adsabs/AstroCLIMB huggingface dataset:
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: (Left panel) Multimessenger overview of Lense–Thirring precession about BH central engines for M87 and AT2020ocn providing a cons﻿traint on their stellar-mass counterparts such as GW170817B/GRB170817A. Navy blue and pink curves show K  W  values for a running ﹩\hat{a}=a/M﹩ based on the the observational values for wind precession frequency for the central SMBH of M87 and AT2020ocn (Y. Cui et al. 2023; D. R. Pasham et al. 2024). The ﹩\hat{a}﹩ values reported for AT2020ocn multiwavelength observations are marked by thicker lines. The gray dashed line shows ﹩\hat{a}=0.36﹩, which is the boundary to stop accretion from the disk in BH–torus system. By the universality of K  W  for BHs, the ﹩\hat{a}﹩ interval for M87 is estimated by horizontal mapping from AT2020ocn (green band) giving ﹩0.76\lt \hat{a}\lt 0.86﹩. K GW for GW170817B is shown by the red triangle, and the uncertainties are marked by the yellow box, illustrative of (7). (Right panel) The product of Lense–Thirring angular velocity and mass of the BH (MΩLT) for K  W  and K GW derived from (4), within the uncertainty range of ﹩\hat{a}﹩ borrowed from the observational results of M87 and AT2020ocn for K  W  (green) and GW170817B for K GW (yellow) (see Figure 5). Yellow and green bands are observational support for (7). The red triangle shows the central value of MΩLT for GW170817B using (4), based on updated results from M. H. P. M. van Putten et al. (2019). Recent observational results for M87 and AT2020ocn jet precessions are shown by the pink and navy blue dots, respectively. The navy blue line corresponds to the thick navy blue band for AT2020ocn in the left panel. Likewise, the pink line corresponds to the inferred range of ﹩\hat{a}﹩ for M87 in the left panel.
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: (Left panel) Detector strain–noise amplitude in O2, smoothed by a moving average in frequency. Shown is the mean with 1σ variation of strain H1 (blue) and L1 (red). The bandwidth of maximal sensitivity B ≃ 100–250  Hz corresponds to the minimum of these curves. O4 realizes an improvement by a factor k  D  ≃ 1.8 compared to O2 with a commensurate increase in horizon distances. (Reprinted from M. Aghaei Abchouyeh et al. 2023.) (Right panel) Signal-to-noise ratios in observing BH spin-down improves as the frequency sweep Δf GW = Δf GW(M 0/M) moves closer to the bandwidth of maximal sensitivity B (Figure 9) when M ≥ M 0, where M 0 ≃ 2.8M ⊙ is the mass of the black hole in GW170817B/GRB170817A. Highlighted is the gain k  n  ≃ 1.27 for M = 5M ⊙ expected to be produced in CC-SNe. Additional gain k  M  derives from the scaling ﹩{E}_{{\rm{GW}}}={{ \mathcal E }}_{{\rm{GW}}}(M/{M}_{0})﹩, where ﹩{{ \mathcal E }}_{{GW}}﹩ denotes the energy output (2).
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: (Top) BH central engines are a universal outcome of mergers (DNS, NSBH; left, middle) and core-collapse (CC) of sufficiently massive stars (right). DNS produces rapidly rotating BHs in prompt or delayed gravitational collapse of an initial HMNS (left). NS–BH and CC are expected to produce BHs with diversity in spin, the latter following a surge of hyperaccretion (see Figure 7 in Appendix B). High-density matter surrounding the BH provides a catalyst to convert its ample energy reservoir into multimessenger emission. A descending GW chirp signals an initially rapidly rotating BH. Accompanying subdominant emissions in MeV neutrinos, magnetic winds, and a baryon-poor jet emanating from the BH (not shown) accounts, from mergers, for SGRBEEs or LGRBs with no SNe (LGRBN) sharing the Amati correlation and, from CC, CC-SNe. (Reprinted from van Putten 2015.) (Bottom panels) Observation of the descending GW chirp GW170817B/GRB170817 following the ascending GW chirp GW170817 of a DNS, signaling spin-down of a Kerr BH formed in delayed gravitational collapse of the initial HMNS. (After M. H. P. M. van Putten 2001, M. H. P. M. van Putten & A. Levinson 2003, M. H. P. M. van Putten 2015, and M. H. P. M. van Putten & M. Della Valle 2019.)
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: Following the birth of the BH shown is the opening (dashed), middlegame (slide line), and endgame (solid thick line) of its evolution, referring to, respectively, direct accretion of initially low specific angular momentum, Bardeen accretion, and BH spin-down against a surrounding high-density inner accretion disk. Included are the various gravitational-wave frequencies f GW,i  at the various junctions. Here M 0 is the progenitor helium-core mass. Not all three phases are necessarily passed through in all events. For instance, a sufficiently low angular momentum progenitor may enter the middlegame but not beyond by premature accretion of all of M 0 into the BH. (Reprinted from M. H. P. M. van Putten & M. Della Valle 2017.)
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: Horizon distances as a function of mass of initially rapidly spinning black holes by mass scaling of GW170817B/GRB170817A (blue dot) and detector improvement in O4 over O2. Highlighted is the expected mass range of black holes produced in energetic CC-SNe (magenta). The upper limit of the excluded zone, representative of neutron stars (gray), is uncertain, indicated by a mass gap of a few tenths of a solar mass (white). Likewise, the upper limit of black hole masses produced in energetic CC-SNe is uncertain, awaiting detailed probes by gravitational-wave observations.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46–0.16 Using ALMA
Authors: Piyali Saha, Patricio Sanhueza, Marco Padovani, Josep M. Girart, Paulo C. Cortés, Kaho Morii, Junhao Liu, Á. Sánchez-Monge, Daniele Galli, Shantanu Basu, Patrick M. Koch, Maria T. Beltrán, Shanghuo Li, Henrik Beuther, Ian W. Stephens, Fumitaka Nakamura, Qizhou Zhang, Wenyu Jiao, M. Fernández-López, Jihye Hwang, Eun Jung Chung, Kate Pattle, Luis A. Zapata, Fengwei Xu, Fernando A. Olguin, Ji-hyun Kang, Janik Karoly, Chi-Yan Law, Jia-Wei Wang, Timea Csengeri, Xing Lu, Yu Cheng, Jongsoo Kim, Spandan Choudhury, Huei-Ru Vivien Chen, Charles L. H. Hull
Figure caption: (a) The B POS geometry (black line segments) toward G333, obtained after rotating the polarization segments by 90°, overplotted on ALMA 1.2 mm dust continuum emission. The B POS segments have arbitrary length and are plotted above the 3σ (σ = 29 μJy beam−1 for Stokes Q and U) level. Contours correspond to dust continuum emission 5, 10, 50, 100, 190, 230, 300, and 340 times σ (=160 μJy beam−1). The positions of MM1 and MM2 are marked as plus symbols. The circle in magenta represents the area of analysis. The scale bar and the beam size of 880 au are displayed on the bottom right and bottom left sides, respectively. The line segments are drawn following the Nyquist sampling (every 3 pixels each of size 0.″05). (b) Magnified view of the area of analysis. Symbols are the same as in panel (a).
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46–0.16 Using ALMA
Authors: Piyali Saha, Patricio Sanhueza, Marco Padovani, Josep M. Girart, Paulo C. Cortés, Kaho Morii, Junhao Liu, Á. Sánchez-Monge, Daniele Galli, Shantanu Basu, Patrick M. Koch, Maria T. Beltrán, Shanghuo Li, Henrik Beuther, Ian W. Stephens, Fumitaka Nakamura, Qizhou Zhang, Wenyu Jiao, M. Fernández-López, Jihye Hwang, Eun Jung Chung, Kate Pattle, Luis A. Zapata, Fengwei Xu, Fernando A. Olguin, Ji-hyun Kang, Janik Karoly, Chi-Yan Law, Jia-Wei Wang, Timea Csengeri, Xing Lu, Yu Cheng, Jongsoo Kim, Spandan Choudhury, Huei-Ru Vivien Chen, Charles L. H. Hull
Figure caption: (a) The moment zero or integrated intensity map of H13CO+ line emission. (b) The moment 1 or intensity-weighted velocity map of the same. The white line segments show the B POS geometry, and the contours outline the dust continuum emission (same as Figure 1). The positions of MM1 and MM2 are marked as plus symbols. The scale bar and the spatial resolution are displayed on the bottom right and bottom left sides, respectively, in all panels.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46–0.16 Using ALMA
Authors: Piyali Saha, Patricio Sanhueza, Marco Padovani, Josep M. Girart, Paulo C. Cortés, Kaho Morii, Junhao Liu, Á. Sánchez-Monge, Daniele Galli, Shantanu Basu, Patrick M. Koch, Maria T. Beltrán, Shanghuo Li, Henrik Beuther, Ian W. Stephens, Fumitaka Nakamura, Qizhou Zhang, Wenyu Jiao, M. Fernández-López, Jihye Hwang, Eun Jung Chung, Kate Pattle, Luis A. Zapata, Fengwei Xu, Fernando A. Olguin, Ji-hyun Kang, Janik Karoly, Chi-Yan Law, Jia-Wei Wang, Timea Csengeri, Xing Lu, Yu Cheng, Jongsoo Kim, Spandan Choudhury, Huei-Ru Vivien Chen, Charles L. H. Hull
Figure caption: Molecular outflows identified in 12CO (J = 3–2) overplotted on our observed 1.2 mm dust continuum emission. The plus symbols mark the positions of MM1 and MM2. The circle in cyan shows the region of analysis. The blueshifted and redshifted outflows are shown in blue and red contours, respectively. The blue contours are drawn with levels 3, 5, 7, 9, 12, and 18 times 0.13 Jy beam−1. The red contours are drawn with levels 3, 5, 7, 9, 11, 15, 20, and 25 times 0.10 Jy beam−1. The possible sources driving the outflows are marked using green crosses. The red and blue arrows show the directions of the redshifted and blueshifted outflows, respectively.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46–0.16 Using ALMA
Authors: Piyali Saha, Patricio Sanhueza, Marco Padovani, Josep M. Girart, Paulo C. Cortés, Kaho Morii, Junhao Liu, Á. Sánchez-Monge, Daniele Galli, Shantanu Basu, Patrick M. Koch, Maria T. Beltrán, Shanghuo Li, Henrik Beuther, Ian W. Stephens, Fumitaka Nakamura, Qizhou Zhang, Wenyu Jiao, M. Fernández-López, Jihye Hwang, Eun Jung Chung, Kate Pattle, Luis A. Zapata, Fengwei Xu, Fernando A. Olguin, Ji-hyun Kang, Janik Karoly, Chi-Yan Law, Jia-Wei Wang, Timea Csengeri, Xing Lu, Yu Cheng, Jongsoo Kim, Spandan Choudhury, Huei-Ru Vivien Chen, Charles L. H. Hull
Figure caption: (a) Comparison between the observed (green segments) and modeled (yellow segments) magnetic field orientations overplotted on the polarized intensity map (gray scale). The black contours are the same as Figure 1. (b) Histogram of the polarization angle residuals (Δψ) along with the Gaussian fitting.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46–0.16 Using ALMA
Authors: Piyali Saha, Patricio Sanhueza, Marco Padovani, Josep M. Girart, Paulo C. Cortés, Kaho Morii, Junhao Liu, Á. Sánchez-Monge, Daniele Galli, Shantanu Basu, Patrick M. Koch, Maria T. Beltrán, Shanghuo Li, Henrik Beuther, Ian W. Stephens, Fumitaka Nakamura, Qizhou Zhang, Wenyu Jiao, M. Fernández-López, Jihye Hwang, Eun Jung Chung, Kate Pattle, Luis A. Zapata, Fengwei Xu, Fernando A. Olguin, Ji-hyun Kang, Janik Karoly, Chi-Yan Law, Jia-Wei Wang, Timea Csengeri, Xing Lu, Yu Cheng, Jongsoo Kim, Spandan Choudhury, Huei-Ru Vivien Chen, Charles L. H. Hull
Figure caption: The spectra of CH3CN (J = 14–13) toward G333. The black line shows the observed spectrum, and the dashed blue line shows the fitted spectrum.
Paper: Infrared Spectra of Solid HCN Embedded in Various Molecular Environments for Comparison with the Data Obtained with JWST
Authors: Maksim Ozhiganov, Mikhail Medvedev, Varvara Karteyeva, Ruslan Nakibov, Uliana Sapunova, Vadim Krushinsky, Ksenia Stepanova, Anastasia Tryastsina, Aleksandr Gorkovenko, Gleb Fedoseev, Anton Vasyunin
Figure caption: Top part: the position and profile of the (ν 3) absorption feature of HCN molecules embedded in various astrochemically relevant molecular environments, including most abundant molecular constituents of interstellar ices. All spectra are obtained using the ISEAge UHV setup at a 10 K substrate temperature. The spectra presented with solid lines are obtained in the experiments using an identical HCN deposition rate and the total time of codeposition. The column density of HCN molecules is equal to 5 × 1015 cm−2 for each of the experiments. Bottom part: the JWST (NIRSpec) IR spectra of pristine cloud ices toward two background stars, NIR38 and J110621.63, using JWST (NIRSpec) presented for comparison (McClure et al. 2023). Spectra are presented with an offset. The JWST spectra are multiplied by a factor of 0.05 for clarity. Consequently, the column density of HCN in the laboratory experiments should be treated as 1 × 1017 cm−2 while comparing with the data from JWST. This corresponds to the abundance of ∼1% with respect to the H2O ice (McClure et al. 2023).
Paper: Infrared Spectra of Solid HCN Embedded in Various Molecular Environments for Comparison with the Data Obtained with JWST
Authors: Maksim Ozhiganov, Mikhail Medvedev, Varvara Karteyeva, Ruslan Nakibov, Uliana Sapunova, Vadim Krushinsky, Ksenia Stepanova, Anastasia Tryastsina, Aleksandr Gorkovenko, Gleb Fedoseev, Anton Vasyunin
Figure caption: Left part: a schematic view of the ISEAge UHV setup. The IR beam path is shown in red. The T-shaped optical holder with the Ge window is shown in green. The direction of the molecular species injection is shown by the arrow. Cad models are taken from the Kurt J. Lesker catalog (http://www.lesker.com/vacuum-flanges-components.cfm/). The radiation shield is omitted for clarity. Right part: a typical image of the Ge window surface obtained with the scanning probe microscope for the 10 × 10 μm area. The color scheme indicates the registered peak to the valley height from the lowest point (dark brown) to the highest point (light yellow) in nm.
Paper: Infrared Spectra of Solid HCN Embedded in Various Molecular Environments for Comparison with the Data Obtained with JWST
Authors: Maksim Ozhiganov, Mikhail Medvedev, Varvara Karteyeva, Ruslan Nakibov, Uliana Sapunova, Vadim Krushinsky, Ksenia Stepanova, Anastasia Tryastsina, Aleksandr Gorkovenko, Gleb Fedoseev, Anton Vasyunin
Figure caption: The evolution of the position and profile of the (ν 3) absorption feature of HCN molecules embedded in C6H6 and C6H5NH2 ices with the ratio of 1–8 upon the ice warm-up. The initial column density of HCN molecules is equal to ∼1 × 1016 cm−2 for each of the experiments. Spectra are presented with an offset. The spectrum of pure HCN ice is presented for a comparison. The dashed vertical line indicates the position of the 4.78 μm band identified on the JWST (NIRSpec) spectra and assigned to 13CO; see McClure et al. (2023).
Paper: Infrared Spectra of Solid HCN Embedded in Various Molecular Environments for Comparison with the Data Obtained with JWST
Authors: Maksim Ozhiganov, Mikhail Medvedev, Varvara Karteyeva, Ruslan Nakibov, Uliana Sapunova, Vadim Krushinsky, Ksenia Stepanova, Anastasia Tryastsina, Aleksandr Gorkovenko, Gleb Fedoseev, Anton Vasyunin
Figure caption: The fragments of IR spectra obtained upon the mixed HCN:NH3:H2O (1:3:8) ice warm-up. Left: evolution of the position and profile of the 2087 cm−1 absorption feature. Right: appearance and evolution of the NH4 + absorption feature. The initial column density of HCN molecules is equal to ∼1 × 1016 cm−2. Spectra are presented with an offset. The spectrum of pure HCN ice are presented for a comparison. The dashed vertical line indicates the position of the 4.78 μm band identified on the JWST (NIRSpec) spectra and assigned to 13CO; see McClure et al. (2023).
Paper: Infrared Spectra of Solid HCN Embedded in Various Molecular Environments for Comparison with the Data Obtained with JWST
Authors: Maksim Ozhiganov, Mikhail Medvedev, Varvara Karteyeva, Ruslan Nakibov, Uliana Sapunova, Vadim Krushinsky, Ksenia Stepanova, Anastasia Tryastsina, Aleksandr Gorkovenko, Gleb Fedoseev, Anton Vasyunin
Figure caption: The relative HCN (ν 3) band strength values in different molecular environments. The value for pure HCN ice is adopted from Gerakines et al. (2021). The tentative values are marked with asterisks. The corresponding band strength values obtained for the HCN (ν 3) absorption feature in various molecular environments are reported in the Table A1 of Appendix A.
Paper: Infrared Spectra of Solid HCN Embedded in Various Molecular Environments for Comparison with the Data Obtained with JWST
Authors: Maksim Ozhiganov, Mikhail Medvedev, Varvara Karteyeva, Ruslan Nakibov, Uliana Sapunova, Vadim Krushinsky, Ksenia Stepanova, Anastasia Tryastsina, Aleksandr Gorkovenko, Gleb Fedoseev, Anton Vasyunin
Figure caption: Similarly to Figure 2, a comparison between the position and profile of the (ν 1) absorption feature of HCN molecules. The dotted spectra are obtained for the pure molecular environment without addition of HCN molecules and are presented for the reference.
Paper: Delayed Emission from Luminous Blue Optical Transients in Black Hole Binary Systems
Authors: Davide Lazzati, Rosalba Perna, Taeho Ryu, Katelyn Breivik
Figure caption: Delay and luminosity of the BH-powered transients from accretion induced by an SN in the binary system as a function of the binary separation and the ejecta velocity. Time delay is shown in pseudocolors (see color bar), while average luminosity from Equations (5) and (16) is shown with contour levels. A vertical black line separates the region in which accretion from individual clumps dominates (left, Equation (16)) and the region in which accretion is dominated by the intraclump medium. The location in the parameter space of the late emission from the three considered FBOTs is also shown. Except for binary separation d and ejecta velocity v ej, all parameters are set to their fiducial values shown in Table 1.
Paper: Delayed Emission from Luminous Blue Optical Transients in Black Hole Binary Systems
Authors: Davide Lazzati, Rosalba Perna, Taeho Ryu, Katelyn Breivik
Figure caption: Cartoon of the post-SN explosion binary system, as envisioned in this model. The SN ejecta have expanded to reach the orbit of the companion BH, which is accreting mass via the Hoyle–Littleton mechanism. Ejecta clumps are shredded into an accretion disk, and the accreting BH is ejecting a collimated relativistic outflow that is eventually responsible for the observed nonthermal electromagnetic emission.
Paper: Delayed Emission from Luminous Blue Optical Transients in Black Hole Binary Systems
Authors: Davide Lazzati, Rosalba Perna, Taeho Ryu, Katelyn Breivik
Figure caption: Various components of the emission spectrum of a BH accreting from SN ejecta: an accretion disk, Comptonized disk emission, and radiation from an external shock formed from the interaction of an accretion-driven outflow with the dense SN medium. Dashed lines are used to emphasize that an accretion-driven outflow might not form when the accretion is sub-Eddington. A thin line is used, instead, for the high-frequency slope of the external shock component in case of a steeper electron distribution. For each source, the model parameters are varied to produce the best match to the late-time observations (see text).
Paper: Delayed Emission from Luminous Blue Optical Transients in Black Hole Binary Systems
Authors: Davide Lazzati, Rosalba Perna, Taeho Ryu, Katelyn Breivik
Figure caption: A corner plot showing the BH mass, pre-SN stripped-star mass, and separation at the time of the SN for our fiducial model in black. Model variations are shown in the one-dimensional histograms with different colors.
Paper: Delayed Emission from Luminous Blue Optical Transients in Black Hole Binary Systems
Authors: Davide Lazzati, Rosalba Perna, Taeho Ryu, Katelyn Breivik
Figure caption: Opacity between the transient emission site and the observer at infinity for different scenarios in both the optical/NIR and X-ray bands (see Section 3.3 for more details).
Paper: Irregular Moons Possibly Injected from the Outer Solar System by a Stellar Flyby
Authors: Susanne Pfalzner, Amith Govind, Frank W. Wagner
Figure caption: Top: origin of the injected TNOs in the unperturbed disk of 300 au in size. The disk has a color gradient from reddish to grayish corresponding to the color of planetesimals. The patches represent the feeding zones or origin of the injected TNOs. The color bar gives the inclination of the injected TNOs; blue represents prograde objects and red represents retrograde objects. Bottom: distribution of periastron distance of the ejected particles just before becoming unbound for the prograde (blue), retrograde (red), and total population (gray).
Paper: Irregular Moons Possibly Injected from the Outer Solar System by a Stellar Flyby
Authors: Susanne Pfalzner, Amith Govind, Frank W. Wagner
Figure caption: Distributions of the injected TNOs as a function of periastron distance (top) and inclination (bottom). The solid line shows the results for a primordial disk extending to 300 au and the dashed line for a 150 au primordial disk.
Paper: Irregular Moons Possibly Injected from the Outer Solar System by a Stellar Flyby
Authors: Susanne Pfalzner, Amith Govind, Frank W. Wagner
Figure caption: Evolution of the injected TNO population over the first 1 Gyr after the stellar flyby (300 au initial disk size). Top: distribution of prograde (blue lines) and retrograde (red lines) TNOs as a function of periastron distance at 12 kyr (solid lines) and 1 Gyr (dashed lines). Bottom: distribution of inclination for the test particles remaining bound at 12 kyr, 100 Myr, and 1 Gyr, respectively.
Paper: Irregular Moons Possibly Injected from the Outer Solar System by a Stellar Flyby
Authors: Susanne Pfalzner, Amith Govind, Frank W. Wagner
Figure caption: Snapshot of stellar flyby. Test particle locations at t = 200 yr after periastron passage of perturber star. The turquoise particles indicate the TNOs injected into the planet region by the flyby. The perturber star passed through the disk at a perihelion distance of 110 au on the right-hand side of the picture.