adsabs/AstroCLIMB huggingface dataset:
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: The area in the nucleus of IC 5063 with kinematically distorted gas, as seen by the JWST. Highly turbulent regions are indicated with the aid of the velocity dispersion contours of two bright lines of Figure 7: [S IV] and [Ne V]. Contours are shown at 100, 140 170, 220, and 310 km s−1 for [S IV] and 110, 130, 160, and 290 km s−1 for [Ne V]. The biconical outflow is shown with the aid of the velocity contours of [Ne II], for V = 20 km s−1. The outflows along the NW and SE EELR edges are shown with contours of the [Mg V] −600 < V < −300  km s−1 flux image and of the [Ne III] 300 < V < 500 km s−1flux image, with respective contour levels of 3.5 × 10−21 and 9 × 10−21 W m−2. For  [Mg V], the contours are selectively plotted for outflows at and beyond the NW radio lobe. The [Ne III] contours are plotted further away than the SE radio lobe, in regions not already comprised in the high-σ areas because the outflow and the disk cannot be spatially disentangled close to the EELR base. The b1 bow-shock contours are created from the H2 S(4) 220 < V < 360 km s−1image, for a flux of 1.8 × 10−21 W m−2. All contours are plotted over the optical image of the galaxy that is shown in Figure 1, from NASA/ESA/CSA/J. Schmidt.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Line profiles indicative of outflows. All spectra are extracted within 1″ from the indicated location. Upper row panels: Normalized spectra of the shocked gas tracers H2 and [Fe II]. Lower row: Normalized spectra of other ionized gas lines, sorted by IP. Only spectral lines with signal-to-noise ratio >30 are plotted, so that line wings can be reliably compared.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Left-hand panel: Pseudo-slit position angle and width used for the position–velocity diagram creation, plotted over the  [S IV] moment 1 map. The position angle is identical to the major axis of rotation, as derived from the H2 S(1) rotation field. Right-hand panel: Position–velocity diagram along the major axis of rotation. Pixel values below noise have been masked in this diagram. The black solid line shows the rotational velocity in the Hernquist bulge that best characterizes this galaxy (see the text for more details). The black dotted line shows for completion the same velocity because of the BH potential. The positive and negative escape velocities from the Hernquist bulge are also plotted as a function of radius, using white solid lines. An inclination correction is applied to all theoretical velocities, for consistency with the observations.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: First and second order moment maps (velocity and velocity dispersion) of indicative spectral lines, showing regions with distorted kinematics. Pixels with flux values in the noise were not taken into account for the creation of these maps.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Integrated spectrum in the entire mosaic of channel 1 through channel 4 (from top to bottom).
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Summary, shown as a schematic representation, of all identified regions with outflows. The nomenclature follows that in Figures 4 and 5. The disk plane is in gray. The distances and number of clouds per region are indicative. Red and blue arrows indicate outflows receding from the observer or approaching the observer, respectively.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Upper panels: H2 excitation temperature maps. All temperatures are in units of K. Crosses mark the centers of the indicative regions (of 1″ diameter) in which line fluxes were measured for the excitation diagram. The central three crosses are identical to those of all previous Figures. The cross at the SE EELR corresponds to the location of the b1 bow shock. The T ex is shown for the integrated line flux over all velocities, unless otherwise noted (i.e., except for the biconical outflow, shown in the third column). Lower panels: H2 excitation diagram of the above-shown indicative regions.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Left-hand panel: The [Ar V] line ratio as a function of electron density in LTE conditions for different temperatures. Right-hand panel: [Ar V]-based electron density map. Crosses are as in the previous figures. The dashed circle indicates the region where the density values are uncertain due to PSF residuals. Densities are in units of cm−3.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: [Ne III]/ [Ne II] ratio, integrated over all velocities, as an excitation indicator. The circle and crosses are as in Figure 11.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Emissions due to the cruciform artifact.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: H2-to-PAH flux ratio for the S(1), S(2), and S(3) lines probing thermalized gas emission (left-hand panel) and for all lines (right-hand panel). In both maps, the PAH emission comprises the flux in the two detected complexes at 6.2 μm and 11.3 μm.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Detected gas emissions, indicatively grouped by gas phase, in units of 10−20 W m−2. Ionized gas lines are presented in an order of increasing ionization potential. Crosses mark the location of the nucleus and the EELR bases, as derived from the maxima of all ionized gas lines in our data, at rest-frame velocity.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: H2 mass map, in units of solar masses, calculated for the coldest detected gas, probed by S(2) and S(1).
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Continuum images in the medium band of each channel (i.e., ch1 to ch4 from left to right).
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: Detection statistic ﹩{\hat{\beta }}_{{\rm{S}}/\mathrm{GLtL}r}﹩ as a function of signal frequency for the candidates surviving Stage 0. There are 1.2 × 106 such candidates for Vela Jr., 1.0 × 106 candidates for G347.3 below 400 Hz and 3.1 × 106 candidates for G347.3 above 400 Hz. Note that, for G347.3 at around 1000 Hz, there is a “dent,” which indicates that the number of candidates from that frequency region is significantly smaller than the other frequency region. The cause of this is the large difference of power spectral densities between two detectors, amounting on average to ≈10, which causes lower ﹩{\hat{\beta }}_{{\rm{S}}/\mathrm{GLtL}}﹩ values than if the detectors had comparable sensitivities. This is a known effect already highlighted by D. Keitel & R. Prix (2015).
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption:  R (a) distribution for the Vela Jr. searches below 400 Hz. The orange histograms (leftmost) show the distribution of search result candidates. The blue histograms (rightmost) show the distribution of our target-signal population, and its Gaussian fit is the blue dashed line. All result candidates to the left of the red vertical lines are discarded.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Absorption due to the cruciform artifact.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption:  R (a) distribution for the G347.3 searches from 400 to 1300 Hz. The orange histograms (leftmost) show the distribution of search result candidates. The blue histograms (rightmost) show the distribution of our target-signal population, and its Gaussian fit is the blue dashed line. All result candidates to the left of the red vertical lines are discarded.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption:  R (a) distribution for the G347.3 searches below 400 Hz. The orange histograms (leftmost) show the distribution of search result candidates. The blue histograms (rightmost) show the distribution of our target-signal population, and its Gaussian fit is the blue dashed line. All result candidates to the left of the red vertical lines are discarded.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: Computing cost per candidate of 920 putative Stage 1 setups with T coh = 2670 hr, for the Vela Jr. search. The eight red circles are the lowest computing cost setups at a given mismatch. The thick circle with a red “+” is the chosen Stage 1 setup.
Paper: A Case Study of Gas Impacted by Black-hole Jets with the JWST: Outflows, Bow Shocks, and High Excitation of the Gas in the Galaxy IC 5063
Authors: Kalliopi M. Dasyra, Georgios F. Paraschos, Francoise Combes, Polychronis Patapis, George Helou, Michalis Papachristou, Juan-Antonio Fernandez-Ontiveros, Thomas G. Bisbas, Luigi Spinoglio, Lee Armus, Matthew Malkan
Figure caption: Emissions that could be associated with regions of interest, but that cannot be confirmed to be real due to the cruciform artifact and PSF residuals.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: Number of templates searched in 1 Hz bands as a function of signal frequency for different searches. In the legend, we also show the total number of templates searched for each search.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: 90% confidence upper limits on the gravitational-wave amplitude of continuous gravitational-wave signals from Vela Jr. for signals with frequency between 20 and 400 Hz. The red triangles are the results of this search, and we compare them with results from the LVC search of the O3a (R. Abbott et al. 2022a). The dashed blue line at the top shows the age-based upper limit assuming braking index n = 7, and the solid blue line shows the case assuming n = 5. We show the most constraining age limit for Vela Jr., i.e., the one assuming the object is farther away (900 pc) and older (5100 yr). The limit under the assumption that Vela Jr. is young (700 yr) and close-by (200 pc) is 1.7 × 10−23 for n = 7 and 1.4 × 10−23 for n = 5.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: 90% confidence upper limits on the gravitational-wave amplitude of continuous gravitational-wave signals from G347.3 for signals with frequency between 20 and 1300 Hz. The lower red triangles are the results of this search, and we compare them with results from previous searches: the black dashed line is the upper limits from the LVC search of the O3a (R. Abbott et al. 2021e); the blue triangles are Einstein@Home high threshold search results from O2 data (J. Ming et al. 2022); and blue dots are the Einstein@Home subthreshold search results from O1 data (M. A. Papa et al. 2020). The dashed blue line at the top shows the age-based upper limit assuming braking index n = 7, and the solid blue line shows the case assuming n = 5.
Paper: Visual Orbits of Wolf–Rayet Stars. II. The Orbit of the Nitrogen-rich Wolf–Rayet Binary WR 138 Measured with the CHARA Array
Authors: Amanda Holdsworth, Noel Richardson, Gail H. Schaefer, Jan J. Eldridge, Grant M. Hill, Becca Spejcher, Jonathan Mackey, Anthony F. J. Moffat, Felipe Navarete, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Sorabh Chhabra, Isabelle Codron, Jacob Ennis, Tyler Gardner, Mayra Gutierrez, Noura Ibrahim, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Example bisector fit from the ESI data set, HJD: 2459371 of the He II λ5411 emission line (left) and the Gaussian fit of the He I λ5876 absorption line (right). The gray line represents the spectrum, with the blue line showing where the bisector fit was taken. The red dots along the blue lines show where the measurements were taken in order to average and get the center RV. The red line in the right panel indicates the Gaussian fit to the O-star absorption line.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: Blue crosses: measured detection efficiency C(h 0) from the G347.3 signal search-and-recovery Monte Carlos with signal frequencies between 161.5 and 162 Hz. The solid line is the best fit, and the dashed lines represent 95% confidence intervals on the fit. The red line marks the 90% detection confidence level, with the uncertainties introduced by this fitting procedure is ≤5%. The inset shows a zoom around the 90% confidence level.
Paper: Visual Orbits of Wolf–Rayet Stars. II. The Orbit of the Nitrogen-rich Wolf–Rayet Binary WR 138 Measured with the CHARA Array
Authors: Amanda Holdsworth, Noel Richardson, Gail H. Schaefer, Jan J. Eldridge, Grant M. Hill, Becca Spejcher, Jonathan Mackey, Anthony F. J. Moffat, Felipe Navarete, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Sorabh Chhabra, Isabelle Codron, Jacob Ennis, Tyler Gardner, Mayra Gutierrez, Noura Ibrahim, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: The orbital solution for the CHARA measurements (left), along with the measurements of the WR star’s RVs (right). The visual orbit model is in blue, with the black points representing the measurements of the O star moving around the WR star. Red dots show the measurement errors of the interferometry.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: Upper limits on the ellipticity of the Vela Jr. and G347.3. For Vela Jr. we show two curves, corresponding to two distance estimates: 200 and 900 pc. For G347.3, we assume 1300 pc.
Paper: Deep Einstein@Home Search for Continuous Gravitational Waves from the Central Compact Objects in the Supernova Remnants Vela Jr. and G347.3-0.5 Using LIGO Public Data
Authors: J. Ming, M. A. Papa, H.-B. Eggenstein, B. Beheshtipour, B. Machenschalk, R. Prix, B. Allen, M. Bensch
Figure caption: Upper limits on the r-mode amplitude of the two targets. For Vela Jr., we show two curves, corresponding to two distance estimates: 200 and 900 pc. For G347.3, we assume 1300 pc.
Paper: Temporal and Spectral Analysis of the Unique and Second-brightest Gamma-Ray Burst GRB 230307A: Insights from GECAM and Fermi/GBM Observations
Authors: R. Moradi, C. W. Wang, B. Zhang, 冰 张, Y. Wang, 瑜 王, S.-L. Xiong, 少林 熊, S.-X. Yi, W.-J. Tan, M. Karlica, S.-N. Zhang, 双南 张
Figure caption: The correlations between the peak energy, E p(t), and various parameters such as (A) the flux, F  E (t), N(t), (B) photon fluence, (C) photon number, Φ(t), and (D) φ p(E p), are explored in our analysis. The relationship between E p(t) and F  E (t) aligns with the findings of previous studies by E. W. Liang et al. (2004), G. Ghirlanda et al. (2009), and R.-J. Lu et al. (2012). The hardness–fluence correlation (HFC) is illustrated in panel B, while the hardness–intensity correlation (HIC) is shown in panel C. The optimal fitting time interval ranges from ﹩{t}_{{d}_{1}}=7.2﹩ to ﹩{t}_{{d}_{2}}=27﹩ s. The correlation coefficients of 0.94, 0.70, 0.72, and 0.71 demonstrate strong relationships between E p(t) and F  E (t), Φ(t), N(t), and φ p(E p), respectively. The fits for E p(t) with F  E (t), N(t), and φ p(E p) are performed using a logarithmic model: ﹩\mathrm{log}({E}_{{\rm{p}}})=A\,+\,B\cdot \mathrm{log}(x)﹩, where x represents F  E (t), N(t), and φ p(E p).
Paper: Visual Orbits of Wolf–Rayet Stars. II. The Orbit of the Nitrogen-rich Wolf–Rayet Binary WR 138 Measured with the CHARA Array
Authors: Amanda Holdsworth, Noel Richardson, Gail H. Schaefer, Jan J. Eldridge, Grant M. Hill, Becca Spejcher, Jonathan Mackey, Anthony F. J. Moffat, Felipe Navarete, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Sorabh Chhabra, Isabelle Codron, Jacob Ennis, Tyler Gardner, Mayra Gutierrez, Noura Ibrahim, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Different aspects of evolution of the WR 138 system are shown in these three panels. In each of the figures, the blue and red bold lines represent the model with the best-matching initial parameters with thinner lined models that match the observed masses and period within 3σ uncertainties. The mean model is shown as a thick dashed line, while the mode model is shown as a thick solid line; note in the lower panels the mean and mode models are almost identical. The lower panels are for the lower initial mass evolutionary pathway, while the upper panels are for the higher initial mass evolutionary pathway for WR 138. In the left panels, we show the Hertzsprung–Russell diagram for the past and future evolution of the WR star. In the central panels, we show the primary radius in light/dark blue and the orbital separation in yellow/red. In the right panels, we show the mass of the primary in light/dark blue and the mass of the secondary in yellow/red.