adsabs/AstroCLIMB huggingface dataset:
Paper: Preferential Accretion onto the Secondary Black Hole Strengthens Gravitational-wave Signals
Authors: Julia M. Comerford, Joseph Simon
Figure caption: The relationship between the final binary SMBH mass ratio (q•,f, the mass ratio at ∼milliparsec separations) and the initial SMBH mass ratio (q•,i, the mass ratio at kiloparsec-scale separations) for different models of accretion. Here, q•,i is derived from the mass ratio of the galaxy pair. For no accretion (solid black line), the SMBH mass ratio does not evolve. However, models of preferential accretion onto the secondary SMBH drive q•,f higher, as shown for observationally based estimates of 10% (blue solid line) and 20% (orange solid line) cumulative growth of the total SMBH mass M•,tot. The dotted line shows q•,f = 0.25, which denotes the cutoff between minor SMBH mergers (below the dotted line) and major SMBH mergers (above the dotted line). We highlight that the differential accretion models bring many SMBH binaries from what would be considered a minor SMBH merger event (0.1 ≤ q• < 0.25) into the classification for a major SMBH merger event (0.25 ≤ q• ≤ 1).
Paper: Utilizing Maximum Variability to Discern TDE Emission from AGN Flares
Authors: Samaresh Mondal, K. Decker French
Figure caption: The nearest-neighbor distance distribution obtained by comparing the XMM-Newton (top panel) and Swift-XRT (bottom panel) sources with the MILLIQUAS catalog. The histograms show a bimodal distribution, which is modeled with two Gaussians. We use these fits to obtain the maximum distance used for cross-matching the X-ray sources with the AGN sample. The black dashed line shows the 3σ distance from the mean of the nearest Gaussian.
Paper: GX 340+0: In and Out of Focus
Authors: S. Li, R. M. Ludlam, D. J. K. Buisson, M. Sudha, S. Rossland, G. Mastroserio, M. C. Brumback, J. A. García, B. W. Grefenstette, F. La Monaca, E. A. Saavedra, A. Di Marco
Figure caption: Corner plot for F02A_UN. Gray dashed line is the 90% confident level. The disk ionization parameter is not degenerate with the reflection fraction, and thus the correlation we see between ionization and reflection fraction is likely due to a physical correlation between the two parameters in the system.
Paper: Utilizing Maximum Variability to Discern TDE Emission from AGN Flares
Authors: Samaresh Mondal, K. Decker French
Figure caption: The illustration of MaxVar from an artificial light curve that consists of six measurements.
Paper: Spectrotemporal Analysis of X-Ray Reverberation in the Seyfert 1.5 Galaxy 4U 1344–60
Authors: Adam G. Gonzalez, Luigi C. Gallo, Adam Ingram, Yerong Xu, Margaret Z. Buhariwalla
Figure caption: Top: lag–frequency spectra for the Suzaku (red) and NuSTAR (blue) power-law (7.2–11 keV) vs. Fe-band (4.8–7.2 keV) light curves. A positive/negative lag indicates that power-law variations lag/lead Fe-band variations. The spectra are binned to contain six points in each bin, except for the first bin, which bins frequencies ﹩\nu \in \left[1/{t}_{\rm{max}\,},3/{t}_{\,\rm{max}}\right)﹩ and therefore only contains two points. The vertical gray shaded region highlights the reverberation frequency range ﹩{\nu }_{\,\rm{rev}\,}\in \left[2.0,5.6\right]\times 1{0}^{-5}\,\,\rm{Hz}\,﹩. Black dotted curves mark the phase-wrapping effect (i.e., τ = ±1/2ν). Bottom: lag–energy spectra for Suzaku (red) and NuSTAR (blue) in the reverberation frequency range ﹩{\nu }_{\,\rm{rev}\,}\in \left[2.0,5.6\right]\times 1{0}^{-5}\,\,\rm{Hz}\,﹩. The vertical black dotted line denotes the source-frame Fe Kα line at 6.4 keV.
Paper: Signatures of Black Hole Seeding on the M•–σ Relation: Predictions from the BRAHMA Simulations
Authors: Jonathan Kho, Aklant Kumar Bhowmick, Paul Torrey, Alex M. Garcia, Niusha Ahvazi, Laura Blecha, Mark Vogelsberger
Figure caption: Approximated trends of the LHS (blue) and RHS (red) of Equation (2) as a function of redshift for σ = 101.5, 101.75, and 102 km s−1. Even with the various approximations we made, the trends clearly follow the same redshift evolution, and show that a combination of the slope of the M•–M* relation, the stellar mass at constant σ redshift evolution, and the explicit BH mass redshift dependence does a good job at explaining the redshift evolution in the M•–σ relation.
Paper: Spectrotemporal Analysis of X-Ray Reverberation in the Seyfert 1.5 Galaxy 4U 1344–60
Authors: Adam G. Gonzalez, Luigi C. Gallo, Adam Ingram, Yerong Xu, Margaret Z. Buhariwalla
Figure caption: Median (solid black curves) and 68% range (filled gray regions) for 1000 posterior samples of the spectral model for the 2011 epoch (left), which have been overlaid onto the 2016 epoch (right). The data (colored points) are shown in the top panel of each column, with ratio residuals against the model shown in the bottom panel of each column. The data are rebinned for visual clarity.
Paper: Spectrotemporal Analysis of X-Ray Reverberation in the Seyfert 1.5 Galaxy 4U 1344–60
Authors: Adam G. Gonzalez, Luigi C. Gallo, Adam Ingram, Yerong Xu, Margaret Z. Buhariwalla
Figure caption: Median (dashed gray/solid black curves) and 68% range (hatched/filled gray regions) for 1000 posterior samples of the joint/free h and ﹩1/{ \mathcal B }﹩ spectral model for the 2016 epoch flux (left) and lag (right) spectra. The data (colored points) are shown in the top panel of each column, with residuals in terms of nσ for the joint/free h and ﹩1/{ \mathcal B }﹩ model shown in the middle/bottom panel of each column. The flux data are rebinned for visual clarity.
Paper: Signatures of Black Hole Seeding on the M•–σ Relation: Predictions from the BRAHMA Simulations
Authors: Jonathan Kho, Aklant Kumar Bhowmick, Paul Torrey, Alex M. Garcia, Niusha Ahvazi, Laura Blecha, Mark Vogelsberger
Figure caption: Redshift evolution in the scatter (shown using the IQR) of the M•–σ relation for subhalos of fixed σ. Error bars again represent 95% confidence intervals calculated via bootstrapping. With increasingly more restrictive seed models, the scatter and the variation in the scatter across all redshifts tend to increase for σ = 102 km s−1, while the scatter remains very small at σ = 101.5 km s−1for the more restrictive seed models.
Paper: Signatures of Black Hole Seeding on the M•–σ Relation: Predictions from the BRAHMA Simulations
Authors: Jonathan Kho, Aklant Kumar Bhowmick, Paul Torrey, Alex M. Garcia, Niusha Ahvazi, Laura Blecha, Mark Vogelsberger
Figure caption: Redshift evolution of the HMR of subhalos in the BI (most lenient model) for fixed stellar masses. The redshift evolution seen in the other three BRAHMA boxes is identical to that seen here, and so they are omitted to avoid redundancy. There is a strong increase in the size of subhalos with decreasing redshift, which explains the redshift evolution seen in Figure 6(a).
Paper: Spectrotemporal Analysis of X-Ray Reverberation in the Seyfert 1.5 Galaxy 4U 1344–60
Authors: Adam G. Gonzalez, Luigi C. Gallo, Adam Ingram, Yerong Xu, Margaret Z. Buhariwalla
Figure caption: Posterior distributions of the BH mass for the constant ξ and ne (purple) and radial profiles in ξ and ne (orange) scenarios with both h and ﹩1/{ \mathcal B }﹩ free. Color-coded data points indicate the posterior modes and 68% highest-density intervals. Vertical black dashed lines indicate the various BH mass estimates in the literature.
Paper: Spectrotemporal Analysis of X-Ray Reverberation in the Seyfert 1.5 Galaxy 4U 1344–60
Authors: Adam G. Gonzalez, Luigi C. Gallo, Adam Ingram, Yerong Xu, Margaret Z. Buhariwalla
Figure caption: The 2011 Suzaku XIS 0+3 1–10 keV (left) and 2016 NuSTAR FPM A+B 3.4–50 keV (right) light curves binned by 400 s.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Left panel: a view of the entire coronagraphic F300M field of the HD 141569 system. The two unocculted M-star companions are located to the upper left. The color map has been chosen to highlight the coronagraphic PSF and as a result the M-star PSF cores visually appear saturated. In reality, the detector has not been saturated by the M-stars. Center panel: a zoom in on the central regions of HD 141569A, shown with a log image normalization. Right panel: a zoom in on the central regions of the PSF reference star.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Mock analysis for the key physical parameters used in this study. The x-axis shows the values recovered with the mock fluxes, while the y-axis displays the values obtained from the observed SEDs. Each point is colored by the reduced χ2 value of the observed fit. The black diagonal line indicates the 1:1 relation, the red line shows the best linear fit, and the dashed lines show the 3σ range.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Comparison of physical properties of dual AGN measured using one vs. two AGN components. Each point represents the difference between the values obtained with two AGN components and those derived from a single-component model. For AGN luminosities in the two-component model, the total value corresponds to the sum of both luminosities.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: AGN intrinsic disk luminosity as a function of the merger stage. Each box is colored by the difference between the median AGN intrinsic disk luminosity and the median AGN observed disk luminosity. Symbols are the same as those defined in Figure 10.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Fraction of the AGN luminosity in the IR band as a function of the merger stage, along with the cumulative distribution function (CDF) for each stage. Symbols are the same as those defined in Figure 10.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Best-fit SED for BAT ID 841 using a one-AGN model (left) and a two-AGN model (right). The two-AGN model provides a better fit while preserving the same host galaxy parameters.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Left and center panels: the final PSF-subtracted images for both filters. No point sources were detected. Subtracting off the M-star and disk models leaves significant residuals that affect the contrast floor. Right panel: the mass sensitivity of our observations, as measured from the data and simulated with pyNRC.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: The same as in Figure 6, but for reconvolution of the deconvolved images following the procedure outlined in Appendix B. Gray contours in the right column indicate ±3σ thresholds for the residuals. To approximate the noise level for this purpose, we adopt the propagated pixel-wise uncertainties from the ERR FITS extensions. As these estimates neglect residual speckle noise, they should be assumed to underestimate the noise where speckle residuals are nonnegligible (at very small separations and near the M dwarfs). The residual maps used for the contours were convolved with an FWHM-diameter tophat filter, which serves to mitigate the appearance of the single-pixel deviations expected from Gaussian noise but does not qualitatively alter the result.
Paper: Statistical Overview of Long-lived Active Regions Observed across Multiple Carrington Rotations
Authors: Emily I. Mason, Kara L. Kniezewski
Figure caption: (a) Histogram comparing LLAR and non-LLAR magnetic flux by year and percent of the median AR flux (calculated over all ARs) in the years 2011–2019. (b) Analogous plot but for area as a percent of the overall median AR size (calculated over all ARs). (c) Scatter plot showing the relationship between AR area and total unsigned flux for both LLARs and non-LLARs and linear fits to both categories (the x-axis is log-scaled). The r-squared values for the LLAR and non-LLAR fits are about 0.91 and 0.78, respectively. Note: the number of overlapping points in the 10%–100% range is very high; this plot is not in contradiction to the distributions seen in (b).
Paper: Statistical Overview of Long-lived Active Regions Observed across Multiple Carrington Rotations
Authors: Emily I. Mason, Kara L. Kniezewski
Figure caption: Example of the methodology used to identify LLARs. (a) An LLAR’s initial NOAA AR designation, as displayed with Helioviewer with AR labels plotted from HEK. The LLAR is highlighted with a cyan box. (b) The same AR, highlighted with a magenta box, as confirmed through visual inspection in the CHMAP annual Carrington map movie. (c) One Carrington rotation later in the CHMAP movie, the LLAR still appears at the same location. (d) Identification of the new NOAA AR designation for the LLAR.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Comparison of F300M and F360M residuals after the flux fitting procedure. The residuals have been divided by the local noise to show the signal-to-noise ratios. The fitting was carried out simultaneously on the individual roll data without being derotated and roll-combined. Only one roll angle is shown here, but the results are similar for both rolls.
Paper: Statistical Overview of Long-lived Active Regions Observed across Multiple Carrington Rotations
Authors: Emily I. Mason, Kara L. Kniezewski
Figure caption: (a) Plot of the annual sunspot number and the number of LLARs detected in each year from 2011 to 2019. (b) Median latitudinal distribution of LLARs and non-LLARs in each year over the same period.
Paper: Statistical Overview of Long-lived Active Regions Observed across Multiple Carrington Rotations
Authors: Emily I. Mason, Kara L. Kniezewski
Figure caption: (a) Distribution of magnetic complexity, as measured by Mt. Wilson class at disk-center passage, across LLARs and non-LLARs. (b) The same plot but for the maximum Mt. Wilson class recorded during frontside passage.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Corner plots from the flux fitting procedure for the F300M (left panel) and F360M (right panel) filters.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: The fraction of X-ray weak sources (by a factor of ∼3.3 compared to typical quasars with similar UV luminosity) as a function of EW(C IV), represented by the green points with error bars. The three segments of dark blue polyline represent the best-fit linear relation in each region. The vertical blue lines and lighter shaded areas represent the location of the breakpoints between the three segments and their error bars.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: Comparing the median composite spectra of our WLQ sample, normal quasar sample, and that from D. E. Vanden Berk et al. (2001), all normalized at 2500 Å, which are represented by the red, blue, and black lines, respectively, in the upper panel. Major emission lines are marked with vertical dotted lines. The dashed red, blue, and black lines illustrate the best-fit continua corresponding to each median composite spectrum. In the lower panels, we display five emission lines or complexes for WLQs and normal quasars after continuum subtraction, focusing on Lyα, Si IV, C IV, C III], and Mg II, with one panel for each line (complex). The composite spectrum from D. E. Vanden Berk et al. (2001) is excluded from comparison in the lower panels due to its lower redshift and higher luminosity on average, which differ significantly from our WLQ and normal quasar samples.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: Comparing the EW distribution of a variety of emission lines for WLQs and normal quasars. The red, blue, and gray histograms in each panel represent the EW distributions of WLQs, normal quasars, and the full quasar population, respectively. The red, blue, and gray vertical lines correspond to the median EW values of WLQs, normal quasars, and the full quasar sample, obtained by fitting their respective distributions using log-normal models. In the upper left corner of each panel, we report σNQ, σWLQ, and Δσ for each emission line, with Δσ representing the difference between the σ values of normal quasars and WLQs. The attenuation factor (Δσ) serves as a measure of how much weaker the emission lines of WLQs are compared to those of normal quasars.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: The relationship between emission line attenuation factor (depicted by Δσ) and the ionization energy of the corresponding ion (retrieved from D. E. Vanden Berk et al. 2001). Lyα λ1216 and N V λ1240 are represented by blue crosses, C IV λ1549 is represented by a red cross, while other emission lines are represented by red triangles. The correlation coefficient ρ and p-value are given in the lower right. Note that Lyα λ1216 and N V λ1240 are excluded when calculating the correlation coefficient.