adsabs/AstroCLIMB huggingface dataset:
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: Reconstruction results of Cygnus-A with the VLA coverage. From top to bottom in rows show the results of the IUWT, SARA, AIRI, and WTF, respectively. From left to right in columns show the reconstructed images (in a log10 scale), the error images (in linear scale), and the residual images (in linear scale) separately.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: Reconstruction results of W28 with the SKA coverage. From top to bottom in rows show the results of the IUWT, SARA, AIRI, and WTF, respectively. From left to right in columns show the reconstructed images (in a log10 scale), the error images (in linear scale) and the residual images (in linear scale) separately.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: Left-hand panel: u-v coverage of the SKA radio telescope. Right-hand panels: original 1024 × 1024 test images, shown in a log10 scale.
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Left: SED and WISE images of a selected candidate that is rejected by our visual inspection. The top panels show the WISE images of this source, and the target location is marked as a white plus sign in each panel. The bottom panel shows the SED of the candidate. Blue, orange, and red circles represent optical, NIR, and WISE photometry, respectively. The solid line represents the best-fitted stellar photosphere (see Section 4.2). Right: same as the left panels, but for a source passing our visual inspection.
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Illustration of our spectral typing for Gaia DR3 147605282796916992, where the nonveiled model is the preferred fit to the observed spectrum. Left: best-fitted templates with (red) and without (blue) veiling overplotted on the observed spectrum (gray). The inset shows the distribution of the reduced χ2 derived from the fitting with the spectral types of the templates. Right: zoomed-in comparison of the target spectra and the best-fitted templates with (red) and without (blue) veiling in the wavelength ranges 6100–6220 Å and 7000–7220 Å.
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Spatial distribution of the disked objects studied in this work. Red and blue circles represent young and old populations, respectively, and the Peter Pan disks identified in this work are marked with additional cyan circles, with arrows denoting their proper motions. The gray filled rectangles represent the sky coverage of nearby star-forming regions (C. Zucker et al. 2019).
Paper: LAMOST Reveals Long-lived Protoplanetary Disks
Authors: Xiao-Long Wang, Min Fang, Yao Liu, Miao-Miao Zhang, Wen-Yuan Cui
Figure caption: Same as Figure 11, but for the source Gaia DR3 121394677937069184, which is better fitted with a veiled template (red). The inset in the left panel displays the reduced χ2 as a function of different combinations of spectral type and r7465.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Median 1.8 m spectra of PS, constructed by taking the pixel-by-pixel median of individual campaign spectra after aligning to the rest wavelengths of Hγ and He I λ4471. As with all other figures in this paper, the vertical axis is a measure of the density of activated grains in the emulsion, and has not been corrected for departures from linearity. Given the relative brightnesses of the component stars, the median spectra are largely representative of the primary, as features associated with the secondary are suppressed or blurred. Still, some features that are associated with the secondary remain (see text). The S/N diminishes near the blue and red edges of the spectra due to the lower throughput at these wavelengths. The difference between the two spectra is shown at the bottom. The depths of the Balmer lines and He I λ4026 differ at the ∼5% level. However, between 4400 and 4800 Å, where the throughput is highest, the variance in the difference is ∼±1%. It is argued in the text that the difference in the depth of Hγ is not due to plate characteristics.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Comparing line profiles near phases 0.25 and 0.75. The black lines are the mean profiles for orbital phases 0.15–0.35, while the red lines are for phases 0.65-0.85. The spectra for phases 0.65–0.85 from 1937 have been scaled by a factor of 1.5 to adjust for the difference in line depths seen in Figure 7. The line profiles do not mirror each other, in the sense that the notch produced by the spectrum of the secondary, which is marked with the green lines near the 1922 and 1937 Hγ profiles, does not occur at the same depths at the two phases. This is most noticeable in the Hγ profiles of the 1922 campaign spectra. To the extent that Hγ tracks the orbital kinematics of the system, then these comparisons indicate that the systemic velocity measured for the secondary from the 1922 campaign spectra differs from that obtained from the 1937 campaign spectra, and this is confirmed with a cross-correlation analysis in Section 6. There is also a tendency for the N III emission lines near 4640 Å and for He II λ4686 emission/absorption to move with wavelength in a manner that is consistent with the secondary. The presence of N III and He II λ4686 emission is consistent with an Of supergiant designation for that star.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Spectra recorded with the 1.8 m telescope on the night of 1939 March 4. The hour angle at the start of the exposures is shown in brackets; spectrum A22113 was recorded as PS transited the meridian. The spectra have been normalized to a high-order polynomial that was fit to the pseudo-continuum in an attempt to remove large-scale variations in the system response, while not affecting the depths of absorption lines. However, the highest-order polynomial that could safely be applied to the A22112 and A22114 spectra left residual variations in the pseudo-continuum. These variations are periodic and synced in phase, suggesting a common origin. There is a tendency for the absorption lines to be broader and shallower in A22112 than in the other spectra, while the A22113 spectrum has a comparatively flat pseudo-continuum coupled with the sharpest and deepest lines. In contrast to plate A22113, the arc lines on the A22112 and A22114 plates have conspicuous satellites, suggesting that the variations in the pseudo-continuum are due to optical alignment issues, possibly arising from flexure in the spectrograph due to the orientation of the telescope (‘flopture’).
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Composite 1975 campaign spectrum of PS, constructed from the five spectra recorded during that campaign which do not have major cosmetic defects. As with the spectra in Figure 1, individual spectra were shifted to align Hγ and He I λ4471 with their rest wavelengths before taking the median at each pixel. The median 1922 campaign spectrum from Figure 1 is also shown. The differences between the 1975 and 1922 campaign spectra are similar to those between the 1937 and 1922 spectra in Figure 1. Still, while there is not a large difference in the widths of the absorption lines, there is a noticeable difference in the properties of He II λ4686 emission, which appears as two distinct components in the 1.2 m spectrum.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Selected spectra in the wavelength interval 4300–4500 Å that were recorded during the 1920s and 1930s. Orbital phases are in brackets next to the plate numbers. Spectrum-to-spectrum variations in the absolute and relative depths of Hγ and He I λ4471 are seen. The depths of Hγ and He I λ 4471 vary in sync in most cases, as expected if the range in line characteristics is not a result of intrinsic spectroscopic variations, but is instead due to observational effects, such as seeing variations. Still, the depths of Hγ and He I λ4471 in spectra 6953 and 26568 are comparable, hinting at an intrinsic origin for the variation in some features. With the exception of spectrum 26646, the sharpest and deepest features are seen in the 1922 campaign spectra, consistent with the relative depths of features in the median spectra in Figure 1.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Mean 1922 campaign spectra in the orbital phase intervals 0.15–0.35 and 0.65–0.85. The horizontal red line in the middle panel shows the maximum shift in wavelength due to the motion of the primary (i.e., ∼6 Å). Shifts in the mean wavelengths of H and He absorption lines as well as changes in their profiles due to the motion of the secondary are seen. While N III emission is weak between phases 0.15 and 0.35, it is more pronounced near phase 0.75. The character of He II λ4686 and the emission in the shoulders of Hβ both change with orbital phase. The central absorption component of He II λ4686 and the Hβ emission follows the motion of the secondary.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Same as Figure 6, but comparing the 1937 campaign spectra. As in Figure 6, (1) the spectrum of the secondary is clearly evident in many of the absorption lines, (2) the character of N III emission changes with orbital phase, and (3) the emission associated with He II λ4686 and in the shoulders of Hβ tracks the motion of the secondary.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Same as Figure 4, but showing Hβ. Hβ is on the shoulder of the response curve where the overall throughput is markedly lower than near Hγ and He I λ4471, and so the spectra are noisier than in Figure 3. There is a clear dispersion in the depths and shape of Hβ, in the sense that the character of the line core varies with time, changing from a pointed to a flat or double-pointed morphology.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Same as Figure 6, but comparing the 1975 campaign spectra. The wavelength interval covering Hβ is not shown as the S/N is too low to permit a meaningful comparison between orbital phases. The behaviors of the absorption and emission lines are similar to that in Figures 6 and 7.
Paper: Adding RR Lyrae y-Band Template Light Curves to gatspy
Authors: Chow-Choong Ngeow, Chia-Yu Cheng
Figure caption: Illustration of selecting a pair of similar light curves. A light curve was selected from a list of RR Lyrae (usually the one with the smallest σ) as the preliminary template (PT) light curve, which has a light curve dispersion of σPT. This PT is shown in the left panel, where the magenta curve is the best-fit light curve to the data points for this RR Lyrae (open circles). The best-fit light curve (the same magenta curve on the left panel) was then used to fit the jth observed light curve in the list, represented as filled circles in the right panels, and the light curve dispersion σj was calculated from the fitting. The top-right panel shows an example of the jth light curve which is similar to the PT light curve, which satisfied σj/σPT < 1.4. In contrast, the bottom-right panel is an example of the jth light curve that is not similar to the PT light curve. Note that the magenta curves and the open circles in the right panels are same as those in the left panel (i.e., the PT light curve).
Paper: Adding RR Lyrae y-Band Template Light Curves to gatspy
Authors: Chow-Choong Ngeow, Chia-Yu Cheng
Figure caption: The left panel shows a randomly selected y-band reduced image, where fringe patterns can be clearly seen. The middle panel presents the “fringe-bias” image produced from the fringez package (for more details, see M. S. Medford et al. 2021), and the right panel demonstrated the fringe patterns have been successfully removed. Specifically, we ran the fringez-generate on a subset of images without any bright pixels (>35,000 ADU; to avoid artifacts from bright stars). The generated fringe models, separately in the zy-band, were then applied to all of the reduced images using fringez-clean.
Paper: Adding RR Lyrae y-Band Template Light Curves to gatspy
Authors: Chow-Choong Ngeow, Chia-Yu Cheng
Figure caption: Examples of the y-band light curves for two RRab and one RRc stars. The observed light curves are presented in the left panels, where the crosses are rejected data points (see text for more details). The solid magenta curves are the best-fit Fourier expansion, and the dashed magenta curves represent the ±2σ boundaries. The right panels show the corresponding normalized light curves, which have been shifted such that the maximum light located at (0, 0).
Paper: Adding RR Lyrae y-Band Template Light Curves to gatspy
Authors: Chow-Choong Ngeow, Chia-Yu Cheng
Figure caption: Fitting of the y-band template light curves (red dashed curves) to two randomly selected RRab (left panel) and RRc (right panel) stars with gatspy. The black points are the transformed SDSS light curve data (see Section 2) for these two RR Lyrae. Periods found by using the y-band templates (Py) are in good agreement with the periods given in B. Sesar et al. (2010).
Paper: Adding RR Lyrae y-Band Template Light Curves to gatspy
Authors: Chow-Choong Ngeow, Chia-Yu Cheng
Figure caption: The constructed y-band template light curves for RRab (left panel) and RRc (right panel) based on the procedures described in Section 4. These y-band template light curves were presented in a number of ASCII files with filenames convention following the ugriz-band template light curves given in B. Sesar et al. (2010).
Paper: The Clear Sky Corridor: Insights Towards Aerosol Formation in Exoplanets Using an AI-based Survey of Exoplanet Atmospheres
Authors: Reza Ashtari, Kevin B. Stevenson, David Sing, Mercedes López-Morales, Munazza K. Alam, Nikolay K. Nikolov, Thomas M. Evans-Soma
Figure caption: Aerosol-formation trends observed between regimes of Jovian and sub-Neptune class exoplanets. Top: Jovian and sub-Neptunes analyzed in this and previous works, compared against notable published models for Jovian aerosol formation (P. Gao et al. 2020). Bottom: Jovian and sub-Neptunes analyzed in this and previous works. Jovian exoplanets are shown above the dotted boundary region (~0.1–0.13 MJ), and sub-Neptunes are shown below. A novel, separate pattern for H2O aerosol formation among the sub-Neptune regime is clear. Furthermore, a newly found corridor yielding a prominent increase in measured water-band amplitudes is evident. This region presents favorable, clear sky conditions toward identifying atmospheric chemical species across exoplanet regimes, and is defined by a yellow-shaded region. The condensation point for forsterite (Mg2SiO4) and aluminum oxide (Al2O3), located at ~2100 K, causes the anomalous decrease in water feature amplitude observed in some of the hot Jupiters (P. Gao et al. 2020).
Paper: The Clear Sky Corridor: Insights Towards Aerosol Formation in Exoplanets Using an AI-based Survey of Exoplanet Atmospheres
Authors: Reza Ashtari, Kevin B. Stevenson, David Sing, Mercedes López-Morales, Munazza K. Alam, Nikolay K. Nikolov, Thomas M. Evans-Soma
Figure caption: A visualization of local minimum vs. global minimum. In AI-based optimization, the solution should converge to a minimum by design. The type of AI used for optimization will determine which type of minimum is achievable. Global minima are the best solutions in the entire search space. Local minima can be, but are not necessarily the best solutions possible (P. Charbonneau 1995; Y. Rahmat-Samii & E. Michielssen 1999). In this example, a search space for two simultaneously solved variables is shown in the X- and Y-axes. The fitness score, shown on the Z-axis, is based on application-specific criteria. Here, lower fitness scores are more optimal solutions.
Paper: The Clear Sky Corridor: Insights Towards Aerosol Formation in Exoplanets Using an AI-based Survey of Exoplanet Atmospheres
Authors: Reza Ashtari, Kevin B. Stevenson, David Sing, Mercedes López-Morales, Munazza K. Alam, Nikolay K. Nikolov, Thomas M. Evans-Soma
Figure caption: Two separate case studies demonstrating proof-of-concept for the proposed AI-based processing, with HST WFC3 observations. Top: white light and 2D light curves after initial processing and after AI-based processing. Bottom: in this scenario, Eureka!’s optimal estimates for the spectrum location were very poor, yielding an unusable data reduction. The AI corrected for this during its optimization, producing an outstandingly improved result.
Paper: The Clear Sky Corridor: Insights Towards Aerosol Formation in Exoplanets Using an AI-based Survey of Exoplanet Atmospheres
Authors: Reza Ashtari, Kevin B. Stevenson, David Sing, Mercedes López-Morales, Munazza K. Alam, Nikolay K. Nikolov, Thomas M. Evans-Soma
Figure caption: Top: an illustration of how each individual is “sequenced” with an assortment of variable-value pairs relative to transit processing. Bottom: the process for how optimization via parametric sweeps and genetic algorithms operate. While parametric sweeps only optimize to local minima, their optimization is very repeatable, and thus are preferred to genetic optimizers for this application.
Paper: The Clear Sky Corridor: Insights Towards Aerosol Formation in Exoplanets Using an AI-based Survey of Exoplanet Atmospheres
Authors: Reza Ashtari, Kevin B. Stevenson, David Sing, Mercedes López-Morales, Munazza K. Alam, Nikolay K. Nikolov, Thomas M. Evans-Soma
Figure caption: An example output from Eureka!’s HST optimizer, demonstrating sequential optimization of the pipeline's parameters. For simplicity, the optimization shown here selects the best parameter values solely based on the MAD of the white light curve generated (MADWLC). As each parameter's optimal value is selected, it is stored and used in the optimization of the next parameter, yielding the best sequentially optimized solution.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: Mass–radius diagram of all warm giants (planet masses between 0.1 ≤MJup≤ 10 and temperatures below 1000 K). The gray dashed lines are lines of constant bulk density. TOI-4994b is represented by a diamond, and Saturn is overplotted for reference.
Paper: The Clear Sky Corridor: Insights Towards Aerosol Formation in Exoplanets Using an AI-based Survey of Exoplanet Atmospheres
Authors: Reza Ashtari, Kevin B. Stevenson, David Sing, Mercedes López-Morales, Munazza K. Alam, Nikolay K. Nikolov, Thomas M. Evans-Soma
Figure caption: Transmission spectra of the 20 exoplanets analyzed as part of this survey.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: Corner plots showing the covariances for some of the stellar and planetary parameters in our analysis.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: Reconstruction results of M31. From top to bottom in rows show the results of the IUWT, SARA, AIRI and WTF, respectively. From left to right in columns show the reconstructed images (in a log10 scale), the error images (in linear scale) and the residual images (in linear scale) separately.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: The reconstruction performance against coverage percentage. Left: average SNR values. Middle: average SNRlog values. Right: average computation time.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: The performance of reconstruction methods against noise interference. Left: average SNR values. Right: average SNRlog values.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: Testing data. Left: the test image in a log10 scale. Right: a variable density sampling pattern for 40% visibility coverage.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: Left-hand panel: u-v coverage of the VLA radio telescope. Right-hand panels: original 477 × 1024 test images, shown in a log10 scale.
Paper: A Radio-interferometric Imaging Method Based on the Wavelet Tight Frame
Authors: Xiaocheng Yang, Xiang You, Lin Wu, Jingye Yan, Feng Liu, Mingfeng Jiang, Junbao Zheng
Figure caption: Convergence performance under noise interference of different levels.