adsabs/AstroCLIMB huggingface dataset:
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: The relationship between the EHD parameter and intrinsic duration T90,i. Gray and reddish-orange symbols represent the SGRB and LGRB samples, respectively, taken from P. Y. Minaev & A. S. Pozanenko (2020). The yellow and green pentagrams correspond to the ME and EE phases of GRB 240619A, respectively, while the yellow and green diamonds represent the ME and EE phases of GRB 211211A.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: Fitting results of the GRB 240619A light curve using the FRED function. The red line represents the best-fit FRED model. Black squares indicate the flux values obtained from spectral fitting in each time bin, while the gray dashed line shows the fit to the flux using a power-law function.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: Local event rate density of short (blue) and long (red) GRBs, along with the value for GRB 240619A (black). The blue and red solid lines represent the empirical fits obtained by H. Sun et al. (2015).
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: Testing the closure relation of the curvature effect in the decay phase of pulses during the ME and EE stages using time-resolved spectral data. Red and black symbols represent the ME and EE phases, respectively. The blue solid line denotes the expected relation ﹩\widehat{\alpha }=2+\widehat{\beta }﹩.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: X-ray afterglow light curves. Gray and blue lines represent the LGRB and SGRB samples, respectively. The red, orange, and green curves correspond to GRB 240619A, GRB 211211A, and GRB 060614, respectively.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: Left: the positions of potential stellar companions in a Hertzsprung–Russell (H-R) diagram, allowed and ruled out by our photometric upper limits, assuming an R. L. Kurucz (1993) H-rich model. We assume solar metallicity, and ﹩\mathrm{log}\,g﹩ is set to four at temperatures below 36,000 K and to five at temperatures above 36,000 K. The single-star evolution predicted by POSYDON is shown for different masses in temperature–luminosity space, and the colors in the background indicate areas of temperature and luminosity space allowed by our nondetections. For MS companions (dotted line), we rule out log(L/L⊙) > 3.35. Because our deepest data are in blue and UV bands, our mass limits are most constraining for less-evolved hot stars. Right: spectral fits to the upper limits of our HST photometry. The pink spectrum represents MS stars with the most constrained luminosity, corresponding to the pink point of the H-R diagram in the left panel. The blue spectrum represents stars with the tightest constraint on luminosity at 13,000 K, which is located at the dark blue point in the left panel. The triangles indicate the upper limits of our observations, which are compared to the synthetic-photometry outputs from the model spectra.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: The probability of a stellar companion below our luminosity limits (blue), nondetectable compact-object companion (black), and companion absence (red) at the site of SN 2012fh according to our POSYDON population-synthesis models, given the luminosity constraints on a possible luminous companion. The gray shaded portion is ruled out by the upper limits on a possible companion luminosity in this work. At left, we assume all massive core-collapse progenitors to result in a successful explosion, whereas (right) we accept only the successful explosions. We show the case of no age constraint for the SN (dotted–dashed line), and also including an age constraint of 8–20 Myr from the surrounding region (solid line).
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: The relationship between initial stellar mass (Minit) and final BLAP mass (MBLAP) for our binary evolution models. The models separate into two distinct populations based on their initial binary separation. A linear regression fit is shown for each group: a shallow trend for close separation systems (red line) and a much steeper, stronger correlation for wide separation systems (blue line). The color of each point corresponds to its population synthesis weight (﹩\mathrm{log}{W}_{\,\rm{pop}\,}﹩), as indicated by the color bar.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: A corner plot illustrating the distributions and pairwise correlations for key parameters of our simulated BLAPs. The parameters shown are the initial mass (Minit), final BLAP mass (MBLAP), orbital period (Porb), BLAP lifetime, initial mass ratio (qinit), and age. The diagonal panels display the 1D histograms for each parameter, annotated with their mean (μ) and standard deviation (σ). The off-diagonal panels show the 2D scatter plots for each parameter pair. The models are separated into primary BLAPs (red dots) and secondary BLAPs (orange triangles), with their corresponding distributions in the histograms shown by the red and orange outlines, respectively. The filled gray histogram in the background represents the combined statistical distribution of all models together, serving as a reference for the overall trends.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: The Kiel diagram displaying the effective temperature vs. surface gravity of helium-burning BLAP candidates. Observed BLAPs are shown as crosses: black crosses denote objects with ﹩\mathrm{log}({N}_{{\rm{He}}}/{N}_{{\rm{H}}})\gt ﹩ −2, while orange plus symbols denote objects with ﹩\mathrm{log}({N}_{{\rm{He}}}/{N}_{{\rm{H}}})\,\leqslant \,﹩−2. He core burning models are indicated by blue circles (203 models), and He shell burning models are indicated by red asterisks (6 models).
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: The distribution of pulsation periods as a function of effective temperature for our model predictions and observed BLAPs. Our theoretical models are represented by blue dots for core helium-burning models and red asterisks for shell helium-burning models. Observed BLAPs are plotted with error bars and are distinguished by helium abundance: black crosses denote helium-rich objects with ﹩\mathrm{log}({N}_{{\rm{He}}}/{N}_{{\rm{H}}})\gt -2﹩, while orange plus signs indicate helium-poor objects with ﹩\mathrm{log}({N}_{{\rm{He}}}/{N}_{{\rm{H}}})\leqslant -2﹩.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: Helium abundance [He/H] vs. effective temperature log(T/K). Blue dots represent our 203 core helium-burning models, while red asterisks show the 6 shell helium-burning models. Observed BLAPs are plotted with error bars and are distinguished by helium content: black crosses denote helium-rich objects with ﹩\mathrm{log}({N}_{{\rm{He}}}/{N}_{{\rm{H}}})\gt -2﹩, and orange plus signs indicate helium-poor objects with ﹩\mathrm{log}({N}_{{\rm{He}}}/{N}_{{\rm{H}}})\leqslant -2﹩.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: Temporal distribution of BLAPs in the Milky Way based on our population synthesis calculations. The total number of BLAPs (red circle) is approximately 14,351, comprising 12,799 primary stars (green triangles) and 1551 secondary stars (blue squares).
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: The upper panel: the backward ejecta luminosities summing over bands hν = 100.0–1584.9 eV. The lower panel: the forward ejecta luminosities summing over bands hν = 100.0–1584.9 eV. Green lines are the fiducial multigroup simulation H1_md_v0.1c (H = R*, Σdisk ∼ 104 g cm−2); purple lines are the fiducial disk but with a lower incident velocity of v* = 0.07c; red lines are the simulation with lower disk surface density H1_ld_v0.1c (Σdisk ∼ 103 g cm−2); blue lines are the disk with larger scale height H3_md_v0.1c (H = 3R*); yellow lines are a disk with larger scale height and low surface density (H = 3R*, Σdisk ∼ 102 g cm−2); gray lines are from the optically thin disk with larger scale height (H = 3R*, τdisk ≲ 10). The thick dotted lines in the backward ejecta rising and forward decay are the fitting according to Equations (8) and (9). The x-axis time sets the peak bolometric luminosity time to be zero.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Snapshots of estimated broadband SEDs from the H1_md_v0.1c multigroup dynamic run. We drop the last group of 4 keV to infinity. The time label is the time since the star is at the disk midplane. The first plot (upper panel) is the backward ejecta. In the inset plot, we plot the shape of the gray light curve as the solid gray line; the y-axis is log-spaced and labeled, and the x-axis is linear-spaced and not labeled. The star marks correspond to the sum of νLν of all frequency groups from the multigroup simulation, i.e., an estimation of bolometric luminosity from multigroup run. They are higher than the gray RHD run values due to the frequency-dependent opacity. The second plot (lower panel) is the forward ejecta. The inset figure shows its “hardness–luminosity” cycle. We defined a “soft X-ray to UV-optical” ratio as the ratio of luminosity above and below 250 eV, which is the x-axis. The y-axis shows luminosity above 250 eV. The solid line and filled data points include emission from a standard, thin accretion disk; the dashed line and hollow data points are directly from the simulation.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: SED snapshots from the low optical depth disk. The first plot is from the backward ejecta, and the second plot is from the forward ejecta. The time labels are the time since the star is at the disk midplane. The solid lines and circles are calculated from the dynamic multigroup run. The dashed line and hollow circles are from the postprocess multigroup run, i.e., the radiation quasi steady state with Compton scattering. The gray shaded region labels the proposed UVEX far-UV band.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: The SED snapshots from H1_ld_v0.1c backward ejecta in the postprocessing run restarting from t = 5.0 minutes after the star is at disk midplane. The blue line is from the beginning of the postprocessing run, equivalent to the dynamic run results. The other colored lines show series of SEDs when radiation evolves to a quasi steady state, so they are similar. The solid lines show the dynamic run without Compton scattering; the dashed lines show the dynamic run with Compton scattering. The thick gray solid line shows a single blackbody spectrum at T = 1.9 × 105 K for reference. The time label is the time since the star is at disk midplane.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: The numerical solutions for density (left) and pressure (right) of the polytrope star in the simulation. The density and pressure are normalized to density scaling unit ρ0 = 7.8 × 10−7 g cm−3 and pressure scaling unit ﹩{P}_{0}={\rho }_{0}{v}_{0}^{2}=8.1\times 1{0}^{7}\,\mathrm{dyne}\,{\mathrm{cm}}^{-2}﹩. The gray dashed lines show the ram pressure of the disk midplane. The dots show 32 interpolated points between x/l0, y/l0 = [0.001, 0.313], roughly corresponding to our highest-resolution region near the star; 11 points are closely overlapping at the coordinate M/M⊙ = 1.0.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Quasi-steady-state SEDs in postprocess run for H1_ld_v0.1c. The first plot is for the backward ejecta, and the second plot is for the forward ejecta. In each plot, the solid lines and filled circles are quasi-steady-state SEDs without Compton scattering; the dashed lines and hollowed circles are quasi-steady-state SEDs with Compton scattering. The four sets of dashed and solid lines are with colors corresponding to four restarting times since the star is at disk midplane: t = 3.5 minutes (red), t = 5.0 minutes (green), t = 7.9 minutes (blue), and t = 10.1 minutes (yellow). The gray solid line shows single-temperature blackbody spectrum for reference; the dotted gray line shows a fitting of the Compton tail with slope labeled by the text.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: The multigroup Planck mean opacity from TOPS (J. Colgan et al. 2016) for fixed density ρ = 10−10 g cm−3 (solid lines) with solar abundance. This retrieval includes 10 photon frequency groups that are logarithmically spaced between 10−3 and 4 keV (marked by dots). Each line corresponds to a specific gas temperature: 3.16 × 104 K (deep blue), 105 K (light blue), 3.16 × 105 K (green), 106 K (orange), and 3.16 × 106 K (red). The dotted lines with the same color correspond to free–free opacity for the same gas temperature. The gray dashed line labels κs = 0.34 g−1 cm2.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Density and radiation energy density snapshot from collision with a low optical depth disk at t = 3.5 minutes. The left plot shows the gas density, and the middle and right plots are radiation energy density maps for hν = 100.0 eV and hν = 251.2 eV energy groups. Similar to Figure 9, the ray effect of radiation energy density shows up in the backward ejecta direction, where the background gas is optically thin.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Evolution of νLν of five photon frequency groups: 40 eV (red), 100 eV (orange), 250 eV (green), 630 eV (blue), and 1.58 keV (purple) for the backward ejecta (upper) and forward ejecta (lower). The time axis is the time since the star is at the disk midplane. The gray solid line in each plot shows the bolometric luminosity measured in the gray RHD simulation, which can underestimate the bolometric luminosity compared to the multigroup simulation.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Left: Heyer–Keto plot showing the variation of σv/R0.5 with surface density Σmol. Leaves are plotted in blue and branches in orange, with their brightness scaled by a Gaussian KDE reflecting the smoothed density distribution. Dotted gridlines indicate fixed Pturb with 1 dex spacing. The dashed and solid black lines represent the boundaries for structures in virial equilibrium (αvir = 1) and energy equipartition (αvir = 2) in the absence of external pressure. A linmix regression to the leaf sample, giving ﹩{\sigma }_{{\rm{v}}}/{R}^{0.5}\propto {{\rm{\Sigma }}}_{{\rm{mol}}}^{0.42\,\pm \,0.01}﹩, is shown in red. The median bootstrapped leaf uncertainty is given by an error bar in the bottom right. Right: comparing the Heyer–Keto relation in our leaf sample against the literature catalogs of E. Rosolowsky et al. (2021; 90 pc resolution, extragalactic GMCs with 12CO), M. Heyer et al. (2009; ≤ 3 pc resolution, Galactic GMCs with 13CO), and J. Sun et al. (2020; 90 pc, extragalactic beam-scale measurements with 12CO). Each distribution is smoothed and visualized with a 2D Gaussian KDE at the 16%, 50%, and 84% density contours. Structural decompositions, unlike the beam-scale approach, occupy a similar region of the parameter space despite observing at very different scales.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Left: unextrapolated virial parameter against intensity for internal traces of individual leaves (blue) and branches (orange). Each trace represents a single structure for which αvir is continuously recalculated as we raise the contour in ΔI = 0.1 K intensity steps. The traces are cut where they contain fewer pixels than half the beam size (Ω = 0.2″2 = 29 pix). We exclude 55 leaves that span < 0.5 K in intensity. Binned medians are shown in black, with their 16–84% ranges in gray. The dashed, horizontal lines show αvir = 1 and 2. A beam-sized Gaussian model with realistic noise modeling is shown in red, with the 16–84% range of 2,000 draws shaded. Right: the same as the left panel, but normalized from the minimum to the maximum intensity of each structure.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Structure velocity dispersion against radius for all leaves (blue) and branches (orange) in the dendrogram. Each point’s lightness is scaled by a KDE as in Figure 4. Bins of 0.15 dex are shown with their medians in black and 16–84% ranges in gray. A linmix fit to the centers of bins above the completeness limit gives σv ∝ R0.58 ± 0.04, plotted in red. We show N. Krieger et al.'s (2020) CO(1 − 0) fitted relations for the center of NGC 253 (pink) and the Milky Way (green) as dotted lines, with M.-A. Miville-Deschênes et al.'s (2017) fit for the Milky Way disk as a green dashed line. The estimated 50% completeness limits (Section 3.3) are demarcated by the hatched boundaries.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: The ratio Rvir = αchild/αparent plotted against structure parameters for all leaves (blue) and branches (orange) in the dendrogram, analogous to Figure 4 (top row), Figure 5 (middle row), and Figure 6 (bottom row). Bins are the same as in those figures and point lightness is similarly scaled by a Gaussian KDE. The dashed, horizontal lines in gray show ﹩{\mathrm{log}}_{10}\left({R}_{{\rm{vir}}}\right)=0﹩, below which structures are more bound than their parents.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Linear regression linmix fit slopes resulting from varying dendrogram parameters. Each row shows results for a different scaling relation: αvir–R (Figure 4), σv–R (Figure 10), and Heyer–Keto (Figure 11). For each column, we have varied the parameter on the x-axis while keeping the others constant. Canonical parameter values are the same as in Figure 12, with the corresponding slopes and standard deviations marked by the red horizontal lines and shaded regions.