adsabs/AstroCLIMB huggingface dataset:
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: Distribution of (a) central velocity V  c , (b) S/N, (c) total flux F, and (d) observed velocity width V 85 for the main sample (black) and SDSS subsample (blue).
Paper: Entropy-conserving Scheme for Modeling Nonthermal Energies in Fluid Dynamics Simulations
Authors: Vadim A. Semenov, Andrey V. Kravtsov, Benedikt Diemer
Figure caption: Effect of thermal and nonthermal energy modeling on the star formation in the average disk, i.e., at R > 1 kpc. The panels show the total star formation rate, mass of star-forming gas, and its average density. When the entropy-conserving scheme is used, a lower σ turb in dense gas (see Figure 8) results in a larger amount of star-forming gas but also in a lower average density of such gas. These trends partially cancel out, leading to only a moderate increase in the SFR.
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: Comparison of our measurements of (a) central velocity V  c  and (b) total flux F with measurements from the ALFALFA catalog, as a function of the S/N derived by the CoG method. Representative error bars are given in the bottom-right corner of each panel. The contours in each panel show the levels of sample inclusion, which are 20%, 40%, 60%, and 80% from inside out.
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 the method to measure the profile shape parameter K for (a) seven mock profiles that vary from single-peaked to flat-topped and double-horned and (b) their corresponding normalized CoGs. In panel (c), the shaded areas are the values of K, which are given in the lower right corner of the panel; areas below the diagonal line are negative and correspond to double-horned profiles, while those above are positive and represent single-peaked profiles.
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: Flowchart of sample selection process.
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: Example AGN at different redshifts selected by the 2em search. Left: r-band images collected from various surveys. More information of the r-band imaging surveys searched can be found in Appendix B. The blue crosses show the positions of all detections in the raw emission-line and continuum catalogs within the field. The orange cross shows the emission-line flux-weighted friend-of-friend (fof) center of these detections (see Section 4.5 for more details), while the red cross indicates the position of the best detection (detectidbest), i.e., the detection closest to the emission-line flux-weighted fof center among all member detections. The red dashed circle shows the aperture of the PSF-extracted spectra of detectidbest. The PSF extraction collects all fibers within a 3.″5 radius aperture and then applies flux weights to each fiber spectrum that consider both the PSF and the differential atmospheric refraction (DAR) of light across the aperture. Right: The spectrum of the detectidbest of each AGN extracted with the aperture shown by the red circle in the left panels. The black data points with error bars are the observed spectra. The red curve shows our best-fit spectrum. The cyan dashed line is our best-fit model to the continuum with the green shaded windows. The best-fit redshift of each AGN is labeled in the upper right corner.
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: Example AGN selected by the sBL method. The black data points with error bars are the observed spectrum, the red curve is the best-fit model of the emission-line window, and the gray shaded area is the window for the fit of the emission line. The cyan dashed line is a simple linear fit to the data points outside the gray shaded area. The yellow dotted line shows the sum of all emission components in the multi-Gaussian fit. The title of each panel is the catalog AGN ID (Appendix A). We give eight possible redshifts in the upper left corner of each panel, corresponding to the detected emission line being Lyα, C IV λ1549, Mg II λ2799, N V λ1241, C III] λ1909, O VI λ1034, He II λ1640, and Si IV+O IV] λ1400. The blue dashed vertical lines accompanied with line names above show the positions of common emission lines, assuming the four single broad emissions of AGN 18, 1058, 4810, 5024 are O VI λ1034, Lyα, C III] λ1909, and Mg II λ2799, 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: Visibility of strong AGN emission lines as a function of the redshift in the wavelength range of the HETDEX survey. The O VI λ1034 emission is usually highly noisy due to strong foreground absorbers, and N V λ1241 is often blended with Lyα. These two lines are thus plotted as dashed lines. The gray shaded region at 0.96 < z < 1.26 shows one representative redshift range where only one emission is visible. We note here that MgII λ2799 is the reddest emission we searched in this paper. We leave the search for emission lines of AGN at lower redshifts, such as the [NeV] λ3426 emission and the Balmer emissions, for the next data release.
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: Upper: completeness of the HETDEX pipeline and that of the HETDEX AGN catalog out of the 1155 broad-line AGN identified in Zhang et al. (2021) as a function of the S/N of their broad emissions. Bottom: line widths vs. S/N of the 1155 broad emissions identified in Zhang et al. (2021).
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: Example AGN that is missed by both the 2em selection and the sBL selection, but caught by the crossmatch with the SDSS DR14Q catalog and added back into our HETDEX AGN catalog.
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: Image in the extension 2 of the FITS file. The vertical direction has the AGN arranged with descending redshifts from bottom to top. agnid is the unique sequential numerical identifiers for each AGN. The horizontal direction has the 1D spectrum with increasing observed wavelengths from left to right.
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: Recovery fraction of 77 X-ray identified AGN with spectral redshifts that have HETDEX observations for the HETDEX AGN catalog (black open circles connected by solid line) and the HETDEX pipeline (gray crosses connected by dotted line) as a function of the S/N of the emission lines.
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: Flowchart that summarizes the selection of the AGN catalog from the HETDEX database. For simplicity, only the major selection criteria are included. More details can be found in Section 4.
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Top panel: Lindblad diagram of the identified MW substructures. The different structures are associated with the colors outlined in the legend. Bottom panel: the projected-action plot of the same substructures. This space is represented by J  ϕ /J Tot for the horizontal axis and (J z − J r)/J Tot for the vertical axis with J Tot = J r + ∣J  ϕ ∣ + J z. For more details on the projected-action space, see Figure 3.25 in Binney & Tremaine (2008).
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Left panel: histogram of the residuals of the difference between the photometric metallicity values ([Fe/H]Phot) and the metallicity values obtained from medium-resolution spectra (Fe/H]Spec) for the Full Sample. The biweight locations and scales are noted. Right panel: the residuals between [Fe/H]Phot and [Fe/H]Spec, as a function of [Fe/H]Spec, for the Full Sample. CEMP stars are indicated with red outlined points. The blue dashed line is the biweight location, while the shaded regions represent the first (1σ) and second (2σ) biweight scale ranges. The apparent systematic discrepancy at high metallicity in this panel is likely due to difficulties in the n-SSPP estimates in this range (see text).
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Top panel: histogram of the residuals of the difference between the RAVE DR6 radial velocities and the Gaia EDR3 values in the Full Sample. The biweight location and scale are noted. Bottom panel: the residuals between the RAVE DR6 and Gaia EDR3 radial velocities in the Full Sample, as a function of the Gaia radial velocities. The blue dashed line is the biweight location of the residual difference (μ = −0.1 km s−1), while the shaded regions represent the first (1σ = 2.5 km s−1), and second (2σ = 5.0 km s−1) biweight scale ranges.
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Left: comparison plot between the spectroscopic metallicity from the n-SSPP ([Fe/H]Spec) and the RAVE DR6 metallicity ([Fe/H]RAVE) in the Full Sample. Right: comparison plot between the spectroscopic metallicity from the n-SSPP ([Fe/H]Spec) and the photometric metallicity estimates from Huang et al. (2022) ([Fe/H]Phot) in the Full Sample.
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Top panel: comparison between the StarHorse distances and BJ21 distances in the Full Sample. Stars with the red outlined points indicate that the relative distance error in StarHorse is ϵ > 0.3. Bottom panel: the same comparison as the top panel, but with the red outlined points indicating the relative distance error in BJ21 is ϵ > 0.3. In both plots the dashed line indicates a one-to-one comparison between the two samples.
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: The Yoon–Beers diagram of A(C) c , as a function of [Fe/H], for stars in the Initial Sample. The CEMP cutoff ([C/Fe] c  = +0.7) is indicated with a blue dashed line. The CEMP stars ([C/Fe] c  > + 0.7) are shown as red outlined points. [C/Fe] c  = 0 is indicated with a solid black line. The ellipses represent the three different morphological groups of CEMP stars (see Figure 1 in Yoon et al. 2016 for a comparison and more information).
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Top panel: the corrected carbon abundance ([C/Fe] c ) of the Initial Sample, as a function of the final metallicity ([Fe/H]) for stars with [Fe/H] ≤ −0.8. The CEMP cutoff ([C/Fe] c  = +0.7) is noted as the blue dashed line; CEMP stars are indicated with red outlined points. The solar value is indicated as the solid black line. Bottom panel: the α-element abundance ([α/Fe]) of the Initial Sample, as a function of the final metallicity ([Fe/H]). The solar value is indicated with a solid black line.
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Left panel: histogram of the metallicity for the spectroscopic ([Fe/H]Spec, blue) and photometric ([Fe/H]Phot, gray) stars for the Full Sample. Right panel: histogram of the effective temperatures for the spectroscopic (T eff Spec, blue) and photometric (T eff Phot, gray) stars for the Full Sample. Although the effective temperature distributions for the two subsets appear similar, the spectroscopic sample of stars clearly favors stars with lower [Fe/H], by design.
Paper: Dynamically Tagged Groups of Metal-poor Stars. II. The Radial Velocity Experiment Data Release 6
Authors: Derek Shank, Dante Komater, Timothy C. Beers, Vinicius M. Placco, Yang Huang
Figure caption: Logarithmic histograms of the orbital parameters r peri (top), r apo (middle), and ﹩{Z}_{\max }﹩ (bottom) for the RAVE DR6 Final Sample. Note that a few stars have r apo and ﹩{Z}_{\max }﹩ outside the range shown in the panels.
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 evolution of the magnetic monopoles among all divergence-free handling methods we have explored. The L 1-norms of the magnetic monopoles for the cases of hyperbolic cleaning (GLM) and purely elliptic cleaning (MG) are roughly of the order ﹩{ \mathcal O }\left({10}^{-12}\right)﹩ and ﹩{ \mathcal O }\left({10}^{-13}\right)﹩ respectively. In addition, the L 1-norms of the magnetic monopoles are well controlled below ﹩{ \mathcal O }\left({10}^{-22}\right)﹩ when upwind constrained transport (UCT) is employed. The L 1-norms of the magnetic monopoles can be further suppressed to ﹩{ \mathcal O }\left({10}^{-25}\right)﹩ (three orders of magnitude smaller) if elliptic cleaning is activated as well as the upwind constrained transport scheme (UCT+MG). Although the differences in the magnetic fields are minimal among different divergence-free handling approaches (see Figure 19), such a huge difference in the magnitude of magnetic monopoles could significantly alter the results in long-term simulations.