adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that in the top panel of Figure 1, except now for Filament 10.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Caption is the same as that of Figure 5, but now only showing data in the second quartile for column density.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that in the bottom panel of Figure 1, except now for Filament 10.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that in the bottom panel of Figure 1, except now for G24.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that in the top panel of Figure 1, except now for G24.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Figure caption is the same as that of Figure 1, except now for G47.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Caption is the same as that of Figure 5, but now only showing data in the fourth quartile (highest values) for column density.
Paper: Magnetic Fields in the Bones of the Milky Way
Authors: Ian W. Stephens, Simon Coudé, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Andrés E. Guzmán, Alyssa Goodman, Takayoshi Kusune, Miaomiao Zhang, Nicole Karnath, Jessy Marin
Figure caption: Caption is the same as that of Figure 5, but now only showing data in the third quartile for column density.
Paper: Irradiated Atmospheres. IV. Effect of Mixing Heat Flux on Chemistry
Authors: Zhen-Tai Zhang, Wei Zhong, Wei Wang, Jianheng Guo, Xianyu Tan, Bo Ma, Ruyi Wei, Cong Yu
Figure caption: The mixing ratios of CH4, H2O, CO, NH3, NO, and CO2 across varying intensities of vertical mixing. The dotted line (Case 0) corresponds to the case where there is no vertical mixing in the atmosphere. The solid lines (Case K) represent the scenarios where only the effect of material transport due to vertical mixing is considered, without accounting for the mixing heat flux. The dashed lines (Case KT) consider both the material mixing and the heat flux brought about by vertical mixing. The different colors correspond to different values of Kzz, with the temperature profile displayed in Figure 1.
Paper: Irradiated Atmospheres. IV. Effect of Mixing Heat Flux on Chemistry
Authors: Zhen-Tai Zhang, Wei Zhong, Wei Wang, Jianheng Guo, Xianyu Tan, Bo Ma, Ruyi Wei, Cong Yu
Figure caption: The first row shows the mixing ratios of CO at 1 mbar across varying intensities of vertical mixing, and the second row presents those at 10 bar. The solid lines (Case K) represent the scenarios where only the effect of material transport due to vertical mixing is considered, without accounting for the mixing heat flux. The dashed lines (Case KT) consider both the material mixing and the heat flux brought about by vertical mixing. The different colors correspond to different values of irradiation temperature Tirr.
Paper: The SDSS-V Black Hole Mapper Reverberation Mapping Project: Light Echoes of the Coronal-line Region in a Luminous Quasar
Authors: Theodore B. Smith, Logan B. Fries, Jonathan R. Trump, Catherine J. Grier, Yue Shen, Scott F. Anderson, W. N. Brandt, Megan C. Davis, Tom Dwelly, P. B. Hall, Keith Horne, Y. Homayouni, J. McKaig, Sean Morrison, Hugh W. Sharp, Roberto J. Assef, Franz E. Bauer, Anton M. Koekemoer, Donald P. Schneider, Benny Trakhtenbrot, Hector Javier Ibarra-Medel, Castalia Alenka Negrete Peñaloza
Figure caption: PyROA best-fit light curves for Hα and Hβ (bottom), as well as [Ne V] λ3427 (top). The top panel in each plot shows the continuum light curve binned every 30 epochs (with gray points representing the raw data), with the best-fit PyROA model as a solid black line with a corresponding error envelope. The bottom panel in each plot shows the measured emission-line light curve with its corresponding PyROA model. The PyROA best-fit observed-frame time delays are shown in the emission-line light-curve panels with their corresponding error margins. The bottom-right panel displays the posterior time delay distribution for each emission-line light curve with median and 68th percent errors as solid and dashed lines, respectively.
Paper: Irradiated Atmospheres. IV. Effect of Mixing Heat Flux on Chemistry
Authors: Zhen-Tai Zhang, Wei Zhong, Wei Wang, Jianheng Guo, Xianyu Tan, Bo Ma, Ruyi Wei, Cong Yu
Figure caption: The temperature profiles for different values of Kzz under the fiducial model outlined in Section 2.2.
Paper: The SDSS-V Black Hole Mapper Reverberation Mapping Project: Light Echoes of the Coronal-line Region in a Luminous Quasar
Authors: Theodore B. Smith, Logan B. Fries, Jonathan R. Trump, Catherine J. Grier, Yue Shen, Scott F. Anderson, W. N. Brandt, Megan C. Davis, Tom Dwelly, P. B. Hall, Keith Horne, Y. Homayouni, J. McKaig, Sean Morrison, Hugh W. Sharp, Roberto J. Assef, Franz E. Bauer, Anton M. Koekemoer, Donald P. Schneider, Benny Trakhtenbrot, Hector Javier Ibarra-Medel, Castalia Alenka Negrete Peñaloza
Figure caption: Cross-sectional diagram of the AGN COS168 (not to scale). Shown are the measured distances to the BLR from Hα  the dusty torus (see Section 4.2) and the coronal-line region from [Ne V]. The distance to the NLR is an estimation based on previous studies into the NLR in AGN (B. M. Peterson et al. 2013).
Paper: The SDSS-V Black Hole Mapper Reverberation Mapping Project: Light Echoes of the Coronal-line Region in a Luminous Quasar
Authors: Theodore B. Smith, Logan B. Fries, Jonathan R. Trump, Catherine J. Grier, Yue Shen, Scott F. Anderson, W. N. Brandt, Megan C. Davis, Tom Dwelly, P. B. Hall, Keith Horne, Y. Homayouni, J. McKaig, Sean Morrison, Hugh W. Sharp, Roberto J. Assef, Franz E. Bauer, Anton M. Koekemoer, Donald P. Schneider, Benny Trakhtenbrot, Hector Javier Ibarra-Medel, Castalia Alenka Negrete Peñaloza
Figure caption: Line profiles of the rms flux of the [Ne V] λ3427 and Hα line in COS168. The Gaussian fit of the emission profile and the measured FWHM of the data are shown on each plot. The Hα line is particularly noisy due to skyline emission. Despite this, both the Gaussian fit and measured FWHM qualitatively fit the data.
Paper: The SDSS-V Black Hole Mapper Reverberation Mapping Project: Light Echoes of the Coronal-line Region in a Luminous Quasar
Authors: Theodore B. Smith, Logan B. Fries, Jonathan R. Trump, Catherine J. Grier, Yue Shen, Scott F. Anderson, W. N. Brandt, Megan C. Davis, Tom Dwelly, P. B. Hall, Keith Horne, Y. Homayouni, J. McKaig, Sean Morrison, Hugh W. Sharp, Roberto J. Assef, Franz E. Bauer, Anton M. Koekemoer, Donald P. Schneider, Benny Trakhtenbrot, Hector Javier Ibarra-Medel, Castalia Alenka Negrete Peñaloza
Figure caption: JAVELIN best-fit light curves for [Ne V] λ3427. The continuum data are the same binned data from Figure 3 but without the added variance from PyROA. Much like the PyROA best-fit light curves, the best-fit model created by JAVELIN is represented with a solid black line with a corresponding error envelope, as well as a posterior lag distribution shown in the right panels.
Paper: Unexpected Near-Resonant and Metastable States of Young Multiplanet Systems
Authors: Zhecheng Hu, 哲程 胡, Fei Dai, 飞 戴, Wei Zhu, 伟 祝, Mu-Tian Wang, 牧天 王, Max Goldberg, Caleb Lammers, Kento Masuda, 田賢人 増
Figure caption: Upper panel: orbital architecture of the young multiplanet systems studied here. The eccentricity and mass constraint from TTV modeling is shown above and below each planet, respectively (J. Livingston et al. 2025, in preparation, M. Wang et al. 2025, J. M. Wittrock et al. 2023). The size of each planet in the upper panel is proportional to its mass. Lower panels: pairwise period ratio deviation from exact commensurability (∣Δ∣, Equation (2)) versus the planet-to-star mass ratio (μ = (m1 + m2)/M⋆). Red and blue colors correspond to first-order (q = 1) and second-order (q = 2) MMRs, respectively. The solid lines indicate the theoretical resonance width, ﹩{{\rm{\Delta }}}_{{\rm{\max }}}﹩, calculated using Equation (6) for a combined eccentricity of ﹩| \tilde{e}| =0.1﹩. The corresponding shaded regions show how this width varies as ﹩| \tilde{e}| ﹩ ranges from 0.05 to 0.15 for reference. The horizontal red dotted line at ∣Δ∣ = 0.006 represents the empirical libration threshold from M. Goldberg & K. Batygin (2023). Each planetary system contains at least one pair whose ∣Δ∣ is outside the libration width, and is thus suggestive of a circulating state. Full TTV analysis also confirms the circulating states of these pairs, with the possible exception of the innermost pair of V1298 Tau.
Paper: Unexpected Near-Resonant and Metastable States of Young Multiplanet Systems
Authors: Zhecheng Hu, 哲程 胡, Fei Dai, 飞 戴, Wei Zhu, 伟 祝, Mu-Tian Wang, 牧天 王, Max Goldberg, Caleb Lammers, Kento Masuda, 田賢人 増
Figure caption: Proximity to three-body Laplace-like resonance ∣Bnorm∣ = ∣k1n1 − k2n2 + k3n3∣/〈n〉 for neighboring triplets of planets versus system age. Triplets with reported librating 3BR angles, either from TTV or from dynamical analysis, are shown in cyan (Kepler-80 (M. G. MacDonald et al. 2016), TRAPPIST-1 (M. Gillon et al. 2017), TOI-178 (A. Leleu et al. 2021), Kepler-60 (K. Goździewski et al. 2016), HD 110067 (R. Luque et al. 2023; C. Lammers & J. N. Winn 2024), Kepler-223 (S. M. Mills et al. 2016), K2-138 (J. L. Christiansen et al. 2018; M. G. MacDonald et al. 2022), TOI-1136 (F. Dai et al. 2023)). All other triplets without a confirmed librating 3BR angle are shown in gray. The nonadjacent Kepler-221 b-c-e triplet, which is suspected to be librating, is also included (M. Goldberg & K. Batygin 2021; T. Yi et al. 2025). The plot reveals two distinct populations: the librating triplets (cyan) have ∣Bnorm∣ values approximately two orders of magnitude smaller than the nonlibrating general population (gray). The young planetary systems (AU Mic, V1298 Tau, TOI-2076; shown in red) have triplets whose ∣Bnorm∣ are so large that the resonant angle is most likely circulating. We omit the nonadjacent triplets for V1298 Tau and TOI-2076 for clarity and note that they are all far from 3BR with ∣Bnorm∣ > 0.02.
Paper: Unexpected Near-Resonant and Metastable States of Young Multiplanet Systems
Authors: Zhecheng Hu, 哲程 胡, Fei Dai, 飞 戴, Wei Zhu, 伟 祝, Mu-Tian Wang, 牧天 王, Max Goldberg, Caleb Lammers, Kento Masuda, 田賢人 増
Figure caption: Lyapunov timescale maps for the AU Mic system with circulating (left) and librating (right) resonant angle at e = 0.04. The color scale represents the logarithm of the Lyapunov timescale in years, with warmer colors indicating shorter timescales and more chaotic behavior. The red star marks the nominal position of AU Mic. Given that AU Mic likely exhibits circulating behavior near-resonance, it is only shown in the left panel. Cyan circles denote confirmed librating 3BR systems (e.g., TRAPPIST-1), while green squares represent observed nonresonant multiplanet systems (corresponding to systems shown in Figure 2). Yellow triangles indicate resonant chains from N-body migration simulations (F. Keller et al. 2025). Black solid lines mark the locations 3BR, with shaded regions showing estimated resonance widths (A. C. Petit et al. 2020). The clustering of cyan points near these lines suggests the dynamical protection offered by librating 3BRs. The dashed black line and dotted gray line indicate the nominal 2BR location and width computed by Equation (6). Notably, the deep resonance region near the 2BR, which appears regular under libration, becomes chaotic under circulation. These maps reveal that the near-resonant configuration of AU Mic places it within a region of substantial dynamical chaos.
Paper: Unexpected Near-Resonant and Metastable States of Young Multiplanet Systems
Authors: Zhecheng Hu, 哲程 胡, Fei Dai, 飞 戴, Wei Zhu, 伟 祝, Mu-Tian Wang, 牧天 王, Max Goldberg, Caleb Lammers, Kento Masuda, 田賢人 増
Figure caption: Top panel: instability timescale as a function of initial eccentricity. Filled triangles indicate that the instability timescale exceeds the simulation duration of 300 Myr. Hollow points with left arrows denote observed eccentricity upper limits measured via TTVs and system age for each system. The upper horizontal double arrow shows the eccentricity range for observed planet systems (V. Van Eylen & S. Albrecht 2015; J.-W. Xie et al. 2016; S. Hadden & Y. Lithwick 2017; G. J. Gilbert et al. 2025). The lower horizontal double arrow shows the eccentricity range from N-body migration simulations (A. Izidoro et al. 2017; F. Keller et al. 2025). Bottom panels: comparison between instability timescales for the near-resonant (hollow symbols/lines) and in-resonance configurations (dashed lines). Near-resonant systems are much more susceptible to orbital instability. Shaded regions indicate the critical eccentricity beyond which neighboring 2BRs begin to overlap (K. M. Deck et al. 2013; S. Hadden & Y. Lithwick 2018). Even an in-resonant system becomes unstable beyond this point.
Paper: Unexpected Near-Resonant and Metastable States of Young Multiplanet Systems
Authors: Zhecheng Hu, 哲程 胡, Fei Dai, 飞 戴, Wei Zhu, 伟 祝, Mu-Tian Wang, 牧天 王, Max Goldberg, Caleb Lammers, Kento Masuda, 田賢人 増
Figure caption: The instability timescale versus planetary masses. The markers are the same as in Figure 3. The simulations were initialized with an eccentricity where each system has an instability time of approximately 10 Myr with its measured masses. The dependence of the instability timescale on planetary mass is steep, likely between the third or fourth power of the planetary mass.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Fully calibrated GTC Optical System for Imaging and low- to intermediate-Resolution Integrated Spectroscopy (OSIRIS) long-slit spectra of PN G048.5+04.2 (top) and PN G068.7+14.8 (bottom) obtained using the grisms R1000B (blue) and R1000R (red). The abscissa ranges of both panels are set to accommodate the height of the Hβ line. Prominent emission lines in the spectra are identified and labeled. Extinction has not been corrected for. In the R1000B spectrum, the weak features between [O II] λλ7320, 7330 and [Ar III] λ7751 are second-order contaminations; in the R1000R spectrum, the strong emission features redward of [S III] λ9531 are also affected by second-order contamination. The R1000B spectrum of PN G048.5+04.2 is contaminated by a field star, resulting in an elevated continuum in the red region. Overlaid in each panel is the HST/WFC3 F502N image (field of view ∼ 15″ × 15″), along with the GTC long slit (1″ width) marked as white dashed lines. The field star that contaminates the R1000B spectrum of PN G048.5+04.2 is also marked.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Spitzer/IRS spectrum of PN G048.5+04.2 (top) and PN G068.7+14.8 (bottom), with all emission features labeled and identified in red; an unidentified feature at ∼25.2 μm in PN G048.5+04.2 is marked as “?.” The AIB bands at ∼6.2, 7.7, 8.6, and 11.2 μm are also marked in the spectrum of PN G068.7+14.8 (L. Stanghellini et al. 2012). In each panel, the red dashed curve is the empirically fitted continuum.
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Plasma-diagnostic diagrams of PN G048.5+04.2 (left) and PN G068.7+14.8 (right) based on the CEL ratios. Different line types represent the temperature or density diagnostics using different line ratios (see Table 3).
Paper: Gran Telescopio Canarias/OSIRIS Deep Spectroscopy of Galactic Compact Planetary Nebulae: PN G048.5+04.2 and PN G068.7+14.8
Authors: Haomiao Huang, Xuan Fang, Letizia Stanghellini, Ting-Hui Lee, Martín A. Guerrero, Xiaohu Li, Richard Shaw, Jifeng Liu
Figure caption: Top: GTC/OSIRIS R1000B spectrum of PN G048.5+04.2 overlaid with the segmented quartic polynomial fits to the continuum (red; see the description in the text). Bottom: continuum-subtracted spectrum of this PN.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Contours of density and velocity vectors (arrows) in the first row, temperature (in kelvin) in the second row, and angular momentum (λ) in the third row with the α = 0.05 for model L2. The first, second, third, and last columns are captured at times 85,000tg, 95,000tg, 104,000tg, and 112,500tg, respectively. See text for details.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Distribution of logarithmic density(ρ) in code unit overlaid with velocity vectors, logarithmic temperature (T) in kelvin, and the angular momentum(λ) at dynamical time t = 50000tg for model L1. The first, second, third, and last columns are for α = 0.005, α = 0.01, α = 0.025, and α = 0.05, respectively. See the text for more details.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Initial condition: contours of logarithmic density (in code unit) overlaid with velocity vectors for the model L1 (first row), L2 (second row), and L3(third row). The times of snapshots are mentioned in the plots. The red and white dashed lines in the fourth column correspond to the shock surface and vr = 0, respectively. See text (Section 3.3) for details.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Angle and time-averaged radial distribution of density(〈ρ〉), temperature(〈T〉) in kelvin, and angular momentum(〈λ〉). The first, second, and third rows are for models L1, L2, and L3, respectively.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Contours of log(ρ) overlaid with velocity vectors and λ for model L3. The panels are snapshots of density contours captured at times t = 100,000. Panels (a), (b), (c), and (d) are for α = 0.005, α = 0.01, α = 0.025, and α = 0.05, respectively. Corresponding angular momentum contours are in the lower panels. The density contours are plotted in logarithmic scale, ranging from 0 to 1.0, and are shown with black solid lines. See text for details.
Paper: Dynamical Properties of Oscillating, Viscous, Transonic Accretion Disks around Black Holes
Authors: Sanjit Debnath, Indranil Chattopadhyay, Raj Kishor Joshi, Philippe Laurent, Priyesh Kumar Tripathi, M. Saleem Khan
Figure caption: Time evolution of the outer shock position(rs) with time for α = 0.002, 0.005, 0.01, 0.025, and 0.05 for model L1 (left column) and model L2 (right column). The time taken to achieve the initial condition for the simulation is rescaled as tini = 0.0 in the plots above.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: The dashed lines in the left panel indicate the separate angular momenta of the disks and halos, while the solid lines are their sum, demonstrating that this global integral is well conserved. The right panel gives the rates at which angular momentum is taken from the disk component and added to the halo.
Paper: After 54 Yr of Bar Instability Studies: A Fresh Surprise
Authors: J. A. Sellwood, Victor P. Debattista, R. G. Carlberg
Figure caption: The amplitude evolution of the bar-like logarithmic spiral component in the disks of three simulations having different compressed live halos.
Paper: The Hot Circumgalactic Medium in Stacked X-Rays: Observations versus Simulations
Authors: Skylar Grayson, Evan Scannapieco, Johan Comparat, John A. ZuHone, Yi Zhang, Soumya Shreeram, Marcus Brüggen, Esra Bulbul
Figure caption: Galaxy sample characteristics for the SIMBA (top) and EAGLE (bottom) analysis prior to resampling. Here we see redshift against stellar mass, with galaxies color-coded by halo mass. Star-forming galaxies (those with an sSFR > 0.01) are represented with crosses, while quiescent galaxies are shown as circles. Appendix A gives the sample sizes for the different simulated galaxy samples.