adsabs/AstroCLIMB huggingface dataset:
Paper: Optical Continuum Reverberation in the Dwarf Seyfert Nucleus of NGC 4395
Authors: John W. Montano, Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Vivian U, Raymond Remigio, Diego H. González-Buitrago, Juan V. Hernández Santisteban
Figure caption: Rest-frame interband lag τ gz as a function of AGN continuum luminosity at 5100 Å (left), BH mass (middle), and the product L × M BH (right). The g –z lags of eight local AGN are from literature sources as described in the text. The AGN continuum luminosities and black hole masses for the comparison sample are from Bentz & Katz (2015). The quantity L 5100 refers to λ L  λ  at 5100 Å. For NGC 4395, the horizontal error bar on M BH denotes the range spanning 1.7 × 104 to 4 × 105 M ⊙ corresponding to the mass measurements from Cho et al. (2021) and den Brok et al. (2015). The black solid and dotted lines in each panel denote the power-law model fit and its 1σ uncertainty range.
Paper: Optical Continuum Reverberation in the Dwarf Seyfert Nucleus of NGC 4395
Authors: John W. Montano, Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Vivian U, Raymond Remigio, Diego H. González-Buitrago, Juan V. Hernández Santisteban
Figure caption: Lags as a function of wavelength in the rest frame of NGC 4395, from the combined Night 1 + Night 2 data. Horizontal error bars denote the width of each filter. The β = 4/3 power-law fit to the riz data points is shown as a red curve. Blue dashed and dotted curves represent SSD lag–wavelength models calculated for BH masses of 1.7 × 104 and 4 × 105 M ⊙, respectively.
Paper: Optical Continuum Reverberation in the Dwarf Seyfert Nucleus of NGC 4395
Authors: John W. Montano, Hengxiao Guo, 恒潇 郭, Aaron J. Barth, Vivian U, Raymond Remigio, Diego H. González-Buitrago, Juan V. Hernández Santisteban
Figure caption: NGC 4395 light curves and cross-correlation lags. Left: MuSCAT3 light curves in the griz bands. Right: cross-correlation results for each band, measured relative to the g band. Each panel shows cross-correlation functions (curves across the upper portion of the panel) and cross-correlation centroid distributions (histograms, renormalized to arbitrary units) for the data from Night 1 and from Night 2 separately, and for the combined Night 1 + Night 2 light curves. The g-band panel displays the autocorrelation functions and autocorrelation centroid distributions of the g-band light curves.
Paper: Inefficient Growth of SiOx Grains: Implications for Circumstellar Outflows
Authors: Yuki Kimura, Kyoko K. Tanaka, Yuko Inatomi, Frank T. Ferguson, Joseph A. Nuth
Figure caption: Snapshots of in situ observations at the moment of nucleation of SiO from hot vapor. Left and right panels show double-wavelength interference fringes and the real image, respectively, (A) before heating (T+358.94 s), (B) just before nucleation (T+366.01 s), and (C) during nucleation (T+366.88 s). T is time of launch. The 0.2 mm diameter Ta rod is connected to Cu electrodes (ϕ 6.0 mm). (D) Color-separated interference fringes of panel (C) and corresponding time series images at the position indicated by white lines from 5 s before heating. The vertical dashed line and horizontal and vertical axes in the time series images are the time of nucleation and time from 358.93 to 384.91 s and position from X1 to X2, respectively. The center of the dotted circle, 4.5 mm in radius, is approximately at the center of evaporation as seen in the right plot of panel (C).
Paper: Inefficient Growth of SiOx Grains: Implications for Circumstellar Outflows
Authors: Yuki Kimura, Kyoko K. Tanaka, Yuko Inatomi, Frank T. Ferguson, Joseph A. Nuth
Figure caption: Temperature profile and SiO concentration at nucleation. (A) Temperature distribution in terms of the distance from the evaporation source in time after the start of heating. The bar, diamond, triangle, star, and circle symbols show 0.5, 0.9, 1.3, 1.9, and 2.1 s after the start of heating of the evaporation source, respectively. The red square at 4.5 s shows the nucleation point and temperature. (B) The black cross shows the temperature and concentration of SiO molecules just before nucleation. The green and red lines show the relationship between the temperature and the concentration of the SiO molecule to explain the deviations in the interference fringes for the green and red lasers, respectively.
Paper: Inefficient Growth of SiOx Grains: Implications for Circumstellar Outflows
Authors: Yuki Kimura, Kyoko K. Tanaka, Yuko Inatomi, Frank T. Ferguson, Joseph A. Nuth
Figure caption: Particle characteristics. (A) Bright field TEM image of SiO grains. (B) Corresponding electron diffraction pattern of panel (A) indicates the amorphous structure of the SiO particles. (C) Size distribution of SiO grains. The median and mean diameters are 18.4 nm and 24.4 nm, respectively; 95% of particles are in the range of 8–56 nm. (D) Energy dispersive X-ray spectrum of the particles suggests that the atomic ratio of silicon and oxygen is Si/O = 3/4.
Paper: Inefficient Growth of SiOx Grains: Implications for Circumstellar Outflows
Authors: Yuki Kimura, Kyoko K. Tanaka, Yuko Inatomi, Frank T. Ferguson, Joseph A. Nuth
Figure caption: Plots of sticking probabilities and surface tensions regarding the nucleation temperature and mean radius using MCNT. Each line shows the mean particle radius and condensation temperature obtained from the calculations when the surface tension is 1.0, 1.33, and 1.4 N m−1, respectively. The numbers of points on the line indicate the value of α used in the calculations. The sticking probability and surface tension to explain the experimental results, which are the nucleation temperature of 950 K and mean radius of 12.2 nm, are α = 1.6 × 10−2 and σ = 1.33 N m−1 (1330 erg cm−1), respectively. The error bar on the y-axis includes a size range of 95% of the particles, 4–28 nm in radius.
Paper: Inefficient Growth of SiOx Grains: Implications for Circumstellar Outflows
Authors: Yuki Kimura, Kyoko K. Tanaka, Yuko Inatomi, Frank T. Ferguson, Joseph A. Nuth
Figure caption: MCNT calculated results for the formation of silica grains. (A) The dashed and solid curves show the time variation in the nucleation rate and the number density of gas-phase SiO molecules n 1(t), respectively, in the case of a sticking probability of α = 1.6 × 10−2 and a surface tension of σ =1.33 N m−1 (1330 erg cm−1). The vertical dotted line shows the nucleation temperature derived from the experiment. (B) Growth curve of a typical SiO grain.
Paper: GRB 211211A: a Prolonged Central Engine under a Strong Magnetic Field Environment
Authors: He Gao, Wei-Hua Lei, Zi-Pei Zhu
Figure caption: Illustration of our model. With the magnetic barrier effect, the accretion of the major inflow corresponds to the hard spiky ME of GRB 211211A, and the accretion of the residual inflow corresponds to the soft EE of GRB 211211A. The GRB jet is powered by the Blandford–Znajek (BZ) mechanism, which extracts the rotational energy of the Kerr BH through a large-scale magnetic field. Here R halt marks the radius where the radial magnetic force can give support against the gravitational force. R ms marks the radius of the marginally stable orbit. The light-curve picture of GRB 211211A is adopted from Xiao et al. (2022).
Paper:  r-process Viable Outflows are Suppressed in Global Alpha-viscosity Models of Collapsar Disks
Authors: O. Just, M. A. Aloy, M. Obergaulinger, S. Nagataki
Figure caption: Color maps showing, for the viscous model a03, the distributions of density, ρ, radial velocity, v  r , electron fraction, Y  e , and entropy per baryon, s/k  B , at several characteristic times: (a) shortly before disk formation, (b) shortly after disk formation before the NDAF-to-ADAF transition, (c) for the same time as (b) but showing the expanding shock, (d) right after the transition to ADAF, (e) shortly after shock breakout from the stellar surface, and (f) during transition to the homologous expansion phase. Black arrows indicate the velocity field, while their length is capped above velocities of 109 cm s−1. Isocontours of relevant temperatures are marked with various black lines (see legend in panel (a)).
Paper:  r-process Viable Outflows are Suppressed in Global Alpha-viscosity Models of Collapsar Disks
Authors: O. Just, M. A. Aloy, M. Obergaulinger, S. Nagataki
Figure caption: Same as Figure 3, but for the nonviscous model a0, with velocity arrows whose length is capped at 108 cm s−1, and at the characteristic times right before (a) and after disk formation (b), during the shock expansion through the stellar mantle (c), and shortly after shock breakout (d).
Paper: HST/WFC3 Hα Direct-imaging Detection of a Pointlike Source in the Disk Cavity of AB Aur
Authors: Yifan Zhou, Aniket Sanghi, Brendan P. Bowler, Ya-Lin Wu, Laird M. Close, Feng Long, Kimberly Ward-Duong, Zhaohuan Zhu, Adam L. Kraus, Katherine B. Follette, Jaehan Bae
Figure caption: Primary-subtracted images (upper) and the S/N maps (lower) of AB Aur observed by HST/WFC3/UVIS in the F656N filter. The left column shows the primary-subtracted natively sampled images (pixel scale = 40 mas), and the right column shows the reconstructed images (pixel scale = 20 mas). The upper panels show the intensity maps (in units of e− s−1). These images, as well as the upper panels of Figure 2, the left panel of Figure 3, and Figure 4 are smoothed using a Gaussian kernel with FWHM = 0.″07 (1.0 × PSF FWHM). Smoothing improves visualization by reducing high-frequency noise but is not applied in the sensitivity or contrast curve estimates. The lower panels are the S/N maps. For all four images, the color maps have a linear stretch. The central r = 0.″3 radius circle is masked out, because in this region the detection sensitivity is poor due to high contrasts, and saturation. In the upper left panel, an ellipse marks the transition disk cavity identified by Francis & van der Marel (2020). In the lower left panel, gray dashed lines indicate the spiral disk structures (S1–S4) detected in our images. The pointlike source at 0.″6 south of AB Aur is visible in all panels.
Paper: HST/WFC3 Hα Direct-imaging Detection of a Pointlike Source in the Disk Cavity of AB Aur
Authors: Yifan Zhou, Aniket Sanghi, Brendan P. Bowler, Ya-Lin Wu, Laird M. Close, Feng Long, Kimberly Ward-Duong, Zhaohuan Zhu, Adam L. Kraus, Katherine B. Follette, Jaehan Bae
Figure caption: Primary-subtracted images and S/N maps in Epochs 1 (left four panels) and 2 (right four panels). The intensity and S/N maps obtained from processing the natively sampled and reconstructed images are organized in the same way as Figure 1. The pointlike source is consistently recovered in both epochs, although the detection S/Ns are below 5 in the second epoch due to shorter integration time. Systematic residuals near the diffraction spikes are also prominent in the second epoch.
Paper: HST/WFC3 Hα Direct-imaging Detection of a Pointlike Source in the Disk Cavity of AB Aur
Authors: Yifan Zhou, Aniket Sanghi, Brendan P. Bowler, Ya-Lin Wu, Laird M. Close, Feng Long, Kimberly Ward-Duong, Zhaohuan Zhu, Adam L. Kraus, Katherine B. Follette, Jaehan Bae
Figure caption: The SED of AB Aur b (upper left), PDS 70 b (upper right), a comparison of the two SEDs (lower left), and a comparison to the stellar Hα emission of AB Aur (lower right). The SED of AB Aur b includes optical to near-IR measurements from Currie et al. (2022; blue squares and solid line) and the Hα flux from the combined HST data in this work (orange square). All AB Aur b fluxes are dereddened based on A  V  = 0.5 mag and R  V  = 3.1. The best-fitting blackbody (3800 K) is shown in a green dashed line. In contrast, the near-IR SED of PDS 70 b (gray circles; data source: Müller et al. 2018; Mesa et al. 2019; Wang et al. 2020; Stolker et al. 2020) is best-fit by a 1200 K blackbody (black dashed line). In the bottom left panel, we normalize the two SEDs by their respective Hα flux, so the Hα points (orange square for AB Aur b, black circle for PDS 70 b) overlap. AB Aur b is bluer and has a stronger optical continuum. In the bottom right panel, flux is normalized to the continuum (for AB Aur b, it is the HST/STIS flux). The Hα of AB Aur b is consistent with the stellar value within 1σ.
Paper: HST/WFC3 Hα Direct-imaging Detection of a Pointlike Source in the Disk Cavity of AB Aur
Authors: Yifan Zhou, Aniket Sanghi, Brendan P. Bowler, Ya-Lin Wu, Laird M. Close, Feng Long, Kimberly Ward-Duong, Zhaohuan Zhu, Adam L. Kraus, Katherine B. Follette, Jaehan Bae
Figure caption: The injection-and-recovery image (left) and the 5σ contrast curve (right). The injection-and-recovery test is conducted on the natively sampled images. Injected artificial planets with the same brightness as the one measured in the pointlike source are consistently recovered, and their recovered photometry is used in correcting companion flux loss in primary subtraction and calibrating the contrast curve. The inset in the left panel is the inner r = 0.″7 circular region of the injection-and-recovery image, where the artificial sources have the same angular separations as AB Aur b. In the right panel, the 5σ contrast measurements are shown in squares, which are connected by a spline interpolation (solid line). The loss of sensitivity at 3.″6 to 4.″0 is due to a known filter ghost.
Paper: HST/WFC3 Hα Direct-imaging Detection of a Pointlike Source in the Disk Cavity of AB Aur
Authors: Yifan Zhou, Aniket Sanghi, Brendan P. Bowler, Ya-Lin Wu, Laird M. Close, Feng Long, Kimberly Ward-Duong, Zhaohuan Zhu, Adam L. Kraus, Katherine B. Follette, Jaehan Bae
Figure caption: A zoomed-in (﹩2^{\prime\prime} \times 2^{\prime\prime} ﹩) natively sampled primary-subtracted image highlighting the detection of the pointlike source. The source is at a P.A. of 182° and a separation of 600 mas relative to the host star. This detection is at the location of AB Aur b, a candidate embedded planet recently reported by Currie et al. (2022).
Paper: Standing Solitary Waves as Transitions to Spiral Structures in Gravitationally Unstable Accretion Disks
Authors: Hongping Deng, Gordon I. Ogilvie
Figure caption: Nonlinear periodic ring structures and solitary waves. (a) Periodic structures (only one wavelength is shown) with base wavenumber K in an isothermal disk with Q −1  =  0.95. As K decreases, the solutions transition to a solitary pattern (only the central part is shown here). (b), (c) Solitary waves for different Q −1 and different Γ parameters, focusing on the central part of the solitary waves. The different line colors sweep the K, Q −1, or Γ parameters at constant rates, with the cooler colors representing smaller coefficients.
Paper: PSR J0952−0607: The Fastest and Heaviest Known Galactic Neutron Star
Authors: Roger W. Romani, D. Kandel, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng
Figure caption: Left: calibrated ugriz light curves from Keck LRIS spectrophotometry (filled dots) and direct imaging (open dots). Outlier points excluded in the “trimmed” model fitting are indicated by orange crosses. The curves show the best-fit ugriz models and the dotted line marks pulsar inferior conjunction. Right: residuals to the best model fit. Optionally excluded points are again marked by orange crosses. The spectra used for Figures 1–3 are available as data behind the Figure.
Paper: PSR J0952−0607: The Fastest and Heaviest Known Galactic Neutron Star
Authors: Roger W. Romani, D. Kandel, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng
Figure caption: RV measurements for J0952. Dot size is proportional to the correlation coefficient R; low-significance correlations with R < 2 are marked with black crosses and are excluded from all fits. Three higher-significance points marked with green crosses appear as outliers and are optionally excluded for the “trimmed” fit. The background curve is the best-fit RV curve for the heating model fit to the light curve in Figure 1. The lower panel shows the fit residuals.
Paper: Standing Solitary Waves as Transitions to Spiral Structures in Gravitationally Unstable Accretion Disks
Authors: Hongping Deng, Gordon I. Ogilvie
Figure caption: Nonaxisymmetric modes attacking the solitary waves, and their growth rates. (a) Growing modes (﹩{v}_{x}^{{\prime} }﹩) attacking the solitary wave in a direct numerical simulation (K = 0.08, only the central part plotted) of an isothermal disk with Q −1  =  0.95. (b) Fastest-growing mode (Floquet analysis, arbitrary units) attacking the same solitary wave as in (a). (c) Growth rates of modes with various k  y  in isothermal disks with solitary waves. The star symbol indicates the fastest growth rate measured in the numerical simulation in (a).
Paper: Standing Solitary Waves as Transitions to Spiral Structures in Gravitationally Unstable Accretion Disks
Authors: Hongping Deng, Gordon I. Ogilvie
Figure caption: Energy change per unit area due to periodic rings or solitary waves. (a) Energy change for K = 1 solutions. (b) Energy change as a function of the base wavenumber K in isothermal disks. At a sufficiently small K, ΔE/K tends to a constant because the solution transits to a solitary wave and the total energy change is invariant. (c) Energy change due to solitary waves (calculated with K = 0.08). The total energy change per unit length in the y-direction is 78.54 ΔE.
Paper: PSR J0952−0607: The Fastest and Heaviest Known Galactic Neutron Star
Authors: Roger W. Romani, D. Kandel, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng
Figure caption: Spectrum of the heated face. S/N-weighted average of 27 individual spectra, Doppler corrected to zero velocity, using the best-fit RV model. Select lines are indicated.
Paper: PSR J0952−0607: The Fastest and Heaviest Known Galactic Neutron Star
Authors: Roger W. Romani, D. Kandel, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng
Figure caption: Corner plot from the MCMC light-curve fit to the “trimmed” photometry points. Contours are at 0.5σ, 1.0σ, 1.5σ, and 2σ.
Paper: Standing Solitary Waves as Transitions to Spiral Structures in Gravitationally Unstable Accretion Disks
Authors: Hongping Deng, Gordon I. Ogilvie
Figure caption: The maxima of σ as a function of Q −1 when K = 1.
Paper: PSR J0952−0607: The Fastest and Heaviest Known Galactic Neutron Star
Authors: Roger W. Romani, D. Kandel, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng
Figure caption: Mass estimates for heavy NSs. The dashed curves show the two heaviest WD–pulsar binaries with masses measured from radio pulse timing (supplemented by WD atmosphere modeling for J0348). The solid curves show the best mass estimates from companion spectroscopy and light-curve fitting for four BWs (J1810, J1653, J1311, and J0952) and one RB (J2215). The bottom panel shows the normalized Ln(Likelihood) for various combinations of these measurements, assuming a flat distribution of masses from 1.8 M ⊙ up to some ﹩{M}_{\max }﹩. The inset legend gives the median estimator for ﹩{M}_{\max }﹩ as well as the 1σ, 2σ, and 3σ lower bounds on its value, for various data subsets.
Paper: Water Shielding in the Terrestrial Planet-forming Zone: Implication for Inner Disk Organics
Authors: Sara E. Duval, Arthur D. Bosman, Edwin A. Bergin
Figure caption: The molecular abundance of various species over the inner 5 au, determined from the IR-emitting layer, for the standard and water-shielding models. The locations of the water and CO2 ice lines are at 0.27 and 0.94 au, respectively. The drops in abundance near 0.9 au are a result of drops in the gas temperature in the surface layer (see Section 4).
Paper: Water Shielding in the Terrestrial Planet-forming Zone: Implication for Inner Disk Organics
Authors: Sara E. Duval, Arthur D. Bosman, Edwin A. Bergin
Figure caption: The 2D abundance distributions of the six species for the standard and water-shielding models in the inner 5 au. The red line signifies the location of our estimate of the IR-emitting layer above z/r ∼ 0.15. It is clear that with the inclusion of water UV shielding, these species reach higher abundances at locations higher up in the disk atmosphere.
Paper: 10 Yr Transformation of the Obscuring Wind in NGC 5548
Authors: Missagh Mehdipour, Gerard A. Kriss, Elisa Costantini, Liyi Gu, Jelle S. Kaastra, Hermine Landt, Junjie Mao
Figure caption: Swift/XRT hardness ratio (R) lightcurve of NGC 5548. It spans from 2005 April to 2022 April with a time binning of one month. Vertical dotted lines are drawn on the first day of each calendar year for reference. For data since 2012, the corresponding X-ray covering fraction (C X) of the obscuring wind is shown on the right axis. The 2005 and 2007 data are not obscured (see Section 3). The horizontal dashed line is drawn at R with zero obscuration (C X = 0) derived from the 2002 unobscured Chandra spectrum. The long-term rise and decline of the obscuration are evident.
Paper: 10 Yr Transformation of the Obscuring Wind in NGC 5548
Authors: Missagh Mehdipour, Gerard A. Kriss, Elisa Costantini, Liyi Gu, Jelle S. Kaastra, Hermine Landt, Junjie Mao
Figure caption: Top panel: relation between the equivalent width (EW) of the broad C IV UV absorption feature and the X-ray hardness ratio (R). Bottom panel: relation between the C IV UV covering fraction (C UV) and the X-ray covering fraction (C X) of the obscuring wind. Data correspond to contemporaneous Swift and HST/COS observations, taken in 2013, 2014, 2016, and 2022. A time bin size of one week is used to average the data. The Spearman’s rank correlation coefficient (r  s ) and the null hypothesis probability (p null) are given in the inset, showing both relations are statistically highly significant. The best-fit function describing each relation is given in the inset and displayed as a dashed line.
Paper: Water Shielding in the Terrestrial Planet-forming Zone: Implication for Inner Disk Organics
Authors: Sara E. Duval, Arthur D. Bosman, Edwin A. Bergin
Figure caption: 2D distributions of water and CO2 for a full and reduced chemical network shown in the top and bottom panels, respectively. The reduced chemical network is used in Bosman et al. (2022a). The region above the red line at z/r ∼ 0.15 corresponds to the location of our estimation of the IR-emitting layer. For water, we can see specifically around 1 au near the IR-emitting layer that the model with UV shielding has a noticeably larger abundance than the standard model, as expected. For a reduced chemical network, the abundances drop at closer-in radii due to the fact that the water-ice lines are at smaller radii (Bosman et al. 2022a). We are focusing on the region in the IR-emitting layer, so between the models, the abundance is about the same, validating the use of a smaller chemical network to obtain the emitting area of water. For CO2, we also see very similar abundances in the IR-emitting layer between a full and reduced chemical network.
Paper: 10 Yr Transformation of the Obscuring Wind in NGC 5548
Authors: Missagh Mehdipour, Gerard A. Kriss, Elisa Costantini, Liyi Gu, Jelle S. Kaastra, Hermine Landt, Junjie Mao
Figure caption: X-ray (top panel) and UV (middle and bottom panels) spectra of NGC 5548 taken at epochs of zero obscuration (2002), strong obscuration (2013), and diminished obscuration (2022). The 2002 spectra are from Chandra/LETG and HST/STIS. The 2013 and 2022 spectra are from Swift/XRT and HST/COS. The UV spectral regions of interest are highlighted in yellow. In 2022, the X-ray obscuration (top panel), the broad C IV absorption (middle panel), and the narrow C II absorption (bottom panel) are diminished together.
Paper: Water Shielding in the Terrestrial Planet-forming Zone: Implication for Inner Disk Organics
Authors: Sara E. Duval, Arthur D. Bosman, Edwin A. Bergin
Figure caption: Abundant gas-phase species for the standard and water-shielding models at 0.3 au and 0.6 au. C2H2, CH4, C3, CH3CN, and LCC have abundances below 1012 cm−2 for the standard model. It should be noted that at 0.6 au, there is a higher abundance of LCC in ice form. (LCC signifies large carbon chains containing four or more carbons).