adsabs/AstroCLIMB huggingface dataset:
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: 2023 Reverberation Mapping Results
Authors: Wen-Zhe Xi, Kai-Xing Lu, Jin-Ming Bai, Zhang Yue, Weimin Yi, Liang Xu, Sha-Sha Li, Hai-Cheng Feng, Jian-Guo Wang
Figure caption: Variations of the optical luminosity (a) and the BLR radius (b) for NGC 5548 measured between 1988 and 2023, and the result of cross-correlation analysis (panel (ba)). The different symbols with different colors are used in the left panels to distinguish the different campaigns, The horizontal dotted lines in panels (a) and (b) mark the optical luminosity and BLR radius positions for the 2023 observing season, Both parameters in 2023 have already reached levels comparable to their historical maxima. In panel (ba), the red solid curve is the CCF between the BLR radius and the optical luminosity (﹩{r}_{{\rm{\max }}}=0.66﹩), and the black histogram is the cross-correlation centroid distribution (CCCD), the vertical dashed line marks the measured time lag of ﹩3.{5}_{-1.6}^{+2.0}﹩ yr, the vertical dotted lines are reference lines of zero time lag.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: 2023 Reverberation Mapping Results
Authors: Wen-Zhe Xi, Kai-Xing Lu, Jin-Ming Bai, Zhang Yue, Weimin Yi, Liang Xu, Sha-Sha Li, Hai-Cheng Feng, Jian-Guo Wang
Figure caption: Radial stratification and line responsivity of the BLR in NGC 5548. Panel (a) presents the comparison of radii for broad-line emitters, which exhibits the properties of radial stratification. Panel (b) illustrates the comparison of responsivity for the Balmer and helium lines.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: 2023 Reverberation Mapping Results
Authors: Wen-Zhe Xi, Kai-Xing Lu, Jin-Ming Bai, Zhang Yue, Weimin Yi, Liang Xu, Sha-Sha Li, Hai-Cheng Feng, Jian-Guo Wang
Figure caption: Velocity-resolved RM results for the 2023 season (bottom right). For comparison, updated results from previous seasons (2015, 2018, 2019, 2020, and 2021) are shown. The top panels of each group of 6 panels shows the mean spectrum; the middle panel shows the rms spectra of broad Hγ (right) and Hβ (left). The bottom panel displays centroid time lags versus line-of-sight velocity, based on 15 (circles) and 30 (squares) equal-flux velocity bins. Horizontal error bars represent half the bin width. Gray symbols indicate bins with maximum correlation coefficients below 0.5. No RM detection was obtained in 2020 for Hγ due to weak variability. The horizontal dotted line and pink band mark the average lag and its uncertainty for each season.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: 2023 Reverberation Mapping Results
Authors: Wen-Zhe Xi, Kai-Xing Lu, Jin-Ming Bai, Zhang Yue, Weimin Yi, Liang Xu, Sha-Sha Li, Hai-Cheng Feng, Jian-Guo Wang
Figure caption: The temporal variations of Hβ and Hγ VRLPs are systematically compared across six observing seasons (2015, 2018, 2019, 2020, 2021, and 2023) using 30 equal-flux velocity bins, with lags below a maximum correlation coefficient of 0.5 excluded. Vertical and horizontal dotted lines indicate the line core at zero velocity and zero time lag, respectively.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Percentile of the distribution versus offset from median for each cluster within the t-SNE analysis for Lstellar and stellar metallicities.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Percentile of the distribution versus offset from median for each cluster within the t-SNE analysis for SFR and Ldust.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Percentile of the distribution versus offset from median for each cluster within the t-SNE analysis for redshift and mass.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Percentile of the distribution versus offset from median for each cluster within the t-SNE analysis for excess color.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Distribution of host galaxy parameters for clusters 4, 5, and 7 from the t-SNE dimensionality reduction.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Distribution of host galaxy parameters for clusters 8 and 9 from the t-SNE dimensionality reduction.
Paper: Hadronic Processes in Advection-dominated Accretion Flow as the Origin of TeV Excesses in BL Lac Objects
Authors: Ji-Shun Lian, Ze-Rui Wang, Jin Zhang
Figure caption: Broadband SEDs of the five BL Lacs with fitting results. The observational data, represented by scattered points, are referenced to Section 2. Gray circles and triangles denote data in the observer frame, whereas the corresponding red symbols indicate data corrected using the EBL model of J. D. Finke et al. (2022). The black solid lines represent the sum of each component emission for the sources, including the jet synchrotron radiation (red solid lines), the jet SSC radiation without EBL absorption (green solid lines), the ADAF spectrum (magenta solid lines), the γ-ray emission from the π0 decay in the pγ process (blue solid lines) and in the pp process (gray dashed lines), and the radiation from cascaded electrons (red and green dashed lines) produced by pγ and Bethe–Heitler processes in the ADAF. The differential sensitivity curves (violet short horizontal lines) of IceCube are taken from M. G. Aartsen et al. (2019).
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: Detrended light-curve analysis for Mrk 1048 and Mrk 618. The top left panel shows the photometric g-band continuum with data points from different telescopes labeled. The middle and bottom left panels display the variations in Hβ and Hα emission-line flux (in arbitrary units), each fitted with a best-fit linear trend shown in red, which has been subtracted to obtain the detrended light curves. The g-band continuum is overlaid for comparison, normalized and shifted to the final adopted lag values listed in Table A1. The JAVELIN model for each light curve is shown in steel blue. The right panels show the corresponding lag distributions from ICCF (teal histograms) and JAVELIN (violet histograms). The magenta dashed curve represents the cross-correlation function, with the left axis showing ﹩{r}_{{\rm{\max }}}﹩ and the right axis showing the probability density N. The darker magenta region marks the central 80% of the CCF peak used to determine the ICCF centroid lag. The vertical dashed lines indicate the 16th and 84th percentile uncertainties of the lag distributions.
Paper: Measurement and Modeling of Electron Temperature in Laboratory Photoionized Plasmas Relevant to Astrophysics
Authors: J. J. Rowland, R. C. Mancini, G. S. Jaar, D. C. Mayes, H. Scott, I. E. Golovkin, M. Chatzikos, G. Ferland, G. P. Loisel, J. E. Bailey
Figure caption: Photon-energy-resolved radiation fluxes at the peak X-ray drive (t = 100 ns) from the HeliosCR simulation of the P = 15 Torr case (neon atom number density 5 × 1017 cm−3) showing the flux incident on the Mylar window (green trace), the flux transmitted through the Mylar window (orange trace), and the flux further transported through the first shocked neon layer (blue trace). Blue and orange traces overlap except where indicated.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: The relationship between the Hβ BLR size and the optical continuum luminosity at 5100 Å. A range of reverberation-mapped AGN samples from the literature are overplotted for comparison. These include SEAMBHs (P. Du et al. 2016, 2018; C. Hu et al. 2021; S.-S. Li et al. 2021, gray open circles), SDSSRM-2024 sources (Y. Shen et al. 2024, gray open squares), OzDES AGNs (U. Malik et al. 2023, gray open diamonds), LAMP sources (V. U et al. 2022, gray open circles), and SAMP sources (J.-H. Woo et al. 2024, gray open hexagons). Additional RM sources from various studies (M. C. Bentz et al. 2013; S. Park et al. 2017; S. Rakshit et al. 2019; E. D. Bontà et al. 2020; S. Rakshit 2020; S. Pandey et al. 2022, gray open inverted triangles) are also included. The maroon and black dashed lines represent the best-fit R–L relation as reported by J.-H. Woo et al. (2024) and Y. Shen et al. (2024), respectively. Our target sources, Mrk 1048 and Mrk 618, are marked with a filled blue triangle and a filled red circle, respectively. Mrk 1048 moves toward the upper left, while Mrk 618 moves toward the lower left, to the best-fit relation. These are still lying closer to the best-fit relation.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: The relationship between the Hα BLR size and the monochromatic continuum luminosity at 5100 Å. Reverberation-mapped sources with Hα lag measurements from previous studies are overplotted for comparison, including those from S. Kaspi et al. (2000), M. C. Bentz et al. (2010), C. J. Grier et al. (2017), H. Cho et al. (2020), J.-H. Woo et al. (2024), C. Sobrino Figaredo et al. (2025), and Y. Shen et al. (2024), along with additional sources from S. G. Sergeev et al. (2016), H.-C. Feng et al. (2021), and S.-S. Li et al. (2022). The maroon and black dashed lines represent the best-fit R–L relation as derived by H. Cho et al. (2023) and C. Sobrino Figaredo et al. (2025), respectively. Our target AGNs, Mrk 1048 and Mrk 618, are plotted as a filled blue triangle and a filled red circle, respectively. The previous measure of Hα for Mrk 1048 (C. Sobrino Figaredo et al. 2025) is also marked with an open triangle. Mrk 618 lies closer to the Hα best-fit relation, while Mrk 1048 is slightly more offset than found by C. Sobrino Figaredo et al. (2025).
Paper: Measurement and Modeling of Electron Temperature in Laboratory Photoionized Plasmas Relevant to Astrophysics
Authors: J. J. Rowland, R. C. Mancini, G. S. Jaar, D. C. Mayes, H. Scott, I. E. Golovkin, M. Chatzikos, G. Ferland, G. P. Loisel, J. E. Bailey
Figure caption: Experimental Li-like neon transmission spectrum displaying the line absorption transitions arising from states in the 1s22s and 1s22p configurations employed in the temperature measurement. The data were recorded for a neon gas cell fill pressure P = 30 Torr or neon atom number density of 1018 cm−3. Li-like absorption features are labeled according to the configuration of the initial state; double labels indicate absorption features with contributions from both. The numbers under the Li symbol represent the principal quantum number n of the final (upper) state of the transition. Two transitions in He-like neon are also noted in a similar way.
Paper: Hadronic Processes in Advection-dominated Accretion Flow as the Origin of TeV Excesses in BL Lac Objects
Authors: Ji-Shun Lian, Ze-Rui Wang, Jin Zhang
Figure caption: The γγ optical depth curves for the ADAF model with varying radii in the source 1ES 0347–121.
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: Radio survey images from LoTSS-DR2 (top left; T. W. Shimwell et al. 2022), RACS (top middle and right; S. W. Duchesne et al. 2023, 2024, 2025), and VLASS (bottom; M. Lacy et al. 2020) of the location of PTF11cmh. Crosshairs represent the optical location of the supernova. When applicable, contours represent the 5σ level of the image and crosses represent the location of the brightest pixel near the location of PTF11cmh (we note that the brightest pixel is below a 5σ detection). The observing frequency is stated in the top left, the length scale is stated in the top right, the beam size is represented as an ellipse in the bottom left, and the observation date is stated on the bottom right of each image.
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: Same as Figure A2, but for the location of PTF11qcj. The first VLASS detection (bottom left) was reported in M. C. Stroh et al. (2021). The shape of the radio source in the LoTSS-DR2 image (top left) is inconsistent with the beam size of the observation, indicating at least some of the emission is not associated with PTF11cmh but rather its host galaxy (LEDA 2295826; M. F. Bietenholz et al. 2021).
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: The top panel shows from left to right the H I column density contours at levels [1.5, 5, 15, 25, 35, and 45] × 1020 cm−2 overlaid on the optical pODI r-band image, the H I velocity field of the galaxy, and the H I velocity dispersion map of the galaxy. The bottom panel shows a zoomed-in field of view on the central-most region of the galaxy. From left to right, this panel shows the Hα pODI image with the H I column density contours overlaid in red and the Hα contours overlaid in white and black at levels of [0.2, 0.5, 1, 2, and 4] × 10−17 erg s−1 cm−2, the H I velocity field, and the H I velocity dispersion with the same Hα contours overlaid. The ovals in the bottom left of each panel represent the beam size.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Top row from left to right: optical-continuum subtracted Hα image with selected emission regions overlaid, same narrowband image with SparsePak pointing overlaid, and Hα flux map. Bottom row from left to right: Hα velocity field, Hα velocity dispersion, and Hα− H I gas velocity differences (H I velocity field is shown separately in Figure 4). The filled circles correspond to the SparsePak pointing fiber locations from where we recover flux.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Optical r-band (top) and deep Hα pODI imaging of NGC 3741. The Hα emission is concentrated in a central group of star-forming regions with diffuse clouds of emission extending out from the central region. The stellar component shows a bright concentration coincident with the central H II regions, with some faint extensions of stellar material to the north and south.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Top panel: deep Hα pODI image with 400 pc x 400 pc SFH boxes overlaid. Bottom panel: SFHs for each box are plotted. The SFHs have ≤15 Myr time resolution in the t < 70 Myr time bins. See Section 2.4 for specific time binning. The red shading represents the random uncertainties. All SFHs are plotted with the same y-axis scale. Region 5 is shown in Figure 1 with a full y-axis scale. The black arrows point to the SFRs used to calculate the mass-loading factors for each box, which are listed in Table 3.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Example CMD (left) for a 400 × 400 pc box and the corresponding derived SFH (right) with ≤15 Myr time resolution in the t < 70 Myr time bins. See Section 2.4 for specific time binning. Random uncertainties are represented with red shading.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Top panel: histogram of log([S II]/Hα) for each region of Hα emission. The LSB regions are shown in red, and the HSB regions are shown in purple. The vertical dashed lines correspond to the average log([S II]/Hα) for each population: −0.7 for LSB regions and −0.9 for HSB regions. Bottom panel: Hα emission surface brightness vs. log([S II]/Hα) plot in which the LSB regions are shown in red and the HSB regions are shown in purple.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Top panel: integral H II region luminosity function derived from the selected regions of Hα. The vertical dashed line denotes the completeness limit for the galaxy. The luminosity function is steep with a power-law index of −1.39 ± 0.16. Bottom panel: histogram showing the distribution of the H II emission region luminosities from which the luminosity function was derived.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Single and double Gaussian fits plotted over the spectra for regions 1, 2, and 3. The single Gaussian is a statistically preferred fit in each case.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Left: Zoom-in of the Fe K region of the XRISM/Resolve spectrum divided by the power-law continuum (black points), plotted with the same ratio for the Chandra/HETG data from A. J. Young et al. (2005) (red points). The spectra from both detectors are rebinned identically for comparison. Though the HETG data show clear evidence for the strong, vout ∼ −2000 km s−1  wind in the lines of Fe XXV and Fe XXVI also seen by Resolve, the diminishing effective area of the HETG above ∼7 keV renders it unable to detect the vout ∼ −20,000 km s−1  wind component. Right: The best-fitting model from Section 3.2.2 is plotted against the Resolve data shown in panel (a). In both panels, the blue hashed vertical lines show, from left to right, the rest-frame positions of the Fe Kα, Fe XXV and Fe XXVI lines. Note that, while the emission features of Fe XXV and Fe XXVI appear at their rest-frame energies, the absorption components are blueshifted, indicating an origin in outflowing gas.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Ratios of the 3–55 keV time-averaged broadband data to a series of models (see text for details): (a) a simple photoabsorbed power law; (b) power law plus narrow Gaussian emission line at 6.4 keV; (c) power law plus narrow and broad Gaussian lines at 6.4 and 3.29 keV, respectively; (d) power law plus narrow Gaussian and broad relativistic emission lines at 6.4 keV; (e) cutoff power law plus MYtorus distant reflection; (f) Comptonized coronal emission (nthcomp) plus MYtorus distant and relxilllpCp relativistic reflection. XRISM/Xtend is in black, XMM/pn is in red, NuSTAR/FPMA is in dark blue, and NuSTAR/FPMB is in light blue.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Ratio of the time-averaged XRISM/Resolve data to a simple photoabsorbed power-law model, as in Figure 7 (black points). In each panel, a different, refitted model is plotted in red against the same ratio: (a) the continuum model of the photoabsorbed power law, as in Figure 2; (b) the power law plus narrow emission, i.e., distant neutral reflection and narrow Kα lines from Fe XXV and Fe XXVI, but no HIO or inner disk reflection; (c) the above model plus the multizone HIO; (d) the best-fitting model to the 2024 data, which includes all of the above components plus relativistic, inner disk reflection via the relxilllpCp model. The continuum and narrow features alone cannot replicate the spectral shape; the broad features of inner disk reflection must be included in order to properly fit the data. In all panels, the blue hashed vertical lines show, from left to right, the rest-frame positions of the Fe Kα, Fe XXV, and Fe XXVI features in emission and/or absorption.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Ratio of the time-averaged broadband data from the CCD-resolution detectors to a simple power law modified by Galactic photoabsorption. XRISM/Xtend is in black, XMM/pn is in red, NuSTAR/FPMA is in dark blue, and NuSTAR/FPMB is in light blue. Note the curvature due to low-ionization absorption below ∼3 keV, the soft excess at the lowest energies, and the prominence of reflection in the Fe K band and above 10 keV. Some complexity due to ionized absorption is also evident between ∼6 and 7 keV. The difference between the pn and Xtend is due to their different mirror and detector responses (see text for details).