adsabs/AstroCLIMB huggingface dataset:
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: Left: UVW2 light curve divided into the five time segments identified in Homayouni et al. (2023b; only points within the time segment and within ±0.5 day of a 1180 Å data point are shown). Right: the correlations between the UVW2 and 1180 Å fluxes for the different time segments. Colors and symbols match the time segments on the left. The dashed line is the best-fitting linear relation to the whole data set.
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: A comparison of the normalized UVW2 light curve (black) with normalized light curves (blue) at 1180 Å (top), 1739 Å (second top), U (second bottom), and V (bottom). All light curves are normalized by subtracting the median and dividing by the standard deviation of the full light curve. No time shift was applied.
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: A detailed comparison of the (a) X-ray and (b) UVW2 light curves of Mrk 817. The X-ray light curve is on a log scale to highlight the variability at low count rates better. Generally, the features of the two light curves do not match up, with the exception of a few peaks indicated by vertical dotted lines.
Paper: Fast Gravitational-wave Parameter Estimation without Compromises
Authors: Kaze W. K. Wong, Maximiliano Isi, Thomas D. P. Edwards
Figure caption: GW150914 posterior computed by our code (blue) and BILBY (gray). ✎
Paper: Fast Gravitational-wave Parameter Estimation without Compromises
Authors: Kaze W. K. Wong, Maximiliano Isi, Thomas D. P. Edwards
Figure caption: GW170817 posterior computed by our code (blue) and BILBY (gray). ✎
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: TESS photometry of HD 36644. Left panels: periodograms for the full data set (top; purple), after pre-whitening with the rotational frequency and first harmonic (bottom; magenta), and after prewhitening with all harmonics (bottom; black). The rotational frequency is indicated with a red dash and harmonics with blue dashes. The green dashed curve is a polynomial fit to the fully prewhitened frequency spectrum, used to evaluate the noise floor, and the green solid curve shows 4× the noise floor, the threshold for frequency significance. Right panels: the light curve folded with the rotational frequency (top) and residuals (bottom) after subtraction of the harmonic model determined from frequency analysis (red curve). Different sectors are indicated by color.
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: Light curves of hot magnetic stars detected in VCSS snapshots. The time axis is aligned with the UT of each detection, indicated and labeled in each plot. Upper limits for nondetections (triangles) correspond to three times the PyBDSF-calculated local noise at the stellar positions corrected for primary beam attenuation.
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: Left: surface density with galactic latitude of the hot magnetic star catalog and the fitted Equation (B1). Middle: normalized galactic latitude CDF for the catalog and fit. Right: normalized galactic longitude CDF for the catalog and a continuous uniform distribution.
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: VCSS snapshot cutouts centered on HD 36644, organized chronologically. Pixel intensities have been corrected for primary beam attenuation. Labels indicate the time relative to the detection, the distance of HD 36644 from the snapshot center, and the noise (σ) at the stellar position (circled). The color scale ranges from 0 to 6 times the local noise for each image.
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: Left: average source density around isolated point sources in VCSS epoch 1 (dashed) and epoch 2 (solid). Densities above several S/N cuts are shown. Right: histograms of the number of isotropic artifacts in VCSS snapshots.
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: VCSS snapshot cutouts centered on HD 40759 (top) and HD 175362 (bottom) at the time of detection. Color scale is the same as in Figure 2.
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: The longitudinal magnetic field 〈B z〉 curves for (top) HD 175362 (hydrogen lines; Shultz et al. 2018) and (bottom) HD 40759 (metals; E. Semenko et al. 2023, in preparation).
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: Left: catalog of 761 hot magnetic stars plotted in Galactic coordinates. Right: a randomly generated catalog with the same number of stars and similar distribution.
Paper: Discovery of a Low-redshift Hot Dust-obscured Galaxy
Authors: Guodong Li, Chao-Wei Tsai, Daniel Stern, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Tanio Díaz-Santos, Peter R. M. Eisenhardt, Roger L. Griffith, Thomas H. Jarrett, Hyunsung D. Jun, Sean E. Lake, M. Lynne Saade
Figure caption: Zoomed-in UV-optical SED of W1904+4853. As in Figure 2, the filled magenta data points denote the emission line subtracted, while black open circles represent the photometry before the emission-line corrections. Strong H α emission in the y band puts the observed photometry off-scale, so only the emission-line-subtracted y band is shown here. Filter transmissions for the photometric points are displayed at the bottom of the panel. The blue dashed line shows the unobscured starburst (Im) component from the case 1 best-fit SED model (also shown in Figure 2), which dominates the UV optical. The cyan dashed line shows the mildly obscured (A V ∼ 0.9 mag) AGN (Assef et al. 2010) component from the case 3 model, which again dominates the UV optical, but fails to reproduce the shape of the continuum.
Paper: Discovery of a Low-redshift Hot Dust-obscured Galaxy
Authors: Guodong Li, Chao-Wei Tsai, Daniel Stern, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Tanio Díaz-Santos, Peter R. M. Eisenhardt, Roger L. Griffith, Thomas H. Jarrett, Hyunsung D. Jun, Sean E. Lake, M. Lynne Saade
Figure caption: BPT diagrams for W1904+4853. The magenta points denote the line ratios derived from the narrow-line fluxes of W1904+4853. The error bars are smaller than the symbols; thus, they are not visible in this plot. Solid lines show the demarcation between starburst galaxies and AGN defined by Kewley et al. (2001) for all panels. The dashed line denotes the dividing line between star-forming and composite star-forming (Kauffmann et al. 2003). The dotted line separates Seyfert and LINER-type AGNs (Kewley et al. 2006).
Paper: Discovery of a Low-redshift Hot Dust-obscured Galaxy
Authors: Guodong Li, Chao-Wei Tsai, Daniel Stern, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Tanio Díaz-Santos, Peter R. M. Eisenhardt, Roger L. Griffith, Thomas H. Jarrett, Hyunsung D. Jun, Sean E. Lake, M. Lynne Saade
Figure caption: Observed spectrum of W1904+4853 around strong emission lines. The blue solid line shows the best-fit model in each panel. The green solid line and orange dashed lines represent the broad Gaussian and narrow Gaussian components, respectively. The cyan solid line represents the best-fit power-law continuum model (F  ν [μJy] = (17.9 ± 0.3) × λ[μm]1.53±0.04). The brown solid line shows the Fe II line complex (Tsuzuki et al. 2006). We note that the apparent absorption in the O III 4959 Å emission line is an artifact due to a cosmic ray. This feature is not seen in the Keck/LRIS spectrum.
Paper: Discovery of a Low-redshift Hot Dust-obscured Galaxy
Authors: Guodong Li, Chao-Wei Tsai, Daniel Stern, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Tanio Díaz-Santos, Peter R. M. Eisenhardt, Roger L. Griffith, Thomas H. Jarrett, Hyunsung D. Jun, Sean E. Lake, M. Lynne Saade
Figure caption: SFR vs. stellar mass of W1904+4853 compared with galaxies in the PRIMUS sample (Moustakas et al. 2013). The magenta point represents the lower limit to the SFR based on the UV continuum without considering the extinction from the host galaxy. The yellow point represents the extinction-corrected SFR from the host galaxy, which is close to the SFR inferred from the narrow [O II] line. Both SFRs and stellar masses in the PRIMUS sample are recalculated using the methods discussed in Sections 4.3.1 and 4.3.3. The blue dots represent galaxies with luminosity dominated by the young stellar population in the SED fitting, while the red dots represent galaxies dominated by the old stellar population.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption: Rest-frame mean (black; panels (a) and (c)) and rms (gray; panels (b) and (d)) of Mrk 142 Gemini (top; velocity resolution of 185.6 ± 10.2 km s−1) and LJT (bottom; velocity resolution of 695.2 ± 3.9 km s−1) spectra highlighting the Regions of Interest—Hβ λ4861 and [O III] λλ4960, 5008 (region shaded in green), and He I λ5877 (region shaded in pink). Labels enclosed in dashed (dotted) boxes indicate broad (narrow) lines. The Gemini mean spectrum shows sharp Fe II features (shaded in faint blue), which appear blended with the red wings of Hβ and [O III] λ5008 (blue shaded bars) in the LJT mean. Owing to the high signal-to-noise of the Gemini spectra, the peculiar shape of the He I λ5877 line is clearly evident. The high-ionization coronal lines (shaded in brown) also appear sharp in contrast to the LJT spectrum, as a result. The LJT rms spectrum shows clear variability in He II (shaded in blue). Both rms spectra indicate variability in the broad Hβ. However, no significant variability is evident in He I over the timescale of Gemini+LJT observations. The yellow-shaded region in the Gemini spectra indicates the GMOS chip gap from ∼5350 to ∼5410 Å. (The reduced and calibrated Mrk 142 Gemini spectra are available in a machine-readable form.) (The data used to create this figure are available.)
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption: Composite model fit to epoch 24 of the Mrk 142 Gemini data displaying individual components of the model. Panel (a): Composite model (red solid curve) fit to the data (black solid curve) from 4430 to 6300 Å is shown in the main panel, and the Hβ and He I Regions of Interest are shown in the Inset panels. The individual components of the model are displayed at the bottom of the panel: continuum (cyan solid curve); Fe II I Zw 1 template as a pseudo-continuum (faint blue solid curve); host-galaxy template (orange solid curve); He II broad components (blue dashed Gaussians); Hβ broad components (green dashed Gaussians); He I broad components (pink dashed Gaussians); narrow-line components of Hβ, He I, and [O III] (purple solid Gaussians); and high-ionization coronal lines (brown solid Gaussians). The total broad Hβ and He I profiles are also overplotted (gray solid curves). Panel (b): Residuals of the model with ﹩{{\chi }_{\nu }}^{2}=1.183﹩. The model shows larger residuals around the [O III] λ5008 line indicating a suboptimal fit in that region. The noisier blue end of the spectrum affects the overall fit in that region, thus resulting in larger residuals compared to the red end of the spectrum.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption: Time-lag measurements with reference to the Swift/UVW2 band (top row) with lag distributions modeled as log-Gaussians. Left: the top three panels show continuum light curves—Swift/UVW2 (blue), LCO+Zowada+Liverpool/g (green), and inter-calibrated Gemini+LJT/5100 Å—in units of 10−15 erg s−1 cm−2 Å−1. The bottom two panels show the broad Hβ light curves—LJT only (pink) and Gemini+LJT inter-calibrated (olive)—in units of 10−14 erg s−1 cm−2 Å−1. Right: time-lag distributions (colored histograms for the mean lag and gray shaded uncertainty estimates from a log-Gaussian lag distribution) of the light curves on the left with reference to the Swift/UVW2 band, which has a fixed lag of 0.00 day. Insets in the second and the third panels show a close view of the time-lag distributions for LCO+Zowada+Liverpool/g and Gemini+LJT/5100 Å light curves, respectively. For each of the echo light curves, the black solid vertical line marks the lag measurement, given by the median lag of the colored distribution and the black dashed vertical lines (on either sides of the solid line) mark the corresponding uncertainty.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption: Mean (panel (a)) and the rms spectra for 64 narrow-slit Mrk 142 Gemini spectra processed through PrepSpec showing model fits with individual components. In panel (a), the composite model (dark blue curve), including the components shown at the bottom of the plot—average spectrum (AVG; black), continuum (cont; red), Fe II (Fe2; faint blue), broad-line region (BLR; dark blue), and narrow-line region (NLR; orange), is overlaid on the mean spectrum (black curve). The broad (narrow) emission lines are indicated with green (orange) dotted vertical lines as well as with green (orange) solid horizontal dashes. The broad lines of Hβ (blue label) and He I (purple label) are marked with solid horizontal dashes. In panel (b), model (model; dark gray curve) fit to the residual rms spectrum (rmsx; blue curve) includes the components: continuum (cont; red curve) and BLR (green curve at the bottom of the plot). The raw rms spectrum is the upper green curve. The BLR component comprises the broad lines of Hβ (blue bump around ∼4862 Å) and He I (purple bump around ∼5877 Å) shown at the bottom of the plot. The broad He II emission feature at ∼4687 Å (box-like feature in the model) is contaminated with Fe II and hence difficult to fit given the noise in the region. The deviation in the residual rms spectrum (σ rmsx;  cyan curve) shows large values in the region of the GMOS detector chip gap from ∼5345 to ∼5420 Å. In both panels, the active broad-line windows of Hβ and He I used for PrepSpec modeling are shown in negative-value space.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption:  PrepSpec model including all components (panel (a)) and residuals (data − model in units of standard deviation, σ; panel (b)) with a reduced χ 2 (﹩{\chi }_{\nu }^{2}﹩) of 0.782 for 64 narrow-slit Mrk 142 spectra. In panel (a), dark regions indicate strong emission lines of Hβ and [O III], whereas the weaker He I lines and Fe II emission appears as less prominent features. In panel (b), each row represents a single exposure spectrum (where multiple exposures at a given epoch are not yet combined). The horizontal wiggles strongly evident in some spectra are likely the result of either replacing values with simulated data in those regions or using a higher-order function during flat-fielding (see the text for more details). The smeared region from ∼5345 to ∼5420 Å is one of the chip gaps of the GMOS detector where simulated data was added during reduction.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption: Composite model fit to epoch 24 of the Mrk 142 LJT data displaying individual components of the model. See caption of Figure 5 for a description of the individual model components in Panel (a). The red side of the broad Hβ emission line shows contamination with the Fe II emission at ∼4923 Å. Similarly, the [O III] λ5008 line shows considerable blending with the Fe II feature in its red wing, thus affecting a reliable measurement of the [O III] λ5008 line. Panel (b) shows the residuals of the model with ﹩{{\chi }_{\nu }}^{2}=1.711﹩. The smaller residuals indicate an overall good fit to the spectrum. The model performance drops significantly at both ends of the spectrum although it does not impact measurements in the Regions of Interest.
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption: Mrk 142 continuum light curves—UVW2 band with Swift (blue upright triangles, panel (a)) and the g band with LCO, Zowada, and Liverpool (green flipped triangles, panel (b)) from photometric observations; and 5100 Å (purple diamonds, panel (c)) inter-calibrated from the spectroscopic observations with the Gemini North Telescope (Gemini) and the Lijiang Telescope (LJT). The 5100 Å inter-calibrated light curve displays the combined spectroscopic coverage over 102 epochs. We performed the inter-calibration with a Python-based running optimal average (PyROA; Donnan et al. 2021) technique (see introduction to PyROA in Section 5.1).
Paper: Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
Authors: Viraja C. Khatu, Sarah C. Gallagher, Keith Horne, Edward M. Cackett, Chen Hu, Sofia Pasquini, Patrick Hall, Jian-Min Wang, Wei-Hao Bian, Yan-Rong Li, Jin-Ming Bai, Yong-Jie Chen, Pu Du, Michael Goad, Bo-Wei Jiang, Sha-Sha Li, Yu-Yang Songsheng, Chan Wang, Ming Xiao, Zhe Yu
Figure caption: Broad Hβ light curve from Gemini (dark blue open circles) scaled down (faint blue open circles) to the broad Hβ light curve from LJT (red solid squares). The scaling factor of 0.77 was determined such that the Gemini data points are distributed evenly above and below the LJT light curve. The two light curves show similar behavior except at Modified Julian Date ∼ 58540, where the LJT light curve increases in flux, while the Gemini light curve appears fainter.