adsabs/AstroCLIMB huggingface dataset:
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Left: density profiles (g cm−3) vs. enclosed mass (in M ⊙) for a collection of progenitor models. Right: the evolution of the central baryon mass density for the models depicted in the left panel. Note the outlier behavior of the 40 M ⊙ model in both plots. The slight dip in central density seen for many of the models marks the time after bounce when PNS convection has reached the center. Note that here the 9b model is distinguished from the 9a model, both published in Vartanyan et al. (2023), by the lack of imposed initial perturbations in the former.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Net neutrino heating rate in the gain region as a function of time for a collection of comparison 3D models. Note that the 40 M ⊙ model experiences a significantly higher heating rate than any other model. Note also that this plot does not show the degree of cooling interior to the gain region, but exterior to the inner core and neutrinospheres. This quantity is generally large for those models such as the 14 and 12.25 M ⊙ models shown here for which the stalled shock recedes significantly and which follows one suggested channel of black hole formation.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Baryonic PNS mass in M ⊙ as a function of time after bounce (in seconds) for a collection of 3D CCSN models. Note the outlier behavior of the 40 M ⊙ model, due to its relatively high progenitor compactness and correspondingly high mass infall/accretion rate.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: A cartoon illustrating a physical picture for the LyC leaking star cluster of Sunburst Arc derived from joint analysis of photometry and spectroscopy data. The central energy source, a super star cluster of t age ≲ 4  Myr old, consists of a compact central component and an extended component of outskirt stars. Mass and kinetic energy output from both massive star winds and probably the first SN explosions thermalize and create a hot (T ∼ 106–107 K) cluster gas that blows out as a supersonic cluster wind. Pressed by stellar radiation (and possibly by the cluster wind), high-pressure (n e ∼ 105 cm−3 and P ∼ 109–1010 K cm−3) clouds of large column density N H ≳ 1023 cm−2 linger close to the cluster at ∼5–10  pc, and are subject to a competition between outward pressure force and inward gravitational pull. Photoionized by the stars, these emit strong nebular lines from high-ionization ionic species, are chemically enriched by massive star ejecta, and are dense enough for dust formation. More clouds at lower densities (n e ∼ 103–104 cm−3 and P ∼ 107–8 K cm−3) exist at large distances, where nebular lines from low-ionization ionic species are excited. Photoionized clouds do not completely surround the star cluster, and a fraction of the LyC radiation escapes the system via low-density channels.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Location of SDSO projected onto maps of high-velocity H I clouds near M31. Left panel: map from Thilker et al. (2004, 2005a) with an overlay of SDSO’s [O III] emission shown in blue. The positions of quasars near SDSO studied by Rao et al. (2013) and by Lehner et al. (2015) are indicated by × and ★, respectively. SDSO’s projected position coincides with an H I cloud exhibiting an elongated morphology similar to SDSO’s northeast–southwest appearance. Right panel: H I survey map of HVCs around M31 from Westmeier et al. (2008) with SDSO’s projected location again shown in blue.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: SDSO spectra: the middle panel shows our [O III] λ5007 image of SDSO with the locations of Slits 1 and 2 indicated. Adjacent left and right panels present resulting 2D spectra and the presence of [O III] λ λ4959, 5007 emission, which disappears, marked by dashed lines in the clear area north of SDSO. Night sky line emissions running the full length of the slits, including [N I] λ λ5198, 5200, are marked by arrows at the bottom. The two outer panels show plots of the detected [O III] λ5007 flux running from south to north along the lengths of both slits.
Paper: Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon
Authors: Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
Figure caption: Effect of viewing angle on the observed spectrum. There are three generic viewing perspectives: (1) the observer sees unobscured stellar radiation I  ν , as well as radiation R  ν  emerging from the illuminated faces of photoionized clouds; (2) the observer sees unobscured stellar radiation I  ν , as well as radiation D  ν  emerging from the shaded faces of clouds; (3) the observer sees stellar radiation T  ν  transmitted through the clouds, as well as radiation D  ν  emerging from the shaded faces of the clouds.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Top panel: mosaic of GALEX FUV images of the M31 and its surroundings. Middle and bottom panels: matching GALEX FUV (middle) and [O III] (bottom) images of the SDSO region. The UV bright stars EG And and HD 4336 are marked in the GALEX image.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Location of SDSO relative to M31's stellar streams. Left panel: figure adapted from McConnachie et al. (2004) with SDSO marked by several blue streaks. Right panel: color insert of our [O III] image overlaid on the same figure. SDSO’s projected position lies in a region in between M31's stellar streams with its westernmost extent matching at the edge of the Giant Stream East.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Spectra obtained in Slit 2 around Hβ and [O III] integrated in 10″ bins in the region of SDSO between +40°11.″25″ <δ < +40°19.″10″ (gray lines) and the total averaged spectrum (orange line). The wavelengths shown are in the observed telluric rest frame. The [O III] λ4959 line fit used that measured for the [O III] λ5007 line.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Plot of heliocentric velocities for [O III] λ5007 (green line) and Hβ (dashed blue line) along Slit 2 moving from south to north. The error bars indicate the statistical errors for the global fit solution, −9.8 ± 6.8 km s−1.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Electron vortex detected by MMS during the crossing of the MH. (a) The magnitude of the magnetic field; (b) three components of the magnetic field in GSE coordinates; (c) electron density; (d) parallel temperature (black) and perpendicular temperature (blue) of electrons; (e) three components of the electron velocity in GSE coordinates; (f) energy dissipation J ·  E                   ﹩^{\prime} ;﹩ (g) magnitude of vorticity ∇ × V  e . Two vertical gray dashed lines mark the electron vortex, and the horizontal black dashed line in panel (g) shows the threshold (〈x〉 +3 δ) of ∣∇ × V  e ∣ for selecting the electron vortex. The color bars at the top of the figure mark the exterior region (blue) and interior region (red) of the MH crossing, respectively.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Spatial distribution and occurrence rate of electron vortex in the magnetosheath. Statistical spatial distributions of all 506 electron vortex events are shown in panels (a) and (d), dwell time of orbit coverage of MMS from 2015 September to 2017 December is shown in panels (b) and (e), and occurrence rates of electron vortex events are shown in panels (c) and (f). The gray dashed lines and solid lines in panels (a)–(c) represent the bow shock and magnetopause positions computed using the paraboloidal bow shock model of Filbert & Kellogg (1979) and the magnetopause model of Sibeck et al. (1991), respectively.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Electron vortex detected by MMS during the crossing of the FR. The same format is shown in Figure 1. Two vertical gray dashed lines mark the electron vortex. The color bars at the top of the figure mark the exterior region (blue) and interior region (red) of the FR crossing, respectively.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Electron vortexes detected by MMS during the crossing of the MP. The format is the same as shown in Figure 3. The color bars at the top of the figure mark the exterior region (blue) and interior region (red) of the MP crossing, respectively.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Electron vortexes detected by MMS during the crossing of the BL. The format is the same as shown in Figure 3. The color bars at the top of the figure mark the border region (blue) and center region (red) of the BL crossing, respectively.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Statistical results of J ·  E′ inside electron vortexes associated with different structures: (a) the means of J ·  E′, (b) the medians of J ·  E′, and (c) the maxima of J ·  E′. The exploded pies in panel (a) are all J ·  E′ < 0, and the rest are J ·  E′ > 0.
Paper: Statistical Characteristics of Electron Vortexes in the Terrestrial Magnetosheath
Authors: Z. Wang, S. Y. Huang, Z. G. Yuan, Y. Y. Wei, K. Jiang, S. B. Xu, J. Zhang, R. T. Lin, L. Yu, Q. Y. Xiong, C. M. Wang
Figure caption: Histograms of the durations (a) and the spatial scales (b) of electron vortexes when MMS crossed the CS, MH, FR, MP, and Others.
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Top left: combined HST J+H continuum (blue and green, corresponding to the rest-frame V band), and integrated ALMA CO 4–3 (red), all at ∼0.″2 FWHM resolution. The dotted white line marks the direction of the bar-like structure. Top right: combined HST J+H continuum (blue), integrated ALMA rest frame 460 GHz continuum (red), and Hα-integrated line (green), at ∼0.″25–0.″3 FWHM resolution. Bottom: 1D cuts along the major axis at PAmajor ∼ −20° to −30° in CO 4–3 (red squares), Hα AO (open blue circles), and Hα AO + non-AO (filled blue circles) in line intensity (left), line velocity (center) and line velocity dispersion (right).
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Kinemetry analysis of the highest-resolution line data of Q2343_BX610, the 0.″2 CO 4–3 data from ALMA (see Equations (2)–(4). Top: rotation parameter B 1 as a function of galactocentric radius R, extracted for ellipses of q = 0.75 along PA = −25°. Bottom: ratio of ﹩\tfrac{{A}_{1}}{{B}_{1}}﹩, ﹩\tfrac{{A}_{2}}{{B}_{1}}﹩, and ﹩\tfrac{{B}_{2}}{{B}_{1}}﹩ as a function of distance from the center. The dominant nontangential kinemetry parameter is A 1 with ﹩\tfrac{{A}_{1}}{{B}_{1}}=-0.2\cdots -0.44﹩. Note that this is in excellent agreement with the ﹩\tfrac{{v}_{{\rm{r}}}}{{v}_{{\rm{c}}}\left({R}_{{\rm{e}}}\right)}=-0.32﹩ from the DYSMAL analysis in this line (Table 2).
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Velocity (top) and velocity dispersion (bottom) maps in CO 4–3 (left), Hα AO + non-AO (second from left), Hα AO (third from left), and [N II] 6583 (right), superposed on the HST H-band map in contours. The color indicates the velocity amplitude with the numbers at the bottom of each panel giving the minimum (purple) and maximum (red) values. The yellow arrow denotes 1″. The kinematic major axis of the galaxy at PAmajor ∼ −25° ± 8° (−33 for the most compact CO and -18 for the most extended Hα) is marked as a white line, and the zero isovelocity contour ridge (green color) at PA ∼ 24° is indicated by the gray dashed line in the first panel.
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Velocity residual (top) and velocity dispersion residual (bottom) maps of the CO 4–3 (left), Hα AO + non-AO (second from left), Hα AO (third from left), and [N II] 6583 AO + non-AO data (right), after subtracting the corresponding DYSMAL model maps from our data. Color scheme and amplitudes are the same as in Figure 5.
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Correlation between derived properties of the nine galaxies. For the computation of the theoretically expected converging flow speed (Table 2) we use Equation (11) with a ∼1.75, ζ=2 and γ=0. We also use for each galaxy the estimates of gas fraction and Q as given in Table 1.
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Left: CO 3–2/4–3 intensity, velocity, and velocity dispersion 1D profiles and kinematic fitting results along PAmajor (uniform weighting data: cyan crossed squares, FWHM 0.″43; natural weighting data: filled blue circles, FWHM 0.″68). Right: velocity, velocity dispersion (top), and residual maps (bottom) of CO 4–3/3–2 in EGS_13035123.
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Top and right: images of continuum and Hα velocity, velocity dispersion, and their residuals in zC_403741 (z = 1.45). Bottom left: 1D Hα intensity, velocity, and velocity dispersion cuts along PAmajor, as well as the best-fit DYSMAL model (red line).
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Images of continuum and integrated line emission in EGS_13035123 (z = 1.1).
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Kinemetry of CO velocity maps in EGS_13035123.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Light curves of the progenitor candidate in the mid-IR based on Spitzer data (upper panel) and the near-IR based on UKIRT/WFCAM and Gemini/NIRI data, along with MMT/MMIRS data reported by Jencson et al. (2023) (lower panel). The x-axis origin corresponds to the explosion epoch of SN 2023ixf (Hosseinzadeh et al. 2023).
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Variation of rms amplitude of the light curve of the progenitor candidate as a function of wavelength.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Pre-explosion Spitzer Warm Mission mosaics at Channels 1 and 2 (3.6 and 4.5 μm, respectively). A source can be clearly seen at the absolute position of SN 2023ixf in both channels, which we identify as its progenitor candidate in the mid-IR.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Cutouts around the progenitor candidate for SN 2023ixf from archival NIRI K-band (top left), J-band (top right), and UKIRT/WFCAM H-band (bottom) images.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: A mapping of the explodability of massive-star progenitors in compactness/helium core mass space. The red triangles are nonexploding models, the blue triangles are exploding models, and the black circles are the Sukhbold et al. (2016, 2018) solar-metallicity progenitor suite. The left panel is using the 2D simulations in Wang et al. (2022) and Tsang et al. (2022), and the right panel is for a representative set of the 3D FORNAX simulations we have performed since 2019. Notice the island of nonexplosion in this space, for both 2D and 3D simulations, suggesting a special black hole forming branch. The 40 M ⊙ model highlighted in this paper is in the upper right corner of each panel. We have yet to simulate this model in 2D.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Entropy slices at ∼8.8 s post-bounce for the 40 M ⊙ solar-metallicity progenitor in the z - x, z - y, and y - x planes. The black circle marks the position of the black hole. Neutrino transport is turned off at 1.76 s after bounce, and a flow-in diode boundary condition is applied at 100 km. Our outer grid boundary is at 100,000 km. On this plot at this time the shock wave has penetrated the carbon/oxygen interface (transition from darker blue to lighter blue near ∼60,000 km) in one sector (bottom of the y-x panel), while still interior to it in the other.
Paper: Black Hole Formation Accompanied by the Supernova Explosion of a 40 M ⊙ Progenitor Star
Authors: Adam Burrows, David Vartanyan, Tianshu Wang
Figure caption: Luminosity per steradian of the electron-type neutrinos at 1.76 s after bounce. The two panels are measured at 50 and 150 km, respectively. In both panels we see that the enhanced opacity of the disk and the rotation of the outer PNS together lead to roughly dipolar neutrino emission.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: 2022 burst on the CMD. The color is calculated using photometry taken at epochs separated by no more than one day. The data points are color coded by the time since JD = 2459600.0, the time when the burst reached its brightness maximum. The fainting of burst proceeded until JD = 2459725.0, after which the variability is dominated by the spot modulations. The dotted black line represents the color trend due to accretion enhancement, on the scale of 1–15 times the accretion level inferred from the X-Shooter spectrum. The red line denotes the interstellar reddening law of A  V  = 0.5 mag and R  V  = 3.1.