adsabs/AstroCLIMB huggingface dataset:
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: (a) Spatially resolved diagnostics of PAH band ratios 6.2 μm/7.7 μm vs. 11.3 μm/7.7 μm for spaxels in galaxies classified as SFGs (blue) and AGNs (red). Points with a black dot pertain to the central-most spaxel of each AGN (AGN nucleus). AGN periphery are spaxels from AGNs that exclude the nucleus and cover the periphery of each AGN. Panels (b) and (c), respectively, show the cumulative distribution of 6.2 μm/7.7 μm and 11.3 μm/7.7 μm band ratios, with the median of each distribution indicated by the corresponding short line.
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: (Top) Illustration of high-resolution IRS spectrum of M51, marked with prominent ionic and molecular hydrogen emission lines. (Bottom) Zoom-in of individual narrow emission lines used in this paper (in units of 10−12 erg s−1 cm−2 μm−1); the data are plotted as black histograms, with uncertainties indicated in gray. The red curve is the best-fitting Gaussian profile on top of a linear local continuum (green curve).
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: The PAH band ratios 6.2 μm/7.7 μm and 11.3 μm/7.7 μm for AGN spaxels that have measurements of [S IV]/[Ne III], H2 S(2)/H2 S(0), and [S III] 18.71 μm/[S III] 33.48 μm, color coded according to the ionization parameter calculated based on these line ratios.
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: Integrated low-resolution IRS spectra, with ionic emission lines masked, for the central region of galaxies classified as (a) SFGs and (b) AGNs. The main PAH features are marked in panel (a). Each integrated spectrum is obtained by summing the spectra of all the spaxels within the corresponding central region and normalized by the flux density at 7.7 μm. Panel (c) shows the composite spectra for the regions from SFGs (blue) and AGNs (red).
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: Illustration of PAH decomposition for two sample IRS spectra, from (a) NGC 1097 and (b) NGC 2841. The gray solid lines and black points are the observed IRS spectra and near-IR photometry. The red solid lines give the best-fit model, which is composed of a PAH template (green dashed line), a stellar continuum component (orange dashed line) from Bruzual & Charlot (2003, BC03), and three dust continuum components (blue dashed lines), each represented by a modified blackbody (MBB).
Paper: Experimental Determination of the Dissociative Recombination Rate Coefficient for Rotationally Cold CH+ and Its Implications for Diffuse Cloud Chemistry
Authors: Daniel Paul, Manfred Grieser, Florian Grussie, Robert von Hahn, Leonard W. Isberner, Ábel Kálosi, Claude Krantz, Holger Kreckel, Damian Müll, David A. Neufeld, Daniel W. Savin, Stefan Schippers, Patrick Wilhelm, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: (a) Merged-beams DR rate coefficient of CH+ for two different ion-beam storage-time windows in the CSR. Relative rotational populations in the CSR (see Figure 4) are shown in the inset. The gray areas highlight the storage times for the measurements shown. (b) Comparison of the J = 0 and J = 1 rate coefficients calculated using an MCMC method (see text). In both panels, statistical one-sigma uncertainties are indicated by the error bars and bands, while the absolute scaling uncertainty is ±13%.(The data used to create this figure are available.)
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Correlation between the column density of COMs. The Pearson r coefficient of each pair is presented. The slopes measured in the log–log space are presented as s to give the power-law indices of two given species.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Correlation between the abundances of COMs to N(H2). The Pearson r coefficient of each pair is presented. The slopes measured in the log–log space are presented as s to give the power-law indices of two given species.
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: ISP-corrected observations of SN 2021rhu in the Stokes Q–U plane. The data have been rebinned to 40 Å. The four subpanels on the left (three small square panels for epochs 1–3, plus a larger rectangular panel for epoch 4) present the data in the range 3850–9100 Å, the wavelengths of which are indicated by the left color bar. The ranges of Q and U in the square and rectangular panels are different, but the scales for Q and U are the same in all subpanels. The green long-dashed lines trace the dominant axis of the continuum at different epochs. Note that the dominant axis fitting at day +79 does not represent the orientation of the optical ejecta (see Section 4.2). Data points marked with open black circles indicate the spectral region covering the Ca II NIR3 feature. The corresponding four subpanels on the right show the Ca II line over the velocity range 27,000–2000 km s−1. The right color bar indicates the velocity range of the Ca II NIR3 complex. The light-green long-dashed lines in both left and right subpanels represent the dominant axis fitted to the presented optical wavelength range, while the gray dotted–dashed lines in the right subpanels trace the dominant axis over the Ca II NIR3 feature.
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Keck/HIRES spectra of SN 2021rhu in velocity space relative to Ca II K (top left), Ca II H (top right), Na I D2 (bottom left), and Na I D1 (bottom right) features. The observed spectra have been divided by the respective ambient pseudocontinuum. No apparent temporal evolution between the two epochs has been identified.
Paper: To Rain or Not to Rain: Correlating GOES Flare Class and Coronal Rain Statistics
Authors: E. I. Mason, K. L. Kniezewski
Figure caption: Top left: histogram presenting the percentage frequency of X-class flares hosting post-flare arcade rain of duration ranging from under an hour to over 6 hr. Top right: analogous histogram for M-class flares. Bottom left: analogous histogram for C-class flares; note that these are subdivided into shorter time bins only ranging between <1 hr and 4 hr, due to the absence of any longer post-flare arcade rain events detected in the survey. Bottom right: percentages of flares with post-flare arcade rain by strength within the C-class designation, showing the strong change in post-flare arcade rain occurrence around C5.
Paper: To Rain or Not to Rain: Correlating GOES Flare Class and Coronal Rain Statistics
Authors: E. I. Mason, K. L. Kniezewski
Figure caption: Graph summarizing the duration of post-flare rain events by GOES class. X-class flares have a wide distribution of flare rain durations, while M-class flares’ post-flare arcade rain most often lies in the <1–3 hr range. C-class post-flare arcade rain never exceeded 3 hr in duration in the sample studied here (the bins are not end-inclusive; for a more detailed breakdown of C-class rain times, see Figure 3(d)).
Paper: The Role of Strong Magnetic Fields in Stabilizing Highly Luminous Thin Disks
Authors: Bhupendra Mishra, P. Chris Fragile, Jessica Anderson, Aidan Blankenship, Hui Li, Krzysztof Nalewajko
Figure caption: Pseudocolor plots of the logarithm of gas density. The top panel shows the three-level mesh used in most of the simulations. The remaining panels show the different magnetic field configurations that we consider, with black and white lines showing the different magnetic field polarities: zero net flux, single loop, or dipole (S3Ed, second panel); zero net flux, two loop, or quadrupole (S3Eq, third panel); zero net flux, multiloop (S3Em, fourth panel); and net flux, vertical field (S3Ev, bottom panel). We have truncated the vertical extent of each panel to make the details of the disk more easily visible.
Paper: The Role of Strong Magnetic Fields in Stabilizing Highly Luminous Thin Disks
Authors: Bhupendra Mishra, P. Chris Fragile, Jessica Anderson, Aidan Blankenship, Hui Li, Krzysztof Nalewajko
Figure caption: Spacetime (R − t) plots of the density-squared-weighted scale heights of the disks for the dipole (S3Ed; left), quadrupole (S3Eq; middle), and vertical (S3Ev; right) simulations, showing a vertical collapse for the dipole case and a collapse followed by recovery for the quadrupole and vertical cases. The solid white curves show the estimated thermal timescale.
Paper: The Role of Strong Magnetic Fields in Stabilizing Highly Luminous Thin Disks
Authors: Bhupendra Mishra, P. Chris Fragile, Jessica Anderson, Aidan Blankenship, Hui Li, Krzysztof Nalewajko
Figure caption: Spacetime (R−t) plots of the ratios of the heating rates, Q +, to the cooling rates, Q − for the S3Ed (left), S3Eq (middle), and S3Ev (right) simulations, showing that cooling dominates, especially at smaller radii in S3Ed; heating and cooling balance fairly well in S3Eq; and heating seems to mostly dominate, especially in the outer regions in S3Ev. Inside of ≈10 GM/c 2, the plots are white because the disk is effectively optically thin in those regions, and our heating and cooling formulae do not apply. Beyond that radius, the occasional white patches correspond to locations where the cooling rate takes on negative values, which happens when the flux measured at the photosphere points toward the disk midplane, rather than away. The solid white curves show the estimated thermal timescale.
Paper: The Role of Strong Magnetic Fields in Stabilizing Highly Luminous Thin Disks
Authors: Bhupendra Mishra, P. Chris Fragile, Jessica Anderson, Aidan Blankenship, Hui Li, Krzysztof Nalewajko
Figure caption: Time–space (t−z) plots of ﹩{\beta }_{r}^{-1}﹩ (ratio of azimuthally averaged magnetic pressure to total pressure, P tot = 〈P mag〉 ϕ  + 〈P gas〉 ϕ  + 〈P rad〉 ϕ ) as a function of height in the disks for the S3Ed (left), S3Eq (middle), and S3Ev (right) simulations, evaluated at r = 15 GM/c 2.
Paper:  R-process Rain from Binary Neutron Star Mergers in the Galactic Halo
Authors: Benjamin Amend, Jonathan Zrake, Dieter H. Hartmann
Figure caption: Different regimes of sinking r-process enriched clouds. A BNS merger takes place at an altitude z ej above the midplane of the galactic disk. Material expelled during the merger forms a shell, which decelerates over a length scale ℓ dec (Equation (1)). As it decelerates, the shell becomes corrugated by the Rayleigh–Taylor (RT) instability. The RT structures are denser than the ambient medium, which causes them to begin sinking toward the disk. Clouds which cool slowly (depicted in red) are generally disrupted by Kelvin–Helmholtz (KH) instabilities before they experience significant radiative energy losses. Denser clouds (or those with higher metallicity; depicted in blue) may experience runaway free–free cooling. However, once the temperature drops low enough, the plasma forms neutrals and free–free cooling is suppressed. The cold, dense, neutral clouds are still prone to fragmentation by KH. For any conditions applicable to BNS mergers at altitudes ≳100 pc above the disk, enriched material is fully dissolved into the halo gas. It can only be transported to the ISM through turbulent diffusion (if turbulence operates in the halo) or by large-scale inflowing mass currents.
Paper:  R-process Rain from Binary Neutron Star Mergers in the Galactic Halo
Authors: Benjamin Amend, Jonathan Zrake, Dieter H. Hartmann
Figure caption: Four different timescales associated with solutions to the dynamical heuristic from Section 3.6. The upper panel shows a calculation with the fiducial injection parameters, where the clouds start out and remain in the slow-cooling regime. The lower panel uses a more metal-rich composition, A = 100, corresponding to faster-cooling clouds. After the clouds cool and condense, radiative cooling is suppressed by recombination. The clouds then sink more rapidly, and are ultimately disrupted by the KH instability.
Paper: Erratum: “The Ultraviolet C II Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae” (2022, ApJ, 936, 143)
Authors: Zheng-Wei Yao, Yong Zhang
Figure caption: The C II]λ2326/C II λ1335 CE line intensity ratio vs. T  U  for N e = 1000 cm−3. The curves indicate the theoretical predictions for various κ values, among which the solid line represents the κ = ∞ case (i.e., the Maxwell–Boltzmann, MB, distribution). The circles with error bars are the observed values in PNs that are not corrected for the effects of DR and resonance scattering, where the open and filled circles represent T  M (BJ) (the MB-EED-based electron temperature derived from the Balmer jump) and the derived T  U , respectively. The filled triangles denote the observed values in quasars, where we have assumed T  U  ≡ 1.5 × 104 K. The open and filled squares represent the values corrected for the effects of DR and resonance scattering by assuming C++/C+ = 1 and 5, respectively.
Paper:  R-process Rain from Binary Neutron Star Mergers in the Galactic Halo
Authors: Benjamin Amend, Jonathan Zrake, Dieter H. Hartmann
Figure caption: The evolution of the cloud velocity (top), normalized cloud mass (upper middle), temperature (lower middle), and altitude (bottom) for two different cloud compositions, corresponding to the cases presented in Figure 3. More metal-rich material cools faster. The horizontal dashed line in the middle panel shows the cooling threshold temperature ﹩{T}_{\min }={10}^{4}\,{\rm{K}}﹩.
Paper:  R-process Rain from Binary Neutron Star Mergers in the Galactic Halo
Authors: Benjamin Amend, Jonathan Zrake, Dieter H. Hartmann
Figure caption: Vertical profile of the hydrostatic equilibrium profile that we adopted for the halo atmosphere, for representative values of the number density n disk at the base of the atmosphere. The top panel shows the number density n env as a function of altitude. The middle panel shows the corresponding nominal deceleration length scale ℓ dec (Equation (1)) for the fiducial outflow mass M ej = 0.01M ⊙. The bottom panel shows the vertical temperature profile. Note that it is insensitive to the density normalization.
Paper:  R-process Rain from Binary Neutron Star Mergers in the Galactic Halo
Authors: Benjamin Amend, Jonathan Zrake, Dieter H. Hartmann
Figure caption: The fractional vertical distance below the explosion altitude z ej at which total assimilation of the r-process clouds takes place, as a function of z ej. Different curves represent different cloud compositions, with larger A corresponding to less efficient dilution by the ambient halo medium. These calculations are for the fiducial values of M ej = 10−2 M ⊙, and θ RT = 0.1.
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Schematic depiction of gas in a conical accretion column accreting onto the magnetic pole of a neutron star. Seed photons created via blackbody (gold lines), cyclotron (red lines), and bremsstrahlung (cyan lines) emission are reprocessed via electron scattering and eventually escape through the walls and top of the column to form the observed X-ray spectrum (green lines).
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: The mode-change cross sections are plotted as functions of the propagation angle θ using Equation (29) from Meszaros & Ventura (1979) for parameters appropriate for Her X-1 (left) and X Per (right). Results include the total cross sections (solid lines), the mode-coherent cross sections (dashed lines), and the mode-changing cross sections (dotted lines). The energies of the extraordinary (X) and ordinary (O) mode photons are indicated by the color legends.
Paper: On the X-Ray, Optical, and Radio Afterglows of the BdHN I GRB 180720B Generated by Synchrotron Emission
Authors: J. A. Rueda, Liang Li, R. Moradi, R. Ruffini, N. Sahakyan, Y. Wang
Figure caption: Luminosity of GRB 180720B in the X-ray (0.3–10 keV), optical (r band), and radio (5.0 and 9.0 GHz) energy bands. The X-ray data are produced by the methods developed by the Swift XRT team to produce the the light curves (Evans et al. 2009). The radio data from AMI-LA are retrieved from Rhodes et al. (2020), and the r-band optical data are retrieved from Abdalla et al. (2019).
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Hydrodynamical flow velocity, υ* (green dots), obtained by numerically integrating Equation (197), compared with the model flow velocity, υ (blue lines), computed using Equation (45) for Her X-1 (left) and X Per (right). The good agreement indicates that the dynamical models for the two accretion columns are physically self-consistent.
Paper: On the X-Ray, Optical, and Radio Afterglows of the BdHN I GRB 180720B Generated by Synchrotron Emission
Authors: J. A. Rueda, Liang Li, R. Moradi, R. Ruffini, N. Sahakyan, Y. Wang
Figure caption: Optical luminosity of prototype SN 1998bw (gray) vs. optical (purple) afterglow of GRB 180720B. In this GRB, no optical data were observed ∼16–24 days after the trigger as we predicted in Ruffini et al. (2018b). Most likely, the associated SN could have been detected if optical observations had been made at the time. The r-band optical data are retrieved from Abdalla et al. (2019). The optical luminosity of prototype SN 1998bw is plotted from reference (Iwamoto et al. 1998).
Paper: A Generalized Analytical Model for Thermal and Bulk Comptonization in Accretion-powered X-Ray Pulsars
Authors: Peter A. Becker, Michael T. Wolff
Figure caption: Proton temperature distribution, T  p  (blue lines), plotted as a function of y = R/R * by numerically integrating Equation (193), for Her X-1 (left) and X Per (right). Also plotted for comparison is the isothermal electron temperature, T  e  (green dots).
Paper: On the X-Ray, Optical, and Radio Afterglows of the BdHN I GRB 180720B Generated by Synchrotron Emission
Authors: J. A. Rueda, Liang Li, R. Moradi, R. Ruffini, N. Sahakyan, Y. Wang
Figure caption: Luminosity light curve of GRB 180720B including the observations in gamma rays from Fermi GBM (yellow), soft X-rays from Swift XRT (red), radio data from AMI-LA (brown diamonds; retrieved from Rhodes et al. 2020), and r-band optical data (purple circles; retrieved from Abdalla et al. 2019).
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: (Left) Angular diameter, θ sh, of the shadow of a Ghosh–Culetu black hole, in units of μas, as a function of (a, g). Black lines are for 46.9 μas and 50 μas, corresponding to the Sgr A* black hole shadow bounds. Ghosh–Culetu black holes that have parameters between the two black lines produce a shadow that is consistent with the magnitude of the Sgr A* shadow. (Right) Angular diameter, θ sh, of the shadow of a Bardeen no-horizon spacetime, in units of μas, as a function of (a, g).
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Deviations of the angular diameters of the shadows of Ghosh–Culetu black holes (left) and no-horizon spacetimes (right) from that of a Schwarzschild black hole, as a function of (a, g). The black and green lines are, respectively, for the values of δ = −0.04 (Keck) and δ = −0.08 (VLTI), corresponding to the Sgr A* black hole shadow bounds.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Deviations of the shadows of Hayward black holes (left) and no-horizon spacetimes (right) from that of a Schwarzschild black hole, as a function of (a, g). The black and green lines are, respectively, for the values of δ = −0.04 (Keck) and δ = −0.08 (VLTI), corresponding to the Sgr A* black hole shadow bounds.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Simpson–Visser black hole (left) and no-horizon spacetime (right) shadows' angular diameter deviations from that of a Schwarzschild black hole as a function of (a, g). The black and green lines are, respectively, for the values of δ = −0.04 (Keck) and δ = −0.08 (VLTI) corresponding to the Sgr A* black hole shadow bounds.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Simpson–Visser black hole (left) and no-horizon spacetime (right) shadows' angular diameters θ sh, in units of μas, as a function of (a, g). Black line is for 46.9 μas, corresponding to the Sgr A* black hole shadow bounds.
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Ghosh–Culetu black hole (left) and no-horizon spacetime (right) shadows' circularity deviation observables ΔC as a function of (a, g).
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Hayward black hole (left) and no-horizon spacetime (right) shadows' circularity deviation observables ΔC, as a function of (a, g).
Paper: Testing Rotating Regular Metrics with EHT Results of Sgr A*
Authors: Rahul Kumar Walia, Sushant G. Ghosh, Sunil D. Maharaj
Figure caption: Simpson–Visser black hole (left) and no-horizon spacetime (right) shadows' circularity deviation observables ΔC as a function of (a, g).