adsabs/AstroCLIMB huggingface dataset:
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: Demonstration of pre-processing and demodulation of a single detector’s data over a 150 s window. Top: the raw data calibrated into power units (black) and processed data with the MCE readout Butterworth filtering (blue) and detector time constant (orange) deconvolved. The inset plot zooms into a shorter ∼0.45 s window (in red) to see the impact over a few VPM modulation cycles. The dominant 10 Hz component is due to the VSS. Middle: the deconvolved data were further bandpass filtered around the modulation harmonics lines (black). The VPM transfer functions M  u/v  are shown as green and purple dashed lines, with the amplitudes set to the best-fit values from the data segment, i.e., the demodulated u/v amplitudes. Here the calibration factor ΔT CMB/ΔD  i  defined in Equation (6) is divided out to keep the demodulated data in power units. Bottom: demodulated u/v time streams. The corresponding range to the zoomed-in region is marked in red. The azimuth angle scanned over during this time period is marked on the top axis. The flatness of the demodulated curves indicates the stability of the polarization measurement.
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: The CLASS Sun-centered linear polarization maps and the Sun avoidance cut. The maps are made by coadding all +45° oriented detectors (top row) and all detectors (bottom row) in each era in the telescope boresight coordinates (independent of the boresight rotation) and are presented under orthographic projection. Some diffuse features around the compact structure and with an opposite sign in amplitude are artifacts due to the baseline adjustment in the mapmaking. The location of the lobe on the right in Era 2 corresponds to the location of the opening in the cage of the 90 GHz telescope. The features in Sun-centered maps resemble temperature-to-polarization (T-to-P) leakage that has a canceling effect between +45° and −45° oriented detectors. When all detectors are combined, the residual effect is subdominant to the noise. The inner black circles show the commanded 20° Sun avoidance during the survey; the outer black circles/wedges are the extended boundaries for data flagging based on the relative position of the Sun with respect to the telescope boresight (60° for Era 1 and 40°–60° for Era 2) when the Sun is above the horizon. The position of the horizon changes with the boresight rotation in the telescope boresight coordinates, making regions below the dashed line also accessible from certain boresight angles.
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: The wind-induced signal across the focal plane when the plastic closeout was on and the forebaffle extension was blackened. Each panel shows the demodulated linear polarization signal u binned in the wind bearing angle and wind speed coordinates for the −45° oriented detector in each feedhorn; the other detector in the pair shows a similar signal. As indicated by the legend, the azimuth angle of the polar plots corresponds to the wind bearing angle, and the radial axis marks the wind speed in units of meters per second. The panels are laid out by the detector pointing offsets, similar to Figure 7, with the detectors pointing at higher elevations at the top. Within each panel, the wind-related systematics are mostly confined in the quadrant when the telescope is facing toward the wind. The signal amplitude varies across the focal plane with a quadrupole pattern that increases from the center toward the edge of the focal plane and also rises with the wind speed. The whirlpool-shaped structure in some of the edge detectors is due to the ground pickup (Section 4.1.3)
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: Schematic of the CLASS 40 GHz Telescope. The telescope sits atop the three-axis telescope mount in an enclosed cage structure. Lower-side cage panels are not shown at left to reveal the telescope. Light enters the enclosure by the forebaffle extension, first encountering the VPM, then the primary (obscured) and secondary mirrors, and finally the receiver. The enclosed multireflection design limits spurious signals from stray light. In 2018, the enclosure and forebaffle extension were extended to accommodate the 90 GHz telescope on the same mount.
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: CLASS survey footprint in equatorial coordinates. CLASS observes the sky with large constant-elevation circular scans, illustrated by the black curve that traces the path of the telescope boresight through one 720° sweep. The thickness of the curve in R.A. (separable into two lines upon zooming in) indicates the degree of sky rotation during a sweep. Over a 24 hr period, the sweeps cover the annular survey region shown between the dark blue lines, extending from decl. +30° in the north to −76° in the south. The background image shows the intensity of the Planck component-separated synchrotron map (Planck Collaboration et al. 2020c). Survey footprints from a sampling of other projects are superposed (Ruud et al. 2015; Kusaka et al. 2018; Aiola et al. 2020; Dutcher et al. 2021; BICEP/Keck Collaboration et al. 2022; Spider Collaboration et al. 2022; Rubiño-Martín et al. 2023).
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: Schematic of the CLASS data reduction pipeline. Key processing steps, data products, and ancillary input data are labeled as blue boxes, green pills, and orange ellipses, respectively.
Paper: A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B
Authors: Ketan R. Sand, Daniela Breitman, Daniele Michilli, Victoria M. Kaspi, Pragya Chawla, Emmanuel Fonseca, Ryan Mckinven, Kenzie Nimmo, Ziggy Pleunis, Kaitlyn Shin, Bridget C. Andersen, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Alice P. Curtin, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Jane Kaczmarek, Adam Lanman, Calvin Leung, Kiyoshi W. Masui, Mubdi Rahman, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Masoud Rafiei-Ravandi, Paul Scholz, Vishwangi Shah, Kendrick Smith, Ingrid Stairs, David C. Stenning
Figure caption: Figure showing bursts detected by the baseband system from FRB 20180916B dedispersed at their structure-maximizing DM. In each subfigure, the top panel shows the time series, with red line showing the best fit, the panel below it shows the dynamic spectra, and finally to the right of it is the frequency distribution of the power. The white-dotted lines show the extent of bandwidth. In the top right, we see the DM that it has been dedispersed to and the time resolutions to which it has been plotted in microseconds, and the top left shows the burst number. The number of channels here is 128. Intensity data waterfalls of bursts B1–B15 and B16–B21 have already been published in CHIME/FRB Collaboration et al. (2020b) and Pleunis et al. (2021), respectively.
Paper: A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B
Authors: Ketan R. Sand, Daniela Breitman, Daniele Michilli, Victoria M. Kaspi, Pragya Chawla, Emmanuel Fonseca, Ryan Mckinven, Kenzie Nimmo, Ziggy Pleunis, Kaitlyn Shin, Bridget C. Andersen, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Alice P. Curtin, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Jane Kaczmarek, Adam Lanman, Calvin Leung, Kiyoshi W. Masui, Mubdi Rahman, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Masoud Rafiei-Ravandi, Paul Scholz, Vishwangi Shah, Kendrick Smith, Ingrid Stairs, David C. Stenning
Figure caption: Microstructure analysis of B20 from FRB 20180916B. The top panel shows the burst profile, with the burst number, resolution at which it was extracted and the DM indicated in the top right. The bottom panel shows the temporal ACF (black), Lorentzian fit to the ACF (green dashed), the residual (blue), and ACF of the noise (red). We find a weak peak in the ACF with width of ∼50 μs but cannot constrain the true nature of this structure with the present data set. See Section 3.6 for details.
Paper: A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B
Authors: Ketan R. Sand, Daniela Breitman, Daniele Michilli, Victoria M. Kaspi, Pragya Chawla, Emmanuel Fonseca, Ryan Mckinven, Kenzie Nimmo, Ziggy Pleunis, Kaitlyn Shin, Bridget C. Andersen, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Alice P. Curtin, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Jane Kaczmarek, Adam Lanman, Calvin Leung, Kiyoshi W. Masui, Mubdi Rahman, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Masoud Rafiei-Ravandi, Paul Scholz, Vishwangi Shah, Kendrick Smith, Ingrid Stairs, David C. Stenning
Figure caption: Waterfall figure similar to Figure 8 showing bursts detected from FRB 20180916B only with intensity data from 2020 September 20 until 2021 December 31. All of these bursts are shown at a resolution of 0.983 ms and 128 channels.
Paper: A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B
Authors: Ketan R. Sand, Daniela Breitman, Daniele Michilli, Victoria M. Kaspi, Pragya Chawla, Emmanuel Fonseca, Ryan Mckinven, Kenzie Nimmo, Ziggy Pleunis, Kaitlyn Shin, Bridget C. Andersen, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Alice P. Curtin, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Jane Kaczmarek, Adam Lanman, Calvin Leung, Kiyoshi W. Masui, Mubdi Rahman, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Masoud Rafiei-Ravandi, Paul Scholz, Vishwangi Shah, Kendrick Smith, Ingrid Stairs, David C. Stenning
Figure caption: Continued from Figure 8.
Paper: A Theoretical Approach to the Complex Chemical Evolution of Phosphorus in the Interstellar Medium
Authors: Marina Fernández-Ruz, Izaskun Jiménez-Serra, Jacobo Aguirre
Figure caption: Dependence of the formation of PO, PN and their ratio with the reaction rate coefficients k  i  of the 14 chemical reactions of the system. We plot the Pearson correlation r of the abundance of PO (blue bars), PN (red bars), and their ratio (green bars) with all 14 reaction rate coefficients for (a) T = 10 K, (b) T = 100 K, and (c) T = 300 K, considering times t = 103 (light colors), t = 104 (vivid colors), and t = 105 yr (dark colors). Correlations ∣r∣ > 0.05 are supported by p-values <0.01. The correlations were calculated with sets consisting of all the combinations of three values of each of the 14 k  i  (bars), and also for a finer grid composed of 11 values of each of the five most influential k  i  (black diamonds). In all cases k  i  ranges from k  i /10–10k i , being the values logarithmically distributed, and P-hydrogenation fraction f P = 0.5.
Paper: A Theoretical Approach to the Complex Chemical Evolution of Phosphorus in the Interstellar Medium
Authors: Marina Fernández-Ruz, Izaskun Jiménez-Serra, Jacobo Aguirre
Figure caption: Evolution of the abundances relative to H of the P-bearing molecules (a)–(c) and the ratio [PO]/[PN] (d)–(f) for T = 10, 100, and 300 K, respectively. P-hydrogenation fraction f P = 0.5 (i.e., 50% of initial P locked into atomic P and 50% equally distributed between PH, PH2, and PH3) in all cases. The results were obtained by solving the total model numerically (blue lines) and through the theoretical solution of the minimal system (dashed red lines). Note that the numerical and theoretical approaches yield identical results to the naked eye for all species, times, and temperatures. A dashed vertical line remarks the typical cloud age, t = 104–105 yr, and a dashed horizontal line is marked at [PO]/[PN] = 1 in (d)–(f). For comparison, the curve of [PO]/[PN] obtained from UCLCHEM chemical code (Holdship et al. 2017) has been plotted in (d)–(f) (dashed–dotted green lines).
Paper: A Theoretical Approach to the Complex Chemical Evolution of Phosphorus in the Interstellar Medium
Authors: Marina Fernández-Ruz, Izaskun Jiménez-Serra, Jacobo Aguirre
Figure caption: Complex networks associated with the set of reactions selected from the chemistry of phosphorus in the ISM for our model. (a) Chemical network representing the 17 species and 14 chemical reactions analyzed in this work. Nodes represent chemical species involved in the system, and are classified as follows: abundant (blue nodes), scarce (green), and noninteracting (white) according to the criterion explained in the text. Directed links (arrows) go from the reactants to the products of a reaction and undirected links (dashed lines) connect the reactants of a reaction. (b) Subnetwork of the total network plotted in (a) that sketches the theoretically solved system. We have included the indices i used in Equations (3) and (4) to number the P-bearing species in the minimal system.
Paper: A Theoretical Approach to the Complex Chemical Evolution of Phosphorus in the Interstellar Medium
Authors: Marina Fernández-Ruz, Izaskun Jiménez-Serra, Jacobo Aguirre
Figure caption: Evolution of the abundance of PO, PN and their ratio [PO]/[PN] for (a) T = 10 K, (b) T = 100 K, and (c) T = 300 K and for different values of the P-hydrogenation fraction f P, the fraction of P that has been transformed into PH, PH2, and PH3 via grain-surface reactions before being released to the gas phase.
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption: Illustration of analysis for the multiepoch spectra of SDSS J102530.44+462808.6. Left panels: modeling and removal of the continuum by a linear combination of the first seven eigenspectra that are extracted from the standard single stellar population spectral library developed by Bruzual & Charlot (2003). In each panel, the top blue curve shows the continuum-removed emission-line spectrum. The heavy black curve underneath shows the observed rest-frame spectrum, overplotted by the best-fit continuum indicated by the red curve. Middle panels: an illustration of the line-profile modeling with a linear combination of a set of Gaussian functions for the Hβ region. In each panel, the modeled continuum has already been removed from the originally observed spectrum. The observed and modeled line profiles are plotted with black and red solid lines, respectively. Each Gaussian function used is shown with a dashed line. The subpanel below the line spectrum presents the residuals between the observed and modeled profiles. Right panels: same as the middle panels, but for the Hα region.
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption: Distributions of the CL-AGNs on the diagrams of L bol–M BH (left panels) and L bol–L bol/L Edd (right panels), after combining the nine new “partially obscured” CL-AGNs (denoted by the solid circles) identified in this study and the 26 previously identified CL-AGNs (denoted by the open squares) complied by Wang et al. (2019). The “turn-on” and “turn-off” states are displayed in the upper and lower rows, respectively. The underlying comparison samples are described as follows. Red crosses: quasars with z < 0.5 taken from the value-added SDSS DR7 quasar catalog (Shen et al. 2011); green crosses: the SDSS DR3 NLS1 catalog established by Zhou et al. (2006); magenta crosses: the SDSS DR7 intermediate-type AGNs studied by Wang (2015). The Swift/BAT AGN sample of Winter et al. (2012) is shown by the cyan, yellow, and blue crosses for Seyfert 1, 1.2, and 1.5 galaxies, respectively.
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption:  L bol/L Edd plotted as a function of stellar population age index D n(4000). The nine “partially obscured” CL-AGNs identified by us are shown by the solid and open blue circles for the “turn-off” and “turn-on” states, respectively. The other CL-AGNs (at “turn-on” state) compiled by Liu et al. (2021, and references therein) and identified by López-Navas et al. (2022) are displayed by the open stars in magenta and green, respectively. The small red and cyan open squares are the local “partially obscured” Seyfert galaxies and composite galaxies studied by Wang (2015), respectively. The dashed line is the best-fit nonlinear relationship to these “partially obscured” AGNs.
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption: Swift/XRT X-ray spectra of SDSS J124610.75+275615.9 (upper panel) and SDSS J151652.48+395413.4 (lower panel), both taken on 2023-05-03. The best-fit spectral models expressed as wabs ∗ zwabs ∗ powerlaw with a fixed power-law photon index of 2 are overplotted as the red solid lines. The subpanel below each spectrum shows the deviations, in units of counts s−1 keV−1 , of the observed data from the best-fit model.
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption: A comparison of the line-profile modeling in the Hα region of SDSS J151652.48+295413.4. The spectra obtained by SDSS, Shane 3 m, and Keck II 10 m telescopes at different epochs are displayed from left to right. In the modeling of the Keck spectrum, the narrow Hα emission line is produced from the profile of the adjacent [N II] λ6583 emission line by a fixed line flux ratio of 0.9 determined from the SDSS spectrum, because the narrow Hα emission line falls in the 12 Å chip gap that is ignored in our modeling. Symbols are the same as in Figure 2.
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption: A comparison of the distributions of the D n(4000) index. The distribution of the nine “partially obscured” CL-AGNs is denoted by the red solid line. The blue dashed and blue solid lines show the distributions of the 59 “partially obscured” CL-AGN candidates that are selected according to their variability in the MIR band and the distribution of the total 170 intermediate-type AGNs from which the candidates are selected.
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption:  D n(4000)–Hδ A plane for local CL-AGNs (see the main text for details of the samples). The underlying density contours (dashed black heavy lines) show the distribution of ∼80,000 Seyfert 2 galaxies extracted from the MPA/JHU value-added catalog (e.g., Kauffmann et al. 2003; Heckman & Kauffmann 2006). The solid line marks the stellar population evolution locus of the single stellar population model with solar metallicity, and the dotted–dashed line the model with exponentially decreasing star formation rate ψ(t) ∝ e −(t/4 Gyr).
Paper: Are “Changing-look” Active Galactic Nuclei Special in the Coevolution of Supermassive Black Holes and Their Hosts? I.
Authors: J. Wang, W. K. Zheng, T. G. Brink, D. W. Xu, A. V. Filippenko, C. Gao, C. H. Xie, J. Y. Wei
Figure caption: A comparison of the multiepoch rest-frame spectra of the eight newly identified CL-AGNs. In each panel, the Shane and SDSS DR16 spectra are denoted by the red and blue lines, respectively. The bottom black lines are the differential spectrum, when the SDSS DR16 spectrum is used as a reference. Before the subtraction, the two spectra are matched in the instrumental resolution, and then scaled according to their [O III] λ5007 line fluxes. The spectra are shifted vertically for clarity.