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: The original transmission spectrum of WASP-96b analyzed by Nikolov et al. (2018; black), and a re-reduction of the same data (VLT/FORS2) with the same binning scheme using our CMC+Poly analysis discussed in Section B.2. The two analyses produce similar mean R  p /R  s  precisions (0.00108 for the original and 0.0079 our reanalysis) and have an average difference of depth of only 0.56σ, suggesting strong agreement of the two data. An offset is applied so the means of both data sets are the same.
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: The mean normalized external parameters of the IMACS observations, used to correct for systematics in both the detrending methods (PCA+GP and CMC+Poly). The left column shows the external parameters for UT170804, and the right shows those for UT171108. The rows correspond to the change in air mass, drift of the wavelength solution, FWHM of the target spectra, mean sky flux, and position of the central pixel trace (perpendicular to the dispersion axis), respectively. Plots of the FORS2 external parameters can be seen in Nikolov et al. (2018) Extended Data Figure 4.
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: Corner plot of the PLATON best-fit retrieval model with scatters, which is run against the combined Magellan/IMACS, VLT/FORS2, and HST/WFC3 data. Its corresponding transmission spectrum is shown in Figure 9 (red model). Vertical dashed lines mark the 16% and 84% quantiles.
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: Same as Figure 7, but for Exoretrievals, where its corresponding transmission spectrum is shown in Figure 10 (blue colored model).
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: Pluses (+) represent stars in the three OCs c1(blue), c2(orange), and c3(green) of our study, located in 5D phase space. The corresponding color is adopted through this paper. Other known OCs from literature in this part of the sky are represented by colored triangles.
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: DEC vs. RV for the clusters candidates with Gaia DR3 and LAMOST DR8 RVs. For Gaia RVs, only σ RV less than the mean σ RV in each cluster were used. Data from LAMOST are marked as triangles. The horizontal lines indicate the final estimated RVs for the clusters that are the mean values.
Paper: On the Accuracy of Three-dimensional Kinematic Distances
Authors: M. J. Reid
Figure caption: Fractional distance error vs. true distance for simulated data with 7 km s−1 (red lines) and 20 km s−1 (blue dashed lines) random noise added. Lines are unweighted averages of 10,000 random trials sampled every 0.5 kpc; representative single-trial error bars indicate standard deviations about the mean. Galactic longitudes are indicated in the top right of each panel, with the ± symbol indicating that the same plot holds for both longitudes. Note the significant bias of 3D kinematic distance estimates, which grow toward the origin as the inverse of true distance. See Section 4 for more discussion.
Paper: On the Accuracy of Three-dimensional Kinematic Distances
Authors: M. J. Reid
Figure caption: VLBI parallax and proper motion data from Reid et al. (2019) selecting only sources with fractional parallax uncertainty <5%. Left panel: comparison of 3D kinematic vs. parallax distances. Right panel: uncertainties in the two methods vs. distance. Note that 3D kinematic distance accuracy (red dots) matches and then surpases parallax accuracy (black circles) beyond about 8 kpc.
Paper: On the Accuracy of Three-dimensional Kinematic Distances
Authors: M. J. Reid
Figure caption: Simulated likelihood distribution functions for 3 components of motion for a source at longitude 15° at a distance of 12 kpc and with 7 km s−1 noise added to each component (see listed V LSR and proper motion values, which include noise). The black PDF function combines the three component likelihoods and yields a 3D kinematic distance estimate of 12.2 ± 0.3 (formal) ±0.1 (systematic) kpc (see text for a details).
Paper: On the Accuracy of Three-dimensional Kinematic Distances
Authors: M. J. Reid
Figure caption: Fractional distance error vs. true distance for simulated data allowing for anomalous motions near the end of the Galactic bar toward the Galactic center in addition to random motions. The far end of the bar is near −15° at 12 kpc (top panel). The near end of the bar is near +30° at 4 kpc (bottom panel). See Figure 3 caption for other details.
Paper: On the Accuracy of Three-dimensional Kinematic Distances
Authors: M. J. Reid
Figure caption: Fractional distance error vs. true distance for simulated data allowing for significant uncertainty in the assumed rotation curve speed within 5 kpc of the Galactic center (at a distance of 8.15 kpc from the Sun) in addition to random motions. See Figure 3 caption for other details.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Top: spectra of HR 8799c, d, and e resulting from summing eight hour of data from each night. Night 1 spectra are plotted with solid lines and night 2 spectra are plotted with dashed lines. The error bars only reflect the measurement errors of the spectra and do not include systematic errors due to the spectrophotometric calibration, which are discussed in Section 4. Bottom: the same spectra normalized to the average K-band flux of HR 8799c in each night. The calibrated spectra of the three planets in the top panel are available as the data behind the figure.(The data used to create this figure are available.)
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Plots of the photometric and spectroscopic stability of satellite spots as calibrators. The top row shows the photometric stability of the satellite spots (i.e., how fixed is their flux ratio relative to the primary star, as described in Equation (3)) and the bottom four rows show the spectral stability of different colors of the satellite spots relative to the companion (left-hand side of Equation (5)). The left column shows the data from the first night, and the right column shows the data from the second night. See Section 4.1 for filter definitions including the F190 filter centered at the 1.9 μm water absorption band.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Images of the calibration binary HD 187003. On the left, the primary star is occulted behind the coronagraph, leaving the secondary star and the four satellite spots created by the primary star visible in the image. On the right, the coronagraph is removed and the stars are placed behind a neutral density filter to avoid saturation. Note that four satellite spots, with amplitudes four times as large as the image on the left, are also visible in this image, but are not used in the analysis. Both images correspond to the 1.74 μm channel.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Reduced images of HR 8799 in two hour chunks and full eight hour temporally collapsed images. The images were combined using a weighted mean where each wavelength slice of each exposure is weighted by the noise at the separation of HR 8799e in that image. All the images are in linear scale, scaled to the flux of HR 8799c, but not corrected for signal loss due to post-processing (i.e., algorithm throughput).
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Time series of the flux of HR 8799c (left column) and HR 8799d (right column) integrated over J, H, F190, and K band (see Section 4.1 for the definitions of these bands). In each panel, photometry from both one and two hour bins are plotted. Error bars represent statistical errors and do not incorporate biases due to photometric calibration. The one hour and two hour photometric time series in this figure are available as the data behind the figure.(The data used to create this figure are available.)
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Lomb–Scargle periodograms for HR 8799c (left) and HR 8799d (right) using both the photometric time series (top) and flux ratio time series (bottom). No significant peaks are found in any of the configurations.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Completeness maps to photometric variability in four bands at a given fractional amplitude and period for HR 8799c (left) and HR 8799d (right).
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Time series of the flux ratios between various bands for HR 8799c (left column) and HR 8799d (right column). In each panel, photometry from both one and two hour bins are plotted. Error bars represent statistical errors. The one hour and two hour flux ratio time series in this figure are available as the data behind the figure.(The data used to create this figure are available.)
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Velocities obtained from shell lines and Hα. The filled black squares are velocities measured in the wavelength interval 6335–6465 Å using the iterative cross-correlation procedure that is described in the text. The open black squares are from the velocity curve based on metallic lines at blue wavelengths shown in Figure 4(a) of Aydin et al. (1978). The red triangles are velocities measured from the lower portions of the Si II 6347 (filled) and Fe II 6432 (open) absorption features, while the blue crosses indicate velocities measured in the deepest parts of Hα absorption. The estimated uncertainty in our velocities is ±1 km s−1. The velocity curves have different γ values, and this is attributed to contamination from the donor star spectrum in the upper half of the metallic shell absorption lines. The velocities obtained from Si II 6347 and Fe II 6432 likely provide the most reliable estimate of the shell motion, as they use the part of the line profile that is least affected by the donor star spectrum. Still, even those velocities may be skewed at some low level by substructure in the line profile. The Hα velocities suggest motion in an opposite direction to that of the shell lines. The velocities used to construct this figure are tabulated in the Appendix.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Differences between the median shell spectrum and the mean phase-binned spectra near Si II 6347, Si II 6371, and Fe II 6432. The median shell spectrum is shown at the bottom of each panel. The dotted line marks the point of deepest absorption in each shell line, while the expected locations of the shell lines if they were in the spectrum of the donor star, assuming the composite velocity curve in Figure 6 of Tarasov & Berdyugin (1998), are indicated in red. There is a residual absorption feature that is deepest at phases 0.2 and 0.3 that follows a serpentine-like propagation with phase. The ∼3 Å throw of this feature in wavelength between the two quadrature points is consistent with that expected for the orbital motion of the donor star. Si II lines are among the deepest metallic signatures in the spectra of A-type stars at these wavelengths, whereas Fe II lines tend to be weaker than the Si lines at those spectral types.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Spectra of—from top to bottom—Deneb, the donor star at different phases (ϕ), and the accretion disk. The Deneb spectrum has been smoothed to match the widths of lines in the mean donor spectrum. Donor star spectra in two phase intervals (0.0–0.5 and 0.5–1.0) are shown, as is the mean spectrum over all orbital phases (plotted as a dotted line). The spectrum of the donor star between phases 0.0 and 0.5 is similar to that of Deneb, suggesting that the donor star has features that are consistent with those of a mid-A giant/supergiant in this phase interval. The accretion disk spectra were constructed for two system mass ratios (q), and emission features of Si II and Fe II are apparent. The strengths of the emission features are lower limits to their actual values given the procedure used to construct these spectra (see text). The donor star and accretor spectra have been scaled to produce lines with strengths that are appropriate for a single object, based on the relative luminosities listed in Table 2 of Zola & Ogloza (2001) in the R filter.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Hα residuals near secondary minimum (phase 0.5). Each curve shows the result of subtracting the phase-averaged mean spectrum from an individual spectrum. Spectra are grouped using orbital phase bins having a width of 0.01 phase units, and the spectra are identified by the month and day in that month (e.g., March 16 = 0316). The residual spectra are displayed folded about phase 0.5 so that the brightening and fading of Hα can be compared before and after secondary minimum. The spectra at the top are closest to secondary minimum in terms of orbital phase, while the spectra at the bottom are farthest from secondary minimum. Spectra recorded with phases between 0.51 and 0.55 are shown in red. There are differences between the spectra at each phase offset from secondary minimum, and it is argued in the text that these are likely due to variations in Hα strength with time, rather than orbital phase, in the sense that Hα emission was consistently stronger during 2021 March–June. There is also evidence for systematically stronger Hα emission toward phase 0.5, based on the strengths of spectra that were recorded only 1 day apart in June (0617 and 0618) and July (0724 and 0725).
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Left panel: phase-binned spectra centered on Hα. The spectrum of Deneb is shown at the bottom of the panel, and it is evident that Hα absorption from an A supergiant spectrum like that of Deneb makes only a modest contribution to the total Hα absorption. The dotted line indicates the mean midpoint of Hα absorption, as measured from the lower portions of the line profiles. Modest changes in the central wavelength of the absorption component and in the shape of the emission component are apparent. Right panel: differences between the composite mean Hα spectrum constructed by combining the spectra at all 10 phases and the phase-binned spectra. The residuals highlight changes in the amplitude of the emission and absorption features with orbital phase. The expected location of Hα absorption in the donor spectrum is indicated with red lines, and any signatures of this feature are swamped by noise in the residuals.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Mean phase-binned spectra centered on Si II 6347, Si II 6371, and Fe II 6432. Orbital phases are listed near the left edge of each panel. Substructures propagate with phase through all three lines, and these are most evident at wavelengths blueward of the line centers. It is argued in this paper that much of this substructure is associated with the donor star. The emission associated with Fe II 6432 is more pronounced than for the Si II lines, and it is argued that this emission originates in an accretion disk. The 10 phase-binned spectra are available as the data behind the figure. These spectra can also be used to generate other figures, as the data cover the entire range from 6335 to 6850.(The data used to create this figure are available.)
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Left panel: spectra centered on He I 6678. The median of spectra in all 10 phase bins is shown at the bottom of the panel. Shell lines of Fe II and Ti II dominate at these wavelengths. Right panel: residuals after subtracting the median spectrum from each spectrum in the left panel. The red lines mark the expected location of He I 6678 based on the velocity measurements made by Tarasov & Berdyugin. Emission at a wavelength close to that of He I 6678 in the rest frame is seen in the residual spectra at phase 0.0. This feature is also clearly seen in the phase 0.0 spectrum in the left panel. The median residual spectra after shifting spectra into the rest frame assuming mass ratios q = 0.5 (i.e., that calculated by Tarasov & Berdyugin) and 0.75 are shown at the bottom of the panel. The featureless nature of the combined spectra indicates that He I 6678 is not detected throughout the entire orbital cycle.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Residual structure in the Si II 6347 feature on three different nights that cover the phase interval 0.05–0.15. The orbital phase (ϕ) for each spectrum is shown. The residual spectra were constructed using the same procedure used to make Figure 6, and the dotted red line marks the wavelength where the shell line is deepest. The expected wavelength of Si II 6347 in the donor star spectrum at each orbital phase is indicated in red. The residual spectra on all three nights show broad absorption near 6345 Å, and this is attributed to the donor star spectrum. There is evidence of a second feature near 6346 Å that appears to weaken progressively with time over the range of dates sampled by the spectra. Thus, while much of the residual structure can be attributed to the donor star absorption spectrum, there may be transient components that originate in other sources.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Left panel: mean phase-binned spectra of [O I] 6364. The continuum level for each spectrum is indicated with a red dashed line, while the dotted lines mark the approximate blue and red boundaries of the emission. Emission in the blue part of the [O I] feature is weakest at phases 0.0 and 0.1. The component in the blueward part of the line grows in strength toward progressively later orbital phases, while the strength of the redward signal stays roughly constant. Right panel: differences between a composite mean spectrum constructed by averaging the spectra at all 10 phases and individual phase-binned spectra.
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:                    ﹩P(\mu ^{\prime} | \alpha )﹩ for three different values of α. The distribution for our observed population of binary star systems in the cases where M tot can be estimated from the Mann et al. (2019) relation is given in black. The tail where ﹩\mu ^{\prime} \gt \sqrt{2}﹩, which is nonphysical for bound binary systems, is thought to be the result of intrinsic measurement error and hierarchical star systems misinterpreted as binaries.
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: distribution of molecular hydrogen from the Bonn/Argelander 21 cm radio survey (Kalberla & Haud 2015). Shown is H2 distribution for 10 km s−1 dispersion in the Galactic Bulge. Right: plot of Si K optical depths for the gas (red) and the dust (blue) vs. the column densities from the 21 cm radio survey N H Radio. The red line is a linear dependence for the gas case.
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: The grain columns for a total absorption column of 1020 cm−2 for ten different grain sizes using the self-shielding formalism from Wilms et al. (2000). for the high column (black), medium column (blue), and low column (red) cases fitting our dust grain optical depths as shown in Figure 6 for the 0.3 and 0.025 μm cases. They can be represented by power laws with index of –3, close to what is expected from a standard MRN dust size distribution.