adsabs/AstroCLIMB huggingface dataset:
Paper: Impact of the Accretion Disk Thickness on the Polarization of the Thermal Emission from Stellar Mass Black Holes
Authors: Andrew Thomas West, Henric Krawczynski
Figure caption: Simulation results for different disk scale heights H (from left to right: H = 0.0, 0.1, 0.2, and 0.3) and different inclinations I (from top to bottom: i = 25°, 45°, 65°, and 85°). The color scale gives the total flux (direct and reflected) using a logarithmic color scale. The lengths and directions of the black bars give the linear polarization degree and angle, respectively. The polarization angle is measured with respect to the black hole spin axis, with 180° being aligned with the spin axis and 90° being aligned with the disk and orthogonal to the spin axis. The overall polarization degrees increase with increasing inclinations. At the highest inclination, the disk shadows itself, the cooler outer edges (near 50 r g) blocking some emission from the innermost regions of the disk, as well as some of the lensed emission from below the disk.
Paper: Impact of the Accretion Disk Thickness on the Polarization of the Thermal Emission from Stellar Mass Black Holes
Authors: Andrew Thomas West, Henric Krawczynski
Figure caption: Polarization angle (left) and degree (right) inclinations of 65° (top row) and 75° (bottom row) for both direct and reflected emission. The standard thin disk model is in black. The torus model with a scale height of zero for three different outer radii, 50r  g  (red), 75r  g  (blue), and 100r  g  (pink) is overplotted for comparison. The polarization angle is measured with respect to the black hole spin axis, with 180° being aligned with the spin axis and 90° being aligned with the disk.
Paper: Impact of the Accretion Disk Thickness on the Polarization of the Thermal Emission from Stellar Mass Black Holes
Authors: Andrew Thomas West, Henric Krawczynski
Figure caption: Energy spectra (left), polarization degree (middle), and polarization angle (right) for inclinations of 25° (top row), 45° (second row), 65° (third row), and 85° (bottom row). Flux energy spectra are approximately uniform across scale heights for a given inclination, with the exception of very high—nearly edge-on—inclinations where disk self-shadowing becomes apparent. Polarization degree minima shift to lower energies with increasing scale height, as the geometry leads lower-energy emission to scatter that would otherwise have gone directly to the observer. This same effect causes the polarization angle to swing from horizontal to vertical at lower energies with increasing scale heights.
Paper: Impact of the Accretion Disk Thickness on the Polarization of the Thermal Emission from Stellar Mass Black Holes
Authors: Andrew Thomas West, Henric Krawczynski
Figure caption: Polarization degree (left) and polarization angle (right) for a thin disk (solid lines) and a torus with a scale height of H = 0.2 (dashed lines) for spin values of a = 0.5 (black), 0.8 (red), and 0.9 (blue). These are plotted for two inclinations, i = 65° (top row) and 75° (bottom row). Note that at 65°, a thin disk with a = 0.9 and a torus with a spin of a = 0.5 are degenerate.
Paper: Impact of the Accretion Disk Thickness on the Polarization of the Thermal Emission from Stellar Mass Black Holes
Authors: Andrew Thomas West, Henric Krawczynski
Figure caption: This plot shows the average number of scatterings for photons emitted from various radii for the thin disk and the three scale heights explored. The figure represents scattered photons received for an observer inclination of 65°. Photons launched at small radii, inside the “doughnut hole” of the accretion flow, scatter more often than photons emitted further out, at the outward-facing sides of the disk.
Paper: Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, J. A. García, D. Altamirano, D. J. K. Buisson, E. M. Cackett, J. Chenevez, N. Degenaar, A. C. Fabian, J. Homan, A. Jaodand, S. N. Pike, A. W. Shaw, T. E. Strohmayer, J. A. Tomsick, B. M. Coughenour
Figure caption: Eddington fraction F Edd and the location of the inner disk as measured for several NS LMXBs studied with NuSTAR, and compared to this work. The Eddington fraction is the given luminosity of the source compared to the empirical Eddington luminosity for an NS. We see that there is almost no correlation between F Edd and the inner disk radius, which differs from the more rigid correlation seen in BH LMXBs. A previous measurement of R in from reflection modeling of NuSTAR data for this source is filled in black.
Paper: Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, J. A. García, D. Altamirano, D. J. K. Buisson, E. M. Cackett, J. Chenevez, N. Degenaar, A. C. Fabian, J. Homan, A. Jaodand, S. N. Pike, A. W. Shaw, T. E. Strohmayer, J. A. Tomsick, B. M. Coughenour
Figure caption: The unfolded spectra and model components for each observation as the flux varies. The model components shown here are those displayed in Table 5. The power law, displayed with a blue dotted line, becomes the dominant contributor to the overall spectrum during Obs3, the lowest flux state.
Paper: Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, J. A. García, D. Altamirano, D. J. K. Buisson, E. M. Cackett, J. Chenevez, N. Degenaar, A. C. Fabian, J. Homan, A. Jaodand, S. N. Pike, A. W. Shaw, T. E. Strohmayer, J. A. Tomsick, B. M. Coughenour
Figure caption: Light curve for the NuSTAR/FPMA and NICER observations of 4U 0614+091 binned to 128 s. Each panel represents a unique observation epoch, which is indicated by the unique symbols in each plot. The gray dashed and solid lines indicate the average count rate for NuSTAR and the NICER, respectively. Only one focal plane module is shown for clarity.
Paper: Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, J. A. García, D. Altamirano, D. J. K. Buisson, E. M. Cackett, J. Chenevez, N. Degenaar, A. C. Fabian, J. Homan, A. Jaodand, S. N. Pike, A. W. Shaw, T. E. Strohmayer, J. A. Tomsick, B. M. Coughenour
Figure caption: (Top) O VIII Lyα line profile from NICER for observations 1, 2, 3, and 5 centered at ∼0.7 keV. (Bottom) Fe Kα profile from FPMA in NuSTAR centered at ∼6.5 keV. The Fe features are notably weaker than the O VIII features, with the former peaking at around 6% above the continuum, and the latter peaking at around 15% above the continuum.
Paper: Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, J. A. García, D. Altamirano, D. J. K. Buisson, E. M. Cackett, J. Chenevez, N. Degenaar, A. C. Fabian, J. Homan, A. Jaodand, S. N. Pike, A. W. Shaw, T. E. Strohmayer, J. A. Tomsick, B. M. Coughenour
Figure caption: The plot above demonstrates that while there appears to be some negative correlation between the flux of the power-law component and the flux of the reflected emission, the 90% error bars show that across all observations except observation 3, which is the right-most point, the reflected emission is relatively consistent.
Paper: Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, J. A. García, D. Altamirano, D. J. K. Buisson, E. M. Cackett, J. Chenevez, N. Degenaar, A. C. Fabian, J. Homan, A. Jaodand, S. N. Pike, A. W. Shaw, T. E. Strohmayer, J. A. Tomsick, B. M. Coughenour
Figure caption: The hardness-intensity diagrams for different NICER and NuSTAR energy bands for each joint observation of 4U 0614+091. The top two panels are constructed from NICER data while the bottom panel is NuSTAR.
Paper: Impact of the Accretion Disk Thickness on the Polarization of the Thermal Emission from Stellar Mass Black Holes
Authors: Andrew Thomas West, Henric Krawczynski
Figure caption: Torus geometry for scale heights of 0.1 (dashed line), 0.2 (dotted line), and 0.3 (dashed–dotted line). Axes are in units of r  g .
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Top left: model ring width ratio assuming size-dependent dust trapping for the given dust size ﹩{a}_{\max }﹩ and exponent of dust size distribution p. The orange contour shows the observed constraint in the inner ring, and the red one shows that in the outer ring. Top right: model opacity spectral index β. Middle left and right: constrained parameter space of ﹩{a}_{\max }﹩ and p in the inner ring (left) and in the outer ring (right) from the ring width ratio and spectral index. Bottom left and right: dust opacity in Band 6 (left) and in Band 4 (right).
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Top: normalized optical depth profiles in Band 6 with a linear scale. The horizontal axis is the radial distance normalized by the dust ring width of 1 mm grains w dust(1 mm). The dotted lines are Gaussian fittings for the model profiles, and we define the traced dust size in Section 5.3 from these fitted widths. Middle: normalized optical depth profiles in Band 6 (1.25 mm) and Band 4 (2.14 mm) with a log scale. The solid lines show the opacity distributions in Band 6, and the dashed lines show those in Band 4. Each color corresponds to each exponent of the dust size distribution N(a) ∝ a −p . The gray dotted lines show the distribution of the maximum (a = 10 cm) and the minimum (a = 1μ m) dust. Bottom: radial opacity spectral index profile between Band 6 and Band 4.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The dust opacity profile of compact (solid line) and porous (dashed line) dust. We used the dust model of Birnstiel et al. (2018).
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The same as Figure 13, but for the inner ring in Band 4.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The corner plot for the inner ring in Band 6. The dotted lines in the top panels show the 16th, 50th, and 84th percentiles of the marginal distributions. The blue lines show the parameter set that maximizes the probability.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Representative dust size if p = 3.5 in Band 6 (blue) and Band 4 (orange). The gray line shows ﹩{a}_{\mathrm{rep}}={a}_{\max }﹩.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The same as Figure 8, but assuming porous dust grains with the filling factor f = 0.01.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The same as Figure 13, but for the outer ring in Band 6.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The same as Figure 13, but for the outer ring in Band 4.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: The same as Figure 8, but assuming the dust model of Ricci et al. (2010), which assumes amorphous carbon as a carbonaceous material.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Time series plot for four flares observed by MinXSS-1. These four flares will illustrate the analysis and process of all the flares MinXSS-1 observed. The top left is the 2016 July 23 M5.0 flare; top right the 2016 July 21 M1.0 flare; bottom left is the 2016 July 23 M7.6; and bottom right is the C4.1 2017 February 22 flare. The pink and blue shaded region are the GOES predefined start and end times. The MinXSS-X123 is shown in black boxes, MinXSS-XP in black stars and GOES/XRS 1–8 Å in purple, 0.5–4 Å in blue. On top of each panel the red, yellow, and green bars show the impulsive, peak and decay phase of each flare. Additionally, on the bottom of each flare we show the evolution of reduced chi-square from the spectra fit as a function of time. We note that during the peak of the flare the reduced chi-square value is approximately 1.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Average absolute abundance during the SXR peak for 21 flares observed by MinXSS-1. The white circles are where the elemental abundance parameter are set to coronal values, while the color circles are fitted parameters. The dark blue line shows the coronal abundances from Feldman & Widing (2003) and the purple line shows the photospheric abundances from Asplund et al. (2009). The absolute abundances are on logarithmic scale with A(H) = 12. We note that most fitted parameters are below the coronal abundance implying that the lower atmospheric plasma is filling the coronal loops. The Fe abundance parameter is only fitted for the 6.7 keV feature. The Fe abundance for the C5.6 flare has large uncertainties due to a high abundance value during the nonflaring time period.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Volume emission measure plot for four flares observed by MinXSS-1. The top left is the 2016 July 23 M5.0 flare; top right the 2016 July 21 M1.0 flare; bottom left is the 2016 July 23 M7.6; and bottom right is the C4.1 2017 February 22 flare. These plots show the two background volume emission measures used in red and blue horizontal dashed lines with its respective shaded uncertainty. The best fit for the two volume emission measure components during the flare are denoted in circles. The uncertainties shown for the best-fit parameters are calculated using the Monte Carlo analysis available in OSPEX. Additionally, we plot the derived GOES volume emission measures available in SolarSoftware. We note that the best-fit volume emission measures closely follow the GOES derived volume emission measures.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Temperature plots for four flares observed by MinXSS-1. The top left is the 2016 July 23 M5.0 flare; top right the 2016 July 21 M1.0 flare; bottom left is the 2016 July 23 M7.6; and bottom right is the C4.1 2017 February 22 flare. These plots show the two background temperatures used in red and blue horizontal dashed lines with its respective shaded uncertainty. The best fit for the two temperature components during the flare are denoted in circles. The uncertainties shown for the best-fit parameters are calculated using the Monte Carlo analysis available in OSPEX. We note that the uncertainties during the impulsive phase are large due to the lack of statistical significant signal.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Time evolution of absolute abundance for Fe (blue), Ca (orange), S (green), and Si (red) during the four flares observed by MinXSS-1 X123. The navy line shows the coronal abundances from Feldman & Widing (2003) and the purple line shows the photospheric abundances from Asplund et al. (2009). The white points are where the model assumes a coronal abundance since the count-rate spectra do not have an S/N for the elemental abundance parameter to be fitted. The absolute abundances are on logarithmic scale with A(H) = 12. We note that at the peak of the flare most elements are depleted from coronal toward photospheric values during the peak phase of each flare.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Relationship of volume emission measure and temperature during nonflaring (background) and SXR peaking times. The values are represented in Tables 1 and 2. In the background panel (left), the lower temperature corresponds to a lower volume emission measure. The darker circles are where a both the low and high temperatures converge to a single value. In the average SXR peak panel (right), there is no clear relationship between volume emission measure and temperature.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Count-rate spectra fit during the nonflaring (background) times with normalized residuals for four flares observed by MinXSS-1 X123. The top left is the 2016 July 23 M5.0 flare; top right the 2016 July 21 M1.0 flare; bottom left is the 2016 July 23 M7.6; and bottom right is the C4.1 2017 February 22 flare. The observed MinXSS-1 X123 spectra is shown in dark gray, and the double emission measure and temperature spectra fit in cyan. The black vertical lines represent the low and high energy limits for the fit. The colored vertical lines approximately represent the elemental features for Fe (1.2 and 6.7 keV), Ca (4.0 keV), Mg (1.7 keV), Si (2.1 keV), S (2.7 keV), and Ar (3.0 keV).
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Normalized radial intensity profiles assuming Gaussian optical depth distributions. The width of the Gaussian is σ = 1 for all models. The solid lines are the profiles without beam convolution, and the dotted lines are the profiles with beam convolution corresponding to the Band 6 beam size for the inner ring width (σ = 2.5 au/4.8 au = 0.46). The profile has a flat top if the ring is optically thick and the beam resolves the ring.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Histogram of the average peak volume emission measure and temperature of 21 flares observed by MinXSS-1. The volume emission measure ranges from 1047 to 1049 cm−3 and temperatures from ∼4 to 21 MK.
Paper: Constraints on the Dust Size Distributions in the HD 163296 Disk from the Difference of the Apparent Dust Ring Widths between Two ALMA Bands
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡
Figure caption: Top: the observed radial intensity profile in Band 6 and 4. Bottom: the slope α of the SED at each radius. The left gray regions represent the observed beam size, and the left vertical bar represents the uncertainties from the absolute flux calibration error with 1σ ranges.
Paper: Estimations of Elemental Abundances during Solar Flares Observed in Soft X-Rays by the MinXSS-1 CubeSat Mission
Authors: Crisel Suarez, Christopher S. Moore
Figure caption: Abundance of Fe (7.9 eV), Ca (6.1 eV), S (10.4 eV), Si (8.2 eV), and Ar (15.8 eV) as a function of FIP energy. Black circles are MinXSS-1 weighted arithmetic mean values during the peak of the flare, the orange crosses are the values reported in Dennis et al. (2015) from 526 flares observed by Messenger/SAX, the light blue triangles are from Narendranath et al. (2014) from 20 flares observed by Chandrayaan-1/XSM, the green squares are from from Mondal et al. (2021) from nine flares observed by Chandrayaan-2/XSM, the red stars are from 20 flares observed by RHESSI (Phillips & Dennis 2012) or 33 flares observed by RESIK (Sylwester et al. 2015), brown diamonds are from 10 flares observed by OSO-8 (Veck & Parkinson 1981), and green hexagons are from 21 flares observed by SDO/EVE (Warren 2014). The left panel shows the absolute abundances are on logarithmic scale with A(H) = 12. The navy line shows the coronal abundances from Feldman & Widing (2003) and the purple line shows the photospheric abundances from Asplund et al. (2009). We note how the MinXSS-1 estimated elemental abundances are between the coronal and photospheric values. The right panel shows the elemental abundance in terms of FIP bias with respect to the Asplund et al. (2009) values. The MinXSS-1 estimated low-FIP elements (Ca, Fe, Si) are ≈2–4 times more abundant compare to the photosphere abundance, the mid-FIP element (S) and high-FIP element (Ar) are ≈1.5 more abundant compare to the photosphere abundance.
Paper: The Impulsive Acceleration of a Solar Filament Eruption Associated with a B-class Flare
Authors: Xinyue Wang, Hongqiang Song, Yao Chen, Leping Li, Zhenyong Hou, Ruisheng Zheng
Figure caption: (a) Height–time plot constructed along the yellow dashed line in Figure 1(d) with the flare location as the zero height. The red asterisks delineate the trajectory of the filament's rising motion. The horizontal dashed line marks the solar limb. (b) The projected (red) and corrected (black) heights vs. time.
Paper: The Impulsive Acceleration of a Solar Filament Eruption Associated with a B-class Flare
Authors: Xinyue Wang, Hongqiang Song, Yao Chen, Leping Li, Zhenyong Hou, Ruisheng Zheng
Figure caption: (a) Velocity vs. time plot (black), along with the GOES SXR flux (red line). (b) Acceleration vs. time (black), along with the RHESSI HXR (25–50 keV) flux (red line). The black dashed lines mark the start time of the initiation phase, the start and end times of the impulsive acceleration phase from left to right sequentially, and the red dashed line marks the start time of the flare rise phase.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: Apparent column density profiles for a few LRGs with possible O VI 1031 detection. Blue and orange lines represent O VI 1031 and O VI 1037 apparent column densities multiplied by the length of the velocity intervals corresponding to the velocity bins. Red and green vertical lines correspond to the LRG’s redshift and Mg II LRG–CGM system’s redshift, respectively. LRG name is shown in the upper-right corner.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: The same as Figure 14, but for confirmation of H I in LRG_1237+1106, and for a comparison between O VI 1031 and H I 972 in LRG_0855+5615.