adsabs/AstroCLIMB huggingface dataset:
Paper: BASS. XXII. The BASS DR2 AGN Catalog and Data
Authors: Michael J. Koss, Claudio Ricci, Benny Trakhtenbrot, Kyuseok Oh, Jakob S. den Brok, Julian E. Mejía-Restrepo, Daniel Stern, George C. Privon, Ezequiel Treister, Meredith C. Powell, Richard Mushotzky, Franz E. Bauer, Tonima T. Ananna, Mislav Baloković, Rudolf E. Bär, George Becker, Patricia Bessiere, Leonard Burtscher, Turgay Caglar, Enrico Congiu, Phil Evans, Fiona Harrison, Marianne Heida, Kohei Ichikawa, Nikita Kamraj, Isabella Lamperti, Fabio Pacucci, Federica Ricci, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, Matthew J. Temple, C. Megan Urry, Sylvain Veilleux, Jonathan Williams
Figure caption: Figure showing examples of spectral setups not shown earlier in the text excluding the archival observations. A spectrum from the du Pont telescope with the Bollens & Chivens spectrograph with the 300 line mm–1 grating is shown in the top panel, a spectrum from the VLT with the FORS2 instrument is shown in the middle panel, and a spectrum with Keck using the LRIS instrument is shown in the bottom panel.
Paper: BASS. XXII. The BASS DR2 AGN Catalog and Data
Authors: Michael J. Koss, Claudio Ricci, Benny Trakhtenbrot, Kyuseok Oh, Jakob S. den Brok, Julian E. Mejía-Restrepo, Daniel Stern, George C. Privon, Ezequiel Treister, Meredith C. Powell, Richard Mushotzky, Franz E. Bauer, Tonima T. Ananna, Mislav Baloković, Rudolf E. Bär, George Becker, Patricia Bessiere, Leonard Burtscher, Turgay Caglar, Enrico Congiu, Phil Evans, Fiona Harrison, Marianne Heida, Kohei Ichikawa, Nikita Kamraj, Isabella Lamperti, Fabio Pacucci, Federica Ricci, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, Matthew J. Temple, C. Megan Urry, Sylvain Veilleux, Jonathan Williams
Figure caption: Example absorption-line fit of the model spectrum to the observed spectrum using synthetic kernels of Gaussian kernels in the O2 A-band region (∼7580–7680 Å).
Paper: BASS. XXII. The BASS DR2 AGN Catalog and Data
Authors: Michael J. Koss, Claudio Ricci, Benny Trakhtenbrot, Kyuseok Oh, Jakob S. den Brok, Julian E. Mejía-Restrepo, Daniel Stern, George C. Privon, Ezequiel Treister, Meredith C. Powell, Richard Mushotzky, Franz E. Bauer, Tonima T. Ananna, Mislav Baloković, Rudolf E. Bär, George Becker, Patricia Bessiere, Leonard Burtscher, Turgay Caglar, Enrico Congiu, Phil Evans, Fiona Harrison, Marianne Heida, Kohei Ichikawa, Nikita Kamraj, Isabella Lamperti, Fabio Pacucci, Federica Ricci, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, Matthew J. Temple, C. Megan Urry, Sylvain Veilleux, Jonathan Williams
Figure caption: Figure showing the spectral classification of beamed sources based on the presence of broad lines (BZQ, top), traditional continuum-dominated blazars with no emission lines or host galaxy features (BZB, middle), or only host galaxy features lacking broad lines (BZG, bottom).
Paper: BASS. XXII. The BASS DR2 AGN Catalog and Data
Authors: Michael J. Koss, Claudio Ricci, Benny Trakhtenbrot, Kyuseok Oh, Jakob S. den Brok, Julian E. Mejía-Restrepo, Daniel Stern, George C. Privon, Ezequiel Treister, Meredith C. Powell, Richard Mushotzky, Franz E. Bauer, Tonima T. Ananna, Mislav Baloković, Rudolf E. Bär, George Becker, Patricia Bessiere, Leonard Burtscher, Turgay Caglar, Enrico Congiu, Phil Evans, Fiona Harrison, Marianne Heida, Kohei Ichikawa, Nikita Kamraj, Isabella Lamperti, Fabio Pacucci, Federica Ricci, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, Matthew J. Temple, C. Megan Urry, Sylvain Veilleux, Jonathan Williams
Figure caption: Redshift range of all the AGNs in the sample, split into unbeamed (top left) and beamed AGNs (top right). Additionally, the bottom panel shows the slit width size in kiloparsecs for all the unbeamed AGNs.
Paper: BASS. XXII. The BASS DR2 AGN Catalog and Data
Authors: Michael J. Koss, Claudio Ricci, Benny Trakhtenbrot, Kyuseok Oh, Jakob S. den Brok, Julian E. Mejía-Restrepo, Daniel Stern, George C. Privon, Ezequiel Treister, Meredith C. Powell, Richard Mushotzky, Franz E. Bauer, Tonima T. Ananna, Mislav Baloković, Rudolf E. Bär, George Becker, Patricia Bessiere, Leonard Burtscher, Turgay Caglar, Enrico Congiu, Phil Evans, Fiona Harrison, Marianne Heida, Kohei Ichikawa, Nikita Kamraj, Isabella Lamperti, Fabio Pacucci, Federica Ricci, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, Matthew J. Temple, C. Megan Urry, Sylvain Veilleux, Jonathan Williams
Figure caption: Examples of 47 sources with newly identified redshifts.
Paper: Catalog of High-velocity Dispersion Compact Clouds in the Central Molecular Zone of Our Galaxy
Authors: Tomoharu Oka, Asaka Uruno, Rei Enokiya, Taichi Nakamura, Yuto Yamasaki, Yuto Watanabe, Sekito Tokuyama, Yuhei Iwata
Figure caption: Longitude–velocity maps of CO J = 3 − 2 emission averaged over latitudes. (a) Map of the original CO J = 3 − 2 data. (b) Map of the “pressed” data. (c) Map of the “pressed” and “unsharp-masked” data. (d) HVDCC candidates identified in the “pressed” and “unsharp-masked” data with the modified CLUMPFIND algorithm. Color represents the identification number in Table 4.
Paper: Catalog of High-velocity Dispersion Compact Clouds in the Central Molecular Zone of Our Galaxy
Authors: Tomoharu Oka, Asaka Uruno, Rei Enokiya, Taichi Nakamura, Yuto Yamasaki, Yuto Watanabe, Sekito Tokuyama, Yuhei Iwata
Figure caption: The CO data sets used in this study. Integrated intensity (﹩\int {T}_{{\rm{R}}}^{* }{dV}﹩) maps of (a) CO J = 3 − 2, and (b) CO J = 1 − 0 line emission. The emission was integrated over velocities between V LSR = −220 and +220  km s−1.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Left: distribution of the bolometric luminosity of the full 5.3k HETDEX AGN sample (blue) and the 1548 AGN (orange) selected for the study of type-II AGN. Middle: Bolometric luminosity vs. ﹩{\mathrm{FWHM}}_{{{\rm{C}}}_{\mathrm{IV}}}﹩ for the 1538 AGN (the orange histogram in the left panel and the blue histogram in Figure 16). The black dotted line and the red dashed line again show the positions of FWHM = 1000 and 1200 km s−1. Right: Fraction of type-II AGN (﹩{\mathrm{FWHM}}_{{{\rm{C}}}_{\mathrm{IV}}}\lt 1200﹩  km s−1), f 2 = n type−II/n AGN, as a function of the bolometric luminosity. The error bars are calculated with the Poisson errors (Gehrels 1986).
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Distribution of the r-band aperture magnitudes (see the descriptions of columns 135–139 in Appendices A and B for more details on the measurements). The blue histogram is the distribution of all HETDEX AGN with coverage from the four r-band imaging surveys that we have searched. The orange histogram includes only those HETDEX AGN with secure redshifts. The green histogram is the distribution of the full SDSS DR14Q catalog. The red dashed vertical line at r = 22.5 roughly shows the flux limit of the SDSS.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Distribution of the FWHM of the C IV line for 1538 HETDEX AGN that satisfy: (1) sflag = 2; (2) zflag = 1; (3) ﹩{\mathrm{EW}}_{{{\rm{C}}}_{\mathrm{IV}}}\gt 3﹩ Å (blue). The orange histogram is the completeness-corrected distribution for 970 out of the 1538 AGN with a completeness greater than 0.05. The completeness of each AGN is estimated based on simulations regarding our selection code. Details will be presented in C. Liu et al. (2022, in preparation). The black dotted line at FWHM = 1000 km s−1 and the red dashed line at FWHM = 1200 km s−1 are two commonly used separations between type-I AGN and type-II AGN (see the context for more details). The estimation of the completeness correction for each AGN is very complicated and will be introduced with details in our next paper in the series of the HETDEX AGN for the luminosity function.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption:  r-band HSC images and HETDEX spectra of three AGN with faint continua (r > 22.5). This figure has the same design as Figure 2. The yellow circles are added to show the photometric apertures used by the ELiXer software. The r-band aperture magnitudes for AGN 1383, 2012, 2653 are 24.1, 25.1, and 26.0, measured with aperture sizes of 1.″4, 1.″4, and 2.″0 in diameter. The 5σ depths of these three fields are 26.4, 26.2, and 26.2 respectively.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Flux of the Lyα+N V λ1241 emission vs. the r-band aperture magnitudes for the full HETDEX AGN catalog (blue), the HETDEX AGN with secure redshifts (orange), and the SDSS DR14Q catalog (green). The red dashed line again shows r = 22.5 where the SDSS QSOs stop. The black dotted line (log flux(Lyα+N V) = −0.32 r + 9.5) is a simple linear fit to the SDSS data points.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Baldwin effect (Baldwin 1977) of HETDEX AGN (zflag = 1) shown by the rest-frame EW of the C IV λ1549 emission and the monochromatic luminosity of the continuum at 1550 Å. The red dashed line is the relation in Wu et al. (2009) lowered by 0.2 dex, following Richards et al. (2011). This accounts for the methodology of EW measurements compared to those from the SDSS spectroscopic pipeline (Shen et al. 2011). We note that the C IV λ1549 emission is only visible within the redshift range of 1.26 < z < 2.55 in the HETDEX survey.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Top: distribution of the rest-frame equivalent widths of Lyα+N V (red), C IV λ1549 (blue), C III] λ1909 (orange), and Mg II λ2799 (green) of the HETDEX AGN with secure redshifts (zflag = 1). Bottom: Comparison between the rest-frame equivalent widths of Lyα+N V of HETDEX AGN with secure redshifts (red) and those of the SDSS DR14Q (purple). The number of SDSS QSOs in each bin is divided by 100 for presentation purposes.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: (g − r) vs. (u − g) diagram for the 596 HETDEX AGN at z < 2.5 with photometric measurements in the u, g, and r bands (see Appendix B for more details). The red data points show the 6% of AGN that have u − g > 0.62 and g − r > 0.16.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Redshift distribution for all AGN (blue) and AGN with secure redshifts (orange).
Paper: Water Masers as an Early Tracer of Star Formation
Authors: Dmitry A. Ladeyschikov, Yan Gong, Andrey M. Sobolev, Karl M. Menten, James S. Urquhart, Shari L. Breen, Nadezhda N. Shakhvorostova, Olga S. Bayandina, Alexander P. Tsivilev
Figure caption: Cumulative distribution function of the luminosity-to-mass ratio of the Hi-GAL (top panels) and ATLASGAL (bottom panels) clumps associated with different maser species: 22 GHz H2O, 6, 12, 95 GHz CH3OH, and 1665 MHz OH. Panels (B) and (D) display the distance-limited source sample (2 < D < 5 kpc).
Paper: Water Masers as an Early Tracer of Star Formation
Authors: Dmitry A. Ladeyschikov, Yan Gong, Andrey M. Sobolev, Karl M. Menten, James S. Urquhart, Shari L. Breen, Nadezhda N. Shakhvorostova, Olga S. Bayandina, Alexander P. Tsivilev
Figure caption: Box plot presenting the central 95% distributions of the luminosity-to-mass ratio for the ATLASGAL (upper panel) and Hi-GAL (lower panel) sources associated with different maser species and transitions ordered according to their mean value with the lowest values at the top and the largest value at the bottom.
Paper: Water Masers as an Early Tracer of Star Formation
Authors: Dmitry A. Ladeyschikov, Yan Gong, Andrey M. Sobolev, Karl M. Menten, James S. Urquhart, Shari L. Breen, Nadezhda N. Shakhvorostova, Olga S. Bayandina, Alexander P. Tsivilev
Figure caption: (A) Distribution of the distances to H2O, cIM and cIIM masers with the interferometric positions associated with the ATLASGAL clumps. The black vertical line marks the distance-limited sample used for the construction of the cumulative offsets plot. (B) The cumulative distribution of the physical offsets between the ATLASGAL clump peak and the H2O, cIM, and cIIM positions from the interferometric observations of the distance-limited source sample (2 < D < 6 kpc).
Paper: Water Masers as an Early Tracer of Star Formation
Authors: Dmitry A. Ladeyschikov, Yan Gong, Andrey M. Sobolev, Karl M. Menten, James S. Urquhart, Shari L. Breen, Nadezhda N. Shakhvorostova, Olga S. Bayandina, Alexander P. Tsivilev
Figure caption: The cumulative distribution function of the variability index for different maser species and transitions. The green line corresponds to 95 GHz CH3OH (class I) masers, magenta—12 GHz CH3OH (class II), gray—6.7 GHz CH3OH (class II), yellow—1665 MHz OH, blue—22 GHz H2O (calculated using observations with σ < 0.5 Jy), cyan—22 GHz H2O (using all available observations). For H2O and OH masers, only the sources belonging to the SFR category were included.
Paper: Water Masers as an Early Tracer of Star Formation
Authors: Dmitry A. Ladeyschikov, Yan Gong, Andrey M. Sobolev, Karl M. Menten, James S. Urquhart, Shari L. Breen, Nadezhda N. Shakhvorostova, Olga S. Bayandina, Alexander P. Tsivilev
Figure caption: The histogram distribution of the rms for the sources observed at 22 GHz with the Effelsberg 100 m telescope.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: Composite spectrum of the 3733 HETDEX AGN with secure redshifts (zflag = 1). Upper: The raw composite spectrum of all HETDEX AGN with zflag = 1 is shown in gray. The black line is the smoothed spectrum of the gray curve. The orange line is the composite spectrum of the SDSS BOSS QSOs in Harris et al. (2016). Bottom: Best-fit model (red) and smoothed composite spectrum of the HETDEX AGN (black) in the range of 800–2925 Å. The figure is designed in the same way as Figures 2 and 12, except that the spectrum is in the rest frame rather than in the observed frame, and the y-axis is in relative units of erg cm−2 s−1 Å−1. In both panels, some short blue dotted verticals are added showing the location of weak emission. The Lyman limit at 912 Å is shown as the dashed magenta line.
Paper: An Extension of Gmunu: General-relativistic Resistive Magnetohydrodynamics Based on Staggered-meshed Constrained Transport with Elliptic Cleaning
Authors: Patrick Chi-Kit Cheong, 志杰 張, David Yat Tung Pong, Anson Ka Long Yip, Tjonnie Guang Feng Li
Figure caption: Comparison of the square of the magnetic fields B 2 (left column) and divergence of the magnetic field ∣∣ ∇ · B ∣∣ (right column) for the loop advection test with different divergence-control methods at t = 100 = 10T. To compare directly, the corresponding color bars are set with the ranges [10−7, 10−12] and [10−4, 10−18], for the left and right columns, respectively. In the right column, the place where ∇ ·  B  is identically equal to zero is marked in white.
Paper: An Extension of Gmunu: General-relativistic Resistive Magnetohydrodynamics Based on Staggered-meshed Constrained Transport with Elliptic Cleaning
Authors: Patrick Chi-Kit Cheong, 志杰 張, David Yat Tung Pong, Anson Ka Long Yip, Tjonnie Guang Feng Li
Figure caption: One-dimensional slices along the x-axis (left column) and y-axis (right column) for the density ρ (top row), pressure p (second row), B 2 (third row), and Lorentz factor W (fourth row) for the MHD cylindrical blast wave test at t = 4.0. The red dots show the numerical results by solving resistive MHD equations while the black solid lines show the results by solving ideal MHD equations. There is no visible differences between ideal and resistive MHD cases.
Paper: An Extension of Gmunu: General-relativistic Resistive Magnetohydrodynamics Based on Staggered-meshed Constrained Transport with Elliptic Cleaning
Authors: Patrick Chi-Kit Cheong, 志杰 張, David Yat Tung Pong, Anson Ka Long Yip, Tjonnie Guang Feng Li
Figure caption: The two-dimensional profile for the cylindrical blast wave of the magnetic field strength B  i  B  i  (upper left), ∇ ·  B  (upper right), B  x  (lower left), and B  y  (lower right) at t = 4.0.
Paper: An Extension of Gmunu: General-relativistic Resistive Magnetohydrodynamics Based on Staggered-meshed Constrained Transport with Elliptic Cleaning
Authors: Patrick Chi-Kit Cheong, 志杰 張, David Yat Tung Pong, Anson Ka Long Yip, Tjonnie Guang Feng Li
Figure caption: The y-component of the magnetic field B  y  for the shock tube test at t = 0.4 with the resistivity in the range ﹩\eta \in \left[{10}^{-6},{10}^{3}\right]﹩. For low resistivity e.g., η ≤ 10−3, the result is close to the ideal MHD case (η → 0, black solid line).
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). I. Sample Selection
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Robin Ciardullo, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Yuchen Guo, Gary J. Hill, Lindsay House, Donghui Jeong, Shardha Jogee, Wolfram Kollatschny, Mirko Krumpe, Martin Landriau, Oscar A Chavez Ortiz, Yechi Zhang
Figure caption: The 25 composite spectra of the 25 groups of 150 AGN within different redshift intervals in Section 7.5. The plots are designed in the same way as Figure 2, but the wavelength is in the rest frame. The group number and the redshift range for each group are labeled in the upper right corner.
Paper: An Extension of Gmunu: General-relativistic Resistive Magnetohydrodynamics Based on Staggered-meshed Constrained Transport with Elliptic Cleaning
Authors: Patrick Chi-Kit Cheong, 志杰 張, David Yat Tung Pong, Anson Ka Long Yip, Tjonnie Guang Feng Li
Figure caption: Comparison of the magnetic monopole ∇ ·  B  with different κ at different time steps. As shown in the figures, the damping rate increases as κ increases.
Paper: Statistical Analysis of H I Profile Asymmetry and Shape for Nearby Galaxies
Authors: Niankun Yu, 捻坤 余, Luis C. Ho, Jing Wang, Hangyuan Li
Figure caption: Simulations using mock spectra to test the sensitivity of our parameter measurements to variations in S/N. The mock spectra were generated with five types of representative profiles (flat-topped, symmetric single-peaked, asymmetric single-peaked, symmetric double-horned, and asymmetric double-horned). The panels plot (a) absolute deviations for central velocity V  c  and fractional deviations for (b) flux F, (c) velocity width V 85, (d) flux asymmetry A  F , (e) flux distribution asymmetry A  C , (f) profile concentration C  V , and absolute deviation for (g) profile shape K. The black horizontal line denotes zero offset. The red solid lines show the median, and the dashed lines show the 16th and 84th percentiles of the distribution. Green curves in panels (b)–(g) are polynomial fits to the median distribution of total flux, line widths, asymmetry, and profile shape parameters (Equation (1)).
Paper: Entropy-conserving Scheme for Modeling Nonthermal Energies in Fluid Dynamics Simulations
Authors: Vadim A. Semenov, Andrey V. Kravtsov, Benedikt Diemer
Figure caption: Results of the “pressure-balance” test at t = 0.25. Different columns correspond to different schemes, from left to right: the energy-based scheme described in Section 2, the energy-based scheme that does not synchronize with the solution for e tot, and the entropy-based scheme. The initial conditions are the same as in Gupta et al. (2021): (ρ, u, P th, P cr) = (1, 1, 0.1, 0.9) and (1, 1, 0.9, 0.1) for the left and right initial states, respectively, and the initial location of the discontinuity is marked by the vertical green dotted line. The adiabatic indices of thermal and cosmic ray components are 5/3 and 4/3, respectively. To avoid the overlap in the top panels, the values of ρ and u are shifted by 0.4 and 0.2, respectively. The shaded gray area in the bottom panels shows the range where the scale of the y-axis is linear; the horizontal gray lines indicate the relative error of 1%.
Paper: Statistical Analysis of H I Profile Asymmetry and Shape for Nearby Galaxies
Authors: Niankun Yu, 捻坤 余, Luis C. Ho, Jing Wang, Hangyuan Li
Figure caption: Illustration of five typical profile shapes, as observed (black) and fit (red) with the busy function (Westmeier et al. 2014). The profiles vary from (a) symmetric double-horned (UGC 11861) to (b) asymmetric double-horned (UGC 4278), (c) flat-topped (UGC 1281), (d) symmetric single-peaked (UGC 2053), and (e) asymmetric single-peaked (NGC 1156). The values of asymmetry and shape parameters for the mock spectra are shown in the upper right corner.