adsabs/AstroCLIMB huggingface dataset:
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Optical emission-line ratio ([N II]λ6583/Hα) vs. Eddington ratio (λ Edd) diagram. Black open circles and triangles indicate unobscured AGNs (i.e., Sy1, Sy1.2, Sy1.5, Sy1.8, and Sy1.9) and obscured AGNs (Sy2), respectively. The median in each bin of these AGNs is indicated by blue filled triangles and red filled circles. The black solid line indicates the measured anticorrelation. The gray-shaded regions account for the errors in the slope and intercept. The dotted lines indicate rms deviation. Green filled circles are unobscured AGNs at a higher redshift at 〈z〉 = 1.3 (Oh et al. 2019). Pearson correlation coefficient, p-value, and typical uncertainties are shown in the bottom left corner.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption:                       ﹩{L}_{[\mathrm{OIII}]}^{\mathrm{int}}/{L}_{2\mbox{--}10\ \mathrm{keV}}^{\mathrm{int}}﹩ ratio as a function of 2–10 keV intrinsic luminosity. The red filled dots indicate average values, and the red bars show 1σ deviations in the bins. This figure includes BAT AGNs that are classified into either one of the categories (Seyfert, LINER, composition, and H II) from the [O III]λ5007/Hβ versus [N II]λ6584/Hα diagnostic diagram. Typical uncertainties are shown in the bottom left corner. The 2–10 keV intrinsic luminosity bins are of equal width. The symbols and colors are the same as that of Figure 9.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Example of spectral line fitting. Counterpart name, BAT name, redshift, instrument, observed date, and exposure time are shown at the top. Top left: Digitized Sky Survey image in the arcmin scale. Top right: The black line represents the observed spectrum in the rest frame. The red dashed–dotted line is the best fit. BPT diagnostics diagrams are shown in the insets. Middle and bottom rows show the spectral fitting result in detail, and they include the labels of the detected emission lines. In the case of low A/N, smaller than 3, red labels are used. The blue and green Gaussians are narrow and broad emission-line components, respectively. Residuals are shown as black dots.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Comparison of BAT AGNs with optically selected AGNs in the SDSS from the OSSY catalog (Oh et al. 2011). Left panel: O III luminosity versus redshift. Median and 1σ distribution for BAT AGNs are shown in blue (Sy1−Sy1.8) and red (Sy1.9 and Sy2), respectively. The SDSS AGNs are displayed in light gray dotted lines (broad-line AGNs) and thick dark gray dashed lines (narrow-line AGNs). The contours represent 68% and 95% distributions. The BAT broad-line AGN and narrow-line AGNs exhibit higher O III luminosities than the SDSS AGNs. Right panel: Balmer decrement compared to the SDSS narrow-line AGNs. BAT narrow-line AGNs are dustier than the SDSS narrow-line AGNs, which exhibit a higher fraction of (Hα/Hβ)obs. greater than 5.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Examples of AGNs featuring asymmetric broad lines and double-peaked narrow emission lines. Left panel: Hα spectral complex of RBS 273, which presents the asymmetric broad-line components. The color codes are the same as those of Figure A1. Right panel: Hα spectral complex of IC 4709. Double-peaked narrow emission lines (blue) with underlying wing components (orange) are distinctively decomposed. The measured velocity offset between the narrow emission lines is 328 km s−1.
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: Horizontal bar chart showing the number of spectra taken with each telescope, instrument, or survey. The archival sample is from earlier surveys that were not included in the DR1, including ROSAT AGNs that overlap with BASS in unpublished or published (Grupe et al. 2004) works, from the Palermo surveys of Swift BAT AGNs (Rojas et al. 2017), or as part of an atlas of low-redshift AGNs (Ho & Kim 2009).
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: Summary of the different observing conditions for DR2 spectra for telescopes with more than 15 spectra. Observing dates are shown for the newly observed sample (top left) and archival sample (top right). The spectral resolution at 5000 Å (middle left) and 8500 Å (middle right) for the different observations. Finally, the seeing and average air mass of the observations (bottom row).
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 spectra of sources identified as Galactic based on emission or absorption lines at redshift zero.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Sources of 743 unique AGN spectra used for this study from the BASS DR2 and BASS DR1. Some AGN only BASS DR2 spectra are in short wavelength high-resolution setups not covering the full suite of emission lines, so DR1 data was used. The BASS DR2 obtained spectra are from targeted spectroscopic campaigns using the Hale 200 inch telescope (N = 271), ESO-VLT (N = 169), du Pont (N = 41), SOAR (N = 32), and Keck (N = 5). Spectra from publicly available surveys, such as SDSS (N = 118), 6dF (N = 36), and the BASS DR1 (N = 66), are also used in this study.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Example of spectral line fitting for narrow-line source (NGC 788). The top panel shows the full-range spectral fits. The black line represents the observed spectrum in the rest frame. The red dashed–dotted line is the best fit. The bottom panels show the spectral fitting result in detail, and they include the labels of the detected emission lines. In the case of low A/N, smaller than 3, red labels are used. The blue Gaussians represent narrow emission-line components, which are shown with arbitrary offset for clarity. Residuals are shown using black dots.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Example of spectral line fitting for broad-line source (2MASX J02593756 + 4417180). The format is the same as that of Figure 2. The green Gaussians represent broad emission-line components.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Emission-line classification of the BAT AGNs using line diagnostics diagrams (Baldwin et al. 1981; Kauffmann et al. 2003; Kewley et al. 2001, 2006; Schawinski et al. 2007). Left panels: Histograms for the entire sample. “AGN limit” refers to objects that are located either in the Seyfert or LINER regions, which have a 3σ upper limit in any of the used emission lines. The remaining categories, shown using orange histograms, have features that prevented measurements. “Weak lines” includes objects where the Gaussian amplitude to noise ratios (A/N) of the detected emission lines do not surpass the threshold (A/Nline < 3). “Nondetection” refers to objects not detected in both of the needed emission lines to measure a ratio. “Not applicable” represents objects for which the emission-line strengths are less reliable. This may be owing to either the high E(B − V) at the Galactic plane (>0.5) or the lack of spectral coverage, owing to high-z nature or instrumental limitations. Objects with a poor spectral fit in any of the used emission lines and the two objects without the O III and Hα spectral complex are also included in this category. “No spec.” indicates three missing spectra. The number of sources in each class is written in parenthesis. Right panels: Line diagnostic diagrams for sources with sufficient measurable emission lines to be classified using line diagnostic diagrams. Narrow-line objects are shown with squares and broad-line objects with triangles. The gray filled contours are drawn from the OSSY catalog and the follow-up broad-line AGN study that shows the samples of SDSS emission-line galaxies at z < 0.2 (Oh et al. 2011, 2015). Note that only narrow lines are used to produce the diagnostics diagrams.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: AGN-type fraction as a function of column density. The [O III]λ5007/Hβ versus [N II]λ6583/Hα diagram is used for classification. Left: The left ordinate is for objects classified by emission-line ratios as LINER (orange), composite (green), H II (blue), AGNs with an upper limit (gray), and objects that cannot be diagnosed, such as “Galactic plane,” “high-z,” “undetected [O III]λ5007,” “no spec.,” and objects exhibiting weak emission lines (A/Nline < 3) (black). The right ordinate is for the Seyfert class (red). The total number of objects presented in each bin is 221, 139, 145, 147, and 94, from low to high column density. The number of objects in each class at a given column density bin is shown in the figure next to its fraction. Right: Seyfert AGNs shown in the left panel are further classified into subtypes.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Left: Comparison of O III luminosities (L[O III]DR2 versus L[O III]DR1). Spectral sources used in DR2 are shown with different symbols and colors. Dotted line indicates the one-to-one fiducial line. Objects for which the O III line is decomposed, either to outflows or to double-peaked narrow emission lines, are shown using red thick symbols. Right: Spectral resolution (FWHM [km s−1]) distribution. BASS DR2 and DR1 are shown using blue filled and empty histograms, respectively.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: AGN subclasses (blue), LINERs (green), and unclassifiable cases (orange). We classified 98% of BAT AGNs (732/746) into the subtypes. “Undetected [O III]” refers to objects that lack the O III emission line. “No coverage” indicates objects for which either O III falls into a spectral gap between the blue and red sides of the detector or Hα is lacking in the spectral complex, owing to a limited spectral coverage of the obtained optical spectra. “High-z” represents objects that are not applicable for classification using the obtained spectral coverage, owing to their high redshift nature. “Galactic plane” indicates objects with a poor fitting quality at E(B − V) > 0.5.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Fraction of subclasses of Seyferts and LINERs as a function of 2–10 keV intrinsic luminosity (left panel) and redshift (right panel). Blue filled dots (median at each bin) and a dashed line present Seyfert 1–1.8, which display broad Hβ, whereas AGNs with broad Hα are shown in red. Light purple dots and a dashed line represent Seyfert 2 narrow-line AGNs. Note that the fraction of LINERs selected from the [S II]λλ6717, 6731/Hα diagnostic diagram is shown in green.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: FWHM of Hα as a function of hydrogen column density. There are 199 examples of Sy1-1.5, 7 of Sy1.8, and 9 of Sy1.9 that exhibit a column density with a lower limit (N H = 1020 cm−2). The colors represent AGN subtypes according to the Winkler classification (Winkler 1992).
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Emission-line classification of the BAT AGNs using line diagnostics diagrams (Kewley et al. 2006; Shirazi & Brinchmann 2012). The same scheme as the previous line diagnostic figure is used.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Subtypes of BAT AGNs (blue) in common with the second ROSAT all-sky survey (2RXS, orange) source catalog. In total 554 sources are found in both catalogs out of the 743 BAT AGNs discussed in this study.
Paper: BASS. XXIV. The BASS DR2 Spectroscopic Line Measurements and AGN Demographics
Authors: Kyuseok Oh, Michael J. Koss, Yoshihiro Ueda, Daniel Stern, Claudio Ricci, Benny Trakhtenbrot, Meredith C. Powell, Jakob S. den Brok, Isabella Lamperti, Richard Mushotzky, Federica Ricci, Rudolf E. Bär, Alejandra F. Rojas, Kohei Ichikawa, Rogério Riffel, Ezequiel Treister, Fiona Harrison, C. Megan Urry, Franz E. Bauer, Kevin Schawinski
Figure caption: Redshift distribution of the BASS sample. The number presented next to each bar indicates the number of sources in which that redshift is confirmed and the total number of sources in the given redshift range.
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 molecfit correction on a spectrum within the BASS DR2. Top left: VLT/X-shooter spectra of a broad-line BAT AGN Fairall 9 in the visual arm (5500–10500 Å). The top right panel and middle row show zoom-in regions around absorption features. The red lines are the telluric-absorption-corrected (TAC) spectra, and gray lines are the input raw spectra. The telluric absorption features cover broad Hα, as well as the prominent narrow emission lines at He II λ8237 and [S II] λ9531 emission lines. molecfit recovers these emission lines as shown with the TAC spectra, which are particularly important for accurately measuring Hα, He II λ8237, and [S II] λ9531. The bottom row shows the CaT region before (left) and after (right) molecfit correction when being fit with a galaxy template for a velocity dispersion measurement (Koss et al. 2022b). The model fit is shown in red, with residuals from the fit shown with green dots below the spectra. The TAC spectrum is able to recover a larger region of the Ca II triplet spectral region (8450–8700 Å), which is redshifted into telluric features at z > 0.04 with no significant increase in residuals.
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: Left: histogram of the BH mass estimates excluding broad-line measurements in X-ray-obscured AGNs (N H > 1022 cm−2). Right: histogram of the BH mass estimates in the small number of X-ray-obscured AGNs with only broad-line measurements. While many of these AGNs do have BH masses consistent with the other unobscured distribution (e.g., >107 M ⊙), there is a larger fraction with low masses (<107 M ⊙) that may be significantly underestimated.
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 high-resolution spectral setups not shown earlier in the text excluding the archival observations. Spectra taken at the Palomar telescope with the Doublespec instrument with the 1200 line mm–1 grating are shown in the top panel, with spectra from SOAR with 1200 line mm–1 grating using the Goodman instrument shown in the middle panel and finally an echelle spectrum from Magellan using the magE instrument shown in the bottom panel.