adsabs/AstroCLIMB huggingface dataset:
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: As in Figure 10, but for three high-mass dwarf galaxies between 109.7 < M star/M ⊙ < 1010. Quenching occurs rapidly in a “blowout” phase, in stark contrast to the slow quenching found in lower-mass dwarfs. Outflows within r123 and r126 shutdown within 1 Gyr of t 90, causing a truncation in the energy and flux panels.
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: Fraction of gas to stars vs. stellar mass within quiescent dwarfs (red circles) and star-forming dwarfs (blue dots). Left: Fraction of H I gas to stellar mass, with observations from Catinella et al. (2018, black diamonds) and Bradford et al. (2018, black dashed) overplotted. Quiescent dwarfs contain orders of magnitude less H I gas at fixed stellar mass relative to star-forming dwarfs. Right: Fraction of total gas content to stellar mass. Quiescent dwarfs contain less cool, star-forming gas, and generally less gas overall relative to star-forming galaxies.
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: As in Figure 10, but for three intermediate-mass dwarf galaxies between 108.8 < M star/M ⊙ < 109.2. Quenching can occur both slowly as in lower-mass dwarfs, or rapidly as in higher-mass dwarfs.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The mean ﹩\cos ({\theta }_{3{\rm{D}}})﹩ for galaxies binned first by F acc and further by M vir. Galaxies at each redshift are first divided into 10 equal subsamples sorted by F acc. In each F acc bin, they are further divided into five equal subsamples sorted by M vir. Different M vir bins in each F acc bin are plotted with different colors, with 0 indicating the lowest M vir and 4 indicating the highest. Each column shows the results for one principle axis and each row shows the results for the same redshift. All results are plotted with the mean F acc in each bin.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The relation between the suppression S 2 on ﹩{\tilde{w}}_{{g}_{+}}﹩ and the mean ∣θ 2D∣ from the TSE and Gaussian distributions.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: Left: the projected GI correlations ﹩{\tilde{w}}_{{g}_{+}}﹩ of galaxies (dots) and halos (lines) for the three stellar-mass-limited samples at z = 0. Right: ﹩{\tilde{w}}_{{g}_{+}}﹩ of halos after suppressing the amplitudes with 2D misalignment angles from different models: a constant TSE model (solid lines), an F acc-dependent TSE model (dashed lines), and an M vir-dependent TSE model (dotted lines). The results are compared with the ﹩{\tilde{w}}_{{g}_{+}}﹩ of their galaxies (dots).
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The mean ﹩\cos ({\theta }_{3{\rm{D}}})﹩ for galaxies binned by different properties and at different redshifts. Each column shows the results for one principle axis and each row shows the results for the same property. Results from different redshifts are displayed by different colors. All the properties are plotted with the mean value in each bin.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The distributions of ∣θ 2D∣ for galaxies binned by different galaxy and halo properties at z = 0. Dots show the measurements from TNG300 and lines show the best-fit TSE distribution with only one free parameter, A. For better illustration, we only display results from five out of the total 10 bins for F acc and F disk.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The best-fit parameters A and B of the TSE distribution for galaxies binned by M * (filled circles) and M vir (open triangles) at various redshifts. The relation between A and B can be well described by a fitting formula ﹩B=-0.183\mathrm{ln}(A)+0.336﹩ shown as the solid line.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: Left: comparison between the galaxy and best-fit halo ﹩{\tilde{w}}_{{g}_{+}}﹩ using both the TSE and Gaussian misalignment models. Right: mean ∣θ 2D∣ obtained from different methods: direct counting (red), fitting the ∣θ 2D∣ distribution with the TSE model (blue), fitting the ﹩{\tilde{w}}_{{g}_{+}}﹩ with the TSE model (orange), and fitting the ﹩{\tilde{w}}_{{g}_{+}}﹩ with the Gaussian model (green).
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The mean ﹩| {\theta }_{2{\rm{D}}}^{\mathrm{major}}| ﹩ from the projection of only 3D major axes rather than all particles. Galaxies are binned by different properties and at different redshifts. Results from different redshifts are displayed by different colors. All the properties are plotted with the mean value in each bin.
Paper: Toward a Physical Understanding of Galaxy–Halo Alignment
Authors: Kun Xu, Y. P. Jing, Donghai Zhao
Figure caption: The mean ∣θ 2D∣ of galaxies binned by different properties and at different redshifts. Results from different redshifts are displayed by different colors. All the properties are plotted with the mean value in each bin.
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: Initial and final atmospheric mass fraction X atm and final water mole fraction (color bar) after the atmospheric loss through photoevaporation (ε = 0.1) for 4.6 Gyr. The rocky core is composed of basalt (left panel), CI (middle panel), and EH (right panel). An initial water mass fraction is determined by the empirical relation derived from the giant impact simulations, ﹩{X}_{{\rm{W}}}=8.2\times {10}^{-2}{X}_{\mathrm{atm}}^{-0.41}﹩. The color contour shows the final H2O mole fraction in the remaining atmosphere.
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: Mole fractions of hydrogen + helium (red line) and water (blue line) in the evaporating atmosphere after a giant impact. We considered an Earth-mass planet that initially has a 6.3% H2–H2O atmosphere with an initial water mole fraction of A W = 10%, which is equivalent to a mixing ratio of rocky vapor to H2–He gas of 90 mol%, at a = 1 au around a Sun-like star. The planet loses its atmosphere through photoevaporation (ε = 0.1) for 4.6 Gyr. The green line plots the atmospheric mass fraction. The nonsmooth features of the blue line are due to the sparse table of H2O EOS.
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: Same as Figure 7 but with different initial water mole fractions (1%, 3%, and 10% in the left, middle, and right panels, respectively). The rocky core is assumed to be basalt in all simulations.
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: Major species in a 1 bar atmosphere of an Earth-mass planet with three types of core material after a giant impact: basalt (top panel), CI (middle panel), and EH (bottom panel). We assumed that the mixing ratio of rocky vapor to the primordial atmosphere was 50%. Solid and dashed lines show the mole fractions of atomic and molecular species in the gas phase and the mass fractions of dust species, respectively.
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: Mass fraction of core material in the remaining atmosphere (Z atm) of an Earth-mass planet after a giant impact. We consider head-on collisions between two Earth-mass planets. The semiempirical formula of the Z atm − X atm relationship obtained from our SPH simulations of giant impacts, ﹩{Z}_{\mathrm{atm}}=8.2\times {10}^{-2}{X}_{\mathrm{atm}}^{-0.41}﹩ is also drawn (red line).
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: Mass fractions of H2O at T = 1000 K in the rock-polluted atmosphere after a giant impact. The purple, green, and orange lines correspond to the case of basalt and CI chondrite, and EH chondrite as core material, respectively.
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: Habitat of an Earth-mass planet with a water-rich atmosphere that orbits a Sun-like star. Dashed and solid lines represent a esc (Equation (25)) and a W (Equation (26)) in two models with ε = 0.1 (blue) and 0.01 (green), respectively. Blue and green shaded regions show the conditions where an Earth-mass planet can retain water in the atmosphere for Gyr.
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: Combined NICER spectra from all observations of each source. These are EF(E) spectra that have been unfolded against a constant model to factor out the effective area of the detector. Note that this unfolding leaves some instrumental features around 2 keV.
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: VLBI images of M81* at 8.8, 22, and 44 GHz from 2018 June 10. Panels (a) and (b) show spectral index images with uniform weighting, while panel (c) shows an image with natural weighting. The contours are plotted at increasing powers of 2 from 0.37, 0.67, and 0.61 mJy for panels (a), (b), and (c), respectively. The beam size is plotted in the lower left corner.
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: Upper panel: the distance of the discrete knot to the 22 GHz core and the linear fitting speed (black line). Middle panel: the X-ray light curve in the 2–10 keV band observed by SWIFT and Chandra (Niu et al. 2023). The brown solid line and dotted line represent the average flux μ and the standard deviation σ, respectively. Bottom panel: the light curve of the core (green) and the knot (red). The yellow region represents the possible date on which the knot passed through the 22 GHz core with a confidence of 95%.
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: Relative location of the compact core as a function of observing frequency. The fitted model is shown in black.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Flux ratios ﹩{\mathrm{log}}_{10}[{f}_{\nu }(100\,\mu {\rm{m}})/{f}_{\nu }(z)]﹩ vs. ﹩{\mathrm{log}}_{10}[{f}_{\nu }(\mathrm{FUV})/{{\rm{f}}}_{\nu }({\rm{z}})]﹩ before (left) and after (right) excluding NIHAO galaxies with total stellar mass below 109.5 M ⊙ with τ clear = 2.5  Myr and f dust = 0.1. The red points are DustPedia galaxies that can only provide a limit on the flux ratio. In each plot, we only show DustPedia galaxies with stellar masses and sSFRs that are within the corresponding NIHAO ranges.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Residuals relative to the expected face-on flux ratio given each galaxies sSFR, as described fully in the text. The left panel shows the ﹩{\mathrm{log}}_{10}[{f}_{\nu }(\mathrm{FUV})/{{\rm{f}}}_{\nu }({\rm{J}})]﹩ color residual, and the right panel shows the ﹩{\mathrm{log}}_{10}[{f}_{\nu }(i)/{f}_{\nu }(J)]﹩ color residual. NIHAO galaxies use τ clear = 2.5 Myr and f dust = 0.1.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Parameter search showing the distribution of the fractional difference in axis ratio color plot slope between DustPedia and the simulations. Parameter values are evenly separated in log space: f dust = [0.05, 0.1, 0.2, 0.4] and τ clear = [0.625, 1.25, 2.5, 5, 10]  Myr. The shaded region shows the bootstrap standard error averaged over all the data points, centered at y = 0.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Parameter space search showing the distribution of ﹩{\mathrm{log}}_{10}[{f}_{\nu }(100\mu m)/{f}_{\nu }(z)]﹩ vs. ﹩{\mathrm{log}}_{10}[{f}_{\nu }(\mathrm{FUV})/{{\rm{f}}}_{\nu }({\rm{z}})]﹩ for DustPedia and NIHAO. As in the previous plots, green diamonds represent NIHAO colors and black circles represent DustPedia colors. Our final parameter choices are f dust = 0.1 and τ clear = 2.5  Myr.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Distribution of sSFR vs. stellar mass for the DustPedia sample. The inlaid boxes show the sSFR and stellar mass ranges of the NIHAO galaxies before (red) and after (black) excluding galaxies with stellar mass below 109.5 M ⊙.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Flux ratios ﹩{\mathrm{log}}_{10}[{f}_{\nu }(\mathrm{FUV})/{{\rm{f}}}_{\nu }({\rm{J}})]﹩ and ﹩{\mathrm{log}}_{10}[{f}_{\nu }(i)/{f}_{\nu }(J)]﹩ vs. sSFR for DustPedia and NIHAO. Both samples are here limited to face-on, disk galaxies. For NIHAO, we show the results for τ clear = 2.5 Myr and f dust = 0.1.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Similar to Figure 9, but in this case the NIHAO galaxy residuals are relative to each galaxy's actual face-on colors.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Color–color plots for all orientations of NIHAO galaxies with τ clear = 2.5  Myr and f dust = 0.1, excluding galaxies with total stellar mass below 109.5 M ⊙.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Face-on (left five columns) and edge-on (right five columns) composite images of full galaxy sample.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: SEDs of a NIHAO disk galaxy (g1.92e12) viewed from different orientations, and in the absence of dust, modeled at a distance of 100 Mpc with τ clear = 2.5 Myr and f dust = 0.1. The plot on the left shows the SEDs from the far-ultraviolet to the far-infrared, and the plot on the right shows the same SEDs zoomed in to the wavelengths corresponding to MaNGA with matched resolution. Vertical lines indicate emission (blue) and absorption (red) lines. Although the black SEDs are nominally “dust-free,” they still have a small amount of IR emission due to the H II regions included in the spectra of the star-forming particles (even with f PDR = 0); see Section 3.2 for a quantitative analysis of this subgrid attenuated energy. We note that the face-on orientation has less of its UV-optical light attenuated while having nearly identical IR emission. This comparison alone shows that strictly following energy balance when modeling dust attenuation and emission along a particular line of sight is not well motivated.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption:  A  V  vs. stellar mass for all 10 selected orientations of each NIHAO galaxy with τ clear = 2.5  Myr and f dust = 0.1. It is clear that very small values of A  V  are strongly correlated with low-stellar-mass galaxies. Galaxies with total stellar mass below 109.5 M ⊙ are plotted in red.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption:                       ﹩{\mathrm{log}}_{10}[{f}_{\nu }({\rm{W}}4)/{f}_{\nu }(z)]﹩ vs. ﹩{\mathrm{log}}_{10}[{f}_{\nu }(\mathrm{FUV})/{f}_{\nu }(z)]﹩ before and after the applications of the age-smoothing recipe with τ clear = 2.5  Myr and f dust = 0.1. The red points are DustPedia galaxies that can only provide a limit on the flux ratio. The green diamonds that appear opaque result from the overlapping symbols associated with different viewing orientations of galaxies that have colors that do not change significantly at different viewing orientations.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Distribution of NIHAO galaxies’ sSFR and total stellar mass before and after age smoothing. Red arrows indicate an original sSFR equal to zero. DustPedia galaxies with total stellar masses and sSFRs that fall within the range of the NIHAO galaxies before age smoothing are shown in gray.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: SFHs before and after smoothing for two different galaxies. SFH after smoothing is binned 10 times more finely.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Unnormalized attenuation curves (left) and attenuation curves normalized by A  V  (right) for the NIHAO galaxies with τ clear = 2.5  Myr and f dust = 0.1, excluding those with total stellar mass below 109.5 M ⊙. Red lines represent galaxies that have total stellar mass below 109.5 M ⊙, blue lines represent galaxies above this mass with A  V  < 0.2, and black lines represent galaxies above this mass and with A  V  > 0.2. The right-hand panel only includes the gray curves, i.e. those galaxies with A  V  > 0.2 mag. The darker regions are due to the increased spectral resolution between 3600 and 10,300 Å.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: SEDs (left) and normalized attenuation curves (right) for a single disk galaxy viewed from 10 different orientations. The black curves show the results without dust, the blue curves show the results for the face-on case, the red curves show the results for the most edge-on case, and the gray curves show intermediate axis ratios.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Color–color plots for all orientations of NIHAO galaxies with no star-forming particles and f dust = 0.1, excluding galaxies with total stellar mass below 109.5 M ⊙.
Paper: Panchromatic Simulated Galaxy Observations from the NIHAO Project
Authors: Nicholas Faucher, Michael R. Blanton, Andrea V. Macciò
Figure caption: Energy balance plot for the NIHAO galaxies with τ clear = 2.5  Myr and f dust = 0.1, excluding those with total stellar mass below 109.5 M ⊙.
Paper: Joint Constraints on the Hubble Constant, Spatial Curvature, and Sound Horizon from the Late-time Universe with Cosmography
Authors: Kaituo Zhang, Tianyao Zhou, Bing Xu, Qihong Huang, Yangsheng Yuan
Figure caption: One-dimensional and two-dimensional marginalized distributions with 1σ and 2σ contours for the selected parameters under the third order.
Paper: Joint Constraints on the Hubble Constant, Spatial Curvature, and Sound Horizon from the Late-time Universe with Cosmography
Authors: Kaituo Zhang, Tianyao Zhou, Bing Xu, Qihong Huang, Yangsheng Yuan
Figure caption: One-dimensional and two-dimensional marginalized distributions with 1σ and 2σ contours for the selected parameters under the fifth order.
Paper: Joint Constraints on the Hubble Constant, Spatial Curvature, and Sound Horizon from the Late-time Universe with Cosmography
Authors: Kaituo Zhang, Tianyao Zhou, Bing Xu, Qihong Huang, Yangsheng Yuan
Figure caption: The reconstructed evolutions of H(z) with the flat ΛCDM, ﹩{y}_{1}^{(3)}﹩, ﹩{y}_{3}^{(3)}﹩, and P 22 models. The black lines show the center values and 1σ errors of H(z) for the flat ΛCDM model. The dark green, blue, and red lines with light bands show the center values and 1σ errors of H(z) for the ﹩{y}_{1}^{(3)}﹩, ﹩{y}_{3}^{(3)}﹩, and P 22 models, respectively.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Observed images in Band 6 (1.25 mm) and Band 4 (2.14 mm) shown with brightness temperature, assuming the Rayleigh–Jeans law. The middle and bottom rows show the same images as the top row, but with different color ranges, which emphasize the azimuthal asymmetry of the inner ring (middle) and the outer ring (bottom).
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Azimuthally averaged radial profiles. Top: the observed profiles (solid lines) and the fitted model profiles (dotted lines) in Band 6 and 4. Bottom: the observed profiles normalized at the peak of each ring.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Azimuthal profile of the observations and best-fit models along the two rings. The position angle is measured in a counterclockwise direction from the southeast major axis. The vertical lines at the bottom left indicate the thermal noise. The gray areas denote regions excluded from fitting due to the crescent-shaped nonaxisymmetric structure.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The deprojected images of the observations and models. We calculate χ 2 from the residuals of these images.
Paper: Joint Constraints on the Hubble Constant, Spatial Curvature, and Sound Horizon from the Late-time Universe with Cosmography
Authors: Kaituo Zhang, Tianyao Zhou, Bing Xu, Qihong Huang, Yangsheng Yuan
Figure caption: One-dimensional and two-dimensional marginalized distributions with 1σ and 2σ contours for the selected parameters under the fourth order.