adsabs/AstroCLIMB huggingface dataset:
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The distribution of 13CO emission fluxes within the 12CO cloud G139.73 extracted by three techniques at cutoff levels of 2σ to 10σ. The σ for clipping and DBSCAN is 0.27 K, which is calculated using the raw 13CO line data. The σ for the moment mask is 0.05 K, estimated from the smoothed 13CO line data.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: (a) A diagram demonstrating the distribution of 12CO molecular clouds, 13CO line emission, and the background region for estimating the rms noise. (b) The distribution of the rms noise of the 13CO line for each molecular cloud.
Paper: Wavelengths and Energy Levels of Singly Ionized Nickel (Ni II) Measured Using Fourier Transform Spectroscopy
Authors: Christian P. Clear, Juliet C. Pickering, Gillian Nave, Peter Uylings, Ton Raassen
Figure caption: Comparison of Ni II FT wavenumbers in this work with the grating wavenumbers of Shenstone (1970). (a) Full wavenumber range of Shenstone (1970). (b) Expanded region of (a) (highlighted with the red background) from 40,000–60,000 cm−1. Red dotted lines on both plots indicate the approximate spectral regions covered by the two problematic photographic plates recorded by Shenstone.
Paper: Wavelengths and Energy Levels of Singly Ionized Nickel (Ni II) Measured Using Fourier Transform Spectroscopy
Authors: Christian P. Clear, Juliet C. Pickering, Gillian Nave, Peter Uylings, Ton Raassen
Figure caption: Comparison of the revised Ni II energy levels of this work and previously published values of Sugar & Corliss (1985). The uncertainties of S+C are shown in red and our uncertainties are in black. The dashed line indicates the position of the −0.17 cm−1 shift discussed in Section 2.3.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption:  13CO structures identified by DBSCAN, but not by the moment mask. The color maps represent the distributions of the velocity-integrated intensities of 13CO line emission. The black contours indicate the boundaries and the level of 50% at the 12CO line velocity-integrated intensities.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Same as Figure C3, but for the 13CO structures extracted by the DBSCAN algorithm at cutoff levels of 2σ, 3σ, 4σ, and 5σ.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Same as Figure C3, but for the 13CO structures identified by the moment mask at cutoff levels of 8σ sm, 9σ sm, 10σ sm, and 11σ sm. The noise σ sm is calculated from the smoothed data. Its value is 0.05 K.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Same as Figure C4, but using DBSCAN at the cutoff level of 2σ (0.54 K).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Same as Figure C4, but using the moment mask at the cutoff level of 9σ sm (0.45 K).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Same as Figure C4, but using the moment mask at the cutoff level of 8σ sm (0.4 K).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Same as Figure C4, but using clipping at the cutoff level of 4σ (1.08 K).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Same as Figure C4, but using DBSCAN at the cutoff level of 3σ (0.81 K).
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Hβ vs. Hα FWHMs (left) and BH masses (right) in BASS/DR2. Black solid crosses represent the median error bars associated with the FWHM and M BH estimates. The relation we find between FWHM(Hα) and FWHM(Hβ) (black dotted line) is broadly consistent with the relation derived in Greene & Ho (2005, red dotted line), which supports our use of their Hα-based M BH prescription. The black solid line represents the 1:1 relation.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: The distribution of BASS/DR2 AGNs among AGN type subclasses in bins of ultrahard X-ray luminosity (﹩\mathrm{log}{L}_{14-150\,\mathrm{keV}}﹩), as indicated in each panel. Higher (lower) luminosity AGNs tend to preferentially belong to the Sy1–1.2 (Sy1.9–2) classes.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: The fraction of BASS/DR2 AGNs of various AGN type subclasses as a function of ultrahard X-ray luminosity (﹩\mathrm{log}{L}_{14-150\,\mathrm{keV}}﹩). The various symbols and lines trace AGNs belonging to the Sy1–1.5 (blue), Sy1.9 (red), and Sy2 (purple) subclasses.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: The distribution of BASS/DR2 AGNs in terms of various AGN type subclasses. We show the percentages and total numbers of Sy1 (blue), Sy1.2 (orange), Sy1.5 (green), Sy1.9 (red), Sy2 (purple), and BZQ (magenta) sources. See text for classification details.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: The Balmer decrement (﹩L\left(\mathrm{bH}\alpha \right)﹩/﹩L\left(\mathrm{bH}\beta \right)﹩) for broad-line BASS/DR2 AGNs. Left:  the distribution of ﹩\mathrm{log}(L\left(\mathrm{bH}\alpha \right)/L\left(\mathrm{bH}\beta \right))﹩ among unbeamed, broad-line BASS/DR2 AGNs, excluding Type 1.9 sources and further split into sources with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\gt 20﹩ and ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\leqslant 20﹩ (top—probability distribution function; bottom—cumulative distribution function). Right: ﹩\mathrm{log}(L\left(\mathrm{bH}\alpha \right)/L\left(\mathrm{bH}\beta \right))﹩ vs. ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})﹩ for AGNs with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\gt 20﹩, again excluding Type 1.9 sources. Note the mild (yet statistically significant) positive correlation between the quantities. In all panels we mark the median values for the ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\leqslant 20﹩ (completely unobscured) and ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\gt 20﹩ subsamples, as well as two reference values from the literature (see legends and text for details).
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Broad Balmer line strength relative to ultrahard X-rays for ﹩L\left(\mathrm{bH}\alpha \right)﹩/L 14−150 keV (left) and ﹩L\left(\mathrm{bH}\beta \right)﹩/L 14−150 keV (right), vs. line-of-sight column density, N H, and the projected distributions of these quantities. Broad-line BASS/DR2 AGNs of various AGN subclasses are marked with different colors and symbols (see legend). Large crosses represent the median values of ﹩L\left(\mathrm{bH}\alpha \right)﹩/L 14−150 keV and ﹩L\left(\mathrm{bH}\beta \right)﹩/L 14−150 keV within equally spaced bins of ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ and the corresponding 90% confidence intervals as determined from bootstrapping. Black thin crosses represent Types 1, 1.2, and 1.5 AGNs, while thick red crosses represent Type 1.9 sources. Type 1.9 AGNs typically have ﹩L\left(\mathrm{bH}\alpha \right)﹩/L 14−150 keV that are significantly lower than those of Types 1–1.5 AGNs, but only in the ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\gtrsim 22﹩ regime.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: The luminosities, BH masses, and Eddington ratios of BASS/DR2 broad-line AGNs. Top: the distribution of BASS/DR2 AGNs in the L/L Edd–M BH plane. Our AGNs are further split by AGN type (left panel) and by redshift range (right panel). Bottom: cumulative distributions of L bol (left), M BH (center) and L/L Edd (right). The M BH of Sy1.9 sources are likely underestimated, and their L/L Edd are thus overestimated (see text for discussion). The small arrows in the top panels indicate the direction of a simple, uniform correction toward the true M BH and L/L Edd of Sy1.9s (see Section 4.5 for a more detailed discussion of mass corrections). The L bol and L/L Edd of beamed AGNs may be significantly overestimated due to jet emission and/or relativistic boosting.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Left: broad-Hα-based vs. σ ⋆-based M BH estimates. Right: ﹩\mathrm{log}\left({M}_{\mathrm{BH},\mathrm{BLR}}/{M}_{\mathrm{BH},{\sigma }_{\star }}\right)﹩ vs. ﹩\mathrm{log}{N}_{{\rm{H}}}﹩. In both panels, light-shaded symbols mark objects for which the measurement-related (i.e., fitting-related) uncertainties on M BH estimates from σ ⋆, ﹩{\rm{\Delta }}\mathrm{log}{M}_{\mathrm{BH},{\sigma }_{\star }}﹩, are larger than 0.1 dex.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Hα FWHMs vs. N H and the projected distribution of these quantities for Sy1 (light blue), Sy1.2 (orange), Sy1.5 (light green), and Sy1.9 (red) AGNs. Horizontal error bars represent the bin edges, and vertical error bars represent the errors in the median FWHM from each bin estimated from bootstrapping. For completeness, Figure 16 shows the complementary FWHM(Hβ) vs. N H parameter space.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Left: ﹩L\left({\rm{H}}\alpha \right)/L﹩(14–150 KeV) vs. FWHM﹩\left({\rm{H}}\alpha \right)﹩. Right: ﹩L\left({\rm{H}}\alpha \right)/L﹩(14–150 KeV) vs. ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ color-coded by FWHM﹩\left({\rm{H}}\alpha \right)﹩. The vertical error bar squares represent the median values of ﹩L\left({\rm{H}}\alpha \right)/L﹩(14–150 KeV) after binning in FWHM﹩\left({\rm{H}}\alpha \right)﹩ (left panel) and ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ (right panel) in equally spaced quantiles. Horizontal error bars represent the bin edges and vertical error bars the errors in the median ﹩L\left({\rm{H}}\alpha \right)/L﹩(14–150 KeV) estimated from bootstrapping.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Spectral fit-quality flag (f Q) examples in order of descending quality for the Hβ (top) and Hα (bottom) spectral complexes: f Q = 1 (left), f Q = 2 (center), and f Q = 3 (right). In each case, the observed spectrum (solid black line) should be compared with the total spectral model (red). We also show the broad Balmer emission-line model (green), the blended iron emission (blue), and the narrow emission lines (dashed black). The black solid line at the bottom of each panel represents the fit residuals.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Broad Hα emission-line luminosity (﹩L\left(\mathrm{bH}\alpha \right)﹩) vs. ultrahard X-ray luminosity (L 14−150 keV) for BASS/DR2 AGNs. Symbol colors mark AGNs of different (emission line) subclasses, as indicated in the legend. The dashed line marks a scaling of ﹩\mathrm{log}(L[\mathrm{bH}\alpha ]/{L}_{14-150\,\mathrm{keV}})=-1.5﹩, which describes the general trend seen in most of our bona fide broad-line AGNs. The broad Hα emission in Type 1.9 AGNs, however, appears suppressed relative to AGNs of other subclasses with comparable L 14−150 keV.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Median FWHM(Hα) for objects with N H smaller than the N H in the ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ (horizontal) axis. The error bars are obtained from bootstrapping and correspond to a confidence level of 90%. Type 1.9 AGNs, which tend to have higher column densities (﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\gt 22﹩) typically also have narrower Hα broad emission lines.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Left: ﹩L\left(\mathrm{bH}\alpha \right)﹩/L 12 μm vs. FWHM(Hα). Right: ﹩L\left(\mathrm{bH}\alpha \right)﹩/L 12 μm vs. ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ color coded by FWHM(Hα). Large crosses represent the median values of ﹩L\left(\mathrm{bH}\alpha \right)﹩/L 12 μm after binning in FWHM(Hα) (left panel) and ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ (right panel) in equally spaced quantiles. Horizontal error bars represent the bin edges and vertical error bars the errors in the median ﹩L\left(\mathrm{bH}\alpha \right)﹩/L 12 μm estimated from bootstrapping.
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Hβ FWHMs vs. N H and the projected distribution of these quantities for Sy1 (light blue), Sy1.2 (orange), Sy1.5 (light green), and Sy1.9 (red). Horizontal error bars represent the bin edges and vertical error bars represent the errors in the median FWHM from each bin estimated from bootstrapping. This figure complements Figure 9; however, in contrast to FWHM(Hα), here the median FWHM(Hβ) does not vary with ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ (within the error bars).
Paper: BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration
Authors: Julian E. Mejía-Restrepo, Benny Trakhtenbrot, Michael J. Koss, Kyuseok Oh, Jakob den Brok, Daniel Stern, Meredith C. Powell, Federica Ricci, Turgay Caglar, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Fiona A. Harrison, C. M. Urry, Tonima Tasnim Ananna, Daniel Asmus, Roberto J. Assef, Rudolf E. Bär, Patricia S. Bessiere, Leonard Burtscher, Kohei Ichikawa, Darshan Kakkad, Nikita Kamraj, Richard Mushotzky, George C. Privon, Alejandra F. Rojas, Eleonora Sani, Kevin Schawinski, Sylvain Veilleux
Figure caption: Comparison between DR1 and DR2 measurements: line widths (FWHM; top) and BH masses (M BH; bottom), for both Hα (left) and Hβ (right). In all panels, black solid lines represent the 1:1 relation and black dashed lines trace the median offsets between DR1 and DR2 measurements.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: Distributions of redshift (top panels), narrow-line flux ratios of O3HB and N2HA (middle two panels), and the luminosity of the core components of the [O III] line (bottom panels) of Type 1 AGNs (histogram filled with blue lines) and Type 2 AGNs (histogram filled with red lines) in the main samples (left panels) and subsamples (right panels). In each right panel, the significance level provided by the Kolmogorov–Smirnov statistic technique is marked in red. In each left panel, the mean values of Type 1 and Type 2 AGNs are marked in blue and red in the top region.