adsabs/AstroCLIMB huggingface dataset:
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Median extracted spectra of WASP-96 and comparisons, excluding the oversaturated COMP 3. The top row shows IMACS data (UT170804 and UT171108) and the bottom shows FORS2 data from Nikolov et al. (2018; UT170729 and UT170822). Each spectroscopic bin used is shaded in light gray and demarcated by dotted lines. Telluric regions with less than 0.1 transmission are shaded in light red. The only gap in the binning scheme is the strong telluric region from 7594.0–7672.0 Å.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: High-resolution FEROS spectrum of WASP-96: Both Ca II H and K lines (top), where the dashed red lines correspond to the K line core centered at 393.366 nm and the H line core centered at 396.847 nm. The left bottom panel is zoomed in on the K line, and the bottom right is zoomed in on the H line, with the central cores highlighted with red dotted lines in both. There is no emission seen in either of the cores.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: W2 images of V367 Cyg and two stars in the same WISE image tile. All images are displayed with the same brightness stretch. The V367 Cyg isophotes are not flattened, suggesting that the emitting material is not confined to a disk. The FWHM of the stellar images is ∼9″. V367 Cyg is not a point source, and there are localized peaks in the light distribution that may be companion stars. However, point sources alone cannot account for the angular extent of the light distribution at 4.5 μm.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: Data from LCOGT NRES spectra of the primary star HIP 5319 A compared to a PHOENIX model spectrum for an F5IV star surrounding the Ca II H line at its vacuum wavelength λ = 3969.5 Å. The model spectrum has been broadened by 100 km s−1 to match the best-fit vsin(i) value for the Ca II H line from the LCOGT spectra. (Left top) Model spectra plotted over data from the 12 LCOGT spectra between λ = 3955–3985 Å. (Left bottom) The O−C (Observed−Calculated) plot showing the residuals between measured data and model. Gray points are the residuals from each of the 12 spectra, while the red points are rebinned to the original NRES spectral resolution. (Right) The same data and residuals between λ = 3968–3972 Å. In both cases it can be clearly seen that there is no excess flux beyond the 1% level in the spectrum at any point near the Ca H line.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: (Top) Radial-velocity (left) and vsin(i) (right) values measured for HIP 5319A. The dotted lines in each panel are the best-fit constant velocity to the data, where RV = 16.71 km s−1 and vsin(i) = 94.21 km s−1. Neither metric shows either significant variation in time or obvious periodicity. (Bottom) Periodograms of the residuals from the radial-velocity (left) and vsin(i) (right) values. The residuals for each metric are calculated by taking the measured data and subtracting the best-fit constant velocity. The false-alarm probability of 1%, calculated using bootstrap randomization, is shown by the dashed lines.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Light profiles of V367 Cyg (solid line) and the PSF (dotted line) in the W2 filter. The profiles have been normalized to their peak values, and each pixel along the x-axis subtends 1.″5. The V367 Cyg profile is that of the central column that passes through the image in Figure 13. The V367 Cyg light profile is wider than that of the PSF, and this cannot be explained by multiple point sources (see text). Rather, there appears to be emitting material in the W2 image that is spread out over ∼19,000 au around V367 Cyg.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: Detection of HIP 5319 B from SCExAO coupled with MEC, CHARIS, and VAMPIRES, and Keck II Adaptive optics coupled with NIRC2. The MEC and VAMPIRES images retain some residual signal from satellite spots used for spectrophotometric and astrometric calibration. In MEC data, these spots appear with different brightnesses due to vignetting from the optics in MEC and dead pixels on the array, both of which have since been corrected. The NIRC2 image also retains some signal from the primary that was not removed by RDI-KLIP. The CHARIS data do retain some residual signal although the signal is so low that it cannot be seen without drastically lowering the maximum value of intensity in the image and saturating the PSF.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: Combined SCExAO/CHARIS spectra, SCExAO/MEC photometry, SCExAO/VAMPIRES and Keck/NIRC2 photometry of the low-mass companion HIP 5319 B taken on 2020 July 31 (CHARIS and MEC), 2021 September 11 (CHARIS and VAMPIRES), and 2022 January 15 (NIRC2) at the Subaru and Keck II telescopes. The reddest CHARIS channel has substantially higher uncertainty in our spectrophotometric calibration because we did not obtain sky frames.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: (Top) Minimum detectable binary companion mass for various periods (P) and inclinations (i). For a given combination of period and inclination, the reported “minimum detectable mass” can be found, which corresponds to the lowest mass a companion would have that would result in a semiamplitude K > 3 km s−1. Any companions less than that mass would be undetectable in the spectroscopic data and any companions that were more massive would have been detected. (Bottom) Minimum detectable mass as a function of period for selected inclinations.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: The CHARIS HIP 5319 B spectrum (black) compared to those of field brown dwarfs (magenta) with spectral types M0, M5, and L0 from the Montreal Spectral Library binned to CHARIS’s resolution.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: Corner plot showing the posterior distributions of selected orbital parameters using a Gaussian prior of 0.2 ± 0.1M ⊙ for the mass of the secondary companion. The orbit fits used Hipparcos and Gaia (HGCA) absolute astrometry and relative astrometry from SCExAO/CHARIS and MEC data. The inset in the figure shows the best fit orbit (black) with 50 random orbits drawn from the MCMC fits color coded by the mass of HIP 5319 B. The red-colored points in the orbit represent relative astrometry points from the three epochs where data were taken, and the unfilled circles show the predicted location of the companion at different past and future epochs. The companion is orbiting counterclockwise.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: Corner plot showing the posterior distributions of selected orbital parameters using a log-normal (1/M) prior for the mass of the secondary companion. The orbit fits used Hipparcos and Gaia (HGCA) absolute astrometry and relative astrometry from SCExAO/CHARIS and MEC data. The inset in the figure shows the best-fit orbit (black) with 50 random orbits drawn from the MCMC fits color coded by the mass of HIP 5319 B. The red-colored points in the orbit represent relative astrometry points from the three epochs where data were taken, and the unfilled circles show the predicted location of the companion at different past and future epochs. The companion is orbiting counterclockwise.
Paper: SCExAO and Keck Direct Imaging Discovery of a Low-mass Companion Around the Accelerating F5 Star HIP 5319 
Authors: Noah Swimmer, Thayne Currie, Sarah Steiger, G. Mirek Brandt, Timothy D. Brandt, Olivier Guyon, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor Tobin, Tyler D. Groff, Julien Lozi, John I. III Bailey, Alexander B. Walter, Neelay Fruitwala, Nicholas Zobrist, Jennifer Pearl Smith, Gregoire Coiffard, Rupert Dodkins, Kristina K. Davis, Miguel Daal, Bruce Bumble, Sebastien Vievard, Nour Skaf, Vincent Deo, Nemanja Jovanovic, Frantz Martinache, Motohide Tamura, N. Jeremy Kasdin, Benjamin A. Mazin
Figure caption: (Left) BT-Settl model for solar metallicity with T = 3200 K and log(g) = 5.5. CHARIS spectra is shown in dark blue, VAMPIRES, MEC, and NIRC2 photometry in cyan compared to the model-predicted CHARIS spectrophotometry in light green, and predicted VAMPIRES/MEC/NIRC2 photometry (dark green crosses). Although the S/N of the spectrum is quite high, the spectral covariance in the CHARIS data is also high, leading to a large value of χ 2. (Right) Corresponding contour plots for χ 2 as a function of temperature and surface gravity. The best-fit solution is shown with a red diamond while the 1σ, 2σ, 3σ, and 5σ contours are shown in white, magenta, blue, and purple, respectively.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: A top-down view of the planetary system HD 45364, showing the orbits of the (b) and (c) planets, where the left panel shows those reported by C09. The green annuli represent the extent of the HZ for the system, where the light green indicates the extent of the CHZ, and the dark green indicates the OHZ extension to the CHZ. The right panel shows the revised orbits with the new RV data presented later in this paper.
Paper: A Mass–Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake
Figure caption: Stellar mass as a function of absolute G RP magnitude. Stars from our sample of binary systems that have 2MASS measurements with ﹩10.5\,\gt \,{M}_{{K}_{s}}\,\gt \,4.5﹩ and K  s  < 14.0 can have their masses estimated via the Mann et al. (2019) relation and are shown in blue. Green points show the masses derived from isochrones and high-resolution spectra by Brewer et al. (2016). Our best-fit M GORP mass estimates and corresponding uncertainties are shown for each bin in absolute G RP magnitude as white points at each bin center. The best-fit mass–magnitude relation from Equation (8) is shown as the red dashed line and the 68% confidence interval for that relation is shown by the red dotted lines. The MIST evolutionary track for 5 Gyr solar metallicity stars is overplotted in gold for reference. The square point at ﹩{M}_{{G}_{\mathrm{RP}}}=14.5﹩ is from the literature and is not derived from our analyses, and as such is denoted with a square.
Paper: A Mass–Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake
Figure caption: Comparing the observed μ′ distributions for stars with Mann et al. (2019) masses for systems with different physical separations and distances. Residual systematic effects in eDR3 proper motions may impact the relative proper motion measurement in systems where the components are closer together on the sky. We find broad agreement in the μ′ distributions of these different subsamples. Top: μ′ distribution for all systems, those with physical separations larger than 1083 au and smaller than 1083 au. Bottom: μ′ distribution for all systems, those closer than 135 pc and farther than 135 pc.
Paper: A Mass–Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake
Figure caption: Distribution of mass ratios q = M 2/M 1 inferred from our mass–magnitude relation using binary star systems with 0.8 M ⊙ < M < 0.9 M ⊙ within d < 210 pc. We find that the distribution of q increases toward lower values of q. Our sample is not necessarily volume-limited for q < 0.2, denoted by the shaded region.
Paper: A Mass–Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake
Figure caption: Distribution of D within the ﹩8.5\,\gt \,{M}_{{G}_{\mathrm{RP}}}\,\gt \,8.0﹩ bin. The best-fit model for these data is indicated by the dashed line. For this particular set of 223 twin binary systems, the best-fit parameters for the model given in Equation (5) are M tot = 0.88 ± 0.08 M ⊙, α = 0.90 ± 0.49, N = 0.22 ± 0.09, and σ = 0.68 ± 0.28.
Paper: A Mass–Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake
Figure caption: Relative errors in our M GORP mass estimates compared to those calculated from the Mann et al. (2019) method. The relative internal uncertainties, σ GORP/M Mann, are shown as error bars.
Paper: A Mass–Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake
Figure caption: Mass function estimated using our M GORP relation over the volume-limited Gaia sample of stars in the range 10 pc < d < 50 pc and ∣b∣ > 10°. The mean number density of stars per cubic parsec per solar mass is shown in red, along with the 68% confidence interval.
Paper: A Mass–Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake
Figure caption: Sample posterior distributions for three of our specified absolute magnitude bins. The 68% highest density interval is shown underneath the distribution with the modal value indicated by a dashed line.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Top panels: PM VPD for clusters Pi 2, Pi 3, and Pi 7 based on Gaia EDR3. Bottom panels: G vs. (G  BP  − G  RP ) CMDs. Left: the entire sample. Middle: stars in VPDs within a circle of 0.3, 0.6, and 0.4 mas yr−1 of the cluster’s mean for Pi 2, Pi 3, and Pi 7, respectively. Right: probable background/foreground field stars in the direction of these clusters. We have used only stars with PM σ smaller than 0.5 mas yr−1 in each coordinate.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Same as Figure 3, but for clusters Pi 12 and Pi 15. The radii of circles for both clusters are 0.4 and 0.3 mas yr−1.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: The finding chart of clusters Pi 2, Pi 3, and Pi 7 taken from the Leicester Database and Archive Service (LEDAS). The inner circle shows the cluster’s radius (5.′5, 6.′5, and 4.′5 for clusters Pi 2, Pi 3, and Pi 7), and the outer ring denotes our data extraction radius of 10.′ for all clusters.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: PM histograms of 0.1 mas yr−1 bins in R.A. and decl. of the clusters Pi 2, Pi 3, and Pi 7. The Gaussian function fit to the central bins provides the mean values in both directions as shown in each panel.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Same as Figure 1, but for clusters Pi 12 and Pi 15. The inner circle indicates the radius value as 5.′5 and 6.′5 for clusters Pi 12 and Pi 15, respectively.
Paper: The Si K Edge Gas and Dust Optical Depths Toward the Galactic Bulge
Authors: Jun Yang, Norbert S. Schulz, Daniele Rogantini, Claude R. Canizares, Lia Corrales, Ioanna Psaradaki
Figure caption: Left: the modeled optical depths in comparison with the directly determined optical depths. The dashed line indicates equality. The red data points represent the gas depth values, the blue data points the dust depth values. Right: the modeled optical depths now plotted vs. the measured broadband column densities. The red data points represent gas, the blue data points dust. The red dashed line shows the expectation for the gas optical depths growing linearly with column density. The blue dashed line shows the same for the dust optical depths. Here we used the dust model calculations based on olivine as was used in Schulz et al. (2016).
Paper: The Si K Edge Gas and Dust Optical Depths Toward the Galactic Bulge
Authors: Jun Yang, Norbert S. Schulz, Daniele Rogantini, Claude R. Canizares, Lia Corrales, Ioanna Psaradaki
Figure caption: Left: HETG broadband N H fit results in comparison with previous missions with significantly lower spatial resolution. Previous mission data mostly are from RXTE and XMM-Newton. Right: the Si abundance excess determined in the broadband fits. This shows that by not addressing dust in the Si K edge structure, the fit produces an overabundances by about a factor of 2 for silicon.
Paper: The Si K Edge Gas and Dust Optical Depths Toward the Galactic Bulge
Authors: Jun Yang, Norbert S. Schulz, Daniele Rogantini, Claude R. Canizares, Lia Corrales, Ioanna Psaradaki
Figure caption: Plot of the direct extraction of gas and dust optical depths. The x-axis reflects the gas optical depth, similar to what is designated as “Case A” in Schulz et al. (2016), the y-axis the total optical depth (gas + dust), as designated as “Case B.”
Paper: The Si K Edge Gas and Dust Optical Depths Toward the Galactic Bulge
Authors: Jun Yang, Norbert S. Schulz, Daniele Rogantini, Claude R. Canizares, Lia Corrales, Ioanna Psaradaki
Figure caption: Calculating optical depths of dust grains using the self-shielding formalism outlined in Wilms et al. (2000). The measured depths can then be represented by three different dust columns in the various lines of sight. Plotted are calculations for two different dust sizes, 0.025 μm (left) and 0.3 μm (right).
Paper: The Si K Edge Gas and Dust Optical Depths Toward the Galactic Bulge
Authors: Jun Yang, Norbert S. Schulz, Daniele Rogantini, Claude R. Canizares, Lia Corrales, Ioanna Psaradaki
Figure caption: Two examples of unfolded data spectra around the Si K edge. Left: this is the edge for GX 3+1 with more than twice the number of data shown in Schulz et al. (2016). Marked are the locations of the gas and dust edges as they appear in the data. Right: the same for the data of GX 5−1.