adsabs/AstroCLIMB huggingface dataset:
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The left panel shows the best-fitting results (solid red line) to emission lines around Hβ (solid dark green line) including the apparent optical Fe II emission features in the Type 1 AGN 0856-52339-0050. Double-dotted–dashed red line shows the determined power-law continuum emissions, the solid green line shows the determined broad Hβ, solid purple lines show the determined optical Fe II lines, the dashed green line shows the determined broad He II line, solid pink lines show the determined core [O III] components, and thick blue solid lines show the determined broad blueshifted [O III] components. The right panel shows the best-fitting results (solid red line) to the emission lines around Hβ (solid dark green line) in the Type 2 AGN 0332-52367-0317, the SDSS spectrum of which is shown in Figure 1 and Figure 2, after subtracting the host-galaxy contributions. The solid green line shows the determined narrow Hβ, and the solid lines in pink and in blue show the determined core and extended components of the [O III] doublet. The calculated χ 2 values for the best-fitting results are marked in the top-left corners of the panels.
Paper: Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: XueGuang Zhang
Figure caption: The top panel shows the correlation between the measured stellar velocity dispersions σ and the SDSS-pipeline-provided σ SDSS for Type 2 AGNs. The solid blue line shows the best-fitting results, and the solid red line shows σ = σ SDSS. The middle and bottom panels show the best-fitting results to the absorption features around 4000 Å using the fitting procedure in the article with σ ∼ 95 km s−1 and the fitting results to the absorption features around 4000 Å with stellar velocity dispersion fixed to the SDSS-pipeline-provided 320 km s−1.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: Distributions of the black hole masses with redshift of our GPQ sample. Yellow circles represent the Hβ-based mass estimates, green triangles represent the Mg II-based mass estimates, and blue diamonds represent the C IV-based mass estimates. Measurement errors derived from the MC errors of spectral fitting are shown as brown error bars. The black hole masses of SDSS DR7Q reported in Shen et al. (2011) are shown as gray dots, and the median black hole masses of DR7Q in 24 redshift bins are shown as black squares.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Phase-folded, phase-aligned, mean-subtracted light curves of the K  s -band (left) and G-band (right) development data sets after all preprocessing steps have been applied. Gray dots show all data; black circles highlight the data for a single RRab star. We note that the vertical structures in the left panel are due to data binning (see text).
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Period–amplitude–metallicity distributions of the VVV K  s -band (left) and Gaia G-band (right) light curves of the RRab stars in our respective development data sets. The metallicity values were estimated from the I-band light curves of the same objects (see text) and are denoted with a color map shown at the right side of the figure.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: Histograms of virial black hole masses (left column) and continuum luminosities (right column) of the SDSS DR7Q sample in Shen et al. (2011) (unfilled bars) and our GPQ sample (filled in blue). The mean values of the DR7Q sample (μ 1) are marked in black dashed lines, while the mean values of our GPQ sample (μ 2) are marked in red dotted lines.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: The spectra of the stellar and galaxy contaminants. For the spectra of stellar contaminants, red dashed lines mark the wavelengths of the Hα (6563 Å), Hβ (4861 Å), and Hγ (4341 Å) emission/absorption lines. For the spectra of galaxies, blue dotted lines mark the central wavelengths of the redshifted Hα emission lines.
Paper: Photometric Metallicity Prediction of Fundamental-mode RR Lyrae Stars in the Gaia Optical and K  s  Infrared Wave Bands by Deep Learning
Authors: István Dékány, Eva K. Grebel
Figure caption: Cumulative distributions of the S/N of the Gaia light curves in the G, bp, and rp wave bands for the Galactic RRab stars in the common sample with the OCVS.
Paper: Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at ∣b∣ < 20°
Authors: Yuming Fu, Xue-Bing Wu, Linhua Jiang, Yanxia Zhang, Zhi-Ying Huo, Y. L. Ai, Qian Yang, Qinchun Ma, Xiaotong Feng, Ravi Joshi, Wei Jeat Hon, Christian Wolf, Jiang-Tao Li, Jun-Jie Jin, Su Yao, Yuxuan Pang, Jian-Guo Wang, Kai-Xing Lu, Chuan-Jun Wang, Jie Zheng, Liang Xu, Xiao-Guang Yu, Bao-Li Lun, Pei Zuo
Figure caption: Photometric redshift from the GPQ candidate catalog in Paper I against the spectral redshift for the identified GPQs. The red dashed line denotes z phot = z spec, and the blue dotted lines mark the margin within one rms error from the red dashed line.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Stellar spectral types and effective temperature distributions of our objects in the different surveys.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Relationship of the EWs of Hα and stellar effective temperature, where the left panel shows LAMOST low-resolution spectra and the right panel shows LAMOST middle-resolution spectra. The red line is the activity judgment line formulated by the standard stars, the stars above this line are active, and the stars below this line are inactive.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: These are two examples of TESS flare search results. The left panels show a standard flare model, and the right panels show a flare search result with eclipse interference and a slight jitter of the light curve.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: These are two examples of Kepler flare search results. The picture on the left is an example of 1-minute data with missing data, and the picture on the right is an example of 30-minute data.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: (a) The relationship between ﹩{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ and Ro. (b) The relationship between the ratio of flare energy to luminosity and Ro. (c) The relationship between the flare amplitude and EWs of Hα. (d) The relationship between the ratio of flare energy to stellar luminosity and EWs of Hα.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Blue circles represent all identified exoplanets, and red and green circles represent the distribution of exoplanets that can be observed by various telescopes. Left panel: LAMOST field; middle panel: TESS field; right panel: Kepler and K2 fields.
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Spectra of the six examples showing the Hα emission line from the LAMOST low-resolution survey. Each panel contains the original spectrum (upper) and the normalized version (lower).
Paper: Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Xianming L. Han, Prabhakar Misra, Gang Meng, Qingfeng Pi, ZiLu Yang, Jiawei Yang
Figure caption: Spectra of four examples showing the Hα emission line from the LAMOST medium-resolution survey. Each panel contains the original spectrum (upper) and the normalized version (lower).
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: Hard X-ray (14−195 keV) attenuation curve for the BAT survey, assuming two torus opening angles: 60° (the solid blue line) and 35° (the dotted blue line). For extremely obscured sources, with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\gt 25﹩, the fraction of observed luminosity relative to the intrinsic luminosity is less than 5%, making them very difficult to detect, even with the high-energy X-ray window of BAT. This is an update to the Ricci et al. (2015) attenuation curve, with a newer torus model (see the text for details).
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: Swift/BAT cumulative number counts (left) and differential number counts (right) from the 70 month survey, with beamed sources, low-flux dual sources, sources close to the Galactic plane, and weak associations removed (672 sources, at z ≤ 0.3; turquoise data points); the same sample with an additional redshift cut applied (z ≥ 0.01, 619 sources; yellow data points); and then with all Table 1 cuts applied (586 sources; red data points). The latter sample is used in our BHMF and ERDF calculations, and, as seen in this figure, it is representative of the redshift-restricted sample. We produce fits to these data using Equation (6), and report the slope and normalization of the fitted line in Section 2.3. To produce the fits, we apply a flux cut at F 14−195, obs > 10−11.1 erg s−1 cm−2 (shown in the left panel with the black dashed line), because the flux–area curve below that flux limit is not well constrained (Section 3 and Figure 3), artificially affecting the slope of the number counts (shown in the top left corner of the cumulative counts).
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: Flux–area curve of the Swift/BAT 70 month all-sky survey. To compute the XLF and gain initial guesses for the BHMF and the ERDF, we use this flux–area curve rather than a constant flux limit. For bright, ultra-hard X-ray sources, ﹩\mathrm{log}({F}_{14-195,\mathrm{obs}}/\mathrm{erg}\,{\mathrm{cm}}^{-2}\,{{\rm{s}}}^{-1})\gt -10.7﹩, the survey is complete over the entire sky. For fainter sources, the completeness decreases as a function of the observed 14−195 keV X-ray flux. This figure converts Figure 10 of the Baumgartner et al. (2013) cumulative flux–area curve from mCrab to erg cm−2 s−1 units.
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: Venn diagrams of all Swift/BAT 70 month sources below z = 0.3, after removing all beamed sources and Galactic-plane sources (∣b∣ < 5°), as well as making more subtle cuts that exclude a total of 181 sources (see the text for details). The diagrams show how the final samples of 366 Type 1 objects and 220 Type 2 objects were selected. All cuts applied to the parent sample are explicitly listed in Table 1. For each of the AGN subsamples, the red circle denotes the set of objects that fall within 0.01 ≤ z ≤ 0.3, the green circle denotes the set that falls within ﹩6.5\leqslant \mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })\leqslant 10.5﹩, and the black circle denotes the set that falls within ﹩-3\leqslant \mathrm{log}{\lambda }_{{\rm{E}}}\leqslant 1﹩. The numbers of sources in all sets and intersections of sets are also noted.
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 2 AGNs for two mock catalogs. For the top three panels (Mock #1), the parameters are fixed at ﹩\mathrm{log}({{\rm{\Phi }}}^{* }/{{h}}^{3}\,{\mathrm{Mpc}}^{-3})=-3.16﹩, ﹩\mathrm{log}({M}_{\mathrm{BH}}^{* }/{M}_{\odot })=8﹩, α = −1.6, β = 0.6, ﹩\mathrm{log}({\xi }^{* }/{{h}}^{3}\,{\mathrm{Mpc}}^{-3})=-4.8﹩, ﹩\mathrm{log}{\lambda }_{{\rm{E}}}^{* }=-1﹩, δ 1 = 0.6, and ﹩{\epsilon }_{{\lambda }_{{\rm{E}}}}=2.5﹩. For the bottom three panels (Mock #2), the parameters are fixed at ﹩\mathrm{log}({{\rm{\Phi }}}^{* }/{{h}}^{3}\,{\mathrm{Mpc}}^{-3})=-3.16﹩, ﹩\mathrm{log}({M}_{\mathrm{BH}}^{* }/{M}_{\odot })=8.2﹩, α = −1.4, β = 0.7, ﹩\mathrm{log}({\xi }^{* }/{{h}}^{3}\,{\mathrm{Mpc}}^{-3})=-4.8﹩, ﹩\mathrm{log}{\lambda }_{{\rm{E}}}^{* }=-1.4﹩, δ 1 = 0.8, and ﹩{\epsilon }_{{\lambda }_{{\rm{E}}}}=2﹩. Each column represents a different dispersion in BH mass and Eddington ratio. From left to right, ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}﹩ and ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}﹩ are increased from 0 to 0.3 to 0.5. For each plot, the green lines show the intrinsic function assumed for the mock catalog, the red data points show the results from 1/V max, the red dashed lines show MCMC fits to these data points, and the red solid lines show our attempts to recover the underlying distributions according to the method outlined in Section 3.4. As in the previous figure, 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 BHMFs, ERDFs, and reconstructed XLFs of the BASS/DR2 AGNs, derived using a luminosity-dependent bolometric correction. The distributions of BH mass, Eddington ratio, and luminosity 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 are calculated using the luminosity-dependent bolometric corrections of Duras et al. (2020). For each type of AGN, 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 shaded areas show the final, bias-corrected intrinsic distribution functions. We illustrate the intrinsic distributions, derived assuming uncertainties of ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}={\sigma }_{{\lambda }_{{\rm{E}}}}0.3﹩ and ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}=0.3,\,{\sigma }_{\mathrm{log}L,\mathrm{scatt}}=0.37﹩ (i.e., ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.47﹩ dex), with the blue solid and dotted lines for Type 1 AGNs, respectively (and the red solid and dotted lines for Type 2 AGNs, respectively). The green dotted lines in the left (right) panels are calculated assuming ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}=0.5,\,{\sigma }_{\mathrm{log}L,\mathrm{scatt}}=0.37﹩ (i.e., ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.62﹩ dex) for Type 1 (Type 2) AGNs. The best-fit distributions of Type 1 AGNs (for the ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}={\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.3﹩ case) are shown also in the right panels, to highlight the differences between Type 1 and Type 2 AGNs. Both panels are also overplotted with constant bolometric correction results (the orange solid line) from the main part of the text (the ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}={\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}=0.3﹩ case) for comparison. The 1/V max values (split by AGN type) 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: Results for Type 1 AGNs for two mock catalogs. For the top three panels (Mock #1), the parameters are fixed at ﹩\mathrm{log}({{\rm{\Phi }}}^{* }/{{h}}^{3}\,{\mathrm{Mpc}}^{-3})=-3.16﹩, ﹩\mathrm{log}({M}_{\mathrm{BH}}^{* }/{M}_{\odot })=8﹩, α = − 1.6, β = 0.6, ﹩\mathrm{log}({\xi }^{* }/{{h}}^{3}\,{\mathrm{Mpc}}^{-3})=-4.8﹩, ﹩\mathrm{log}{\lambda }_{{\rm{E}}}^{* }=-1﹩, δ 1 = 0.6, and ﹩{\epsilon }_{{\lambda }_{{\rm{E}}}}=2.5﹩. For the bottom three panels (Mock #2), the parameters are fixed at ﹩\mathrm{log}({{\rm{\Phi }}}^{* }/{{h}}^{3}\,{\mathrm{Mpc}}^{-3})=-3.16﹩, ﹩\mathrm{log}({M}_{\mathrm{BH}}^{* }/{M}_{\odot })=8.2﹩, α = −1.4, β = 0.7, log ξ = −4.8, log ﹩{\lambda }_{{\rm{E}}}^{\ast }﹩ = −1.4, Δ1 = 0.8, and ﹩{\epsilon }_{{\lambda }_{{\rm{E}}}}=2.0﹩. Each column represents a different dispersion in BH mass and Eddington ratio. From left to right, ﹩{\sigma }_{\mathrm{log}{M}_{\mathrm{BH}}}﹩ and ﹩{\sigma }_{\mathrm{log}{\lambda }_{{\rm{E}}}}﹩ are increased from 0 to 0.3 to 0.5. For each plot, the green lines show the intrinsic function assumed for the mock catalog, the blue data points show the results from 1/V max, the blue dashed lines show the MCMC fits to these data points, and the blue solid lines show our attempts to recover the underlying distributions according to the method outlined in Section 3.4. 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 impact on our analysis due to the lowest-luminosity and lowest-redshift object within our redshift-restricted sample (NGC 5283, or BAT ID 684). The green points show the 1/V max measurements excluding this single source, as is the case throughout our main analysis, while the red point shows how these change when the source is included in the sample (affecting only one bin in luminosity, M BH, and λ E). This object falls at the flux threshold of the overall survey (according to the curve shown in Figure 4), but given the variation in the sky sensitivity (i.e., flux–area relation) across the surveyed area, the corresponding 1/V max value is likely to be inaccurate. The different lines demonstrate that—unlike some of the fits to 1/V max measurements—the intrinsic distribution functions are robust to the choice of including or excluding this single source; for all three distribution functions, the solid lines of the two cases (almost) completely overlap, while the dashed lines do not. We provide all 1/V max measurements, both with and without this single source, in Tables F2–F4.