adsabs/AstroCLIMB huggingface dataset:
Paper: A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium
Authors: A. Tasa-Chaveli, Á. Sánchez-Monge, A. Fuente, A. Ginsburg, H. S. P. Müller, T. Möller, P. Rivière-Marichalar, D. Navarro-Almaida, G. Esplugues, P. Schilke, M. Rodríguez-Baras, S. Thorwirth, L. Beitia-Antero
Figure caption: Spectra around the CaS 22→21 transition at 232.372 GHz observed toward G351.77-mm1, from ALMA archival data: (left panel) project 2017.1.00237.S (see A. Ginsburg et al. 2023), (right panel) project 2015.1.00496.S (see H. Beuther et al. 2019). The observed spectra are shown in black with gray-filled histograms. A Gaussian convolution was applied to match the beam size (﹩\sim 0\mathop{.}\limits{^{\prime\prime} }16﹩) of our observations, and the spectra were extracted toward the same position at α(J2000)  =  17h26m42﹩\mathop{.}\limits^{{\rm{s}}}﹩533 and ﹩\delta ({\rm{J2000}})\,=\,-3{6}^{\circ }9^{\prime} 17.37^{\prime\prime} ﹩. The synthetic spectrum generated, including all the identified molecules listed in Table A1, is shown in blue, while the best CaS synthetic spectrum is shown in red. The red-shaded area around the red solid line represents the uncertainty derived from different fits assuming different rotational temperatures (see Table A4). The compound C2H3CHO is suggested as the carrier of the ∼232.365 GHz feature. However, this molecule does not exhibit intense lines in our observations, which precludes robust confirmation. The shaded vertical bands cover the molecular lines that appear self-absorbed.
Paper: A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium
Authors: A. Tasa-Chaveli, Á. Sánchez-Monge, A. Fuente, A. Ginsburg, H. S. P. Müller, T. Möller, P. Rivière-Marichalar, D. Navarro-Almaida, G. Esplugues, P. Schilke, M. Rodríguez-Baras, S. Thorwirth, L. Beitia-Antero
Figure caption: Zoom-in panels around the CaS and KS transitions included in the spectra of G351.77-mm1. The observed spectra are shown with gray-filled histograms. The synthetic spectrum generated without including the S-bearing refractory species is shown with a blue line, while the best fits of CaS and KS are shown in red. The best fits of the KSH and CaSH lines are shown with a green line (see Figure A2 for additional frequency ranges covering nondetected CaSH transitions).
Paper: A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium
Authors: A. Tasa-Chaveli, Á. Sánchez-Monge, A. Fuente, A. Ginsburg, H. S. P. Müller, T. Möller, P. Rivière-Marichalar, D. Navarro-Almaida, G. Esplugues, P. Schilke, M. Rodríguez-Baras, S. Thorwirth, L. Beitia-Antero
Figure caption: Synthetic spectra of potential contaminants of CaS (19–18; ν = 0) listed in Table A3. The left panel in each row shows the observed spectrum (gray histogram) around the frequency of the CaS (19–18; ν = 0) transition, which is highlighted with a vertical dashed line. The red solid line corresponds to the maximum intensity of each potential contaminant (labeled in black in the top-left corner of each panel) required to fully account for the observed line feature. These species are discarded on the basis of the predicted emission in other parts of the spectra (see right panels), which would be too bright to reproduce the observations. Red, dotted lines represent the maximum intensity of the potential contaminants, allowed by the upper limits derived from transitions distributed throughout the observed spectral range.
Paper: A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium
Authors: A. Tasa-Chaveli, Á. Sánchez-Monge, A. Fuente, A. Ginsburg, H. S. P. Müller, T. Möller, P. Rivière-Marichalar, D. Navarro-Almaida, G. Esplugues, P. Schilke, M. Rodríguez-Baras, S. Thorwirth, L. Beitia-Antero
Figure caption: Zoom-in panel around the CaSH transitions included in the spectra of G351.77-mm1. The observed spectrum is shown with gray-filled histograms. The synthetic spectrum generated without including the S-bearing refractory species is shown with a blue line, while the best fit of CaSH is shown in green.
Paper: Mystery behind the Peeling of a Filament and the Associated Sudden Disappearance of a Sunspot Penumbra
Authors: Ju Jing, Mia Mancuso, Satoshi Inoue, Jeongwoo Lee, Qin Li, Wen He, Yan Xu, Wenda Cao, Haimin Wang
Figure caption: The spatial correlation between the penumbra disappearance and the filament peeling. (a) GST Hα image taken at 18:21 UT. The box marks a region of interest for the close-up views shown in panels (b)–(f). (b)–(f) The GST images of the Hα center line, Hα+0.6 Å, TiO, Dopplergram, and horizontal field strength ∣Bh∣, all obtained approximately at 18:21 UT. The arrows in these panels point to a strand peeling off from the main body of the filament, and the ovals highlight the area where the penumbra disappears significantly.
Paper: Mystery behind the Peeling of a Filament and the Associated Sudden Disappearance of a Sunspot Penumbra
Authors: Ju Jing, Mia Mancuso, Satoshi Inoue, Jeongwoo Lee, Qin Li, Wen He, Yan Xu, Wenda Cao, Haimin Wang
Figure caption: The MFR in the NLFFF model and the MHD simulation of magnetic field evolution. Top two panels: top and side views of the MFR, superimposed on the HMI photospheric Bz map taken at 17 UT. The red arrow indicates the location of the magnetic NP. Middle panels: simulated 3D magnetic field lines (with vertical cross sections of ∣J∣/∣B∣) at Alfvén time t = 0.0, 1.6, and 3.2. Bottom panels: the top views of simulated horizontal magnetic field strengths in the photospheric layer (at an altitude of ∼400 km) at t = 0.0, 1.6, and 3.2. The color bar values for Bz and ∣Bh∣ represent percentages relative to their maximum values.
Paper: Mystery behind the Peeling of a Filament and the Associated Sudden Disappearance of a Sunspot Penumbra
Authors: Ju Jing, Mia Mancuso, Satoshi Inoue, Jeongwoo Lee, Qin Li, Wen He, Yan Xu, Wenda Cao, Haimin Wang
Figure caption: The evolution of penumbral horizontal and vertical field strength in the simulation. Left: HMI Bz map at 17:00 UT, showing the FOV of the bottom boundary of the NLFFF model and the simulation. The box indicates the region of penumbra disappearance, which is the same as the region shown by the box in Figure 3(f). Right: time profiles of ∣Bh∣ (solid) and ∣Bz∣ (dotted), averaged over the boxed region shown in the left panel. The simulation time “0” corresponds to 17:00 UT.
Paper: Spinning into the Gap: Direct-horizon Collapse as the Origin of GW231123 from End-to-end General-relativistic Magnetohydrodynamic Simulations
Authors: Ore Gottlieb, Brian D. Metzger, Danat Issa, Sean E. Li, Mathieu Renzo, Maximiliano Isi
Figure caption: Outline of the evolutionary pathway leading to the GW231123 BBH merger, originating from a binary of low-metallicity massive stars that undergo direct-horizon collapse. (1) The star initially contains a ∼250 M⊙ helium core, which is subject to mass loss through stellar winds and/or binary interaction. (2) The helium core, now weighing ∼150 M⊙, has undergone fusion into carbon and oxygen and becomes unstable to pair production, triggering contraction. (3) As the temperature rises, heavy nuclei begin to photodisintegrate in a runaway process that culminates in a direct-horizon collapse, forming a moderately spinning ∼40 M⊙ BH surrounded by an accretion disk formed as a result of the star’s rotation. (4) Magnetic fields threading the BH regulate its final spin and mass. They extract rotational energy, enabling the formation of BHs with a range of spin values, and drive mass loss through relativistic jets and disk winds, allowing BHs to form within the upper mass gap. A moderate seed magnetic field in the star yields a BH with MBH ≈ 100 M⊙ and a ≈ 0.8. Turbulent accretion imparts a kick to the BH, potentially misaligning its spin axis relative to the binary orbit. (5) A similar process occurs in the companion, but with weaker magnetic fields that extract less rotational energy from the BH and unbind less stellar mass. This results in the formation of a BH with MBH ≈ 130 M⊙ and a ≈ 0.9. The independent evolution of each component leads to a BBH system with misaligned spins. (6) The BBH merges after the inspiral driven by GW emission, yielding a Mf ≈ 225 M⊙ remnant with spin af ≈ 0.9, consistent with GW231123.
Paper: Spinning into the Gap: Direct-horizon Collapse as the Origin of GW231123 from End-to-end General-relativistic Magnetohydrodynamic Simulations
Authors: Ore Gottlieb, Brian D. Metzger, Danat Issa, Sean E. Li, Mathieu Renzo, Maximiliano Isi
Figure caption: 3D renderings of the late-time evolution in models Bw (weak magnetic field) at t −  tBH = 5.9 s, Bm (moderate strength field) at t −  tBH = 5.7 s, and Bvs (very strong field) at t −  tBH = 1.3 s. The ﹩\hat{z}﹩-axis aligns with the stellar rotation and BH spin. All models develop an accretion disk as a result of the star’s rotational profile. In model Bw, the rendering shows a rising mass density toward the BH, with no outflows emerging from the weakly magnetized accretion disk. By t = 5.7 s, the BH in this model has grown to  MBH ≈ 110 M⊙, and we depict the BH horizon at rg = 1.65 × 107 cm ∼ 1% of the disk radius. In contrast, model Bvs represents the opposite extreme, where relativistic outflows are electromagnetically launched from the BH and reach r ≈ 4 RHe. The accretion disk is shown in gray, the ultrarelativistic jet in red, and the shocked jet (stellar) cocoon material in yellow (blue-gray). By t = 1.3 s, the outflows have unbound all plasma in the system, leaving the remaining gas either in the disk or in the cocoon. Model Bm represents an intermediate regime in which jets marginally emerge from the BH ergosphere, leading to intermittent jet launching. In the snapshot shown, only one jet is visible up to r ≈ RHe, as the counterjet is momentarily choked by the ram pressure of the infalling plasma.
Paper: Spinning into the Gap: Direct-horizon Collapse as the Origin of GW231123 from End-to-end General-relativistic Magnetohydrodynamic Simulations
Authors: Ore Gottlieb, Brian D. Metzger, Danat Issa, Sean E. Li, Mathieu Renzo, Maximiliano Isi
Figure caption: (a) The time evolution of the BH mass (solid lines) and its asymptotic value, given by the sum of the BH mass and bound mass in the system (dashed lines), demonstrates that strong outflows halt accretion, unbind the surrounding plasma, and reduce the final BH mass. In all models, the BH mass converges to its asymptotic value by the end of the simulation. (b) The time evolution of the BH spin. When no outflows are present (model Bw), the BH spins up to the maximal value. In models with outflows, halted accretion and magnetic torques that extract rotational energy from the BH lead to spin-down. Strong outflows, as in models Bs and Bvs, drive the spin down toward an equilibrium value between accretion and extraction of angular momentum. In contrast, in model Bm, where the outflows are launched later, the BH continues to spin-up until jet launching, reaching a ≈ 0.8. (c) Final BH spin–mass (including all bound plasma at the end of our simulations) diagram. Colored circles indicate our models, while the contours are representative of the BHs inferred from GW231123 using the NRSUR7DQ4 waveform (V. Varma et al. 2019). The results show that a direct-horizon-collapse binary with weak to moderate magnetic fields can reproduce the properties of the BHs observed in GW231123.
Paper: Spinning into the Gap: Direct-horizon Collapse as the Origin of GW231123 from End-to-end General-relativistic Magnetohydrodynamic Simulations
Authors: Ore Gottlieb, Brian D. Metzger, Danat Issa, Sean E. Li, Mathieu Renzo, Maximiliano Isi
Figure caption: Time evolution post-BH formation (t − tBH) of various quantities measured at the BH horizon (except for the mass accretion rate, which is calculated at r = 5 rg). (a) The mass accretion rate initially peaks at ﹩\,{\dot{M}}_{{\rm{BH}}}\gtrsim 100\,\,{M}_{\odot }\,\,{{\rm{s}}}^{-1}﹩ as the plasma free-falls onto the BH. This is followed by the formation of an accretion disk, which stabilizes the inflow until the bulk of the stellar material is accreted at t ≈ 1 s, after which the accretion rate begins to decline. (b) The high dimensionless magnetic flux, ϕ, indicates that rotational energy is extracted from the BH via magnetic torques in models Bvs and Bs, leading to a nonnegligible jet launching efficiency ﹩{\eta }_{{\rm{sim}}}﹩ (panel (c)). (d) The resulting jets in models Bvs and Bs are extremely powerful, with luminosities ﹩P={\eta }_{{\rm{sim}}}\,{\dot{M}}_{{\rm{BH}}}{c}^{2}\sim 1{0}^{54}\,\,{\rm{erg}}\,\,{{\rm{s}}}^{-1}﹩, enabled by the combination of high mass accretion rates and strong magnetic fluxes threading the BH.
Paper: Spinning into the Gap: Direct-horizon Collapse as the Origin of GW231123 from End-to-end General-relativistic Magnetohydrodynamic Simulations
Authors: Ore Gottlieb, Brian D. Metzger, Danat Issa, Sean E. Li, Mathieu Renzo, Maximiliano Isi
Figure caption: Evolution of the mass density profile from the onset of core collapse (blue) to  MBH ≈ 40 M⊙ BH formation at  tBH = 4.29 s after core collapse (red). The black area indicates the Schwarzschild radius of the BH, rs = 2G MBH/c2 ≈ 1.2 × 107 cm.
Paper: The Landscape of Collapsar Outflows: Structure, Signatures, and Origins of Einstein Probe Relativistic Supernova Transients
Authors: Ore Gottlieb
Figure caption: Schematic illustration of collapsar outflows and emission. Structure: The collapse results in the formation of a PM, which launches subrelativistic outflows (violet) prior to collapsing into a BH. The ensuing formation of a BH surrounded by an accretion disk drives moderately collimated, magnetized disk ejecta (turquoise) and a wobbling ultrarelativistic episodic jet powered by the BZ mechanism (yellow). As the jet propagates, it shocks the surrounding stellar material, generating a collimated, mildly relativistic cocoon (blue). An additional subrelativistic SN shock wave from core bounce (magenta) is possible; however, the PM and/or disk ejecta are consistent with the energy and velocity distributions observed in stripped-envelope SNe, rendering the SN shock wave unnecessary to account for observations. We note that the illustrated collimation of the cocoon and disk ejecta represents characteristic angles where the bulk of the energy is concentrated. In practice, the outflows mix in a spherical morphology, with the energy distributed as a function of angle. Emission: Observers detect intermittent emission as the jets aligned with their line of sight generate γ-ray emission, while misaligned jets and a cocoon produce lower-efficiency X-ray emission. Both on-axis and off-axis observers may detect a sharp afterglow rebrightening when the emission from a “top-hat,” wobbling jet episode enters their line of sight. During the first day, the thermal optical cooling emission is dominated by the cocoon, after which the disk ejecta and later the PM outflows take over. Enhanced nucleosynthesis in the disk and PM outflows promotes 56Ni mixing in the outer regions of the ejecta, producing the bright 56Ni-powered peak in the light curve.
Paper: The Landscape of Collapsar Outflows: Structure, Signatures, and Origins of Einstein Probe Relativistic Supernova Transients
Authors: Ore Gottlieb
Figure caption: 3D renderings of a collapsar jet simulation from O. Gottlieb et al. (2022b) illustrating the velocity of relativistic outflows when they reach 10 stellar radii, viewed edge-on (left) and face-on (right). Relativistic jet elements appear in red, slower components in yellow, and the surrounding cocoon in blue. The left panel demonstrates the wobbling and episodic nature of collapsar jets. During phases when none of the jet episodes are directed toward the observer, the cocoon and the misaligned off-axis wobbling jets may produce low-efficiency softer emission. This leads to intermittency and spectral variability in the GRB prompt emission along a given line of sight (e.g., at θ = 0 in the right panel). As the outflow decelerates during the afterglow phase, the light curve initially decays, followed by rising off-axis wobbling jet emission as misaligned relativistic jet components gradually enter the observer’s beaming cone. This results in potentially multiple rebrightening episodes in the afterglow light curve.
Paper: The Landscape of Collapsar Outflows: Structure, Signatures, and Origins of Einstein Probe Relativistic Supernova Transients
Authors: Ore Gottlieb
Figure caption: (a) Radially integrated (north hemisphere in blue and south hemisphere in red) isotropic-equivalent energy, as a function of angular separation from the stellar axis of rotation (θ = 0). The global outflow shows a gradual decline in energy with angle. (b) Isotropic-equivalent energy and (c) energy density-weighted Lorentz factor through a shell containing a bipolar wobbling jet (jet and its counterjet rotated by 180°) episode at ∼3 stellar radii (delineated in dark red in Figure 2). The two peaks shown by the solid lines indicate that the jets’ cores deviate from the rotation axis owing to wobbling. Both jets exhibit steep angular gradients (top hat) in Lorentz factor and isotropic-equivalent energy, in contrast to the smoother global angular profiles obtained for the full volumetric distribution (whose renormalized shape is shown with dashed lines in panel (b) for comparison).
Paper: The Landscape of Collapsar Outflows: Structure, Signatures, and Origins of Einstein Probe Relativistic Supernova Transients
Authors: Ore Gottlieb
Figure caption: Total energy distribution per logarithmic interval of asymptotic proper velocity of collapsar outflows. Solid lines represent the total energy distribution for disk ejecta (green), cocoon (blue), and their combined total (black). The disk ejecta dominates the energy at β ≲ 0.3, whereas the cocoon exhibits a flat distribution and dominates at mildly relativistic velocities, consistent with the velocity distribution inferred from stripped-envelope SNe. Dashed lines indicate the thermal energy fraction of the respective total energies. The distribution is truncated at low velocities (﹩{\beta }_{{\rm{\min }}}\approx 0.05﹩), as material moving at slower velocities has not escaped the stellar envelope by the end of the simulations.
Paper: The Landscape of Collapsar Outflows: Structure, Signatures, and Origins of Einstein Probe Relativistic Supernova Transients
Authors: Ore Gottlieb
Figure caption: (a) Analytic (dashed gray lines) and numerical (solid lines) calculations of cocoon (blue), disk ejecta (green), and total (black lines) cooling emission are compared with the estimated bolometric luminosity of EP250108a (black circles; G. P. Srinivasaragavan et al. 2025). The temporal evolution indicates that cocoon emission may contribute to the first data point at t ≈ 1 day, but it decays too rapidly to account for the later observations. The disk ejecta emission dominates the observations at 3 days ≲ t  ≲ 7 days, before the main SN peak at t ≈ 12 days. (b) The νLν light curve of EP240414a across optical/infrared bands (S. Srivastav et al. 2025; H. Sun et al. 2025; J. N. D. van Dalen et al. 2025) presents three phases of optical evolution: cooling emission produces the shallow power-law decline during the first day (blue shaded background), a subsequent peak powered by a nonthermal afterglow from a wobbling top-hat jet (green shaded background), and the emergence of thermal emission generated by 56Ni decay (red shaded background).
Paper: The Landscape of Collapsar Outflows: Structure, Signatures, and Origins of Einstein Probe Relativistic Supernova Transients
Authors: Ore Gottlieb
Figure caption: Meridional maps of ﹩{\rm{log}}({{\rm{\Gamma }}}_{\infty })={\rm{log}}(h{\rm{\Gamma }})﹩ (a) shortly after the jet breaks out of the star (dashed white line) at t = 6  s after launching and (b) upon reaching the outer edge of the CSM at t = 20 minutes. While the jet head is mildly relativistic, the bulk of the jet retains ultrarelativistic velocities throughout its interaction with the CSM, indicating that the surrounding medium is insufficiently massive to choke the jet.
Paper: Spectroscopic Characterization of Interstellar Object 3I/ATLAS: Water Ice in the Coma
Authors: Bin Yang, Karen J. Meech, Michael Connelley, Ruining Zhao, Jacqueline V. Keane
Figure caption: Visible-wavelength reflectance spectrum of 3I/ATLAS obtained with GMOS instrument on Gemini-S, normalized at 0.55 μm. The colored lines and shaded regions represent the mean and 1σ ranges for three major asteroid spectral types: S-type (blue), D-type (red), and L-type (green), taken from F. E. DeMeo et al. (2009). The solid colored lines indicate the average reflectance for each class, while the surrounding shaded regions show the typical variability (1σ) within each class. The dark red spectrum is (20000) Varuna, a large trans-Neptunian object in the Kuiper Belt, representative of ultrared objects in the outer solar system, taken from S. Fornasier et al. (2009). The comparison shows that 3I/ATLAS has a featureless, red spectral slope, consistent with D-type asteroids; its coma shows no evidence for ultrared matter.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectroscopic Characterization of Interstellar Object 3I/ATLAS: Water Ice in the Coma
Authors: Bin Yang, Karen J. Meech, Michael Connelley, Ruining Zhao, Jacqueline V. Keane
Figure caption: The black line shows the IRTF/SpeX spectrum of 3I/ATLAS, normalized at 0.85 μm. Colored lines and shaded regions represent the mean and ±σ ranges for S-type (blue), D-type (red), and L-type (green) asteroids, as in Figure 1. A 40 pixel running mean is overplotted on the original IRTF spectrum to illustrate the overall spectral trend. A red arrow marks the broad feature centered near 2.05 μm, which may be due to water ice. A black arrow indicates a narrow absorption band centered near 2.23 μm of uncertain origin, possibly related to C-H vibrations in organics or hydrocarbons. Gray shaded regions (1.35–1.45 μm and 1.80–1.95 μm) indicate strong telluric absorption due to water vapor.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectroscopic Characterization of Interstellar Object 3I/ATLAS: Water Ice in the Coma
Authors: Bin Yang, Karen J. Meech, Michael Connelley, Ruining Zhao, Jacqueline V. Keane
Figure caption: Reflectance spectrum of 3I/ATLAS, obtained with Gemini-S GMOS (pink) and NASA IRTF SpeX (red), shown alongside spectra of other known interstellar objects (ISOs) and solar system bodies. Among the ISOs, 3I/ATLAS exhibits the highest SNR and an intermediate spectral slope. In the NIR, its spectrum closely resembles that of comet C/2006 W3 (B. Yang 2009), a bright Oort Cloud comet; both exhibit a moderately red slope and a broad water-ice absorption band at 2.0 μm.
Paper: Spectroscopic Characterization of Interstellar Object 3I/ATLAS: Water Ice in the Coma
Authors: Bin Yang, Karen J. Meech, Michael Connelley, Ruining Zhao, Jacqueline V. Keane
Figure caption: Near-infrared spectrum of 3I compared with the best-fit spectra model. The black line shows the smoothed reflectance spectrum of 3I/ATLAS, obtained with the IRTF/SpeX instrument and normalized at 1.0 μm. The thick red line represents the best-fit volume mixing model, consisting of 37% water ice (H2O) and 63% amorphous carbon. The faint orange and blue bands show the spectral profiles of the two individual components used in the model with different size distributions and peak particle sizes.