adsabs/AstroCLIMB huggingface dataset:
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Redshift vs. M UV. The magnification correction is applied for the lensed sources. The red circles represent our spec-z-confirmed sources in UNCOVER at z ≥ 8.5, efficiently increasing the sample at the faint (M UV ≳ − 19) and high-redshift (z ≳ 9.5) regime. The gold pentagons and the black squares show recent JWST spectroscopic results from other field surveys such as JADES (e.g., A. J. Bunker et al. 2023), FRESCO (e.g., P. A. Oesch et al. 2023), and CEERS (e.g., S. L. Finkelstein et al. 2023), where the values are taken from K. N. Hainline et al. (2024). The blue triangles denote recent JWST/NIRSpec observation results for high-redshift lensed galaxies (C. C. Williams et al. 2023; T. Y.-Y. Hsiao et al. 2024). The gray crosses indicate the photometric candidates with NIRCam publicly available in JADES v1.0 catalog (K. N. Hainline et al. 2024).
Paper: Fast and Flexible Inference Framework for Continuum Reverberation Mapping Using Simulation-based Inference with Deep Learning
Authors: Jennifer I-Hsiu Li, Sean D. Johnson, Camille Avestruz, Sreevani Jarugula, Yue Shen, Elise Kesler, Zhuoqi (Will) Liu, Nishant Mishra
Figure caption: Evaluation results of testing data. The top row shows the comparison between the true and predicted values along with the mean absolute error (MAE), the middle row shows the distribution of the difference between the true and predicted values, and the bottom row shows the distribution of the difference between the true and predicted values, normalized by the 1σ uncertainties of the SBI posterior. The red lines in the top row trace the 1:1 relation, and the solid (dotted) black lines in the middle and bottom rows denote the median (and 16th, 84th percentile) of the distributions. The blue curves in the bottom panels show the best-fit Gaussian, with the width of the Gaussian noted in the upper right corner. The trained SBI model can constrain M BH and ﹩\dot{M}﹩ to ∼0.08 dex, and cos(i) to 0.01 (a few degrees in the prior range i = 0°–45°).
Paper: Fast and Flexible Inference Framework for Continuum Reverberation Mapping Using Simulation-based Inference with Deep Learning
Authors: Jennifer I-Hsiu Li, Sean D. Johnson, Camille Avestruz, Sreevani Jarugula, Yue Shen, Elise Kesler, Zhuoqi (Will) Liu, Nishant Mishra
Figure caption: Accuracy of the cos(i) (top) and ﹩\mathrm{log}{M}_{\mathrm{BH}}\dot{M}﹩ (bottom) prediction as functions of the “expected” DRW parameters. The color of each point shows the deviation from the truth, and the black points indicate the failed evaluation. The Pearson-r correlation coefficient between the prediction accuracy and τ DRW/﹩{{SF}}_{\inf }﹩ is listed in the top right corner of each panel; the black texts show r with a p-value <0.05 (statistically significant), and the gray text shows r with a p-value >0.05 (statistically insignificant). The accuracy of the ﹩\mathrm{log}{M}_{\mathrm{BH}}\dot{M}﹩ prediction is more correlated with the expected DRW damping timescale, and the accuracy of cos(i) prediction is more correlated with ﹩{{SF}}_{\inf }﹩, suggesting the neural network has extracted features related to the damping timescale and variability.
Paper: Fast and Flexible Inference Framework for Continuum Reverberation Mapping Using Simulation-based Inference with Deep Learning
Authors: Jennifer I-Hsiu Li, Sean D. Johnson, Camille Avestruz, Sreevani Jarugula, Yue Shen, Elise Kesler, Zhuoqi (Will) Liu, Nishant Mishra
Figure caption: Rank distributions from SBC, from left to right panels, are cos(i), M BH, and ﹩\dot{M}﹩. The gray shaded areas indicate the 99% variance of a uniform distribution, i.e., a well-calibrated inference should only have one bar outside of the gray area. The SBC test indicates the posterior is robust for M BH and ﹩\dot{M}﹩ and slightly underestimated for cos(i).
Paper: Fast and Flexible Inference Framework for Continuum Reverberation Mapping Using Simulation-based Inference with Deep Learning
Authors: Jennifer I-Hsiu Li, Sean D. Johnson, Camille Avestruz, Sreevani Jarugula, Yue Shen, Elise Kesler, Zhuoqi (Will) Liu, Nishant Mishra
Figure caption: Posterior distribution of ﹩{M}_{\mathrm{BH}}\dot{M}﹩ and i from SBI and traditional inference methods. The histograms show results from 10 different sets of testing light curves with the same BH parameters, as described in Section 4.2. The dashed lines show the median of the combined posteriors.
Paper: Fast and Flexible Inference Framework for Continuum Reverberation Mapping Using Simulation-based Inference with Deep Learning
Authors: Jennifer I-Hsiu Li, Sean D. Johnson, Camille Avestruz, Sreevani Jarugula, Yue Shen, Elise Kesler, Zhuoqi (Will) Liu, Nishant Mishra
Figure caption: Evaluation results of testing data with large filter gaps (Section 5.1). Figure description is the same as Figure 3. The trained SBI model can constrain M BH and ﹩\dot{M}﹩ to ∼0.09 dex, and i to ≲10°.
Paper: Fast and Flexible Inference Framework for Continuum Reverberation Mapping Using Simulation-based Inference with Deep Learning
Authors: Jennifer I-Hsiu Li, Sean D. Johnson, Camille Avestruz, Sreevani Jarugula, Yue Shen, Elise Kesler, Zhuoqi (Will) Liu, Nishant Mishra
Figure caption: Evaluation results for light curves with out-of-distribution uncertainties at SNR ≈ 20, 50, 200, 500. The top panels display the MAE for each parameter, while the bottom panels show the difference between predicted and true values. The solid gray histogram represents baseline results for light curves at SNR ≈ 100. Prediction accuracy decreases with lower SNR and remains stable with higher SNR.
Paper: Fast and Flexible Inference Framework for Continuum Reverberation Mapping Using Simulation-based Inference with Deep Learning
Authors: Jennifer I-Hsiu Li, Sean D. Johnson, Camille Avestruz, Sreevani Jarugula, Yue Shen, Elise Kesler, Zhuoqi (Will) Liu, Nishant Mishra
Figure caption: Evaluation results for cos(i) (top) and ﹩\mathrm{log}{M}_{\mathrm{BH}}\dot{M}﹩ (bottom) of the power-law PSD light curves with β = 1, 2, 3 (left to right). The solid red lines denote the 1:1 relation.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: Left—The top panel shows each spectrum as a function of radial velocity for Hγ λ4340, with the normalized continuum offset to the associated orbital phase of the observation. The bottom panel shows the same plotted as a grayscale intensity between deepest absorption (black) and brightest emission (white) interpolated across orbital phase. Hγ appears in the center and is flanked by shell lines of Ti II λ4337.925 (−201 km s−1), Ti II λ4341.371 (+37 km s−1), and Ti II λ4344.290 (+239 km s−1), among other weaker lines. Right—Cross-correlation functions of the shell lines with a model template spectrum. These CCFs are offset vertically with the local background shifted to the associated orbital phase of the observation. The lower panel is a grayscale representation of the CCFs with the orbital velocity curve from C. A. Bauer (1945) overplotted as a solid white line.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: Estimated angular positions of the donor (fainter) relative to the gainer (placed at the origin) from partially resolved interferometry with the CHARA Array. The black circles show the measured positions from fits of the visibility and closure phase (Table 3). The surrounding red ellipses show the nominal error ellipses. The observations are connected to X symbols that show the predicted positions along the orbit (solid blue) determined from the spectroscopic and light-curve analyses and a fit for the longitude of the ascending node Ω.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: The V-band light curve from the ASAS Catalog of Variable Stars with two ELC fits overplotted. The solid line is a fit made by assuming that the gainer has a typical B-type star temperature T(gainer) = 17,900 K but large size (R  g  = 13.2 R ⊙). The thick gray line is a second fit with a small gainer (R  g  = 3.8 R ⊙) surrounded by a large, optically thick disk (R  d  = 14.3 R ⊙).
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: Top—Observed APO/ARCES spectrum of W Ser obtained near the primary eclipse (HJD 2,459,364.830, ϕ = 0.014) in the rest frame with identifications of several prominent lines. Middle—Tomographic reconstruction of the donor’s spectrum, offset for clarity. Bottom—MARCS model spectrum for T eff = 5000 K, rebinned to the observed wavelength, broadened to the apparent projected rotational velocity of the donor star, rescaled for additional continuum flux from the system, and offset for clarity.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: Left—Hα λ6563 profiles (top panel) and the associated grayscale diagram (bottom panel) in the same format as Figure 2. The normalized continuum is shifted to the orbital phase of observation. Right—He I λ5876 profiles. Our estimated radial velocity curve for the mass gainer is overplotted on the grayscale diagram as a solid black line.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: A section of the tomographic reconstructed spectra of the shell component (bottom) and the gainer torus component (top, offset by +1 for clarity) along with line identifications of the most prominent lines. An AMBRE/MARCS model spectrum for T eff = 8000 K is included between these (offset by +0.5 and Gaussian smoothed with FWHM = 40 km s−1). The absorption features for the gainer torus are similar to those of a stellar spectrum that is hotter than that for the circumbinary disk component.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: Left—Ca II λ8498 profiles in the same format as Figure 2. Right—O I λ7775 profiles.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: CCF radial velocity measurements (points) for the donor’s spectral lines in the region seen in Figure 5, overplotted with a circular orbital fit (solid line).
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: Several features in the reconstructed spectrum of the mass gainer star, with two appearing disk-like. They are offset for clarity by +1.2, +0.5, 0, and −0.7 for Hγ λ4340, Fe II λ4924, Si II λ6371, and He I λ6678, respectively. The latter two features appear weak in the reconstructed spectra, so their normalized fluxes are enlarged by factors of 5 and 4, respectively. These features probably form in the torus surrounding the gainer star.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Map of the distance between the coronal-line-emitting circumnuclear gas and the SMBH, based on the line FWHM and the assumption of virialized motion. Using only the FWHMs measured from Gaussian fits of the coronal lines in the higher-resolution SOAR spectra, the gas shows consistent velocities across all epochs. Within the range of black hole masses found for AT 2022upj by light-curve fitting and M BH–M bulge relations, the gas is situated within 0.1 pc of the SMBH.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption:  BAGPIPES spectral fit (orange line) and synthetic photometry (orange points) for the J003113.52+850031.8 photometrical SED (blue points) from the values in Table 7.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Top: power-law fit to AT 2022upj during the “pre-burst” phase (first 250 days from the optical peak). The photon index for this phase is ﹩{\rm{\Gamma }}={2.55}_{-0.35}^{+1.37}﹩. Bottom: power-law fit to AT 2022upj during the “burst” phase (after 250 days from the optical peak). The photon index for this phase is ﹩{\rm{\Gamma }}={3.08}_{-0.21}^{+0.23}﹩.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption:  BAGPIPES corner plots of fitted parameters of the host galaxy of AT 2022upj.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: The solution for stellar mass and black hole mass from the peak temperature and bolometric luminosity of AT 2022upj, as determined by TDEMass.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Light-curve fitting output from MOSFiT for the multiband optical and UV photometry from Las Cumbres, ZTF, and Swift of AT 2022upj.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Corner plots of fitted parameters via nested sampling light-curve fitting from MOSFiT.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Diagram illustrating the post-merger evolution of the LMC X-4 system. After the primary fills its Roche lobe (represented by the blue sphere) and engulfs the NS (represented by the gray sphere), a merger event cannot be avoided (Figure 2). As the engulfment proceeds (Figure 7), the NS rapidly (≈ 13.8 hr) sinks into the core (represented by the orange sphere). As a result, the core spins up due to shocks produced in the course of the inspiral. The further evolution of the rapidly rotating merger product can produce several interesting phenomena. The neutron star is expected to accrete a significant amount of mass to collapse to a BH. The rotating core, as it continues to collapse, will produce an accretion disk (Figure 8), which will likely also power and launch a relativistic jet.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Two-dimensional slices of the logarithm of gas density at two different times (7.3 hr and 13.8 hr) for material near the core of the primary. The top panels show slices in the orbital plane (y–x) while the bottom panels display slices in the meridional plane (y–z). The position of the core’s center of mass is denoted by an X mark, while the position of the NS is denoted by a white circle. The evolution of the trajectory of the NS in the orbital plane from the time the NS reaches the core is shown in the respective inset panels with a characteristic height and width of ﹩{(4{R}_{\odot })}^{2}﹩.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: The accretion rate onto the newly formed BH as a function of time. The rotating infalling core material is assumed to freefall without any pressure support and without mixing of radial layers. A disk is presumed to form from the collapse of every infalling shell and then subsequently accreted before the next shell collapses, as described in S. S. Bavera et al. (2020). When feedback from the accretion disk is taken into account, we show that it can unbind the infalling material on timescales that are comparable to the peak accretion time. The two ejection timescales shown as vertical lines are introduced in Figure 10.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption:  ρT parameter space relevant to TŻO hydrostatic solutions and the inspiral phase of an NS during CE. The gray line shows how temperature varies with density at the base of static TŻO solutions (R. C. Cannon 1993). The inspiral trajectory starts at comparatively low temperature and less dense material (lower corner) and becomes hotter and denser (upper corner) as the NS sinks into the core. The neutrino emission is dominated by electron-positron pair production processes, which are computed for solar metallicity material according to the fit formulae of N. Itoh et al. (1996).
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Relevant energy scales needed to estimate envelope unbinding during the accretion phase onto the newly formed BH. The binding energy of the rotating collapsing envelope, E b, exterior to a given mass coordinate (pink) and the integrated wind accretion energy, E w, expected to be shared with the infalling envelope (blue and dark green) are plotted against the mass coordinate of the post-merger model. The integrated energy required for ejection is uncertain. Here we assume two feedback efficiencies when calculating the fraction of energy that is shared with the collapsing stellar material. These are 1% (blue) and 0.2% (dark green), respectively. The formation of an accretion disk induces feedback, which in turn imposes a limit to the fraction of the star that can collapse and power an accretion event (dashed and dotted vertical lines).
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Two-dimensional slices of the logarithm of gas density in the meridional plane (y–z) at three different times during the inspiral phase (2.3 hr, 4.5 hr, and 13.8 hr). The upper panels in Figure 3 show the corresponding density slices in the orbital plane (y–x).
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: The normalized specific angular momentum content j/j isco of the stellar core at the end of the simulation is shown in mass coordinates (green curve). The profile is calculated by taking the spherical average about the center of mass in the FLASH simulation shown in Figure 7. Here, j isco is the specific angular momentum required for disk formation (dashed vertical line). We note that the simulated stellar model satisfies this condition for disk formation at all radii.