adsabs/AstroCLIMB huggingface dataset:
Paper: BASS. XXI. The Data Release 2 Overview
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Richard Mushotzky, C. Megan Urry, Tonima T. Ananna, Mislav Baloković, Jakob S. den Brok, S. Bradley Cenko, Fiona Harrison, Kohei Ichikawa, Isabella Lamperti, Amy Lein, Julian E. Mejía-Restrepo, Kyuseok Oh, Fabio Pacucci, Ryan W. Pfeifle, Meredith C. Powell, George C. Privon, Federica Ricci, Mara Salvato, Kevin Schawinski, Taro Shimizu, Krista L. Smith, Daniel Stern
Figure caption: Distribution of BH masses (M BH) and Eddington ratios (L bol/L Edd) for the entire sample of BASS AGNs for which redshift measurements are available, including unbeamed AGNs (e.g., Sy1, Sy1.9, and Sy2) and beamed AGNs (BZQs). The lower limits on M BH and L bol/L Edd due to the survey flux limits are illustrated with dashed (antidiagonal) lines, for various redshifts corresponding to z = 0.01 (L bol = 1.8 × 1043 erg s−1), z = 0.04 (L bol = 3.2 × 1044 erg s−1), and z = 0.1 (L bol = 2.0 × 1045 erg s−1). Errors in M BH are of order 0.5 dex owing to systematic uncertainties in virial and σ *-based scaling relations (e.g., Ricci et al. 2022). The BASS unbeamed AGNs occupy narrow, redshift-dependent slices of the M BH − L bol/L Edd plane owing to the Eddington limit and survey flux limits (see text for details). Interestingly, we find that the log(L bol/L Edd) tends to be bounded at −2.5 to −3, possibly associated with BAT identifying disk accretion primarily rather than inefficient accretion and the upper bounds at the Eddington limit (except for beamed AGNs). The lower bound of the BH mass distribution corresponds to ﹩\mathrm{log}\left({M}_{\mathrm{BH}}/{M}_{\odot }\right)﹩ = 5, where the range pushes into intermediate-mass BHs and would only be sensitive to Eddington/super-Eddington accretion, if it exists. The upper limit at ﹩\mathrm{log}\left({M}_{\mathrm{BH}}/{M}_{\odot }\right)﹩ = 10 is largely due to the space density of massive BHs.
Paper: BASS. XXI. The Data Release 2 Overview
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Richard Mushotzky, C. Megan Urry, Tonima T. Ananna, Mislav Baloković, Jakob S. den Brok, S. Bradley Cenko, Fiona Harrison, Kohei Ichikawa, Isabella Lamperti, Amy Lein, Julian E. Mejía-Restrepo, Kyuseok Oh, Fabio Pacucci, Ryan W. Pfeifle, Meredith C. Powell, George C. Privon, Federica Ricci, Mara Salvato, Kevin Schawinski, Taro Shimizu, Krista L. Smith, Daniel Stern
Figure caption: The rest-frame 2–10 keV luminosities of the BASS DR2 AGNs and of higher-redshift X-ray AGN surveys. Although BASS AGNs are selected based on their 14–195 keV emission, we plot the best-fit intrinsic 2–10 keV emission based on detailed X-ray spectral modeling (Ricci et al. 2017b). Unbeamed BASS AGNs are shown with purple stars, while beamed AGNs are shown with purple triangles. The unbeamed AGNs in the BASS sample tend to span the moderate-to-high-luminosity end of the XLF. We also show samples drawn from deeper X-ray AGN surveys, including Stripe 82X (red pentagons; LaMassa et al. 2016; Ananna et al. 2017), CDF-S (brown pentagons; Luo et al. 2017), Chandra COSMOS Legacy survey (blue circles; Civano et al. 2016; Marchesi et al. 2016), XMM XXL (green diamonds; Pierre et al. 2016), and the NuSTAR Serendipitous Survey (yellow squares; Lansbury et al. 2017). We also show contours for eFEDS containing 99% of the data (dashed gray; Salvato et al. 2022). We limit our comparison to X-ray sources with confirmed counterparts with spectroscopic redshifts. For eFEDS, unlike the other surveys, the soft-band flux (0.2–2.3 keV) was used to estimate the hard X-ray 2–10 keV emission assuming a power-law spectral model with Γ = 1.7 since only a small number of sources were detected above 2.3 keV (<1% Brunner et al. 2022). For these higher-redshift X-ray surveys we assumed a power-law spectral model with Γ = 1.7, to bring each X-ray luminosity to the rest frame by K-correcting the apparent luminosities based on the observed redshifts into the 2–10 keV rest frame. The deeper, higher-redshift samples tend to sample a luminosity range that is consistent with that covered by BAT, but at higher redshift.
Paper: BASS. XXI. The Data Release 2 Overview
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Richard Mushotzky, C. Megan Urry, Tonima T. Ananna, Mislav Baloković, Jakob S. den Brok, S. Bradley Cenko, Fiona Harrison, Kohei Ichikawa, Isabella Lamperti, Amy Lein, Julian E. Mejía-Restrepo, Kyuseok Oh, Fabio Pacucci, Ryan W. Pfeifle, Meredith C. Powell, George C. Privon, Federica Ricci, Mara Salvato, Kevin Schawinski, Taro Shimizu, Krista L. Smith, Daniel Stern
Figure caption: The distribution of BASS DR2 AGNs in the Eddington ratio vs. redshift (top) and bolometric luminosity vs. BH mass (bottom) planes. The large squares indicate the binned medians for each AGN subclass with redshift (top) and M BH (bottom). Error bars on the plotted median values are equivalent to 1σ, calculated based on a bootstrap procedure with 100 realizations. The number of bins was fixed to four constructed to have equal numbers of sources in each bin. For comparison, we plot SDSS quasars at z < 0.3 (gray contours; Shen et al. 2011) and lower-luminosity SDSS type 2 Seyferts (purple contours; Greene & Ho 2005). The solid and dashed contours cover 68% and 95% of the data, respectively. We also plot the median for PG quasars (Boroson & Green 1992; black squares) and SDSS type 2 quasars (Kong & Ho 2018) selected based on their ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]\,\lambda 5007﹩ emission (purple squares). The BASS AGNs have roughly similar BH masses and bolometric luminosities to the different SDSS samples but also extend to lower redshifts and BH masses. We note that there is essentially no overlap between BASS DR2 and these SDSS-based samples of powerful AGNs (see text for discussion).
Paper: BASS. XXI. The Data Release 2 Overview
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Richard Mushotzky, C. Megan Urry, Tonima T. Ananna, Mislav Baloković, Jakob S. den Brok, S. Bradley Cenko, Fiona Harrison, Kohei Ichikawa, Isabella Lamperti, Amy Lein, Julian E. Mejía-Restrepo, Kyuseok Oh, Fabio Pacucci, Ryan W. Pfeifle, Meredith C. Powell, George C. Privon, Federica Ricci, Mara Salvato, Kevin Schawinski, Taro Shimizu, Krista L. Smith, Daniel Stern
Figure caption: Summary scatter plots of the line-of-sight hydrogen column density (N H, an obscuration indicator) vs. BH mass (top) and Eddington ratio (bottom). Different symbols mark subclasses of unbeamed BASS AGNs (e.g., Sy1, Sy1.9, and Sy2). X-ray measurements of N H = 1020 cm−2 are essentially upper limits and represent sources with no sign of obscuration. The large squares indicate the binned medians for each subclass. Error bars on the plotted median values are equivalent to 1σ and calculated based on a bootstrap procedure with 100 realizations. The bin sizes were constructed to have equal numbers of sources in each bin. The Sy1 AGNs tend to have higher Eddington ratios than the narrow-line AGNs (Sy1.9 and Sy2). Typical 90% errors in N H are <0.2 dex based on X-ray modeling (Ricci et al. 2017a), but higher for heavily obscured AGNs, log ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})﹩ > 24.5.
Paper: BASS. XXI. The Data Release 2 Overview
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Richard Mushotzky, C. Megan Urry, Tonima T. Ananna, Mislav Baloković, Jakob S. den Brok, S. Bradley Cenko, Fiona Harrison, Kohei Ichikawa, Isabella Lamperti, Amy Lein, Julian E. Mejía-Restrepo, Kyuseok Oh, Fabio Pacucci, Ryan W. Pfeifle, Meredith C. Powell, George C. Privon, Federica Ricci, Mara Salvato, Kevin Schawinski, Taro Shimizu, Krista L. Smith, Daniel Stern
Figure caption: The distribution of BASS DR2 in the bolometric luminosity vs. and redshift (top) and WISE colors vs. bolometric luminosity (bottom) planes. For comparison, we also plot the distributions of WISE-selected AGNs at z < 0.3 (Assef et al. 2018; red contours), with SED fitting and redshifts measured from the SDSS (Barrows et al. 2021). The solid and dashed contours cover 68% and 95% of the WISE AGN data, respectively. A black dashed line indicates the WISE color cut to identify AGNs (W1 − W2 > 0.8; Stern et al. 2012). The BAT AGNs tend to probe similar luminosities to the higher-redshift WISE AGNs, but at lower redshifts.
Paper: BASS. XXI. The Data Release 2 Overview
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Richard Mushotzky, C. Megan Urry, Tonima T. Ananna, Mislav Baloković, Jakob S. den Brok, S. Bradley Cenko, Fiona Harrison, Kohei Ichikawa, Isabella Lamperti, Amy Lein, Julian E. Mejía-Restrepo, Kyuseok Oh, Fabio Pacucci, Ryan W. Pfeifle, Meredith C. Powell, George C. Privon, Federica Ricci, Mara Salvato, Kevin Schawinski, Taro Shimizu, Krista L. Smith, Daniel Stern
Figure caption: Overview of the BASS DR2 optical spectroscopy as observed on the sky (shown in equatorial coordinates and a Mollweide projection). The Galactic plane is indicated by the light-gray line.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Examples of the X-Shooter stellar templates obtained via hierarchical clustering analysis and used in our work. Left: 21 blue (UVB) X-Shooter templates constructed from a subset of 628 X-Shooter stellar spectra, sorted by prominence in the spectral library (see Section 3.2). Right: 19 red (VIS) X-Shooter templates similarly constructed from a subset of 718 X-Shooter stellar spectra (see Section 3.2). The number next to the vertical axis of each template indicates the number of stellar spectra among the parent sample in which the features were found during the clustering analysis. All templates are shown in arbitrarily scaled units of F  λ .
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Summary of the AGN and the different observing conditions for the best 484 spectra in the sample. Top left: redshift range of the AGN in the sample, split into Sy 1.9 and Sy 2. Top right: slit width size in kiloparsecs for our AGN (again split into Sy 1.9 and Sy 2 sources). Bottom panels: instrumental resolution at 5000 (left) and 8500 Å (right) for the best spectra, from which we successfully measured σ * from the 3880–5550 Å or CaT spectral regions (respectively).
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Plot of the distribution of σ * and M BH (based on the Kormendy & Ho 2013 relation) with redshift. The color bar indicates the Eddington ratio (L/L Edd) of the AGN. Error bars in σ * span 1–29  km  s−1, with a median of 7  km  s−1. The effective sensitivity limits on the Eddington ratio due to the survey flux limits are illustrated with diagonal dashed lines. For instance, the flux limit at z = 0.01 (L bol = 1.8 × 1043 erg s−1) corresponds to an L/L Edd = 1 (blue dashed line) source with M BH = 1.5 × 105 M ⊙ or σ * = 35  km  s−1. Therefore, any sources detected at z = 0.01 with σ * < 35  km  s−1  will always be super-Eddington because of the survey flux limits. The black dotted line indicates the instrumental limits of the survey for velocity dispersion measurements. One higher-redshift AGN, BAT ID = 1204 (σ * = 364  km  s−1, Eddington ratio = 0.20, z = 0.597), is not shown.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Top left: velocity dispersion measurements from the best spectra compared to lower-quality different secondary spectra in the blue region (3880–5550 Å). Here Sy 1.9 (with broad Hα) is shown by red triangles, and Sy 2 is shown by blue circles. Error bars (at 1σ) are shown in gray. A solid black line indicates the one-to-one relation with dashed gray lines indicating offsets of 30  km  s−1 . The large squares indicate the binned medians for each subclass. Error bars on the plotted median values are equivalent to 1σ and calculated based on a bootstrap procedure with 100 realizations. The bin sizes were constructed to have equal numbers of sources in each bin. Top right: comparison between the velocity dispersion measurements from the best spectra and the secondary spectra in the CaT region (8350–8730 Å). Bottom right: comparison between the 3880–5550 Å and CaT within the single same best spectrum.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Comparison of the BASS AGN to the velocity dispersion of dwarf galaxies hosting AGN (Baldassare et al. 2020). This dwarf AGN sample was identified in the SDSS at z < 0.055 based on emission line diagnostics and broad lines in Hα (Reines et al. 2013). The dashed blue line indicates the sky sensitivity limit for a source at the Eddington limit (L/L Edd = 1) at the BAT survey all-sky flux limits, so any Sy 1.9 and Sy 2 detected by BAT below this line would be super-Eddington. The black dotted line indicates the BASS instrumental limits for velocity dispersion measurements (σ inst ∼ 25  km  s−1), which is the similar to the the Keck study (σ inst = 23  km  s−1).
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Examples of velocity dispersion fits for three AGN spectra (from top to bottom: BAT IDs 112, 408, and 436), representative of the three most common observational setups (from top to bottom: VLT/X-Shooter, SDSS, and Palomar/DBSP). The three spectra shown here illustrate the fitting quality typical of the top quartile, median, and bottom quartile of the velocity dispersion errors (from top to bottom: Δσ * = 4, 7, and 11  km  s−1, respectively). In all panels, the red lines indicate the observed spectra, and the best-fitting templates are shown in black. The red dashed vertical lines indicate important absorption features, while the blue dashed vertical lines mark possible emission features that are masked out in the gray regions.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Comparison between the velocity dispersion measurements from the best spectra and the literature values for the same AGN. Error bars (at 1σ) are shown in gray. A black solid line indicates the one-to-one relation, with dashed gray lines indicating offsets of 30  km  s−1 . The comparison samples are as follows: H09, Ho et al. (2009); GR05, Garcia-Rissmann et al. (2005); V15, van den Bosch et al. (2015); and NW95, Nelson & Whittle (1995).
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Comparison of nearby obscured BASS AGN (Sy 1.9 and Sy 2, z < 0.1, N = 444) to optically selected nearby (z < 0.1) narrow-line Seyferts (N = 4926) and SFGs (N = 97,216) in the SDSS DR7 from the OSSY catalog (Oh et al. 2011). The orange dashed line indicates the instrumental limit of the SDSS (∼70  km  s−1) compared to the instrumental limits for BASS AGN, shown with a black dashed line (∼25  km  s−1).
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Distributions of velocity dispersions (left) and measurement errors (right) for the 3880–5550 Å (N  =  254) and CaT (N  =  230) fitting regions from the best fits. The median velocity dispersions from the 3880–5550 Å region are somewhat higher than those from the CaT region (173 and 144  km  s−1, respectively). This is due to the typically higher redshifts of the AGN for which a fit from the 3880–5550 Å region is available (median z = 0.042) compared to those with CaT measurements (z = 0.024), as the latter spectral region is limited by the increasing effect of telluric features (at z > 0.065).
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Distributions of velocity dispersions (left) and measurement errors (right) for Sy 1.9 (N  =  113) and Sy 2 (N  =  371). The two subsamples are very similar, with a median of 153 ± 5 and 157 ± 3  km  s−1  for Sy 1.9 and Sy 2, respectively.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Frequency distributions of SMBH masses and Eddington ratios for Sy 1.9 (N = 113) and Sy 2 (N = 371).
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Estimated SOI (r SOI) in parsecs for obscured AGN in this sample based on the velocity dispersion measurements. The dashed lines indicate the ability to detect the dynamical influence of the SMBH, assuming the observations have a minimum spatial resolution of twice the r SOI (Davis 2014). The black dashed lines indicate the limiting resolution for AO observations of stellar dynamics using the CO bandheads in the K band, assuming a good tip-tilt star is available (0.″06 FWHM). The vertical line is due to these bands shifting out of the K band (at z = 0.032). The red dashed line indicates the capabilities of ALMA to resolve the gas dynamics for the CO 2–1 line at higher spatial resolutions (0.″03 FWHM). The large orange squares indicate sources with dynamical and/or megamaser measurements.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Comparison between different velocity dispersion measurements. In all panels, Sy 1.9 (with broad Hα) is shown with red triangles, and Sy 2 is shown with blue circles. Error bars (at 1σ) are shown in gray. A solid black line indicates the one-to-one relation, with dashed gray lines indicating offsets of 30  km  s−1. Top left: comparison between the velocity dispersion measurements from the SDSS for the DR1 and DR2 for DR1 measurements with Δσ * < 20  km  s−1. Top right: comparison between the velocity dispersion measurements from other DR1 samples and the current best measurements. Bottom: comparison between the velocity dispersion measurements from the KP DR1 samples where there is a significant fraction of outliers.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Comparison of the inferred M BH mass estimate from σ * compared to direct measurements using megamaser compilations (Greene et al. 2016), as well as stellar (Neumayer 2010; Medling et al. 2011; Walsh et al. 2012) and gas dynamics (Tadhunter et al. 2003; Capetti et al. 2005; Wold et al. 2006) measurements. Error bars in M BH inferred from σ * have been set to 0.5 dex based on past comparisons with direct measurements (e.g., 0.44 dex; Gultekin et al. 2009).