adsabs/AstroCLIMB huggingface dataset:
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: As in Figure E1, the BHMFs, ERDFs, and reconstructed XLFs are shown in the top, middle, and bottom panels, respectively, for both the Type 1 and Type 2 AGNs in BASS/DR2 (the left and right panels). These functions are calculated assuming a luminosity-dependent bolometric correction (Duras et al. 2020). We show the intrinsic distributions derived for all AGNs, assuming uncertainties of either ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}=0.3﹩ and ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.47﹩ dex or ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}=0.5﹩ and ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.62﹩ dex, in the black and green lines, respectively. The black data points in the bottom panel show the direct 1/V max XLF estimates, and the black dashed line is the fit to those points. The solid black lines show the final, bias-corrected intrinsic distribution functions for the complete AGN sample.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: Results for Type 1 (top three rows) and Type 2 (bottom three rows) AGNs for mock catalog 1 with luminosity-dependent bolometric correction (Duras et al. 2020). The intrinsic distributions are as described in Figures D1 and D2 for Mock #1. In this case, we also assume that the scattered intrinsic luminosity is scattered by σ = 0.37, and therefore the scatter on λ E is ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=\sqrt{{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}^{2}+{\sigma }_{\mathrm{logL},\mathrm{scatt}}^{2}}﹩. Each panel reports the assumed ﹩\sigma ={\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}=0,0.3﹩, or 0.5. Even with these assumptions, the bias-corrected intrinsic distributions are a much better match to the mock input catalog than the 1/V max results.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: The BASS/DR2 BHMFs: Type 1 (the blue solid line), Type 2 (the red solid line), and all AGNs (the black solid line), compared to the Weigel et al. (2016) galaxy stellar mass function (the green dashed–dotted line), shifted left in mass by 2.88 dex to line up the breaks in galaxy Schechter function (the green vertical line) and the modified Schechter function for all AGNs (the black vertical line). The dispersion in the galaxy stellar mass function also includes the galaxy stellar mass functions of Peng et al. (2010), Baldry et al. (2012), and Taylor et al. (2015). All shaded regions show ±1σ errors for each function.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: The three probability chains (Type 1 in blue, Type 2 in red, and overall in black) plotted together.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: Number densities of BASS Type 2 AGNs (left panels; red points/lines) and all AGNs (right panels; black points/lines), assuming an absorption function and attenuation curve for a template spectra with torus opening angle of 60°. The overplotted green lines show the results for a template spectra with torus opening angle of 35°.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: BH mass, Eddington ratio, and luminosity distribution functions of BASS/DR2 Type 1 (left panels) and Type 2 (right panels) AGNs. For both types of AGNs, combining the BHMF (top row) and the ERDF (middle row) reproduces the observed XLF (bottom row). The data points come from the 1/V max analysis, and the dashed lines represent the fits to these data points. The solid lines and the shaded areas show the final, bias-corrected intrinsic distribution functions. The lines of different colors trace the intrinsic distributions, assuming various levels of uncertainty (see the legends for details). Specifically, the blue (left) and red (right) solid lines assume uncertainties of ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}={\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.3;﹩ the orange solid lines assume ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}=0.3﹩ and ﹩{\sigma }_{\mathrm{log}L,\mathrm{scatt}}=0.2﹩ (or ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.36﹩); and the green dotted lines assume ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}={\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.5﹩ dex. The intrinsic distributions of Type 1 AGNs (assuming σ = 0.3) are also shown in the right panels, to highlight the differences between Type 1 and 2 AGNs. Note that the 1/V max points shown for each subset of AGNs were calculated by considering only the AGNs of the respective type (i.e., Type 1 or 2 AGNs). The 1/V max values are reported in Tables F2–F4.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: The XLFs for BASS AGNs in different regimes of N H. Top panels: from left to right, the black points and black lines show the XLF for unobscured Compton-thin (N H < 1022 cm−2), obscured Compton-thin (1022 cm−2 ≤ N H < 1024 cm−2), and Compton-thick (N H > 1024 cm−2) AGNs. The XLF for the entire BASS sample is shown by the blue filled circles and the blue solid lines. Also shown in the top right panel is the XLF of the BAT Compton-thick AGNs from Akylas et al. (2016), which includes objects at z < 0.01, below the limit used in our analysis. Bottom panels: the ratios between the N H subsample XLFs and the XLF of all AGNs in each ﹩\mathrm{log}{L}_{{\rm{X}}}﹩ bin (the black data points), along with the associated Wilson score intervals (the black vertical lines). The numbers refer to the objects in each bin, with the upper and lower rows corresponding to the subsample and the full sample, respectively. These XLFs and ratios should be treated as representing the AGNs observed within BASS/DR2, in the corresponding absorption bins, rather than intrinsic XLFs (which would also account for the AGNs completely missed by our survey; see the main text).
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: The effect of the low redshift cut and obscuration on the BASS XLF. Left panel: the BASS XLF determined without a low-z cut (blue squares; 672 sources), and the corresponding fit (dotted blue line). The Green plus signs show the XLF after excluding nearby sources with z < 0.01 (leaving 659 sources in the sample), with the green dashed line showing the fit to these ΦL values. For comparison, we show the XLFs by Sazonov et al. (2007), Tueller et al. (2008), and Ajello et al. (2012). Right panel: the obscuring column density N H has a small but systematic effect on the XLF. The Green plus signs and the green dashed line show the XLF computed by not taking obscuration into account when computing the 1/V max values, while the orange filled circles (shifted left by 0.05 dex for clarity) illustrate the obscuration-corrected ΦL values. The N H correction consistently increases the space densities in most luminosity bins. The turquoise crosses (shifted right by 0.05 dex for clarity) and the turquoise solid line show the XLF after applying all the cuts in Table 1 (586 sources).
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: Contour plots of the best-fit bivariate distribution functions (top panels), BHMF marginalized over bins of ﹩\mathrm{log}{\lambda }_{{\rm{E}}}﹩ (middle panels), and ERDF marginalized over bins of ﹩\mathrm{log}{M}_{\mathrm{BH}}﹩ (bottom panels). Type 1 AGNs are shown on the left, with Type 2 AGNs on the right. In the top panels, the contours highlight the levels of constant Ψ values, with log-uniform spacing (see the color bar); the black crosses mark the positions of ﹩[\mathrm{log}({\lambda }_{{\rm{E}}}^{* })﹩, ﹩\mathrm{log}({M}_{\mathrm{BH}}^{* }/{M}_{\odot })];﹩ and the black lines highlight the flux limits at different redshifts. In the middle panels, we show the integrals for ﹩\mathrm{log}{\lambda }_{{\rm{E}}}=-2\pm 0.15﹩ (the dotted pink lines), ﹩\mathrm{log}{\lambda }_{{\rm{E}}}=0\pm 0.15﹩ (the dashed pink lines), and all ﹩\mathrm{log}{\lambda }_{{\rm{E}}}﹩ (the solid pink lines). In the bottom panels, we show the integrals for ﹩\mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })=7\pm 0.15﹩ (the dotted orange lines), ﹩\mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })=8.5\pm 0.15﹩ (the dashed orange lines), and all ﹩\mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })﹩. Each ﹩\mathrm{log}{\lambda }_{{\rm{E}}}﹩ and ﹩\mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })﹩ bin over which a function is marginalized is shown in the top panels in the corresponding color and line style (e.g., the purple dashed lines show the ﹩\mathrm{log}{\lambda }_{{\rm{E}}}﹩ range over which the BHMF is marginalized, and the result of the marginalization is shown with the dashed purple lines in the middle panels). For the purpose of this plot, we assume a constant flux limit of ﹩\mathrm{log}({F}_{14-195\,\mathrm{keV}}/\mathrm{erg}\,{{\rm{s}}}^{-1})=-11.1﹩ (which corresponds to a sky coverage completeness of just 2%–3%; see Figure 3). The lines of the constant flux limits in the top left panel are also lines of constant luminosity, and integrating along these lines produces the local XLF. This figure demonstrates that the bivariate distribution function fully captures the statistical properties of AGNs.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: Distribution functions for all BASS/DR2 AGNs that fall within the criteria specified in Table 1 (586 sources). As in Figure 8, the BHMFs, ERDFs, and reconstructed XLFs are shown in the top, middle, and bottom panels, respectively. We show the intrinsic distributions derived for all AGNs, assuming uncertainties of either σ = 0.3 dex or σ = 0.5 dex in ﹩\mathrm{log}{M}_{\mathrm{BH}}﹩ and ﹩\mathrm{log}{\lambda }_{{\rm{E}}}﹩ (the black solid and green dotted lines), respectively. The orange solid lines show intrinsic functions, derived assuming ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}=0.3﹩ and ﹩{\sigma }_{\mathrm{log}L,\mathrm{scatt}}=0.2﹩ (or ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.36﹩). The black data points in the bottom panel show the direct 1/V max XLF estimates, and the black dashed line is the fit to those points. The solid black lines show the final, bias-corrected intrinsic distribution functions for the complete AGN sample. For comparison, we also show the distribution functions of Type 1 and Type 2 AGNs (the blue and red lines), respectively, from Figure 8.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: Left panel: the fraction of AGNs that lie above ﹩\mathrm{log}{\lambda }_{{\rm{E}}}﹩, according to our model, relative to the total number of SMBHs (from Shankar et al. 2009). Right panel: the fraction of AGNs that lie above ﹩\mathrm{log}{\lambda }_{{\rm{E}}}\gt -2﹩ as a function of mass. We divide our best-fit Type 1 (the blue line and shaded region), Type 2 (the red line and shaded region), and overall (the black line and shaded region) functions by the local total BHMF (including inactive SMBHs) from Shankar et al. (2009). For both panels, for the overall curve (black), the shaded regions illustrate the uncertainty due to errors in our ERDFs and BHMFs, while the black dashed lines also include the uncertainty due to the ranges in the total BHMF, as shown in Figure 7 of Shankar et al. (2009). For the curves for Type 1 and Type 2 AGNs only (blue and red), the shaded regions show the errors in ERDFs and BHMFs only, for ease of comparison between the two types. The total SMBH mass density according to Shankar et al. (2009) is ≈ (3 − 5) × 10−5 M ⊙ h 3 Mpc−3, while the active SMBH mass density according to our analysis is ﹩{3.58}_{-0.23}^{+0.41}\times {10}^{-4}﹩                      M ⊙ h 3 Mpc−3 (i.e., 6%–10% of the total mass density).
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: Comparisons of the BASS BHMFs and ERDFs for Type 1 AGNs (left panels) and Type 2 AGNs (right panels) to previous studies. The blue/red solid lines show the intrinsic BASS BHMFs and ERDFs. Top panels: the BHMFs of Type 1 and Type 2 AGNs. The green triangles show the bias-uncorrected 1/V max results from Greene & Ho (2007, 2009), calculated using a sample of local broad-line AGNs from SDSS. The yellow squares and dashed–dotted lines show the 1/V max and incompleteness-corrected (but not uncertainty-corrected) BHMFs of Schulze & Wisotzki (2010), calculated using local broad-line AGNs from HES. The fully bias-corrected Type 1 BHMF and predicted Type 2 BHMF from Schulze et al. (2015), evaluated at 1 < z < 2, are shown with the purple dashed lines. The 1/V max points from Schulze et al. (2015), constrained using VVDS, SDSS, and zCOSMOS data sets, are also shown using open purple circles, open purple triangles, and open purple squares, respectively. For reference, we also plot the total BHMF (including inactive BHs) from Shankar et al. (2009; the turquoise shaded region). Bottom panels: the ERDFs of Type 1 and Type 2 AGNs. The data points and lines from Schulze & Wisotzki (2010) and Schulze et al. (2015) follow the same scheme as in the top panels.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: Top panel: observed histograms of absorbing column density, ﹩\mathrm{log}{N}_{{\rm{H}}}﹩, for Type 1 (blue lines) and Type 2 (red lines) AGNs, and the overall distribution (black dotted lines). Bottom panel: normalized distributions observed for Type 1 (blue stacked bars) and Type 2 (red stacked bars) AGNs, along with the bias-corrected column density distribution of the BASS 70 month survey sample (Ricci et al. 2015), calculated for two luminosity bins: ﹩\mathrm{log}({L}_{14\mbox{--}195\,\mathrm{kev}}/\mathrm{erg}\,{{\rm{s}}}^{-1})\leqslant 43.7﹩ (black solid lines) and ﹩\mathrm{log}({L}_{14\mbox{--}195\,\mathrm{kev}}/\mathrm{erg}\,{{\rm{s}}}^{-1})\gt 43.7﹩ (black dashed lines). For Type 1 AGNs (blue lines), we assume the intrinsic and observed column densities are the same, as Type 1 AGNs tend to be relatively unobscured, then we calculate the Type 2 distribution (red lines) by subtracting the Type 1 distribution from the overall distribution in each luminosity bin. We use the intrinsic distributions when calculating the BHMF and the ERDF for the sample.
Paper: BASS. XXX. Distribution Functions of DR2 Eddington Ratios, Black Hole Masses, and X-Ray Luminosities
Authors: Tonima Tasnim Ananna, Anna K. Weigel, Benny Trakhtenbrot, Michael J. Koss, C. Megan Urry, Claudio Ricci, Ryan C. Hickox, Ezequiel Treister, Franz E. Bauer, Yoshihiro Ueda, Richard Mushotzky, Federica Ricci, Kyuseok Oh, Julian E. Mejía-Restrepo, Jakob Den Brok, Daniel Stern, Meredith C. Powell, Turgay Caglar, Kohei Ichikawa, O. Ivy Wong, Fiona A. Harrison, Kevin Schawinski
Figure caption: The ERDFs of Type 1 (top panel) and Type 2 (bottom panel) AGNs, divided into two mass bins: log M BH ≤ 7.8 (the purple lines and points) and log M BH ≥ 8.2 (the green lines and points). The data points represent 1/V max in each λ E bin, the dashed lines represent the fits to the 1/V max points, and the solid lines represent the bias-corrected intrinsic distribution functions. Dividing the sample in this way shows that, for both Type 1 and Type 2 AGNs, the shape of the ERDF is independent of mass.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption:  H β and Al III profile parameter comparison as a function of luminosity. Left panel: behavior of FWHM Al III and H β (top) and of the ratio FWHM(Al III)/FWHM(H β) as a function of ﹩\mathrm{log}L﹩ at 1700 Å. The filled line traces the expected increase of the FWHM in a virialized system with ﹩{L}^{\tfrac{1}{4}}﹩. The data points are identified on the basis of ST as in Figure 3. The yellow band marks the region where FWHM(Al III)/FWHM(H β) = 1 within the errors: the median value of the uncertainty of the ratios, ≈ ±25%. Right panels: shifts of H β and Al III (top), and their difference s ⋆ as a function of ﹩\mathrm{log}L﹩(1700) (bottom). The vertical dotted lines join H β and Al III parameters for the same object (e.g., they are not error bars).
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Decimal logarithm of black hole mass in units of solar masses computed from the relation of Vestergaard & Peterson (2006) based on FWHM H β vs. the one computed from the Al III FWHM following Equation (5), with subsamples identified by color according to their STs. The solid line traces Equation (4), while the dotted–dashed line is the equality line. The bottom panel shows the residuals as a function of the M BH derived from H β. Average values of the ﹩\mathrm{log}﹩                       M BH differences, standard deviation, and normalized ﹩{\chi }_{\nu }^{2}﹩ are reported for the joint sample minus one outlier with δ > 1 (top row). The bottom row yields the median and the SIQR.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Decimal logarithm of black hole mass in units of solar masses computed from the relation of Vestergaard & Peterson (2006) based on the H β spectral range vs. the one computed from the C III] data following Equation (7), with STs color coded as in Figure 3. As for Figure 11, the filled line traces Equation (6), while the dotted–dashed line is the equality line. The bottom panel shows residuals as a function of M BH derived from H β. Average, standard deviation, and ﹩{\chi }_{\nu }^{2}﹩ of the log M BH difference are reported on the top row of the inside caption; the bottom row reports median and SIQR.