adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Authors: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
Figure caption: Phased light curves of (324) Bamberga (top panel), (13) Egeria (middle panel), and (22) Kalliope (bottom panel) at 2.0 mm, folded over the rotational period and scaled to mean observed solar distance, Earth distance, and solar phase angle as described in Section 4. The dotted blue lines represent the sinusoidal function that best fits the data, although none of these fits are statistically significant. The sinusoidal periods are constrained to half the rotational periods, but the amplitudes and phases are free parameters.
Paper: Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Authors: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
Figure caption: Objects with predicted S/N > 3 at 2.0 mm in all historic and planned future SPT data. We expect to observe (2) Pallas, plotted off scale, with a mean flux density near 650 mJy.
Paper: Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Authors: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
Figure caption: Mean flux measurements of (772) Tanete (top horizontal panels) and (1093) Freda (bottom horizontal panels) at 3.2 mm (left vertical panels), 2.0 mm (middle vertical panels), and 1.4 mm (right vertical panels). These measurements were taken with the SPT-3G camera in the main survey field during the 2020 austral winter.
Paper: Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Authors: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
Figure caption: Observation geometries for (324) Bamberga (top panel), (13) Egeria (middle panel), and (22) Kalliope (bottom panel). Each point represents one observation. Solar distance r ⊙ and Earth distance r ⊕ are plotted in astronomical units, and solar phase angle α is plotted in degrees.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: The ratio of [C/α] against the H I column density (left) and neutral fraction (right) from the KODIAQ-Z (2.2 ≲ z ≲ 3.6), HD-LLS (2.2 ≲ z ≲ 3.6), and CCC (z ≲ 1) surveys. The median values of the [C/α] posterior pdf’s are adopted as the central values with 68% CI.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Comparison of the median metallicities (with 68% CI) of KODIAQ-Z derived using the HM12 and HM05 EUVBs. The dashed line is the 1:1 relationship. The dotted line shows the mean of the differences between the metallicities derived using HM12 and HM05.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: The log U median values as a function of N H I  for 126 absorbers in the KODIAQ-Z sample. The solid line shows a linear fit to the data with ﹩14.6\leqslant \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\leqslant 17.2﹩ (with a slope −0.46 ± 0.10 and intercept +5.56). The plus signs show the mean values of the median values in each N H I  interval indicated by the horizontal bar.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Difference between the median metallicities for the KODIAQ-Z and HD-LLS absorbers derived using the HM12 and HM05 EUVBs against the H I column densities of the absorbers.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Comparison of the metallicities (top) and ionization parameters (bottom) derived without and with using C IV in the photoionization modeling as a function of the H I column density. The median values of posterior pdf’s of the metallicity and log U are adopted as the central values with 68% CI.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Comparison of the posterior metallicity pdf’s of the SLFSs (KODIAQ-Z) and pLLSs+LLSs (KODIAD-Z+HD-LLS). The light-colored region indicates the contribution from the upper limits.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Comparison of the posterior metallicity pdf’s of the LLSs in the KODIAQ-Z and HD-LLS sample. The light-colored region indicates the contribution from the upper limits.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Posterior metallicity pdf of the SLFSs in the KODIAQ-Z sample. The light-colored region indicates the contribution from the upper limits.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Posterior metallicity pdf’s of the pLLSs in the KODIAQ-Z sample. The light-colored region indicates the contribution from the upper limits.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Temperature, mean molecular weight, and energy generation rate for the Strang CFL = 0.2 run with normal tolerances (strang_subch2_cfl0.2) at 0.1 s.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Flowchart of the simplified-SDC approach. An iteratively lagged advection term is used to update the system to the new time, with each iteration improving the coupling.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Temperature, mean molecular weight, and energy generation rate for the simplified-SDC CFL = 0.2 run with normal tolerances (sdc_subch2_cfl0.2) at 0.1 s.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Energy generation rate for the Strang CFL = 0.2 run with normal tolerances (strang_subch2_cfl0.2) shown at four consecutive time steps around t = 0.1 s, zoomed-in at the inward-propagating detonation.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Initial model for the double-detonation test problem.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Comparison of Strang runs showing the nuclear energy generation rate behind the inward-propagating shock.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Comparison of Strang runs, showing the mean molecular weight behind the inward-propagating shock.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Comparison of simplified-SDC runs, showing the nuclear energy generation rate behind the inward-propagating shock.
Paper: An Improved Method for Coupling Hydrodynamics with Astrophysical Reaction Networks
Authors: M. Zingale, M. P. Katz, A. Nonaka, M. Rasmussen
Figure caption: Comparison of simplified-SDC runs, showing the mean molecular weight behind the inward-propagating shock.
Paper: Two-dimensional Configuration and Temporal Evolution of Spark Discharges in Pulsars
Authors: Rahul Basu, George I. Melikidze, Dipanjan Mitra
Figure caption: Single pulse simulations demonstrating bi-drifting behavior. (a) Pulse stack with 128 simulated single pulses. There are four components in the average profile with the two leading components drifting in opposite directions to the trailing ones. (b) LRFS across the pulse window. The drifting periodicity, P 3 = 15.7P is seen as a peak frequency, f  p  ∼ 0.06 cycles/P, in the left window. The time evolution of the spark pattern is reflected in the phase behavior across the profile with the first two components showing a negative slope while the phases show a positive slope in their variations in the trailing components (top window).
Paper: The Effects of a Magnetar Engine on the Gamma-Ray Burst-associated Supernovae: Application to Double-peaked SN 2006aj
Authors: Zhen-Dong Zhang, Yun-Wei Yu, Liang-Duan Liu
Figure caption: The best fit of the multiwavelength double-peaked light curves of SN 2006aj by using the model including a magnetar wind-driven SBO emission and a magnetar-aided supernova emission, for the parameter values listed in Table 1. The left and right panels are shown in a linear and logarithmic-scale x-axis, respectively. The observational data are taken from Nakar (2015) and Campana et al. (2006).
Paper: The Effects of a Magnetar Engine on the Gamma-Ray Burst-associated Supernovae: Application to Double-peaked SN 2006aj
Authors: Zhen-Dong Zhang, Yun-Wei Yu, Liang-Duan Liu
Figure caption: The schematic diagram of the model (not to scale).
Paper: The Effects of a Magnetar Engine on the Gamma-Ray Burst-associated Supernovae: Application to Double-peaked SN 2006aj
Authors: Zhen-Dong Zhang, Yun-Wei Yu, Liang-Duan Liu
Figure caption: Posterior distributions of parameters for the fittings of SN 2006aj.
Paper: Additions to the Spectrum of Fe IX in the 110–200 Å Region
Authors: Alexander N. Ryabtsev, Edward Y. Kononov, Peter R. Young
Figure caption: The iron spectrum in the range 169.0–170.3 Å taken at three modes of the spark operation: cold—black, intermediate—blue, and hot—red. The lines are marked by the symbols: VI—Fe VI (only prominent lines), and IX—Fe IX. The relative intensities in arbitrary units are scaled so that the Fe IX lines have approximately the same intensities in the intermediate and hot spectra, whereas the Fe VI lines have approximately the same intensities in the cold and intermediate spectra.
Paper: Additions to the Spectrum of Fe IX in the 110–200 Å Region
Authors: Alexander N. Ryabtsev, Edward Y. Kononov, Peter R. Young
Figure caption: Two iron spectra correspond to hot (red) and cold (black) excitation conditions. The lines are marked by the symbols: VII—Fe VII, VIII—Fe VIII, and IX—Fe IX. Lines due to the three iron species are distinguished by their relative intensities in the two spectra. Arrows indicate the Fe IX lines at 111.692 and 112.011 Å.
Paper: Additions to the Spectrum of Fe IX in the 110–200 Å Region
Authors: Alexander N. Ryabtsev, Edward Y. Kononov, Peter R. Young
Figure caption: A                       C HIANTI                    synthetic spectrum showing the location of known Fe IX lines. Colors and numbers denote different transition arrays. Line profiles are represented as Gaussians with an FWHM of 3 Å. A temperature of 0.8 MK and an electron number density of 4.0 × 108 cm−3 were used. The wavelength range of the EIS short-wavelength (SW) band is indicated.
Paper: Additions to the Spectrum of Fe IX in the 110–200 Å Region
Authors: Alexander N. Ryabtsev, Edward Y. Kononov, Peter R. Young
Figure caption: The iron spectrum in the 133.8–134.3 Å range taken in the cold (black) and hot (red) modes of the spark operations (see Figure 5).
Paper: Additions to the Spectrum of Fe IX in the 110–200 Å Region
Authors: Alexander N. Ryabtsev, Edward Y. Kononov, Peter R. Young
Figure caption: A section of the photoplate spectrum obtained at a current of 100 kA.
Paper: Additions to the Spectrum of Fe IX in the 110–200 Å Region
Authors: Alexander N. Ryabtsev, Edward Y. Kononov, Peter R. Young
Figure caption: The photoplate spectrum obtained at a current of 40 kA.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage: Evidence for Kinematics Evolution of Broad-line Region
Authors: Sha-Sha Li, Hai-Cheng Feng, H. T. Liu, J. M. Bai, Rui Li, Kai-Xing Lu, Jian-Guo Wang, Ying-Ke Huang, Zhi-Xiang Zhang
Figure caption: Line width vs. time lag. The left panel: our observational results of FWHM vs. time lag. The blue data is τ Mean, and the red data is τ Mean plus τ b−uv. The blue and red dashed lines represent the best-fit lines with slopes of −0.15 ± 0.04 and −0.21 ± 0.06, respectively. The right panel: rms σ line vs. time lag for all of the data. The black dashed line represents the best-fit line with a slope of −0.36 ± 0.10. The black solid line in each panel is the best-fit line using the virial relation with a slope of −0.5.
Paper: Modeling Long-term Variability in Stellar-compact Object Binary Systems for Mass Determinations
Authors: Nicholas M. Sorabella, Sayantan Bhattacharya, Silas G. T. Laycock, Dimitris M. Christodoulou, Alessandro Massarotti
Figure caption: A step-by-step process of a black hole gravitationally lensing a background star. Panel 1 shows the star (circled in red) just outside the Einstein radius (orange). Panel 2 shows the surface area of the star increasing as a secondary image of the star (circled in blue) forms. Panel 3 depicts when the black hole is directly in front of the star; the two images of the stars connect to form a perfect ring around the black hole where maximum amplification occurs. Panel 4 shows the image of the star returning to normal, as the secondary image begins to fade. Finally, panel 5 shows the lensing process having been completed. This figure was created using SpaceEngine.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage: Evidence for Kinematics Evolution of Broad-line Region
Authors: Sha-Sha Li, Hai-Cheng Feng, H. T. Liu, J. M. Bai, Rui Li, Kai-Xing Lu, Jian-Guo Wang, Ying-Ke Huang, Zhi-Xiang Zhang
Figure caption: The velocity-resolved time-delay results of Hα, Hβ, Hγ, He I, and He II. The top panel in each subgraph shows the velocity-resolved structure for each emission line. In each panel, the horizontal dotted line and gray band represent the ICCF measured lag and CCCD estimated errors, respectively. The vertical dashed lines denote the edges of each velocity bin. The bottom panel in each subgraph shows the rms spectrum of each emission line, for which the continuum is subtracted.
Paper: Modeling Long-term Variability in Stellar-compact Object Binary Systems for Mass Determinations
Authors: Nicholas M. Sorabella, Sayantan Bhattacharya, Silas G. T. Laycock, Dimitris M. Christodoulou, Alessandro Massarotti
Figure caption: The orbits of a sunlike star and a 10 M ⊙ black hole. The orbital period is 3 days and the eccentricity is set to e = 0.3. The black hole size is exaggerated, so it can easily be seen, but the size of the star is to scale relative to the size of its orbit. The origin of the coordinate system is the center of mass of the binary.