adsabs/AstroCLIMB huggingface dataset:
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 G mag for the Full Sample. Middle panel: histogram of the V mag for the Full Sample. Right panel: histogram of the G BP − G RP color for the Full Sample. All panels: the spectroscopic subset of the Full Sample is represented as a blue histogram; the photometric subset is represented as a gray histogram.
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: A plot of size (S) vs. velocity dispersion (σ V) for 184 identified HVDCCs. Symbols are the same as in Figure 5. The solid line represents the best-fit line for all identified HVDCCs, ﹩{({\sigma }_{{\rm{V}}}/\mathrm{km}\,{{\rm{s}}}^{-1})=22.9\,(S/\mathrm{pc})}^{0.5}﹩.
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: (a) Spatial distribution of identified HVDCCs superposed on the velocity-integrated map of CO J = 3 − 2 emission. (b) Longitude–velocity distribution of identified HVDCCs superposed on the latitude-integrated map of CO J = 3 − 2 emission. Red circles denote shell-type, red crosses wing-type, magenta filled circles simple-type, cyan crosses bridge-type, and blue crosses complex-type HVDCCs.
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: A plot of molecular mass (M CO) vs. virial mass (M VT) for 184 identified HVDCCs. Symbols are the same as in Figures 5 and 6. The solid line represents the best-fit line for all identified HVDCCs, (M VT/M ☉) = 834 (M CO/M ☉).
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: Venn diagram showing the set relationship between the HVDCCs identified in this study (symbol “O”) and those of (Nagai 2008, symbol “N”). The number in the parentheses denotes that of HVDCCs which belong to each set. The symbol “D” denotes the data coverage of this study. The number of HVDCCs in O ∩ N ∩ D is 39 in N, while it is 43 in O (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: The Galactic positions of the Full Sample of RAVE DR6 stars with the spectroscopic subset shown as blue points and the photometric subset as gray points. The Galactic reddening map, taken from Schlegel et al. (1998), and recalibrated by Schlafly & Finkbeiner (2011), is shown in the background on a gray scale with darker regions corresponding to larger reddening.
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: One-dimensional schematic drawings explaining the meaning of r dip introduced in the modified CLUMPFIND algorithm: (a) the two-clumps case, (b) the one-clump case.
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: (a) Distribution function and (b) cumulative distribution function of the asymmetry parameters A  F  (black) and A  C  (blue). In panel (a), the standard deviations of the half-Gaussian fits of the distributions (thin curves) are given in the legend, and the black and blue arrows mark the values of A  F  and A  C  of the two asymmetry profiles in our simulations (Figures 3 and 4). The fraction of the sample that is asymmetric, defined as A  F  > 1.24 and A  C  > 1.42, is denoted in panel (b).
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 function (left) and cumulative distribution function (right) of the profile shape parameters C  V  (top) and K (bottom). For the distribution functions, objects of the main sample are plotted (thick black histogram), as well as for SDSS subsamples binned by inclination angle: 70° ≤ i ≤ 90° (red), 50° ≤ i < 70° (green), 30° ≤ i < 50° (blue), and i < 30° (cyan). In panels (a) and (c), the black arrows show the values of C  V  and K of three different profile shapes used in our simulations (Figures 3 and 4).
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: The variation of profile concentration C  V  with (top) stellar mass M * and (bottom) optical concentration C for subsamples binned by inclination angle: from left to right, 70° ≤ i ≤ 90°, 50° ≤ i < 70°, 30° ≤ i < 50°, and i < 30°. The density of points is highlighted by gray scale and contours. The Pearson correlation coefficient and a typical error bar for C  V  are given at the bottom 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: The variation of profile shape K with (top) stellar mass M * and (bottom) optical concentration C for subsamples binned by inclination angle: from left to right, 70° ≤ i ≤ 90°, 50° ≤ i < 70°, 30° ≤ i < 50°, and i < 30°. The density of points is highlighted by gray scale and contours. The Pearson correlation coefficient and a typical error bar for K are given at the bottom 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: 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 Venn diagrams presenting the association between objects with water maser detection/nondetection and (upper panel) ATLASGAL and (lower panel) Hi-GAL CSC. For the ATLASGAL CSC, the region of matching is 280° < l < 60°, ∣b∣ < 1.°5, excluding the CMZ region. For the Hi-GAL CSC, the region of matching is shown in Figure 1.
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 accuracy of the GLM maser prediction vs. the maser detection probability threshold. The error bars for accuracy were calculated from the standard error of maser probability. The green and gray lines are the GLM accuracy for 95 GHz cIM masers using Hi-GAL and ATLASGAL CSC data, respectively. The blue and red lines—the accuracy of GLM for the 22 GHz water masers using Hi-GAL and ATLASGAL CSC data, respectively.
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: Comparison of the accuracy of GLM maser prediction using Hi-GAL CSC for different observed source samples. The two red vertical lines display the values of the thresholds discussed in the text: p = 0.5 and p = 0.7.
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 positions of the sources (gray dots) from Hi-GAL CSC. The blue contours correspond to the region used for the H2O maser search. The blue dots mark the positions of the water maser sources known from the literature.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: The blue/purple fit is the HBR line from Linmix, which can take upper limits into account. The shaded region indicates the pointwise 3σ confidence interval of the regression line. The dashed line is scaled to the median flux ratio and has slope 1. The dotted lines are the 0.5 dex offset from the dashed line. The empty points are the 3σ upper limits. The red line shows the OLS bisector. (Left) Comparison of [Si VI] λ1.9640 emission vs. X-ray emission. (Right) Comparison of [Si X] λ1.4300 emission vs. X-ray emission. We use the intrinsic 14–195 keV X-ray flux for sources from the Swift-BAT 70 month survey and the observed 14–195 keV X-ray flux for the remaining sources (indicated by the points marked with a cross). Compton-thick AGN (N H > 1023.5 cm−2) are indicated by circles with increased edgewidth. The typical uncertainty of the X-ray luminosity is indicated by the points in the lower right corner (for a description, see Section 3.1.2).
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: (Left) The percentage of detection of high-ionization lines by AGN type (Seyfert 1–1.8, Seyfert 1.9, and Seyfert 2) sorted according to their IP. (Right) Number of CL detections in a single spectrum separated by AGN type (i.e., Seyfert 1 and 2). In 54/110 (49%) Seyfert 2 galaxies one or more high-ionization emission lines are detected. The error bars are estimated using a 1σ binomial proportion confidence interval.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: (Left) Distribution of the X-ray luminosity of the BAT-detected AGN used in this work as a function of redshift. The dashed line shows the flux limit of the 105 month BAT all-sky survey for 90% of the sky (8.4 × 10−12 erg cm2 s−1) and the dotted line shows that for the 70 month survey (1.34 × 10−11 erg cm2 s−1). (Right) Redshift distribution of our sample. The median redshift is ﹩\bar{z}=0.04﹩, which is consistent with the median of the parent BASS sample (i.e., ﹩\bar{z}=0.037﹩; Koss et al. 2022a).
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Emission of [O III] λ5007 (left) and [Si VI] λ1.9640 (right) vs. X-ray emission for sources where both lines are detected simultaneously. The scatter of [O III] λ5007 emission with respect to X-ray emission is slightly above the value found in Berney et al. (2015) (σ = 0.62 dex). Lines and points follow the description of Figure 4.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Average number of simultaneously detected CLs binned by redshift. The gray shaded area shows the range in number of detections for each of the different sources in a given bin, while the colored lines indicate the mean of detections per redshift bin. The number of sources per bin is shown. The dashed lines indicate the boundaries of the redshift bins.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Scatter plot of Paschen FWHM and hydrogen column density N H. Squares indicate Paβ, circles indicate Paα, and diamonds indicate that the FWHMs of Paα and Paβ are taken. The instrumental FWHM of 56 km s−1 is removed. The horizontal dashed line is the nominal column density threshold separating X-ray obscured and unobscured AGN. The vertical dashed line is the separation into Seyfert 1 and 2 based on the FWHM, where Seyfert 2 galaxies lack broad Balmer lines. A small fraction of optical Seyfert 2 galaxies however show broad NIR Paβ or Paα emission lines, indicating hidden broad lines.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Velocity offset of [Si VI] λ1.9640 and [Si X] λ1.4300. The OLS regression and the orthogonal distance regression (ODR) are computed. The ODR takes into account the uncertainties of the measurements. The blue shaded region marks the 3σ (pointwise) confidence interval of the ODR fit. The points of individual sources are color-coded according to the hydrogen column density. The dashed line marks the 1:1 locus.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Example of offset of [Si X] λ1.4300 and [Si VI] λ1.9640. The [Si X] λ1.4300 line is clearly not blueshifted like the [Si VI] line. The line blueward of [Si VI] λ1.9640 is H2. The dashed lines mark the systemic redshift, based on lower-ionization lines (Paβ or He I).
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption:  (Left) Comparison of black hole mass estimates from velocity dispersion measurements (M BH,veldisp.) and from Paschen or Hα line widths (M BH,FWHM) for Seyfert 2 and 1.9 galaxies with hidden broad lines. For the Seyfert 1.9 galaxies, no offset is seen when using Paschen lines, while Hα gives lower mass by almost 1 dex. The dashed line indicates a 1:1 relation. The dotted line is a linear correlation shifted by 1 dex. (Right) Comparison of the estimated mass of the central black hole using the FWHM of the broad component of Hα and Paα for Seyfert 1.9 galaxies.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption:  Ratio of [O III] λ5007 to [Si VI] λ1.9640 emission as a function of the [Fe II] λ1.257/1.644 μm ratio. The iron line ratio traces to some degree the obscuration (Riffel et al. 2006), while the line ratio on the y-axis traces the IP.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Luminosity of [Si VI] λ1.9640 vs. observed 14–195 keV X-ray luminosity for sources with detections in BASS DR1 and this work, BASS DR2. Purple markers indicate sources from DR1 (N = 44) and orange markers indicate sources from DR2 (N = 57). Edges are color coded by AGN type (Type 1 vs. Type 2). The shaded region indicates the 1σ confidence interval of the respective regression line. Downward triangles indicate upper limits (only separated by DR1 and DR2). The lines and points follow the description in Figure 4.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: The dependence of the ratio of CL emission [Si VI] λ1.9640/[Si X] λ1.4300. The green line is the theoretical prediction from Figure 8 in Cann et al. (2018). The authors assumed a fixed L/L Edd = 0.1, n H = 300 cm−2, and ﹩\mathrm{log}U=-2﹩. The red squares indicate the observed ratios. Upper and lower limits are indicated by upward- and downward-facing triangles. Based on the lack of a downturn in the observed data, we conclude that the conditions of the model in Cann et al. (2018) need to be broadened.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: (Left) The averaged R line/R [Si VI] of the CLs compared with their IP. (Right) The averaged offset of the CLs with respect to the NLR compared with their IP. For both cases only sources where all CLs are present are selected.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Histogram of [Si VI] λ1.9640 luminosity, separated by Seyfert 1 and 2. The lines indicate the kernel density estimation of the two distributions.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: Luminosity of [Si VI] λ1.9640 vs. [Si X] λ1.4300. Empty triangles indicate upper limits. The lines follow the description in Figure 4.
Paper: BASS. XXVIII. Near-infrared Data Release 2: High-ionization and Broad Lines in Active Galactic Nuclei 
Authors: Jakob S. den Brok, Michael J. Koss, Benny Trakhtenbrot, Daniel Stern, Sebastiano Cantalupo, Isabella Lamperti, Federica Ricci, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Rogerio Riffel, Alberto Rodríguez-Ardila, Rudolf Bär, Fiona Harrison, Kohei Ichikawa, Julian E. Mejía-Restrepo, Richard Mushotzky, Meredith C. Powell, Rozenn Boissay-Malaquin, Marko Stalevski, Ezequiel Treister, C. Megan Urry, Sylvain Veilleux
Figure caption: (Left) Correlation of [Si VI] λ1.9640 emission with intrinsic hard X-ray luminosity (14–195 keV), colored by Eddington ratio. (Center) Comparison of [Si VI] λ1.9640 and observed hard X-ray 14–195 keV emission, color-coded by SMBH mass. (Right) Comparison of the X-ray photon index Γ as a function of the [Si VI] λ1.9640 line emission colored by hydrogen column density. Many of our sources are from the Swift-BAT 105 month sample, which do not yet have intrinsic X-ray measurements. Consequently a lower number of sources are presented here in this plot.