adsabs/AstroCLIMB huggingface dataset:
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 green valley fraction (f  g ) on the top panels and effective green valley fraction (﹩\widetilde{{f}_{g}}﹩) on the bottom panels as a function of the normalized host-centric radius in three redshift ranges. From high-mass galaxies, we find an f  g  deficit in clusters relative to the field, indicating an insufficient supply of progenitors of green valley galaxies, i.e., star-forming galaxies. The ﹩\widetilde{{f}_{g}}﹩ is the fraction of star-forming to nonquiescent galaxies to account for the deficit issue. The ﹩\mathop{{f}_{g}}\limits^{\unicode{x0007E}}﹩ decreases with increasing r  p  and is roughly independent of r  p , implying a weakly radial-dependent slow quenching effect in the dense environment, consistent with our results in Section 3.1.1.
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: Best-fit results as a function of mass for the parameter α (the slope) and β (the central f  q ) using a linear function of f  q  = α  ×  (r  p /r 200m ) + β. Three different redshift ranges are 0.2 < z < 0.5 (red), 0.5 < z < 0.8 (green), and 0.8 < z < 1.1 (blue). The slope α is generally steeper for low-mass galaxies than for high-mass ones, implying a stronger radial effect for low-mass galaxies. The other trend is that the central f  q  increases moderately with the decreasing redshift and, apparently, with increasing stellar mass.
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: Similar to Figure 6, the quiescent fraction f  q  is plotted as a function of normalized cluster-centric radius in four density ranges, i.e., 0.2 < log10(1 + δ 6) < 0.5, 0.5 < log10(1 + δ 6) < 0.8, 0.8 < log10(1 + δ 6) < 1.1, and 1.1 < log10(1 + δ 6) < 1.4. In addition, four mass ranges at low z are denoted by four colors and three redshift bins, as indicated in the plot. It is evident that controlling for mass, redshift, and overdensity, the radial trend of f  g , i.e., that f  g  decreases with increasing r  p /r 200m , is apparent. The result implies that the quenching contribution from a pure radial effect is significant, and the mechanism is likely to be ram pressure stripping.
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: Similar to Figure 5, the best-fit results of the fitting slope α and fraction at center β for f  g  (top row) and ﹩\widetilde{{f}_{g}}﹩ (bottom row). For f  g , the radial gradient at low mass is negative and becomes positive at high mass, implying an excess at low mass and a shortage at high mass respective to the field.
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: Similar to Figure 7, the best-fit results of α and β for f  q . From left to right, the cluster galaxy subsamples are for the overdensity in the range of 0.2 < log10(1 + δ 6) < 0.5, 0.5 < log10(1 + δ 6) < 0.8, 0.8 < log10(1 + δ 6) < 1.1, and 1.1 < log10(1 + δ 6) < 1.4. Three different redshift ranges are 0.2 < z < 0.5 (red), 0.5 < z < 0.8 (green), and 0.8 < z < 1.1 (blue). The radial gradient αs are roughly independent of mass, redshift, and overdensity. By contrast, βs moderately depend on redshift and depend on stellar mass but have weak overdensity dependency.
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 fraction of star-forming, quiescent, and green valley galaxies plotted as a function of overdensity log10(1 + δ 6) at low (top row), medium (middle row), and high (bottom row) redshift. In each panel, different color lines represent results in different mass ranges. At low mass, the color–density relation, i.e., the fact that f  q  increases with overdensity, is prominent, while at high mass, the trend becomes weaker. In addition, f  q  appears to be independent of the overdensity but slightly depends on stellar mass and redshift.
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: Left panel: S/N in the HST/ACS filter F160W (empty circles) and JWST/NIRCam F150W (filled circles) against redshift. The horizontal dashed black line shows the reference S/N = 50. Central panel: stellar mass against redshift. Right panel: sSFR against redshift. In the central and right panels red and blue colors are used to identify quiescent and star-forming galaxies. Circles define galaxies used in this work while stars show galaxies rejected according to Sections 2 and 2.2. Black squares are galaxies with S/N < 50 in F150W that are not rejected.
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 long-term average spectra from INTEGRAL SPI (green squares), ISGRI (blue stars) with NuSTAR/FPMA (black diamonds) and FPMB (red triangles) and LAT (magenta crosses). The left panel shows the log-parabola+zpowerlw model (black dashed line) with the individual continuum components shown as red dotted lines. The right panel shows the CompTT+log-parabola+zpowerlw model (black dashed line) with individual continuum components as red dotted lines.
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 long-term average spectra from INTEGRAL SPI (green squares) and ISGRI (blue stars) with NuSTAR/FPMA (black diamonds) and FPMB (red triangles). The best-fit CompTT model with kT  e  = 0.5 keV (cyan dotted–dashed line) and the log-parabola model (black dashed line) are overplotted.
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: Velocity and H2 column density distributions extracted along the main skeleton of the filament. Top panel: density distribution. Density peaks related to the three dense clumps of C1, C2, and C3 are indicated by vertical green solid lines with yellow shadows. The width of each yellow shadow is the size of clump. Bottom panel: the red filled points are 13CO (J = 2–1) velocities, and fitted with a sine function with a wavelength of ∼3.6 pc and an amplitude of ∼0.38 km s−1. The fitting curve is shown as the red solid line. The blue open squares are C18O (J = 2–1) velocities, and fitted with a sine function with a wavelength of ∼3.4 pc and an amplitude of ∼0.31 km s−1. The fitted curve is shown as the solid blue line. The vertical shift of the sine function, representing the systemic velocity, is indicated by a horizontal dashed line at V lsr = −37.7 km s−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: FWHM velocity width distributions of 13CO (left panel) and C18O (right panel) for G326, which were derived from the moment method. 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. The main and branched skeletons are shown as white and black curves, respectively. The filled magenta circle in the lower right corner indicates the beam size of the CO observation by APEX.
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: Mean spectra of HCO+(J = 1–0) and N2H+(J = 1–0) across the two dense clumps C2 (top panel) and C3 (bottom panel). The N2H+(J = 1–0) hfs fit is shown in green. The dashed red lines in the profiles indicate the peak velocities of N2H+(J = 1–0).
Paper: Evolution of a Water-rich Atmosphere Formed by a Giant Impact on an Earth-sized Planet
Authors: Kenji Kurosaki, Yasunori Hori, Masahiro Ogihara, Masanobu Kunitomo
Figure caption: Snapshots of the SPH simulation of a head-on collision with the impact velocity of the mutual escape velocity. From left to right, snapshots show the time at t = 0, 1τ ff, 3τ ff, and 50τ ff. Both the target and the impactor have a 1 M ⊕ core with 10 wt% of the H2 atmosphere. Green and blue particles denote the atmospheric and core components bound on the postimpact planet, respectively. Red and black particles denote the escaping atmospheric and core components, respectively. Both horizontal and vertical axes are normalized by the radius of the target, R T.
Paper: Evolution of a Water-rich Atmosphere Formed by a Giant Impact on an Earth-sized Planet
Authors: Kenji Kurosaki, Yasunori Hori, Masahiro Ogihara, Masanobu Kunitomo
Figure caption: Schematic of our planetary model. The planetary interior is composed of two parts: a spherical symmetry convective interior and a plane-parallel radiative–convective (R-C) equilibrium atmosphere. The interior structure in spherical symmetry is composed of a rocky core and an H2–He–H2O envelope. The plane-parallel atmosphere is composed of H2–He–H2O (see also Section 3.2).
Paper: Measuring the Soft Excess Region Size Relative to the Corona in Active Galactic Nuclei with NICER
Authors: A. Zoghbi, J. M. Miller
Figure caption: Illustration of the different configurations that correspond to the different models proposed for the soft excess. The left scenario is for a relativistic reflection model, where the hot corona (blue) illuminates the disk producing emission lines, which when produced very close to the black hole are broadened and smeared out. The other two images are for the case of a warm corona: a layer above the disk that is heated by internal dissipation that is distinct from the hot corona (Ponti et al. 2013), and a colocated hot and warm corona that radiates inward of some radius R corona, while a standard disk emits outside it (Done et al. 2012).
Paper: Measuring the Soft Excess Region Size Relative to the Corona in Active Galactic Nuclei with NICER
Authors: A. Zoghbi, J. M. Miller
Figure caption: Results of the PSD modeling for the fluxes of the blackbody (F bb) and the coronal power-law components (F  p ) for 1H0707-495, MRK 335, and TON S180. Top: the measured PSD values at 10 frequency bins as calculated using fqlag. The values and errors are the median and standard deviation from the MCMC chains. The y-axis is in units of rms-normalized PSD and x-axis is the logarithm of the Fourier frequency. Bottom: smoothed density estimates for the probability density of the key parameter of interest, resulting from modeling the PSDs in the top panel by either a zero-centered Lorentzian model (1H0707-495) or power-law model (MRK 335 and TON S180). For the former case, the logarithm of the break frequency is plotted, while for the latter, the integrated variability power (integral under the power-law PSD) in percentage units is plotted.
Paper: Measuring the Soft Excess Region Size Relative to the Corona in Active Galactic Nuclei with NICER
Authors: A. Zoghbi, J. M. Miller
Figure caption: Probability density of the relative size of the soft excess to the hot corona. The relative size is obtained as the ratio of the summary parameter for soft excess flux (F bb) and the corona (F  p ). For 1H0707-495, the summary parameter is the PSD break frequency, while for the TON S180 and MRK 335, we use the total integrated rms variability. The 1σ  single value estimates from these probability densities are ﹩{3.7}_{-1.5}^{+2.7}﹩, ﹩{2.2}_{-0.6}^{+1.0}﹩, and ﹩{0.9}_{-0.4}^{+1.0}﹩ for 1H0707-495, MRK 335, and TON S180, respectively.
Paper: Measuring the Soft Excess Region Size Relative to the Corona in Active Galactic Nuclei with NICER
Authors: A. Zoghbi, J. M. Miller
Figure caption: The count rate light curves in the 0.3–10 keV band from all observations. The x-axes are in units of Modified Julian Date, and they all span the same ∼580 days.
Paper: Two Candidate Pulsar TeV Halos Identified from Property-similarity Studies
Authors: Dong Zheng, Zhongxiang Wang
Figure caption:  γ-ray spectra (black dots) of J1958 (left) and J2028 (right) in the 0.1–500 GeV range obtained from their on-pulse data and the corresponding best-fit PLSEC models (dashed curves). From the off-pulse data, the upper limits derived by assuming a power law with Γ = 2 are shown as the red lines. The fluxes or flux upper limits from different VHE observations of the source regions are also shown, which include in the left panel, 1LHAASO J1959+2846u measured with the Kilometer Squared Array (KM2A) and Water Cherenkov Detector Array (WCDA; Cao et al. 2023), MGRO J1958+2848 (Abdo et al. 2009b), VERITAS upper limits on J1958 (Archer et al. 2019), and MAGIC upper limits on the PWN of J1958 (Fernandez-Barral et al. 2017), and in the right panel 1LHAASO J20283352 and MGRO upper limit on J2028.
Paper: Two Candidate Pulsar TeV Halos Identified from Property-similarity Studies
Authors: Dong Zheng, Zhongxiang Wang
Figure caption: TS maps of the J1958 (left) and J2028 (right) regions in the 0.1–500 GeV range calculated for the off-pulse phase ranges of the two pulsars. In the left panel, the positional error circle and extension of 1LHASSO J1959+2846u (Cao et al. 2023) are denoted by white solid and dashed circles, respectively, which are coincident with J1958's position (red diamond). Also shown are the positional error circles of 3HWC J1957+291 (pink dashed circle; Albert et al. 2020) and LHAASO J1956+2845 (red dashed circle; Cao et al. 2021). In addition, two candidate SNRs, G65.8-0.5 and G66.0-0.0 (denoted by yellow dashed and cyan dashed ellipses, respectively), reported in Sabin et al. (2013) are located in the region as well. In the right panel, the positional error circle and extension of 1HASSO J2028+3352 are denoted by white solid and dashed circles, respectively. The pulsar J2028, along with two Fermi-LAT sources, are located in the error circle.
Paper: Two Candidate Pulsar TeV Halos Identified from Property-similarity Studies
Authors: Dong Zheng, Zhongxiang Wang
Figure caption: Left panel: luminosity values at 50 TeV from the LHAASO measurements of the (candidate) teraelectronvolt halos vs. ﹩\dot{E}﹩ of the pulsars. A relationship of ﹩{L}_{50\mathrm{TeV}}\simeq 2.5{\dot{E}}^{0.90}﹩ (denoted as the dashed line) can approximately fit the data points. Right panel: ratios of the luminosity values at 50 TeV to ﹩\dot{E}﹩ of the pulsars, which shows that the ratios are around the value of ≃5.9 × 10−4 (denoted by the dashed line) despite the large age differences of the pulsars. In addition, an age-dependent relationship, ﹩1.2\times {10}^{-3}{\tau }_{\mathrm{kyr}}^{-0.18}﹩, is also shown as the dotted line (see Section 3.3).
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: SFR vs. stellar mass. The colored squares indicate the auroral-line targets included in this study, with blue and orange corresponding to z ∼ 1.7 and z ∼ 2.5, respectively. The gray points indicate the nonauroral targets included in this study. The dashed black line shows a linear fit from Shivaei et al. (2015), while the solid blue and orange lines show the z ∼ 1.7 and z ∼ 2.5 SFR vs. stellar mass relations, respectively, from Speagle et al. (2014). The 1σ scatter for each main-sequence line is shaded in its respective color. The red triangles represent spectral stacks of z ∼ 2.3 galaxies from Sanders et al. (2021).
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: Composite spectra of the [O III] auroral targets. The black curve shows the luminosity density, while the error spectrum is shown in red in the inset axes. Each of the prominent emission lines is labeled and marked with a blue dotted line.
Paper: Two Candidate Pulsar TeV Halos Identified from Property-similarity Studies
Authors: Dong Zheng, Zhongxiang Wang
Figure caption: Phase-connected pulse profile (top) and two-dimensional phaseogram (bottom) constructed for J1958 (left) and J2028 (right). Two spin cycles are shown for clarity. The on-pulse and off-pulse phase ranges are denoted by dashed lines.
Paper: Detection of a ∼0.1c Radio Knot in M81* Associated with a Moderate X-Ray Flare
Authors: Xuezheng Wang, Wu Jiang, Zhiqiang Shen, Zhen Yan, Ya-Ping Li, Ivan Martí-Vidal, Roman Gold
Figure caption: The figure shows the degree of linear polarization with the blue color bar, EVPA, and polarization flux with gray contours at 8.8 GHz observed on 2018 June 10.
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 of the SIMBA samples used for observational comparison. Galaxy samples were chosen to match the mean stellar stellar mass. Left: sample at z = 1. SIMBA galaxies are cut to exclude any with M * < 1.3 × 1011 M ⊙. Observational data from Meinke et al. (2023) is shown in black. Right: sample at z = 0.5. SIMBA galaxies are cut to exclude any with M * > 5.5 × 1011 M ⊙. The distribution of the observational data from Schaan et al. (2021) is shown in black.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Radial profiles showing the ratio of Σ(m = 1)/Σ(m = 0) and Σ(m = 2)/Σ(m = 0) for two galaxy samples at z ≈ 1 (left) and z ≈ 0.5 (right). Here, m refers to the number of folds in the symmetry, and higher values represent more asymmetries in the stacked tSZ signal. The lower signals of the AGN stacks can be attributed to the smoothing of gas by AGN feedback in SIMBA. The difference between the m = 1 and m = 2 curves at z ≈ 0.5 suggests a dipole distribution in the stack, most likely due to galaxies clustering together over time.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Radial profiles of the temperature change in the CMB at 150 GHz due to the tSZ effect at z ≈ 0.5 for stacked galaxies convolved with a 2.′1 beam and CAP filter to compare against observational data from Schaan et al. (2021; black). The kiloparsec scale on the upper x-axis is calculated using the mean z of the three snapshots (≈0.55). At this lower redshift, we see less of an agreement between SIMBA and observation. Shaded regions represent 1σ errors on the SIMBA results.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Compton-y radial profile at small radii for SIMBA data convolved with a 9.″5 beam. Shown are the radial profiles for massive galaxies run with AGN feedback (red), and massive galaxies run without AGN (teal). Also shown in gray is the N-AGN sample without making the upper cut on stellar mass. While this is an unphysical galaxy population, we show it to demonstrate why the behavior at high redshifts differs from that at low. The vertical blue line shows the median virial radius for the AGN galaxy sample, with shaded regions representing the first and third quartiles.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Examples of stacked tSZ-y maps for 165 galaxies larger than 1011 M ⊙ from the AGN sample at z = 1. The regions shown are 15′ across, and the black circle represents a region with a 2′ radius used to calculate the thermal energy. We show how the stacks differ when convolved with two different beams. Left: ACT beam, FWHM = 2.′1 at 90 GHz. Right: TolTEC beam, FWHM = 9.″5 at 150 GHz.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Compton-y radial profiles at z ≈ 1 for stacked galaxies convolved with a 2.′1 beam to compare against observational data from Meinke et al. (2023; black). The kiloparsec scale on the upper x-axis is calculated using the mean z of the three snapshots (≈1.1). We see strong agreement between the observations and the AGN-Q galaxies from SIMBA. Shaded regions represent 1σ errors on the SIMBA results.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Compton-y radial profile as a function of redshift for SIMBA data convolved with a 2.′1 beam. Shown are the radial profiles for massive galaxies run with AGN feedback, quiescent and massive galaxies with AGN feedback (AGN-Q), and massive galaxies run without AGN (N-AGN). The vertical blue line shows the median virial radius for the AGN galaxy sample, with shaded regions representing the first and third quartiles. The median radius in kpc is 480, 420, 300, and 220 for z = 0.2, 0.5, 1, and 1.5, respectively.
Paper: Distinguishing Active Galactic Nuclei Feedback Models with the Thermal Sunyaev–Zel’dovich Effect
Authors: Skylar Grayson, Evan Scannapieco, Romeel Davé
Figure caption: Projected map of the Compton-y parameter at redshift 1 (left) and 0.5 (right) for SIMBA run with all AGN feedback on. The black dots represent the locations of the galaxies used for our analysis. At a redshift of 0.5, the galaxies are more clustered together, largely accounting for the difference in the moment profiles seen in Figure 8.