.0 from left to right, and in redshift ranges of 0.2 < z < 0.5, 0.5 < z < 0.8, and 0.8 < z < 1.1, from top to bottom. Four log-mass ranges are 8.6 < log M < 9.2 (pink), 9.2 < log M < 9.8 (blue), 9.8 < log M < 10.4 (green), and 10.4 < log M < 11.0 (yellow). At fixed r  p /r 200m , mass, and redshift, f  q  correlates with the overdensity, i.e., f  q  moderately increases with increasing overdensity, suggesting a pure density effect functioning in dense regions. The density effect’s contribution seems comparable to the radial effect for low-mass galaxies.