adsabs/AstroCLIMB huggingface dataset:
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Selected 12CO channel maps of J16120. The white isocontour is taken from the dust continuum emission in Figure 2. The synthesized beam and the channel velocity are shown in the bottom-left and top-right corners of each panel, respectively. The color bar is not linear but slightly adjusted to highlight the kink emission.
Paper: Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Anibal Sierra, Laura M. Pérez, Carolina Agurto-Gangas, James Miley, Ke Zhang, Paola Pinilla, Ilaria Pascucci, Leon Trapman, Nicolas Kurtovic, Miguel Vioque, Dingshan Deng, Rossella Anania, John Carpenter, Lucas A. Cieza, Camilo González-Ruilova, Michiel Hogerheijde, Aleksandra Kuznetsova, Giovanni P. Rosotti, Dary A. Ruiz-Rodriguez, Kamber Schwarz, Benoît Tabone, Estephani E. TorresVillanueva
Figure caption: Emission surface extracted from the CO channel maps (gray dots), and binned surface (blue diamonds). The error bars are computed from the 16th and 84th percentiles. The surface parameterization from the velocity map and selected channel maps is shown as a red and yellow line, respectively. The emission surface measurements beyond 1.″1 have a large scatter due to low SNR.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: The BPT line diagnostic diagrams for SDSS optical galaxies (contours) and H I-rich sBDEs (stars and crosses) with S/N > 3 in all five emission lines. Left panel: the [N II]6583/Hα and [O III]5007/Hβ diagnostic diagram. Right panel: the [S II]6717,6731/Hα and [O III]5007/Hβ diagnostic diagram. The empirical SF/AGN boundary of Kauffmann et al. (2003; labeled Ka03), the theoretical relation of Kewley et al. (2001; labeled Ke01), and the division lines between Seyfert galaxies and LINER of Schawinski et al. (2007; left panel, labeled Sc07) and Kewley et al. (2006; right panel, labeled Ke06) are shown in dotted, solid, and dashed black lines, respectively. H I-rich sBDEs above the Ke01 line in the left panel are shown in crosses and below the Ke01 line in the right panel are shown in red and blue stars, respectively. Marked in light red and light blue are those sBDEs below the Ke01 line in the [N II]6583/Hα diagnostic diagram but above the Ke01 line in the [S II]6717,6731/Hα diagnostic diagram.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: The average galaxy numbers (left panel) and the fraction of quiescent galaxies (right panel) within the radius of 500, 1000, 1500, and 2000 kpc. The orange and black lines show the results for H I-rich sBDEs and the control sample with the same stellar mass and redshift distribution as the total H I-rich sBDE sample. The uncertainties are estimated using the bootstrapping method.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: MZR (left panel), FMRSFR using the β = 0.32 from Mannucci et al. (2010; middle panel), and FMRH I  using the β = 0.35 from Bothwell et al. (2013; right panel) for the ALFALFA-FASHI combined H I sample (contours) and H I-rich sBDEs (stars). See the caption of Figure 7 for more details on the color of stars.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: Stacked H I spectra. Each panel displays the control samples of star-forming and quiescent galaxies from ALFALFA in green and gray colors, respectively, in the background. The left two panels show the stacked spectra for H I-rich sBDEs from ALFALFA, while the right two panels display those from FASHI. The stacked spectra of SF-sBDEs and Q-sBDEs are shown in blue and red, respectively. The stacked spectra are normalized by the integrated luminosity to 1. The velocity width of the H I profile, W 50, along with the estimated uncertainty from bootstrapping, is shown in each panel in their respective colors.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: Same as Figure 10, but with H I-rich sBDEs dividing into SF-sBDEs (blue) and Q-sBDEs (red). The control samples are constructed separately for SF-sBDEs and Q-sBDEs, which are from the SDSS sample controlling the same stellar mass and redshift.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: The spatial stellar population properties of three SF-sBDEs (top panels) and three Q-sBDEs (bottom panels) matched to MaNGA, overlapped on the relations of the D n 4000 with EW(Hα) (left panel), EW(Hα) with EW(Hδ  A ) (medial panel), and EW(Hδ  A ) with D n 4000 (right panel). The stars show the measurements from SDSS spectra and the contours show the spatial measurements from MaNGA in corresponding colors.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: The relations of the D n 4000 with EW(Hα) (left panel), EW(Hα) with EW(Hδ  A ) (medial panel), and EW(Hδ  A ) with D n 4000 (right panel). The dashed lines in the left and right panels show the best polynomial fitting. See the caption of Figure 4 for more details on the contours and symbols.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: The three SF-sBDEs (top three rows) and three Q-sBDEs (bottom three rows) observed in MaNGA with the corresponding MaNGA-ID marked on the left. Each column shows, from left to right: 1. SDSS g-r-i image with the MaNGA hexagonal field of view overlaid; 2. the stellar velocity fields; 3. Hα velocity fields; 4. Hα equivalent width; 5. Hδ  A  equivalent width; 6. D n 4000. These maps are obtained from the MaNGA DAP.
Paper: Exploring the Origin of Cold Gas and Star Formation in a Rare Population of Strongly Bulge-dominated Early-type Galaxies
Authors: Fujia Li, Enci Wang, Ming Zhu, Ying-jie Peng, Jing Wang, Chuan-Peng Zhang, Zesen Lin, Yu Rong, Hong-xin Zhang, Xu Kong
Figure caption: Same as Figure 8; however, using the N2O2 calibration from Sanders et al. (2018).
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: The redshift distributions of galaxies and absorbers in the MUDF. Galaxies at or below the redshift of the quasar pair are shown; those with metallicity estimates are shown in red. The horizontal strips show UVES wavelength coverage of strong Mg II, Fe II, and C IV transitions in the QSO spectra, with the redshifts of detected absorption shown by the vertical lines. The width of these vertical lines is indicative of the total EW of that ion at that redshift. The lower panel indicates the redshifts at which strong emission lines can be observed in MUSE (blue) and in the HST grism observations (yellow), and shows the gaps in wavelength coverage between MUSE and HST, as well as the MUSE AO laser gap. The red vertical bands indicate the redshifts at which the three lines required for metallicity measurements are accessible, and therefore, the redshift ranges for which metallicities can be determined.
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: The number of galaxies in our sample within 500 km s−1of detected absorption, as a function of velocity offset and compared with randomly placed absorbers. Left: galaxy-absorber velocity offset against impact parameter for pairs in our sample. Colors indicate the ions detected. Uncertainties shown reflect the spread of absorption components and the galaxy redshift uncertainties. We also show the velocity at which gas becomes unbound from a typical galaxy of stellar mass 109.5 M ⊙ at z ≈1.0 (without transverse velocities and line-of-sight distances, this is only indicative). Right: the number of galaxies found within 500  km s−1 of absorption when absorber redshifts are randomized as described in Section 3.3. The histogram in the upper panel shows the distribution for 5000 sets of absorbers with randomized redshifts, while the red line shows the number of galaxies found with absorption in the real MUDF data. The lower panel is similar, but only considers galaxy-absorber pairs with impact parameters smaller than 200 kpc.
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: Galaxy number counts per square degree as a function of magnitude, comparing the MUDF with other surveys. Poisson errors are also indicated. Left: the photometric completeness of the MUDF F140W imaging (from which our spectra are extracted) in comparison with the F160W results shown in Figure 1 of S. Koushan et al. (2021) and the F140W UVUDF imaging (M. Rafelski et al. 2015). The number of sources with confirmed redshifts z < 3.2 is also shown for comparison. Right: the number of spectroscopic redshifts z < 3.2 in the MUDF and the MXDF (R. Bacon et al. 2023), as a function of F775W magnitude extracted from the MUSE spectra. We also show the contribution from the central area of the MUDF, where the depth of the MUSE data exceeds 90 hr.
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: Coverage of the MUDF using MUSE and WFC3 F140W, and galaxies with confirmed redshifts. The background image is from WFC3/F140W imaging, which has a shallow field (red outline) covering a much wider field than the grism and deep imaging (orange outline). The magenta line shows the limit of the MUSE coverage. Galaxies with spectroscopic redshifts 0.5 < z < 3.2 are also highlighted, as this redshift range is that at which absorption can be detected in our UVES spectra. Galaxies within 500  km s−1 of detected absorption are shown in red; those without detected absorption are in blue. The locations of the two quasars are indicated by yellow stars. We note that redshifts are more difficult to obtain using only the grism data, but the dispersion of the grism also allows redshifts to be determined for galaxies outside the field of view covered by direct imaging. The MUSE observations cover a total area of 4.15 arcmin2.
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: The EW of absorption systems seen along the two lines of sight, against various descriptors of the galaxies within 500 kpc and 500 km s−1along the line of sight. These are: Left: the number of detected galaxies; Center left:  the total galaxy stellar mass of detected galaxies; Center right: the impact parameter to the nearest galaxy in projected distance; Right: the impact parameter normalized by the galaxy virial radius, for whichever galaxy within 500  km s−1 is closest by this measure. Points are colored by ions detected in absorption. Absorbers for which no galaxies are detected within this region are shown by crosses, also colored by ions (note that their locations do not represent detection limits on mass or impact parameter). The gray bands indicate the approximate detection limits for the two quasars. We also note that, due to the asymmetry of the survey field, there is an additional source of incompleteness beyond impact parameters of ≈250 kpc.
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: Azimuthal angle against impact parameter for galaxy-sightline pairs in the MUDF sample. Where absorption is detected within 500  km s−1, we show solid points colored by redshift, with nondetections shown as faint crosses. Only the detections are projected into histograms, also colored by redshift. Note that multiple absorption components are often found for the same galaxy and sightline, leading to one point on the scatter plot corresponding to multiple detections in the histograms.
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: Magnitude in the HST F140W imaging against redshift for sources with confirmed redshifts. Sources shown in blue lie in the redshift range of 0.45 < z < 2.4, where we have coverage of strong absorption lines in the quasar spectra and strong emission lines in the galaxy spectra, as shown in Figure 1. Sources outside this redshift range, shown in red, are excluded from most of our analysis.
Paper: The MUSE Ultra Deep Field (MUDF). VI. The Relationship between Galaxy Properties and Metals in the Circumgalactic Medium
Authors: Alexander Beckett, Marc Rafelski, Mitchell Revalski, Michele Fumagalli, Matteo Fossati, Kalina Nedkova, Rajeshwari Dutta, Rich Bielby, Sebastiano Cantalupo, Pratika Dayal, Valentina D'Odorico, Marta Galbiati, Céline Péroux
Figure caption: Observed magnitudes, stellar masses, and SFRs of our sample of galaxies. Red bars indicate galaxies for which absorption is found within 500  km s−1 of the galaxy redshift; blue bars indicate those without detected absorption, but which lie at redshifts 0.45 < z < 2.39 for which the strong Mg II, Fe II, or C IV lines are covered by the UVES spectra and multiple emission lines are available for galaxy redshift measurements. We also show the sources with redshifts outside the range for which we could detect absorption (and are hence excluded from our samples).
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: Top: obscurer column density over the course of the campaign from the NICER spectral analysis in Paper III (Partington et al. 2023). Dashed lines demarcate the three 140 day epochs in which we compute the lags. Epochs 1 and 3 coincide with times of higher average column density, and Epoch 2 with times of lower average column density. Middle: UVW1 light curve from Figure 1. Bottom: lags as a function of wavelength at frequencies of 0.014−0.048 day−1, equivalent to timescales of 20−70 days. The lags are fit with a τ ∝ λ 4/3 relation (dashed blue line), with best-fit normalization values (τ 0) shown. We compare the lags to the expected lag–wavelength relation given the mass and accretion rate of Mrk 817 using the disk reprocessing model in each frequency range (dashed orange line). The lags in Epochs 1 and 3 are a factor of 2 longer than those measured in Epoch 2.
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: AGN STORM 2 light curves from Swift and ground-based telescopes from THJD = 9177–9597. The ground-based filters are lowercase, except for the ground-based Johnson/Bessel B  g , V  g . A dashed vertical line in the X-ray bands indicates the XMM-Newton observation used in our analysis. The average of 1000 GP realizations is shown by colored lines, with 1σ shaded regions.
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: Left: lags as a function of wavelength at frequencies of 0.014–0.048 day−1, equivalent to timescales of 20–70 days computed during periods of relatively high and low obscurer column density. The lags are fit with a τ ∝ λ 4/3 relation (dashed blue line), with best-fit normalization values (τ 0) shown. The expected lag–wavelength relation of the disk reprocessing model is shown in orange. The disk model lies within 1σ from the τ ∝ λ 4/3 best fit for the unobscured lags. Upper right: obscurer column density over the course of the campaign from the NICER spectral analysis in Paper III (Partington et al. 2023). Lower right: UVW1 light curve from Figure 1. Dashed lines demarcate the two time ranges used to compute the lags. The obscured time range is the same as the original Epoch 1 used in the epoch-resolved analysis. The unobscured time range combines the original Epoch 2 with the (unobscured) first half of the original Epoch 3. We do not use the last 75 days of the campaign (the second half of the original Epoch 3) when the column density is high in this analysis, and thus it is not shown. The lags shown here can be found in Table 3.
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: UVOIR lags as a function of wavelength in the lowest three frequency bins. The lags are fit with a τ ∝ λ 4/3 relation (dashed blue line), with best-fit normalization values (τ 0) shown. We compare the lags to the expected lag–wavelength relation given the mass and accretion rate of Mrk 817 using the disk reprocessing model in each frequency range (dashed orange line). At higher frequencies, the lags approach the expected lag–wavelength, with the lags in the 0.05−0.11 day−1 range (rightmost panel) roughly consistent with the disk reprocessing model. If this discrepancy is due to additional reprocessing from beyond the disk, it is occurring on timescales longer than 20 days, which is consistent with the BLR size scale inferred from the 23 days Hβ lag.