adsabs/AstroCLIMB huggingface dataset:
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Predicted M 500c and λ derived from MaDCOWS2 S/NP-observable relations vs. the published values from external catalogs. These predicted values are derived using Equation (2) with the best fit values in Table 3. The red lines are the one-to-one lines for each property. ﹩{M}_{500{\rm{c}}}^{\mathrm{ACT}}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{SPT}}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{PSZ}2}﹩, and ﹩{M}_{500{\rm{c}}}^{\mathrm{eRASS}}﹩ are given in units of 1014 M ⊙.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Positional offset comparison with external catalogs, where color indicates the density of points. The top two rows show the radial offset d as a function of MaDCoWS2 photometric redshift. The lines denote constant physical radii, as indicated.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: LS DR9 grz images of the 12 highest S/NP detections in the MaDCoWS2 catalog. The size of the images is 1 Mpc × 1 Mpc. In each panel, we provide the name of the cluster candidate, the name of its ACT counterpart, our S/NP, and our photometric redshift (or spectroscopic redshift if available from an external catalog.)
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Radial offset distribution. The distribution is smoothed by a Gaussian filter with a standard deviation of 0.075 Mpc.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Number of simulated halos as a function of redshift for different virial mass thresholds.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The ionization rate by photons with E ph = 5 keV (upper left), 10 keV (upper right), 20 keV (lower left), and 40 keV (lower right) at the peak of flare with ﹩{E}_{\mathrm{flare}}={10}^{35}﹩ erg. The black lines represent the disk scale height described as ﹩H(R)=\sqrt{2}{c}_{s}(R)/{{\rm{\Omega }}}_{K}(R)﹩, where c  s (R) is the isothermal sound speed and ﹩{{\rm{\Omega }}}_{K}(R)=\sqrt{{GM}/{R}^{3}}﹩ is the Keplerian angular velocity. The white solid line represents z = 0.1R. The orange dashed line is the contour for ζ X = 10−17 s−1.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The photon energy dependence of r crit for (a) z = 0.1R and (b)z = 0. The data are taken at the flare peak. The different colors denote the results for flares with different ﹩{E}_{\mathrm{flare}}﹩. The gray-shaded regions indicate the regions that are not covered by our disk model. The upward triangles indicate the critical radii above which ζ X > ζ CR,0, and vice versa.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The ionization rates at (a) z = 0.1R and (b) z = 0 at the peak of the flare with ﹩{E}_{\mathrm{flare}}={10}^{35}﹩  erg. The different line types represent different photon energy, E ph. The gray solid line is the typical value of cosmic ray ionization rate (A. Dalgarno 2006).
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: Absorption (blue) and scattering (orange) cross sections as a function of energy. The gray lines correspond to the absorption due to gas (dashed) and dust (dotted) components, whose sum yields the total absorption (blue). The scattering cross section is independent of energy (Thomson scattering).
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: Comparison of the ionization rates at the midplane for the case of the flare peak with ﹩{E}_{\mathrm{flare}}={10}^{35}﹩ erg. (a) Our fiducial case with M  d  = 0.01M ⊙ and ϵ = 1. (b) The case with a lower disk mass of M  d  = 0.001M ⊙. (c) The case with a lower settling parameter of ϵ = 0.1.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The X-ray spectra for the corona with T = 3 × 106 K (black solid) and the 10 yr averaged flare with ﹩{E}_{\mathrm{flare},\ \mathrm{ave}}=1.84\times {10}^{34}﹩ erg (blue).
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: Left: the X-ray light curves for ﹩{E}_{\mathrm{flare}}={10}^{35}﹩ erg. The different models are compared with black (this work) and blue (XGEN by WC22) lines. Right: ﹩{L}_{{{\rm{X}}}_{\mathrm{peak}}}﹩ vs. ﹩{E}_{\mathrm{flare}}﹩ for the two models.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: Left: the X-ray light curves over 10 yr. Right: the number of flares per year. The blue dots are the data from our calculation, and the gray solid line follows ﹩N\propto {E}_{\mathrm{flare}}^{-0.8}﹩. The blue and orange lines correspond to the flare-frequency distributions obtained by K. V. Getman et al. (2021) for pre-main-sequence stars and T. Shibayama et al. (2013) for slowly rotating G-type dwarfs (P > 10 days), respectively. The flare number from T. Shibayama et al. (2013) is multiplied by 104 for better visibility.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The photon flux values at 20 keV against ﹩{E}_{\mathrm{flare}}﹩. The black dots show data from our model, which incorporates both thermal and nonthermal components. The blue dots indicate data from the thermal-only case adopted in WC22.
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: Mass estimates for high-redshift galaxies from JWST. Colored points based on photometric redshifts are from N. J. Adams et al. (2023; dark blue triangles), H. Atek et al. (2023; green circles), I. Labbé et al. (2023; open squares), R. P. Naidu et al. (2022; open star), Y. Harikane et al. (2023; yellow diamonds), C. M. Casey et al. (2024; light blue left-pointing triangles), and B. Robertson et al. (2024; orange right-pointing triangles). Black points from B. Wang et al. (2023; squares), S. Carniani et al. (2024; triangles), Y. Harikane et al. (2024; circles) and M. Castellano et al. (2024; star) have spectroscopic redshifts. The upper limit for the most massive galaxy in TNG100 (V. Springel et al. 2018) as assessed by B. W. Keller et al. (2023) is shown by the light blue line. This is consistent with the maximum stellar mass expected from the stellar mass–halo mass relation of P. Behroozi et al. (2020; solid blue line). These merge smoothly into the trend predicted by L. Y. A. Yung et al. (2019b) for galaxies with a space density of 10−5 dex−1 Mpc−3 (dashed blue line), though L. Y. A. Yung et al. (2023) have revised this upward by ∼0.4 dex (dotted blue line). This closely follows the most massive objects in TNG300 (A. Pillepich et al. 2018; red line). The light gray region represents the parameter space in which galaxies were not expected in ΛCDM. The dark gray area is excluded by the limit on the available baryon mass (P. Behroozi & J. Silk 2018; M. Boylan-Kolchin 2023).
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The data from Figures 4 and 6 shown together using the same symbols. Additional JWST data with spectroscopic redshifts are shown from M. Xiao et al. (2023; green triangles) and A. C. Carnall et al. (2024). The data of A. C. Carnall et al. (2024) distinguish between star-forming galaxies (small blue circles) and quiescent galaxies (red squares); the latter are in good agreement with the typical ﹩{M}_{* }^{* }﹩ determined from Schechter fits in clusters (large circles). The dashed red lines show the median growth predicted by the Illustris ΛCDM simulation (V. Rodriguez-Gomez et al. 2016) for model galaxies that reach final stellar masses of M * = 1010, 1011, and 1012 M ☉. The solid lines show monolithic models with ﹩{M}_{* }^{f}=9\times {10}^{10}\,{M}_{\odot }﹩ and t  i  = τ = 0.3, 0.4, and 0.5 Gyr (Equation (5)), as might be appropriate for giant elliptical galaxies. The dotted line shows a model appropriate to a spiral galaxy with t  i  = 0.5 and τ = 13.5 Gyr.
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The stellar masses of quiescent galaxies from T. Nanayakkara et al. (2024). The inferred growth of stellar mass is shown for several cases, marking the time when half the stars were present (small green circles) to the quenching time (midsize orange circles) to the epoch of observation (large red circles). Illustrative star formation histories following Equation (5) are shown as dotted lines with parameters t  i , τ in Gyr noted. We omit the remaining lines for clarity, as many cross. There is a wide distribution of formation times from very early (t  i  = 0.2 Gyr) to relatively late (>1 Gyr), but all of the galaxies in this sample are inferred to build their stellar mass rapidly and quench early (τ < 0.5 Gyr).
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: Measured velocity dispersions of protocluster candidates (J. R. Franck & S. S. McGaugh 2016a, 2016b) as a function of redshift. Point size grows with the assessed probability that the identified overdensities correspond to a real structure: all objects are shown as small points, candidates with P > 50% are shown as light blue midsize points, and the large dark blue points meet this criterion and additionally have at least 10 spectroscopically confirmed members. The MOND mass for an equilibrium system in the low-acceleration regime is noted at right; these are comparable to cluster masses at low redshift.
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The baryonic Tully–Fisher (left) and dark matter fraction–surface brightness (right) relations. Local galaxy data (circles) are from F. Lelli et al. (2019; left) and F. Lelli et al. (2016; right). Higher-redshift data (squares) are from A. Nestor Shachar et al. (2023) in bins with equal numbers of galaxies color coded by redshift: 0.6 < z < 1.22 (blue), 1.22 < z < 2.14 (green), and 2.14 < z < 2.53 (red). Open squares with error bars illustrate the typical uncertainties. The relations known at low redshift also appear at higher redshift with no clear indication of evolution over a lookback time up to 11 Gyr.
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The stellar masses and star formation rates of galaxies from T. Nanayakkara et al. (2024; red symbols). Downward-pointing triangles are upper limits; some of these fall well below the edge of the plot and so are illustrated as the line of points along the bottom. Also shown are objects selected from the TNG50 (A. Pillepich et al. 2019; filled squares) and TNG300 (A. Pillepich et al. 2018; open squares) simulations at z = 3 to cover the same range of stellar mass. Simulated objects with stellar masses comparable to real galaxies are mostly forming stars at a rapid pace. In the higher-resolution TNG50, none have quenched as observed.
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: CMDs created from our final stellar catalogs for Leo P with the F090W, F150W filter pair (left) and F090W, F277W filter pair (right). In the left panel, we mark the regions for the main stages of stellar evolution, including the upper main sequence (MS), young blue and red helium-burning (HeB) stars, the red giant branch (RGB), the red clump (RC), the horizontal branch (HB), and the subgiant branch (SGB). The 11 sources that are cospatial with the H II region within a radius of 0.″72 are marked in red. The brightest of these sources located at the top of the main-sequence powers the HII region. Only three sources in the same region are recovered in the F277W photometry, due to the increased impact of crowding in the LW data. Representative uncertainties are shown on the right in each CMD, and the 50% completeness limits determined from artificial star tests are drawn as dashed blue lines. The F150W data are deeper than the F277W data, and the number of point sources recovered in the F090W − F150W catalog is more than 50% greater than the number in the F090W − F277W data. See Section 2.4 for details.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The ratio of the exposure map calibrated with the f(E)g(E, θ) correction to the MC one at the primary energy of 2 GeV. The left and right panels correspond to the HET exposure ε H and total exposure ε tot ≡ ε H + ε L, respectively. The map is binned according to the Aitoff projection in the Galactic coordinate. The black dashed line represents the celestial equator. The green star in the right panel shows the location of the Vela pulsar.
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: Left: F090W image of the full field of view in the native orientation of the observations. Clockwise from the top left, the NIRCam detectors are B3, B1, B2, and B4. The center of the stellar disk falls on the B1 detector in the upper right of the figure. Right: three-color image zoom-in on B1 with the main stellar body of Leo P. The image is created using the F090W (blue), F150W (green), and F277W (red) filters oriented with N up and E to the left. Note the rich range in object colors, including the redder background galaxies and the bluer colors of the stars in Leo P.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The variations of the observed counts and expected counts between 2 and 20 GeV. The observed counts N obs are marked with blue points. The expected counts with correction N ref,cal and without correction N ref,MC are shown with a green solid line and an orange dashed line, respectively. The expected counts are based on the best-fit models of the data set above 2 GeV from 2016 January to 2023 July.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The enhancement of the variation rates on top of the simple energy-dependent correction. It is derived by dividing the relative MC effective area change rates by the relative acceptance change rate. The θ dependence is weak for the primary energy between 1.6 and ∼3 GeV.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The counts of the HET photon data binned according to the reconstructed energy and inclination angle. The E bins are logarithmic from 1.6 to 20 GeV, while the θ bins match those in Figure 4.
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: Zoom-in on the single H II region in Leo P. Individual well-recovered sources that are cospatial within the H II region are marked in the CMDs in Figure 3. The image is oriented with N up and E to the left, with a vertical extent of 2.″8 corresponding to ∼22 pc at the distance of Leo P.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The time evolution of the simulated HET effective area within various bins of primary energies and inclination angles. The points and error bars correspond to the values and uncertainties of the relative effective area derived from the MC simulation. The dashed line in each subfigure is the linear evolution model.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: Radial profiles of shearing-sheet equilibria for (from left to right) bumps, gaps, drops, and jumps of width W and amplitude ﹩{ \mathcal J }={\rm{\Delta }}{\rm{\Pi }}/{({\rm{\Omega }}W)}^{2}=0.5,1,2﹩ (blue, orange, and green curves). Top row: enthalpy. Middle row: epicyclic frequency squared, κ 2. Minima (dots) and maxima (pluses) of vorticity (and equivalently κ 2) are marked in all rows. Bottom row: the effective potential D inc for marginally stable RWI (offset by k  y  2, see the text).
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: Top left: along the RWI boundary for k  y  H= 0.1 in a CSS bump, numbers ①–③ mark the modes investigated. Other panels: the effective potential D (orange curves, with negative regions shaded) and pressure perturbation Ψ (blue curves for magnitude [thick], real and imaginary parts [thin solid and dashed]) of the numbered modes, with the bump width (green dotted lines) and nominal (Keplerian) location of Lindblad resonances (gray dotted lines) marked. ①: distant Lindblad resonances, with a trapped mode in the Rossby zone. ②: the trapped Rossby mode couples to density waves exterior to nearby Lindblad resonances. ③: no Lindblad resonances since κ 2 < 0, and a “leaky” potential (negative everywhere). This Rayleigh unstable region is not our focus.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: Incompressible RWI growth rate s for (left to right) bump, gap, and step features against scaled enthalpy amplitude ﹩{ \mathcal J }\equiv {\rm{\Delta }}{\rm{\Pi }}/({W}^{2}{{\rm{\Omega }}}^{2})﹩ and the ratio of feature width to azimuthal wavelength, k  y  W. The RWI boundary (dotted yellow), ﹩{ \mathcal J }={k}_{y}W﹩ reference line (dashed yellow), and Rayleigh unstable regions (gray shaded) are shown.
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: SPH simulations of BdHNe: model “30m1p1eb” (top) and “15m1p05e” (bottom) of Table 2 in L. Becerra et al. (2019). Top: the binary progenitor comprises a CO star of mass ≈ 9 M ⊙, produced by a ZAMS star of 30 M ⊙, and a 1.9 M ⊙ NS companion. The orbital period is ﹩\approx 6\,\mathrm{minutes}﹩ and the energy of the SN is 3.26 × 1051 erg. Bottom: the binary progenitor is a CO star of mass ≈ 3 M ⊙, produced by a ZAMS star of 15 M ⊙, and a 1.4 M ⊙ NS companion. The orbital period is ﹩\approx 5\,\mathrm{minutes}﹩ and the energy of the SN is 1.1 × 1051 erg. Each frame corresponds to selected increasing times from left to right with t = 0 s the instant of the SN shock breakout. They show the mass and density on the equatorial plane. The reference system is rotated and translated to align the x-axis with the line joining the binary components. The origin of the reference system is located at the NS companion position. Top: the first frame corresponds to ﹩t=0.6\,\mathrm{minutes}﹩, showing that the particles entering the NS capture region form a tail behind them. These particles then circularize around the NS, forming a thick disk already visible in the second frame at ﹩t=1.3\,\mathrm{minutes}﹩. Part of the SN ejecta are also attracted by the νNS accreting onto it; this is appreciable in the third frame at ﹩t=2.4\,\mathrm{minutes}﹩. Bottom: in all three panels, it can be seen how the material leaves the system almost without being affected by the NS companion. This figure has been produced with the SNsplash visualization program (D. J. Price 2011).
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Accretion rate onto the νNS (left) and the NS companion (right) as a function of time, obtained from SPH simulations of BdHNe with various orbital periods and CO star progenitors. The black curves correspond to binaries formed by a CO star evolved from a ZAMS with M ZAMS = 30 M ⊙ and a 1.9 M ⊙ NS companion. The CO star undergoes collapse, ejecting an SN with an energy of 3.26 × 1051 erg. The red curves correspond to binaries formed by a CO star from a ZAMS star with M ZAMS = 15 M ⊙ and a 1.4 M ⊙ NS companion, where the corresponding SN energy is 1.1 × 1051 erg. We refer to Table 1 for the CO–NS binary properties.