adsabs/AstroCLIMB huggingface dataset:
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: The cluster hierarchy (middle panel) and condensed cluster hierarchy (right panel) constructed by HDBSCAN for a sample data set (left panel). The sample data set contains three regions of densely clustered points along with random noise. The cluster hierarchy is constructed by applying successive density cuts. Each branch of the tree represents a cluster of points selected above some density cut. The condensed cluster hierarchy shows the cluster hierarchy after clusters smaller than the minimum cluster size are discarded.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: The selection of clusters from the condensed cluster hierarchy with the excess-of-mass (EOM, top row) and leaf (bottom row) methods. Selected branches of the cluster hierarchy are circled in red in the left panels, and the corresponding set of cluster points are shown in color in the right panel, while noise points are gray. The EOM method selects the clusters that persist for the greatest range of density cuts, while the leaf method selects the “leaves” of the cluster hierarchy, i.e., the smallest surviving clusters.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Area and median LAE overdensity (δ LAE) for the structures selected with HDBSCAN (top) and from the GS map (bottom) in the TNG300 slices compared to those in observations. Solid lines indicate the median values of each property. As with the structures selected from the VT map, the properties of the objects in the simulation and observations are similar.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Descendant masses of the individual protoclusters for all three samples, after applying appropriate corrections to the mass calculated with Equation (6).
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Descendant mass estimated according to Equation (6) compared to the true descendant mass for structures selected with HDBSCAN (left) and from the GS map (right). The dashed lines represent a 1-to-1 relation of estimated and true mass whereas the solid lines represent the median ratio of the two.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Similar to Figure 10, but showing the 2D skeletons extracted with multiple persistence thresholds.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: As Figure 10, but zoomed in on the region surrounding a massive protocluster.
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: Evolution of the Hα line profile as obtained from the FLARIX model and MSDP observations. Different colors represent selected line profiles recorded up to the peak of H3 (P3 profile at 10:21:41.5 UT). Left panel: FLARIX profiles; middle panel: FLARIX profiles with a filling factor FF = 0.20; right panel: MSDP observational profiles. The dashed line indicates the preflare profile (synthetic in the left and middle panels, observational in the right panel). The quiet chromosphere profiles: VAL-C with microturbulence equal to 6 km s−1 (left and middle panels) and measured near the flare for MSDP observations (right panel). Synthetic flaring and preflare profiles were calculated with microturbulence equal to 16 km s−1. All profiles are for μ = 0.56. The spectrum range is ±1.2 Å (analogous to Figure 3).
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: Comparison of observed, calculated, and modified using the filling factor profiles of the Hα line at 10:21:41.5 UT (P3 peak). Profiles are color coded: orange solid line—P3 FLARIX (with microturbulence equal to 16 km s−1); red solid line—observed profile of the P3; pink solid line—observed profile of an activated area (the profile was measured in the close periphery of the flaring kernel); violet dashed line—preflare observed; light-blue dashed line—FLARIX preflare (the profile was calculated using the modified VAL-C model); green dashed line—P3 FLARIX profile modified applying the filling factor (FF = 0.20); dark-blue thick dashed line—P3 FLARIX profile after sampling with step equal to 0.4 Å (squares show the wavelengths of the sampling points) modified applying the filling factor (FF = 0.20); black dotted line—quiet chromosphere profile observed near the flare. All profiles are for μ = 0.56.
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: Two light curves depict the onset of the C1.6 flare at 10:21 UT on 2012 September 10. Upper panel: RHESSI HXR 20–34 keV light curve (data demodulated to 0.25 s time resolution). Lower panel: MSDP Hα light curve at the line center (0.05 s time resolution). The intensity of the Hα light curve is presented in units of the intensity of the quiet chromosphere (QCh) located near the flaring kernel. Both curves underwent smoothing using a 1 s wide box car. Gray (marked as H1, H2) and violet (marked as H3 and H4) arrows indicate the maxima of pulses of the HXR emission recorded within the 20–34 keV energy range (marked analogous to K. Radziszewski et al. 2020). Label P3 indicates the moment of measurement of the Hα profile (during the maximum of the H3 pulse) analyzed here (see also Figures 3, 6, and 8). Two orange vertical solid lines delineate the time interval for parameters of NTE beams prepared for modeling with the FLARIX code. Two green dashed vertical lines indicate the 8.25 s long time interval of the numerical model of the flaring emission’s evolution.
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: Hα line center light curves derived from the FLARIX model (panel (c)) and MSDP observations (panel (d)), along with the energy flux of NTE (panel (b)) and the RHESSI 20–34 keV light curve (panel (a)), over the 8.25 s interval of FLARIX simulations (10:21:36 UT to 10:21:44.25 UT). The solid line in panel (c) represents the synthetic Hα line center light curve for the modified VAL-C model (corresponding to the “FLARIX preflare” profile), whereas the dotted line shows the light curve for simulations for the standard VAL-C quiescent chromosphere model. The gray and red arrows indicate the moments of measurement for the P(max) and P3 Hα profiles, respectively.
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: MSDP Hα line profiles: MSDP P(max) (gray), MSDP P3 (red), “MSDP activated” (orange), “MSDP preflare” (green), and quiet chromosphere (black), were measured, respectively, at 10:21:39.95 UT, 10:21:41.50 UT, and 10:20:00.00 UT. The moment of measuring the P3 profile is indicated by a red arrow in Figures 1, 4, and 7. Small squares denote the wavelengths of subsequent channels of the MSDP spectrograph, separated by 0.4 Å.
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: Parameters of NTEs and HXR light curve obtained from RHESSI data. From the top: (a) power-law index of the electron energy distribution (δ); (b) low-energy cutoff of the electron distribution (E  c ); (c) NTE flux; (d) total flux of NTE energy (flux E); (e) RHESSI 20–34 keV light curve at 10:21:36 UT–10:21:52 UT, on 2012 September 10. The violet arrow indicates the maximum of the H3 HXR pulse. The red arrow indicates the moment of measurement of the Hα P3 profile, as shown in Figures 3, 6, and 8. The gray arrow indicates the moment of measurement of the P(max) Hα profile at the local peak of the emission in the Hα line center at 10:21:39.95 UT (as shown in Figures 3 and 6).
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: MSDP Hα line center image captured during the H3 pulse of the HXR emission, amid the impulsive phase of the C1.6 flare on 2012 September 10, at 10:21:41.5 UT. The black square denotes the location of the flaring profile P3 presented in Figures 3, 6, and 8. The empty square indicates the location where the “MSDP activated” profile was measured. Both squares correspond in size to individual pixels of the MSDP image. The pixel size is 1.″6 × 1.″6. The 5″ long bar is in the upper-left corner. The direction of solar North is denoted by the white arrow in the upper-right corner. Coalignment of the Hα image with UV and X-ray images is shown in the previous paper (K. Radziszewski et al. 2020) in Figure 1.
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: Comparison of the temperature distributions of the modified VAL-C model (red dashed line) and the standard VAL-C model (solid line). The modified VAL-C model with the enhanced temperature in the upper part of the chromosphere was utilized for computing the “FLARIX preflare” profile depicted in Figures 6 and 8.
Paper: First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Krzysztof Radziszewski, Petr Heinzel, Jana Kašparová, Michalina Litwicka, Arkadiusz Berlicki, Paweł Rudawy, Robert Falewicz
Figure caption: Impact of the subsampling on the flaring Hα line profile modeled using the FLARIX code. The black solid line represents the modeled flaring Hα line (calculated without microturbulence), while the red dashed line shows the same line profile reconstructed using data (marked by red squares) sampled every 0.4 Å (as in the applied MSDP spectrograph).
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: The overall reflection energy spectrum (a) and the Fe Kα–line energy spectrum (b). The spectra in both panels are produced using the fiducial model with the default parameters v ∞ = 0.35c, R acc = 4 R  g , H LP = 10 R  g , θ half = π/5, and i = 0 (face-on). The x-axis in panel (a) is the observed energy of the photon (in kiloelectronvolts), while that in panel (b) is the energy shift of the photon g = E obs/E emit, where E emit = 6.7 keV. The y-axes in both panels are the normalized fluxes. The black solid line denotes the total reflection energy spectrum, with the colored curves showing contributions from reflections of different orders: orange—photons that have undergone one reflection; blue—photons that have undergone two reflections; and green—photons that have undergone three or more reflections. For the blue curve in panel (b), we further decompose it into two components: red dotted curve—coronal photons are only scattered in the first reflection, with the scattered photons then producing Fe Kα photons in the second reflection; and red dashed line—coronal photons have already produced Fe Kα photons in the first reflection, with the Fe Kα photons being scattered in the second reflection.
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: Fe Kα line spectrum dependence on the wind terminal velocity v ∞. The color scheme and line styles are the same as in Figure 3. Panel (b) uses the default parameter set (the same as in Figure 3), while the other two panels have different v ∞. One can see that increasing v ∞ increases both the blueshift of the primary peak and the redshift of the secondary peak, as well as increasing the separation but decreasing the flux ratio between the secondary and primary peaks. For very low v ∞, the two peaks merge into one.
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: The wind radial velocities with different v ∞ and R acc (solid curves; with θ half = π/5) in comparison to the Keplerian rotation velocity (dashed red curve). The maximum radial velocity of the wind is determined by v ∞, and R acc controls the wind acceleration profile. The wind radial velocity dominates over the rotation velocity ρ ≳ 5 R  g .
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: A schematic diagram showing how the photons emitted by a BH corona are reflected multiple times inside the super-Eddington funnel surrounded by optically thick wind.
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: Fe Kα line spectrum dependence on the half-open angle θ half. The color scheme and line styles are the same as in Figure 3. Panel (b) uses the default parameter set (the same as in Figure 3), while the other two panels have different θ half. As θ half increases, the flux ratio between the secondary and primary peaks decreases, and the separation between the two peaks increases.
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: Fe Kα line spectrum dependence on the wind acceleration radius R acc. The color scheme and line styles are the same as in Figure 3. Panel (b) uses the default parameter set (the same as in Figure 3), while the other two panels have different R acc. As R acc increases, the wind has a slower acceleration, so increasing R acc produces a similar effect as decreasing v ∞.
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: Fe Kα line spectrum dependence on the height of corona H LP. The color scheme and line styles are the same as in Figure 3. Panel (b) uses the default parameter set (the same as in Figure 3), while the other two panels have different H LP, as indicated in the titles. A higher corona increases the blueshift of the primary peak and reduces the flux ratio between the secondary and primary peaks.
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: Fe Kα line spectrum dependence on the observer inclination i. The color scheme and line styles are the same as in Figure 3. Panel (a) uses the default parameter set (the same as in Figure 3), while panel (b) uses the same parameters but is viewed along the funnel wall (edge-on; i = θ half = π/5). The primary peak of the edge-on case is less blueshifted.
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: Comparison of the Fe Kα line profiles with similar ΔE/E rest and F 21 from the thin-disk sample (dashed–dotted line) and super-Eddington simulations (solid line). We show the line profiles that have very different ΔE/E rest and F 21 in panel (a) and those that have similar ΔE/E rest and F 21 in panel (b). The model parameters are listed below. (a) Thin disk 1: H LP = 11.3 R  g , i = 25.°0; thin disk 2: H LP = 6.8 R  g , i = 19.°3; super-Eddington disk 1: v ∞ = 0.2c, θ half = 0.22π, R acc = 8 R  g , and H LP = 25 R  g ; super-Eddington disk 2: v ∞ = 0.4c, θ half = 0.18π, R acc = 4 R  g , and H LP = 25 R  g . (b) Thin disk 1: H LP = 14.2 R  g , i = 44.°9; thin disk 2: H LP = 18.6 R  g , i = 70.°3; super-Eddington disk 1: v ∞ = 0.35c, θ half = 0.15π, R acc = 12 R  g , and H LP = 17.5 R  g ; super-Eddington disk 2: v ∞ = 0.35c, θ half = 0.17π, R acc = 14 R  g , and H LP = 17.5 R  g .
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: The morphological comparison of the double-peak Fe lines from thin disks and super-Eddington disks. For each panel, the x-axis is the flux ratio between the secondary and primary peaks, and the y-axis is the energy difference between the two peaks normalized by the rest-frame energy of the Fe line. The super-Eddington disk Fe lines are denoted using colored points with dot markers, with the color scale representing the values of (a)v ∞, (b)R acc, (c)H LP, and (d)θ half in each panel, respectively. The thin-disk Fe lines are denoted using gray points with plus markers, with the color scale representing the inclination of the observer in panels (a), (b), and (d). In panel (c), we use the color to represent the corona height. In panel (a), we mark the positions of the four lines plotted in Figure 12 (a) using circle markers and the four lines plotted in Figure 12 (b) using square markers. The colors of these markers are the same as the line colors in Figure 12. Furthermore, we mark the double-peaked Fe line observed in BHB 4U 1543–47 using the yellow star marker in panel (a).
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: The dependence of (a) ΔE, (b) F 21, (c) ΔE × F 21, and (d) ΔE × F 21 weighted by the occurrence rate of the double-peak line feature on the four model parameters v ∞, R acc, H LP, and θ half. The color in each grid is the averaged 2D value of the quantity for the combination of the two parameters on the x- and y-axes (while the other two parameters take values with equal chances). The bar plots show how the averaged 1D values for the quantity depend on the parameter on the x-axis (while the other three parameters are not fixed).
Paper: Modeling Multiple X-Ray Reflection in Super-Eddington Winds
Authors: Zijian Zhang, 子健 张, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García, Erin Kara, Riley Connors, Megan Masterson, Yuhan Yao, Thomas Dauser
Figure caption: Spectra from a NuSTAR observation of 4U1543–47 during the 2021 outburst phase fitted using the tbabs*(diskbb+nthcomp) model. In the top panel, the black and red data points show the unfolded spectra from FPMA and FPMB. For a better visual effect, we only show the modeled FPMA spectrum (blue solid curve), with its decomposed components diskbb (blue dotted line) and nthcomp (blue dashed line). The bottom panel shows the residual between the observed and the modeled spectra.