adsabs/AstroCLIMB huggingface dataset:
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: Detector NEP vs. optical loading. The dark green (light blue) data points and left axis give the measured NEP as a function of loading for the updated (original) detectors. The original detectors comprise only the three best modules saved for the upgraded array (Figure 1(a)). Similarly colored histograms and the right axis show the fraction of data, binned in Pγ, contributing to each data point. Fit to these data, the solid green (blue dashed) line shows the model NEP given in Equation (8) for the updated (original) detectors fit to these data. The black data point at Pγ = 0 is NEPdark of the updated detectors from in-lab measurements. Despite having a higher Pγ, the new detectors have similar NEP to the originals due to their lower NEPdark.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: The 90 GHz TES bolometer. (Main image) The TES was revised to include (1) an Nb-PdAu stepped-impedance termination, (2) a single Pd film for thermal mass, (3) a direct normal metal contact between the MoAu TES and the Pd, and (4) a revised bias-lead filter circuit implementation extending RF chokes onto the bias-lead legs. This image was reproduced from N23. (Top-right inset) The original TES used a left-right symmetric, distributed quarter-wave backshort termination with PdAu absorber. This image was reproduced from S. Dahal et al. (2018).
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: I–V curves (a) for the upgraded detectors on module 2 show a broad range of bias voltages (shaded region 100–250 nV) for which nearly all detectors are on the hyperbola-shaped superconducting transition region. The coloring of the curves is only for visual discrimination; it does not correspond to any physical quantity. The inset plot I–V curves from the original detectors on module W33 require a higher bias target (red shaded region). To maintain all detectors biased above the unstable superconducting I–V endpoint, a larger proportion of the original detectors must operate near their normal resistance, leading to a reduction in the overall array sensitivity. Figure (b) shows the minimum percent RN below which the detectors become unlocked, in an unstable superconducting state. We find that 94% of upgraded detectors are stable down to 15% of their normal resistance. The upgraded detectors allow for a much lower minimum percent RN, increasing the stability of the detectors and widening the biasing window.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: Telescope optical efficiencies for the 353 detectors in the upgraded array with optical efficiencies above 5%. The upgraded detectors provide higher optical efficiency compared to their original counterparts in the upgraded array. (The originals, not included here, that were replaced by the upgraded detectors had poorer performance than those that were retained.) Of the 16 upgraded detectors with optical efficiencies below 0.4, 11 come from wafer 1, which had fabrication issues that were improved for wafers 2–4.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: Optical efficiency comparison between paired detectors within a pixel for the original and upgraded focal planes. The optical efficiencies for the  +45° and  −45° detectors, as labeled in Figure 1(c), are denoted η+ and η−. Each subplot represents a wafer on the focal plane. The subplots with blue edges correspond to the four upgraded wafers of the fielded focal plane shown in Figure 1(a). The originally fielded detectors are shown in gray, and the upgraded detectors are shown in black. In addition to higher efficiencies, the upgraded detectors have less scatter of relative efficiencies within a detector pair. Fabrication issues with wafer 1 resulted in a higher number of lower-efficiency detectors; however, these fabrication issues were improved for wafers 2–4.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: The terminated vialess crossover with the original (a) and updated (b) termination design together with the magic tee (c) with the updated design. In the original design, the superconducting Nb line is overlaid with a wider gold line for adiabatic absorption and impedance matching. The new termination was realized as a stepped-impedance transformer from Nb to PdAu. (The light sections of the termination line are Nb, while the dark sections are PdAu.) This design avoids proximitization, is robust against fabrication variability, and reduces the device footprint. Images with the revised design were adapted from N23.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: Bandpass FTS measurement and simulation. On the left in logarithmic scale and on the right in linear scale. The measured bandpass edges agree well with the simulation. In the text, we present arguments that the decrement in transmission on the high-frequency half of the bandpass is a measurement artifact.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: The optical time constants of the upgraded detectors as a function of optical loading Pγ. Increasing optical loading results in a decrease in bias power and therefore electrothermal feedback. The drop in feedback is consistent with the marginal trend of slowing of the detectors with increasing Pγ.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: (a) The distribution of the objects in this work (blue triangles) and C. Hu et al. (2021) (orange solid cycles) in the plane of Hβ FWHM vs. the flux ratio of Fe II to Hβ (RFe). Objects with published lags from other SEAMBH or MAHA observations (green solid cycles; see the text for the references), and other PG quasars in T. A. Boroson & R. F. Green (1992) (black empty cycles) are also plotted. Both measurements of Hβ FWHM and RFe are taken from T. A. Boroson & R. F. Green (1992) directly. (b), (c) The histograms of RFe and Hβ FWHM for the CAHA sample (red) and the entire PG quasar sample (cyan), respectively. The mean values are indicated by the dotted lines.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: Light curves, interpolation cross-correlation function analysis, and spectral decomposition of the mean and rms spectra for PG 2308+098, plotted in the same manner as in Figure 4.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: ICCF analysis for the continuum light curve from ASAS-SN (upper left) and our Hβ light curve (lower left) for PG 2308+098. The vertical blue dashed line in the upper-left panel marks the beginning of our spectroscopic monitoring to this object. The upper-right panel shows the CCF (in black) and the corresponding CCCD (in blue). The vertical dotted line marks the centroid as the measurement of the time lag.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: Detrended light curves (left column, from top to bottom: Fphot, F5100, and FHβ) and corresponding ICCF results for FHβ with respect to Fphot (right column, top panel) and F5100 (right column, middle panel) for PG 1116+215. For each panel in the right column, the CCF and the corresponding CCCD are shown in black and blue, respectively, while the vertical dotted line marks the position of the centroid as the lag measurement.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: The Hβ time lag vs. AGN luminosity at 5100 Å for the 26 objects in the current CAHA PG quasars reverberation mapping sample. The 11 objects in this work are marked as blue triangles, while the 15 objects previously published in C. Hu et al. (2021) are marked as orange cycles. The dashed line is the fit to the entire sample of 26 objects, whose expression is also displayed at the bottom.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: The mean spectra of PG 2308+098 before (in blue) and after (in orange) the telluric-absorption correction in three bands (marked by ⊕).
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: Light curves, interpolation cross-correlation function analysis, and spectral decomposition of the mean and rms spectra for PG 1444+407, plotted in the same manner as in Figure 4.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: Light curves, interpolation cross-correlation function analysis, and spectral decomposition of the mean and rms spectra for PG 2233+134, plotted in the same manner as in Figure 4.
Paper: Frequency-comb-calibrated Laser Heterodyne Radiometry for Precision Radial Velocity Measurements
Authors: Ryan K. Cole, Connor Fredrick, Winter Parts, Max Kingston, Carolyn Chinatti, Josiah Tusler, Suvrath Mahadevan, Ryan Terrien, Scott A. Diddams
Figure caption: Diurnal pattern in the measured RVs. Gray points show measured RVs for each day plotted on the same axis as a function of time relative to solar noon. The mean RV is subtracted from each day, and the RVs are averaged in 300 s bins to reduce noise. Blue points show the average RV in each 300 s bin across the full, 6-week data set, along with the best-fit sine wave. Error bars indicate the standard error of the mean RV in each bin. The bottom panel shows the residuals (measurement - model) between the average RV and the fit result.
Paper: Frequency-comb-calibrated Laser Heterodyne Radiometry for Precision Radial Velocity Measurements
Authors: Ryan K. Cole, Connor Fredrick, Winter Parts, Max Kingston, Carolyn Chinatti, Josiah Tusler, Suvrath Mahadevan, Ryan Terrien, Scott A. Diddams
Figure caption: Temperature-induced frequency shifts in the measured data. Panel (a) compares the measured RVs for 2023 October 20 to the temperature measured on the mixer in the RF power detection circuit. The RVs have been averaged in ∼250 s bins to reduce noise, and the measured temperatures have been scaled and shifted to best fit the measured frequency shifts. There is a clear correlation (panel (b)) between the shifts and temperatures (ρ = −0.81). Panels (c) and (d) show the same comparison for the RVs measured on 2023 October 13, where no clear correlation is observed.
Paper: Frequency-comb-calibrated Laser Heterodyne Radiometry for Precision Radial Velocity Measurements
Authors: Ryan K. Cole, Connor Fredrick, Winter Parts, Max Kingston, Carolyn Chinatti, Josiah Tusler, Suvrath Mahadevan, Ryan Terrien, Scott A. Diddams
Figure caption: Solar spectrum measured on the morning of 2023 October 4 before and after telluric correction. The spectrum before telluric correction is shown in gray, and the telluric-corrected spectrum is shown in blue. The spectrum is an average of 250 individual measurements (∼20 minutes) with an average air mass of 2.5.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: (a) Photograph of the upgraded 90 GHz focal plane, taken at the CLASS site. The four new modules are outlined in blue and numbered with the convention used throughout the paper. 37 copper feedhorns per module couple detectors to the incoming radiation. (b) Within each module is an indium-bonded stack of silicon wafers into which is built an integrated array of 37 dual-polarization detector pixels. (c) A single pixel shows updated components: the terminated vialess crossover, the magic tee, and the TES. Images are reproduced from N22 and N23.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: The mapping of several electrothermal parameters from Table 1 and optical efficiency onto the 37 pixels of each upgraded wafer. Each pixel contains two detectors, corresponding to  +45° (top left of corresponding circles) and  −45° (bottom right of corresponding circles) as shown in Figure 1(c). No color indicates an absence of a working detector. Low detector yield is likely due to opens and shorts along the bias leads extending from the detector pixels to the bond pads at the edge of the wafer.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: Light curves, interpolation cross-correlation function analysis, and spectral decomposition of the mean and rms spectra for PG 0157+001. Left column: CAHA light curves of the photometric V-band flux (Fphot) in arbitrary linear units (top panel), the spectroscopic continuum flux at 5100 Å (F5100) in units of 10−15 erg s−1 cm−2 Å−1 (middle panel), and the integrated Hβ flux (FHβ) in units of 10−13 erg s−1 cm−2 (bottom panel). Right column, two top panels: The cross-correlation functions (in black) and the corresponding cross-correlation centroid distributions (in blue) for Hβ with respect to F5100 (adopted) and Fphot, respectively. The time lag (in the observed frame) is marked by the vertically dotted line and displayed as the number with the errors in each panel. Right column, two lower panels: The mean and rms spectra after Galactic extinction correction (in green and black for parts in and out of the fitting windows, respectively) and the best-fit models (in red) comprised by spectral components including the AGN power-law continuum (in blue), Fe II (in blue), broad Hβ (in magenta), broad He II (in cyan), narrow lines (in orange, only in the mean spectrum), and the host starlight (low and out of the panel window). In the panel of the mean spectra, the integration windows for the continuum and the Hβ line are also marked by the vertical dotted lines in blue and orange, respectively..
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: Light curves, interpolation cross-correlation function analysis, and spectral decomposition of the mean and rms spectra for PG 1121+422, plotted in the same manner as in Figure 4.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: Light curves, interpolation cross-correlation function analysis, and spectral decomposition of the mean and rms spectra for PG 1116+215, plotted in the same manner as in Figure 4. The blue dashed lines in the left column show the long-term trends of the light curves. See the text in Section 5.2 and Appendix A for the details, and Figure 15 for the results after detrending.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIV. Long-duration High-cadence Reverberation Mapping Results for 11 PG Quasars
Authors: Chen Hu, Zhu-Heng Yao, Yong-Jie Chen, Yu-Yang Songsheng, Yi-Lin Wang, Sen Yang, Hao Zhang, Wei-Jian Guo, Pu Du, Yan-Rong Li, Ming Xiao, Jun-Rong Liu, Hua-Rui Bai, Feng-Na Fang, Yi-Xin Fu, Yue-Chang Peng, Shuo Zhai, Jin-Ming Bai, Luis C. Ho, Michael S. Brotherton, Jesús Aceituno, Hartmut Winkler, Jian-Min Wang
Figure caption: The histograms of the objects in this work (blue), C. Hu et al. (2021) (orange) and the entire PG quasar sample of T. A. Boroson & R. F. Green (1992) (black). The luminosities are calculated from the absolute magnitudes given in T. A. Boroson & R. F. Green (1992).