adsabs/AstroCLIMB huggingface dataset:
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the ratio between the mass-loss and thermal evolution timescales (top), the envelope mass fraction (middle), and the luminosity ratio between the total core cooling and the intrinsic envelope cooling (bottom) for both the GSS18 coupled Parker wind (red) and our decoupled Parker wind (black). This is computed from our numerical model for a 4 M ⊕ planet irradiated with 100 F ⊕, initially with 5% of H/He mass. The top panel shows the linear behavior of the coupled wind and the exponential behavior of the decoupled wind. We compare our transition between boil-off and the long-lived Parker wind (circle) to the GSS18 transition (cross) and W. Misener & H. E. Schlichting (2021) transition (triangle). See Sections 4.4 and 4.5 for discussion.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: The evolution of radius and envelope mass fraction of 3 M ⊕ models with a low core mean molecular weight mu  c  = 34 (solid line; high core heat capacity) and a 10× times mu  c  (dashed line; negligible core heat capacity). The analytical models with the physical improvements (black) show little impact from the change of the core heat capacity, similar to our numerical model. The models with the original GSS18 physics (gray) show a divergent fate of these planets with a large difference between the final interior H/He compositions.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the importance of radiative atmosphere for a 3 M ⊕ planet that receives 100 F ⊕ stellar bolometric flux initially with a 5% H/He mass fraction, based on the GSS16 analytical model with the physics improved. The radiative atmosphere is attached on top of the RCB, which enlarges the planetary radius by a considerable fraction.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: The BBH (top), BHNS (middle), and BNS (bottom) merger rates as a function of redshift for our simulations. The left column shows models from grid A, where we vary the common-envelope efficiency α CE and stable mass transfer efficiency β, and the right column shows models from grid B, where we vary the SN natal kick velocity root mean square ﹩{\sigma }_{\mathrm{rms}}^{1{\rm{D}}}﹩ and the RMP. For the RMP prescription, D, M, and R stand for the delayed, I. Mandel & B. Müller (2020), and rapid prescriptions, respectively. The assumed SFRD from P. Madau & T. Fragos (2017) is scaled arbitrarily and plotted on all panels in black; note that the SFRD is, in reality, orders of magnitude greater than the merger rate, but the scaling helps compare the shapes by eye. For all merger rates, we include the 1σ and 2σ confidence intervals calculated by bootstrapping the simulation results to show the sampling uncertainty. The sharp merger rate drop-off around z ∼ 9 is due to our assumption that star formation starts at z = 10 and mergers are delayed.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: The intrinsic merger rate (﹩{{ \mathcal R }}_{0}﹩), peak redshift (z peak), and merger rate differentials in the z ranges [0, 1], [1, z peak], [z peak, z peak + 1], and [z peak + 1, 9] for BBHs, BHNSs, and BNSs. The top and bottom rows are for models in grid A and B, respectively, and the colors and markers correspond to those in Figure 2. The red vertical lines in the first column are the inferred BBH, BHNS, and BNS local merger rates (90% credible intervals) from R. Abbott et al. (2023a). We include 1σ and 2σ confidence intervals as shaded boxes around each point, which are calculated by bootstrapping the simulation results. Along the y-axis in the left margin, RMP stands for remnant mass prescription and D, M, and R stand for the delayed, I. Mandel & B. Müller (2020), and rapid prescriptions, respectively. The gray dashed–dotted lines in the second to sixth columns correspond to the differential and z peak values for the assumed SFRD.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: Scatter plots of the intensity from bright H2 lines of two different upper levels measured from the spatially resolved spectrum. In the left panel the intensity of 1338.572 Å is plotted on the x-axis and the intensity of 1333.474 Å is plotted on the y-axis (J = 1, v = 0 upper level). In the right panel the intensity of 1342.256 Å is plotted on the x-axis and the intensity of 1333.796 Å is plotted on the y-axis (J = 2, v = 0 upper level). The black data points are plotted with gray 1σ error bars in the total radiance for each line. The line ratio resulting from spectral synthesis is plotted for each pair of lines using solid lines for the optically thick case and dashed lines for the optically thin case of synthesis calculation from the three model atmospheres. The dark-blue dotted–dashed line shows a linear fit to the data points.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: An example of H2 excitation by a source that is not directly above the region sampled by the spectrograph slit of IRIS. The SJI 1400 Å context image (left panel) shows bright emission from a loop-like structure. The brightest part of the structure shows a saturation spike in the image extending left to right along the detector pixels. Segments of the FUV spectrum from the region covered by the spectrograph slit are shown in the right set of panels. The top row shows the spectrum from the region covered by the yellow line in the SJI image. The brightest H2 emission occurs in the region enclosed by the dashed lines, and the average spectral profile from this region is shown in the bottom row. The H2 emission from this region is very strong relative to the local emission from the bright lines of C II and Si IV, with a peak radiance only about an order of magnitude smaller.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: The total H2 line radiance vs. the spectral radiance observed at the wavelength of the pumped H2 line for the (0,0) upper level. The black data points are plotted with the 1σ error bars in the total line radiance. The same quantity was derived from the spectral synthesis results for the three atmospheric models for both optically thin (dashed lines) and optically thick calculations (solid lines).
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: The total H2 line radiance vs. the spectral radiance observed at the wavelength of the pumped H2 lines for the (2,0) upper level. Plot symbols are the same as in Figure 12.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: The total H2 line radiance vs. the spectral radiance observed at the wavelength of the pumped H2 line for the (1,0) upper level. Plot symbols are the same as in Figure 12.
Paper: Investigating the Cosmological Rate of Compact Object Mergers from Isolated Massive Binary Stars
Authors: Adam P. Boesky, Floor S. Broekgaarden, Edo Berger
Figure caption: Schematic overview of the method used in this paper. Step 1: simulate the evolution of binaries with each combination of parameters from the two-parameter grids (Table 1) using the COMPAS binary population synthesis code. Step 2: distribute binaries from simulations across redshift using a metallicity-specific star formation rate. Step 3: infer the BBH, BHNS, and BNS merger rates from the simulation results of each parameter combination in the two-parameter grids.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: SN velocities measured from the Fe II 5169 Å line as a function of the spectroscopic phase for every event in the sample for which a velocity was obtained (26 events). The black points indicate the velocities at the spectral epoch, plotted with measured velocities of SNe Ic-BL from literature, the iPTF sample (F. Taddia et al. 2019), and the samples from S. Anand et al. (2024) and A. Corsi et al. (2023). Red symbols represent GRB-SNe (K. Iwamoto et al. 1998; P. A. Mazzali et al. 2003, 2006b); magenta represents XRF/X-ray transient-SNe (P. A. Mazzali et al. 2006a; E. Pian et al. 2006; M. Modjaz et al. 2009); blue represents SNe Ic-BL (P. A. Mazzali et al. 2000, 2002); and green represents the “normal” Type Ic SN 1994I (D. N. Sauer et al. 2006).
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Example of the convolution fitting of the Fe II feature for the photospheric phase spectra of SN 2018hsf. The spectrum of the transient is shown in gray, with the fitting region bolded in black. The blueshifted Ic template is shown in red, with the fitting region bolded in red. The reduced chi-square value for the fit is shown (﹩{\chi }_{r}^{2}﹩), along with the blueshifted velocity with respect to the Ic template (v), the Doppler broadened line width velocity (σ), the amplitude (a), and the wavelength range (δ w).
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: The peak v ph for the sample, with the mean velocity (16,100 km s−1) shown with a solid line, and 1σ standard deviation (5600 km s−1) range shown with dashed lines.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption:                       ﹩{M}_{{\rm{bol}}}^{max}﹩ of all SNe in the sample, with the mean magnitude (−18.34 mag) shown with a solid line, and 1σ standard deviation range (0.98 mag) shown with dashed lines.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Parameter Δm −10(r) plotted against Δm 15(r) for 32 events in the sample. We found no correlations between the two parameters, with a p-value of 0.98.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Photospheric phase spectra (black) and the SNID best-match templates (red) for the Ic-BL sample that has not been presented in previous works. The text shows the name of the transient, the observer-frame spectroscopic phase since r-band maximum, and the name of the transient template used for the fitting.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption:                       ﹩{{M}}_{{\rm{r}}}^{\max }﹩ plotted against Δm 15(r) for 34 events in the sample. There is no evidence for a Phillips relation, which is shown for SNe Ia as the black line with the dashed lines representing the errors from C. R. Burns et al. (2011).
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Blackbody temperature and radii evolution for the SNe Ic-BL sample, calculated through the methods reported in Section 6.2.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Bolometric luminosity LCs for the SNe Ic-BL sample, calculated using Lyman BC coefficients (described in Section 6.1). The bolometric luminosity LC of SN 1998bw (A. Clocchiatti et al. 2011) is also shown as comparison.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Upper panel: input driving continuum (F1180) for Mrk 817 (black) and output light curves with fractional DC contributions DC/(disk+DC) = 0.5 (blue) and DC only (red). Each light curve has been normalized to its mean value to aid clarity. The location of window 1 (HJD = 2459177–2459377) is indicated by the vertical dashed lines. Lower panel: the measured delay (ICCF centroid) as a function of the DC fractional contribution to the total light for the full light curve (black) and window 1 (red). Also shown is the measured delay for the wind component against its fractional contribution to the total light (blue) without any DC contribution from the BLR. The horizontal dashed lines indicate the measured delay of the DC component only for the full campaign (black; ≈7.5 days), for window 1 (red; ≈6.9 days), and for window 1 for the wind component only (blue; ≈2.7 days). The horizontal dotted lines indicate the MERs for Models 2 and 3 (black; 11.3 days) and for Model 1 (blue; 2.75 days).
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Computed and observed lags for the entire campaign. Data are from C23 and L24, assuming a lag of 0.6 days between the HST/1144 Å and SWIFT/UVW2 bands. An additional lag of 0.5 days is added to all bands to allow for the lag between the ionizing continuum and the HST/1144 Å band (see the text for details). The horizontal red lines show 1/e wavelength limits on the SWIFT and ground-based bands. The BLR models are identical to the ones shown in similar colors in Figures 3, 5, and 6.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: The computed lags of a partly transparent DW (in green), a partly shielded BLR (in blue), and their emissivity-weighted combination (in magenta). The properties of the various components are marked in the figure. The models are compared with two ways of measuring lags in Epoch 2: frequency-resolved lags (L24) and ICCF–PyCCF lags (this work and J. Montano 2024). Note the sharp rise of the r-, i-, and z-band PyCCF-measured lags, which we interpret as due to the torus dust component (see the text for further explanation).
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Various types of MERs over the Hγ and Hβ line region. Black: integrated-line-luminosity MER (the quantity normally measured in 1D RM campaigns). Red: velocity-resolved line lags. Blue: broadband MER lags that include DC MERs in line-free regions of the spectrum or combinations of velocity-resolved lines and DC emission closer to the line core. This is normally smaller than the MER of velocity-resolved lines, since the MER of the DC is considerably smaller (≈50%) than the MER of the Balmer lines.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Various absorbed SEDs characterized by their optical depths at 1 and 4 Ryd.