adsabs/AstroCLIMB huggingface dataset:
Paper: The Correlation between WISE 12 μm Emission and Molecular Gas Tracers on Subkiloparsec Scales in Nearby Star-forming Galaxies
Authors: Yang Gao, Qing-Hua Tan, Yu Gao, Min Fang, Ryan Chown, Qian Jiao, Chun-Sheng Luo
Figure caption: Correlation of the 12CO luminosities with the mid-infrared monochromatic luminosities (L 12μm) from WISE measured in the 12 μm band for galaxies spatially resolved on kiloparsec or subkiloparsec scales. CO detections from different galaxies are indicated with different symbols and colors as indicated in the upper left corner, while a few valuable upper limits are also plotted as downward-pointing arrows. The galaxies are divided into three subsamples in these three panels, and all detected pixels in the entire sample are plotted as a grayscale background for comparison. The black line and two dashed red lines depict respectively the best-fitting relation (with parameters listed in Table 2) and the 1σ total/observed scatter, while the green line shows the relation of global galaxies from Gao et al. (2019). The median measurement uncertainties are illustrated by the characteristic error bars shown in the lower right corner.
Paper: The Correlation between WISE 12 μm Emission and Molecular Gas Tracers on Subkiloparsec Scales in Nearby Star-forming Galaxies
Authors: Yang Gao, Qing-Hua Tan, Yu Gao, Min Fang, Ryan Chown, Qian Jiao, Chun-Sheng Luo
Figure caption: The distribution of (a) Spearman’s correlation coefficient, (b) best-fit slope, and (c) intercept between luminosities of 12 μm band (x-axis) and CO isotopologues (y-axis), which are computed based on individual pixel measurements in each galaxy. We only include the galaxies with at least 12 CO detections or valuable upper limits. In the first three panels, the gray histograms show the logL 12μm versus log ﹩{L}_{{}^{12}\mathrm{CO}(1-0)}﹩ relation obtained for 24 galaxies, and the black ones indicate AGNs, while the ones with red and blue lines show the parameters of logL 12μm versus log ﹩{L}_{{}^{13}\mathrm{CO}(1-0)}﹩ and logL 12μm versus log ﹩{L}_{{}^{12}\mathrm{CO}(1-0)}﹩ based on the measurements of 13CO-detected or tentatively detected pixels in 17 galaxies. In panel (d), we show the distribution of the median Δ log(L CO) in each galaxies, based on the log(﹩{L}_{{}^{12}\mathrm{CO},\mathrm{est}}﹩) from Equation (5) for 24 galaxies and log(﹩{L}_{{}^{13}\mathrm{CO},\mathrm{est}}﹩) from Equation (6) for 21 galaxies. The colored vertical lines indicate the medians.
Paper: The Correlation between WISE 12 μm Emission and Molecular Gas Tracers on Subkiloparsec Scales in Nearby Star-forming Galaxies
Authors: Yang Gao, Qing-Hua Tan, Yu Gao, Min Fang, Ryan Chown, Qian Jiao, Chun-Sheng Luo
Figure caption: Same as Figure 1, the relation between 13CO (left panel) and 12CO (right panel) luminosities and 12 μm luminosities, but only the pixels with significant 13CO emission (detected or with valuable upper limits) are shown. Large filled symbols are used to indicate the galaxies observed by us with PMO and the center of galaxies observed by Nakajima et al. (2018). The parameters of best-fitting linear relations are also listed in Table 2. And in the right panel, the grayscale background in Figure 1 is also plotted for comparison.
Paper: The Correlation between WISE 12 μm Emission and Molecular Gas Tracers on Subkiloparsec Scales in Nearby Star-forming Galaxies
Authors: Yang Gao, Qing-Hua Tan, Yu Gao, Min Fang, Ryan Chown, Qian Jiao, Chun-Sheng Luo
Figure caption: The relation between 12 μm luminosities and Y. From left to right, Y is defined as the HCN (4–3) (detected) luminosities, HCO+ (4–3) (detected) luminosities, and 12CO (1 − 0) luminosities for the same pixels of HCN detections. Different colors and symbols indicate detected pixels in different galaxies, and the error bars show their measurement uncertainties. In each panel, the black and two red lines show, respectively, the best-fitting linear relation (with parameters listed in Table 2) and the 1σ total/observed scatter, while the green line in the right panel still indicates the relation of global galaxies from Gao et al. (2019).
Paper: The Correlation between WISE 12 μm Emission and Molecular Gas Tracers on Subkiloparsec Scales in Nearby Star-forming Galaxies
Authors: Yang Gao, Qing-Hua Tan, Yu Gao, Min Fang, Ryan Chown, Qian Jiao, Chun-Sheng Luo
Figure caption: The residuals about the 12CO vs. 12 μm luminosity relation (Equation (7)) as a function of derived parameters (13CO optical depth τ(13CO), gas kinetic temperature T  k , and molecular gas surface density Σmol).
Paper: The Correlation between WISE 12 μm Emission and Molecular Gas Tracers on Subkiloparsec Scales in Nearby Star-forming Galaxies
Authors: Yang Gao, Qing-Hua Tan, Yu Gao, Min Fang, Ryan Chown, Qian Jiao, Chun-Sheng Luo
Figure caption: Same as Figure 4, but for the residuals of the predicted value from the best-fitting relation between ﹩{L}_{{}^{13}\mathrm{CO}}﹩ and L 12μm.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Left and middle panels: differential rotation as a function of radius for different latitudes and in the meridional plane, respectively, for simulations R1x24, R2x24, and R4x24, from top to bottom. Right panels: mean profile of the latitudinal velocity in the meridional plane. In the northern hemisphere, negative (positive) values correspond to poleward (equatorward) flows.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Angular momentum fluxes integrated over spherical surfaces at different r (upper panels) and conical surfaces at latitudes 90 − θ (bottom), for simulations (a) R1x24, (b) R2x24, and (c) R4x24. The red and blue lines correspond to the MS and RS contributions; the dashed black line is the sum of both contributions.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Same as Figure 6, but for simulations R1x24 (dashed line), R2x24 (dotted), and R1_24 (solid). Note that the peak of the spectra of the rotating simulation is shifted toward the smaller scales, ℓ ∼ 40. Moreover, increasing resolution leads to larger power in the radial component, with the maximum being shifted to the smaller scales. For comparison, the thin solid lines show the spectra of case R4 at the corresponding depths.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Latitudinal variations of temperature perturbations: the red and blue lines correspond to profiles of temperature perturbations at the surface and the bottom of the convection zone for the models (a) R1x24, (b) R2x24, and (c) R4x24. The contrast at the two radial levels is different; therefore, two different scales at the left and right Y-axis are considered. The dashed line shows a third radial level at r = 0.66, where perturbations are not expected. The angled brackets, 〈〉 r , indicate the radial average centered in r = 0.71R ⊙ and r = 0.93R ⊙ in a radial layer of thickness 0.04R ⊙.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Same as Figure 3, but for the rotating simulations with different resolutions, R1x24 (blue), R2x24 (red), and R4x24 (green). For comparison, the profiles corresponding to the nonrotating cases R1x and R4 are presented with black and gray dotted lines, respectively. The thin red vertical lines show the bottom of the convection zone.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Axial torques due to the RS (left column) and the MC (middle), and the sum of the RS and MC (right) torques, presented in the meridional plane for simulations R1x12 (top row), R2x24 (middle), and R4x24 (bottom).
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: The inertia, ﹩{ \mathcal I }﹩ (left), and baroclinic, ﹩{ \mathcal B }﹩ (middle), terms of the TWB, Equation (21). The right column shows the residual ﹩{ \mathcal B }-{ \mathcal I }﹩.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Luminosity carried by the enthalpy flux in the rotating simulations R1x24, R2x24, and R4x24. For comparison to the nonrotating cases, the dotted black and gray lines correspond to simulations R1x and R4, respectively. The inset focuses on the bottom of the convection zone and shows that overshooting decreases because of rotation. The dotted lines show the luminosity carried by the kinetic energy flux.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Two-dimensional kinetic energy spectra for simulation R1x24 at the top (a), middle (b), and bottom (c) of the domain. The bottom left points observed in panels (b) and (c) correspond to inertial modes driven by the Coriolis force.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Dispersion properties of oblique quasi-kink modes in an asymmetric slab configuration, with the obliqueness measured by the angle θ between the equilibrium magnetic field  B  0 and a 2D wavevector  k  = k  y   e   y  + k  z   e   z . The combination [ρ i/ρ L, l/d] is fixed at [10, 0.3], whereas two values of ρ i/ρ R are discriminated, one being 5 (the left column) and the other being 1.2 (right). Plotted are the θ-dependencies of the oscillation frequency (ω, the top row), the y-component of the group velocity (v gr,y , middle), and (c) the z-component (v gr,z , bottom). Several values of kd are examined as labeled. The dotted (solid) portion in any curve corresponds to where m R d < 1/5 (m R d ≥ 1/5), with m R d measuring the capability for the slab to trap oblique quasi-kink modes. See text for more details.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Phase (the thick curves) and group (thin) diagrams of oblique quasi-kink modes in an asymmetric slab configuration. The combination [ρ i/ρ L, l/d] is fixed at [10, 0.3], whereas two values of ρ i/ρ R are discriminated, one being 5 (the left panel) and the other being 1.2 (the middle and right panels). The vertical dashed–dotted line points in the direction of the equilibrium magnetic field  B  0. Any curve is color-coded by θ, the angle that  k  makes with  B  0. See text for more details.
Paper: A New Method of Reconstructing Galactic 3D Structures Using Ultralong-wavelength Radio Observations
Authors: Yanping Cong, 艳平 丛, Bin Yue, 斌 岳, Yidong Xu, 怡冬 徐, Yuan Shi, 嫄 施, Xuelei Chen, 学雷 陈
Figure caption: The reconstructed electron density profiles along seven LOS in the Galactic plane and in high Galactic regions, pointing to different directions: (a) l = 2°, b = 0°; (b) l = 90°, b = 0°; (c) l = 180°, b = 0°; (d) l = 101.°67, b = 49.°70; (e) l = 5.°62, b = 34.°23; (f) l = 260.°16, b = − 41.°81; (g) l = 270°, b = 0°; the bump at ∼0.5 kpc is the Gum Nebula; (h) same as (g) but assume information on the Gum Nebula on this LOS is already known, and 0.1 ≤ ν ≤ 30 MHz data are used for fitting. As a comparison in each panel we also plot the NE2001 density of same r bins. In all panels the reconstructed results and the NE2001 model are smoothed by a Gaussian kernel with radius equal to 1 bin.
Paper: A New Method of Reconstructing Galactic 3D Structures Using Ultralong-wavelength Radio Observations
Authors: Yanping Cong, 艳平 丛, Bin Yue, 斌 岳, Yidong Xu, 怡冬 徐, Yuan Shi, 嫄 施, Xuelei Chen, 学雷 陈
Figure caption: The mock sky maps at 0.1 MHz (top) and 0.5 MHz (bottom) used in this Paper.
Paper: A New Method of Reconstructing Galactic 3D Structures Using Ultralong-wavelength Radio Observations
Authors: Yanping Cong, 艳平 丛, Bin Yue, 斌 岳, Yidong Xu, 怡冬 徐, Yuan Shi, 嫄 施, Xuelei Chen, 学雷 陈
Figure caption: Top: the sky map of ﹩{\chi }_{\min }^{2}/{N}_{\mathrm{freq}}﹩ for all LOS. Bottom: the probability density of the ﹩{\chi }_{\min }^{2}/{N}_{\mathrm{freq}}﹩ distribution. The solid curve is a Gaussian fit, with the peak 1.72, the center 1.12, and the radius 0.23. About 2% of LOS have ﹩{\chi }_{\min }^{2}/{N}_{\mathrm{freq}}\gt 3.0﹩. For displaying purposes, in the top panel they are shown by the same color to 3.0, while in the bottom panel these are not counted.
Paper: A New Method of Reconstructing Galactic 3D Structures Using Ultralong-wavelength Radio Observations
Authors: Yanping Cong, 艳平 丛, Bin Yue, 斌 岳, Yidong Xu, 怡冬 徐, Yuan Shi, 嫄 施, Xuelei Chen, 学雷 陈
Figure caption: Top: the sky map for the mean absolute value of the relative error of all LOS. Bottom: the probability density of the mean absolute value of the relative error distribution.
Paper: A Global Simulation of the Dynamo, Zonal Jets, and Vortices on Saturn
Authors: Rakesh Kumar Yadav, Hao Cao, Jeremy Bloxham
Figure caption: Panel (a) shows the (instantaneous) magnetic power contained in the first 15 spherical harmonics on the simulation surface. Both axisymmetric and nonaxisymmetric components are shown. Panel (b) compares the axisymmetric power in the magnetic field with the values obtained for Saturn (Cao et al. 2020). Note that both spectra are normalized by the power in the dipole mode.
Paper: A Global Simulation of the Dynamo, Zonal Jets, and Vortices on Saturn
Authors: Rakesh Kumar Yadav, Hao Cao, Jeremy Bloxham
Figure caption: Axisymmetric components of the zonal flow and magnetic field at the top of the SSL. Panel (a) shows the zonal flow. Panel (b) shows the total radial magnetic field as well as its large-scale component (only containing the dipole, quadrupole, and octopole). Panel (c) shows the azimuthal magnetic field. Panel (d) compares the smaller-scale radial magnetic field with the total azimuthal magnetic field. All these quantities are obtained at the top of the SSL, which is at 0.8r 0.
Paper: A Global Simulation of the Dynamo, Zonal Jets, and Vortices on Saturn
Authors: Rakesh Kumar Yadav, Hao Cao, Jeremy Bloxham
Figure caption: Radial variation of the nondimensional pressure, density, temperature, and gravity in the anelastic background state. Note that in the MagIC code, the thermodynamic quantities are normalized by their values at the outer boundary.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: The BTFR with V max estimated from fits to the Einasto rotation curves (left; purple circles) and cored Einasto rotation curves (right; purple circles) for our sample of galaxies. Similar to Figure 5, measurements for more-massive galaxies from Lelli et al. (2019, black circles) are included, as well as the best-fitting line to these galaxies (solid black), 1σ dispersion to the fit (shaded gray), and an extrapolation of the fit to lower masses (dashed black). Predictions from the APOSTLE (green line; Sales et al. 2017) and NIHAO (salmon points; Dutton et al. 2017) hydrodynamical simulations are also shown. V max estimates from the Einasto rotation curves yield unphysical values of V max for many galaxies in our sample. V max estimates from the cored Einasto rotation curves result in a turndown in the BTFR that is consistent with predictions from the simulations shown. Points are color-coded by the ratio M bary(<R max)/M dyn(<R max), an approximate upper limit for the baryon-to-dark matter ratio based on integrating M bary from the center of galaxies out to R max; darker shades indicate higher confidence that the galaxies are dark matter dominated at R max (see Section 3.5 for details).
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: The SMHM and BMHM relations showing M * (purple) and M bary (green) vs. M 200 determined from fitting V cor and R max to rotation curves generated from the cored Einasto profiles. The BMHM points are color-coded by log (M gas/M *). Diagonal lines drawn from the lower left to the upper right mark mass/M 200 ratios of 10−1 (dotted), 10−2 (solid), and 10−3 (dashed). The BMHM shows a larger vertical spread than the SMHM, driven by the different gas fractions in the galaxies. The larger range of M bary at M 200 ∼ 1010 M ⊙ is just the turndown in the BTFR seen now in M 200 instead of V max. In addition, galaxies with higher M bary/M 200 ratios tend to have “undersized” stellar disks relative to their gas content.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption:  M bary vs. M 200 determined from fitting V cor and R max to rotation curves generated from the Einasto profile (left) and the cored Einasto profiles (right). Diagonal lines drawn from the lower left to the upper right mark M bary=M 200 (solid), the cosmic baryon fraction f bary where M bary/M 200 = 0.18 (dashed), 10% f bary (dashed–dotted), 1% f bary (dotted), 0.1% f bary (wide-dotted).
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: Radius of the cores in the density profiles from the fits to theoretical rotation curves based on cored Einasto profiles as a function of M * (green points; top x-axis scale) and M */M 200 (blue points; bottom x-axis scale). Values in the top and bottom x-axis scales are independent of each other. As the cored profiles are calibrated to the FIRE simulations, the core radius is dependent on the FIRE feedback prescriptions, which create cores down to M * ∼ 106 M ⊙. Larger cores are formed in galaxies with higher M * and higher ratios of M */M 200, as expected in this mass regime.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: Comparison of the measured velocities (before correcting for inclination angles) and the radius at which they were measured from the PV diagrams using our new technique (blue points) and from rotation curve fitting from Iorio et al. (2017; red points). Each galaxy has a unique plot symbol, as defined in the legend. The values are in overall good agreement.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: PV diagrams for SHIELD galaxies AGC110482, AGC111164, AGC229053, AGC7393005, AGC742601, and AGC749237 with the location of the best-fitting V PV and D PV marked in white.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: PV diagrams for LITTLE THINGS galaxies DDO53, DDO126 F564v3, HoII, and WLM with the location of the best-fitting V PV and D PV marked in white.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: PV diagrams for VLA-ANGST galaxies DDO99, DDO125, DDO181, DDO183, NGC3109, and NGC3741 with the location of the best-fitting V PV and D PV marked in white. Both NGC3109 and NGC3741 have cleaning “bowl” effects visible, but these do not impact our measurements of V PV and D PV.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: PV diagrams for VLA-ANGST galaxies Sextans A, Sextans B, UGC04483, UGC08508, UGC08833, and UGCA292 with the location of the best-fitting V PV and D PV marked in white.
Paper: Tracking Halo Orbits and Their Mass Evolution around Large-scale Filaments
Authors: Hannah Jhee, Hyunmi Song, Rory Smith, Jihye Shin, Inkyu Park, Clotilde Laigle
Figure caption: Stacked mass evolution profiles of recent crossers (t FC < 3 Gyr) subsampled based on their closest filament density as in Figure 8 (left) and those of intermediate crossers (4 ≤ t FC/Gyr < 9) subsampled by the number of orbits (right). Note that the left and right panels are of different halo samples. Each axis is normalized by the value at the first crossing.
Paper: Tracking Halo Orbits and Their Mass Evolution around Large-scale Filaments
Authors: Hannah Jhee, Hyunmi Song, Rory Smith, Jihye Shin, Inkyu Park, Clotilde Laigle
Figure caption: Stacked phase-space trajectories (left) and mass evolution profiles (right) of halos in the five subsamples in Figure 9: 1/2 for recent crossers, 3/4 for intermediate crossers, 5 for ancient crossers, 1/3/5 for mass-gaining halos, and 2/4 for mass-losing halos. Because the first crossing moment differs between halos, individual mass evolution profiles are stacked after making the first crossing moment the zero-point (i.e., t − t FC). That is, t − t FC < 0 and > 0 are before and after the first crossing, respectively.