adsabs/AstroCLIMB huggingface dataset:
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Left: spectral light curve annotated with the mean wavelength for each bin. Right: residuals of the fit, along with the standard deviation relative to the photon noise (﹩\bar{\sigma }﹩), the reduced chi-square (﹩{\bar{\chi }}^{2}﹩), and the square of the correlation (R 2).
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Combined images from each epoch, processed with SNAP and cropped to show the inner planets. The images are shown on a linear scale with correct throughput, normalized using the flux of planet d. Values outside the linear colorscale are shown in gray. Note that, when using SNAP, the forward-processed images should not be used for evaluating the noise. Close to the star, the PSFs of any potential planet can produce secondary positive and negative ghosts at other position angles. Instead, we calculate contrast curves using matching backward-rotated reductions. The top panels are comprised of archival data, while the bottom panels are the new campaign. Significant orbital motion is visible between epochs. The full images including planet b are listed in Appendix.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: 5σ contrast limits at each of the five L′ epochs on a log-log scale. Blue circles mark the average separations and photometry from our results. The contrast achieved close to the star has improved over time, so later epochs have more weight in our modeling.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The velocity-integrated intensity channel maps of the 13CO(1–0) emission toward the Galactic Cassiopeia region. The integrated velocity range is written in the bottom right corner of each panel (in km s−1). The unit of the scale bar is K km s−1.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Transmission spectrum of K2-33b from our data (gray circles) compared to haze models composed of (1) CO tholin (green), (2) CO soot (pink), (3) a combined spot model with CO tholin (purple), and (4) a combined spot model with CO soot (orange). Only the models that produced the lowest chi-square values are shown. All models were normalized to give the best fit to the data. The combined haze and spot models gave a lower chi-square value. All calculations were done with high-resolution models.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Light curves from MEarth and Spitzer for the three transits with overlapping data (transits 186, 188, and 191). Data from both facilities were folded and (median) binned for clarity. One of the MEarth transits was partial (transit 188), and conditions varied both between and during MEarth transits leading to inconsistent data quality. However, the MEarth light curve still clearly favors a deeper transit depth.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Posteriors of spot properties from the stellar spectrum (black/gray), a fit to the transmission spectrum using CO tholin models (purple), and a fit to the transmission spectrum using CO soot models (orange). The two transmission spectrum fits shown here are those using the tholin or soot model with the lowest χ 2 that also yielded spot properties consistent with the fit to the stellar spectrum.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Schematic showing how we model planets across epochs with orbital motion. The solid black line shows the path of a hypothetical planet around a star, with a given set of parameters (a, i, e, Ω, ω, τ, M, and Π). We calculate the position x in each image i using Kepler’s laws, and measure the flux at that location as L  x,i . We then calculate σ  x,i , the uncertainty in L  x,i , by measuring the contrast in an annulus at that separation from the matching backward-rotated image. L  x,i  is then compared to the model parameter L, which is the same for all epochs using the likelihood function given by equation N.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Comparison of the inner planet models against three different data sets. A. An inner planet model applied to the full data set. B. Same as A, but ignoring the best epoch (2021). C. Same as A, but after subtracting the best fitting model found by A from the 2021 epoch. The four panels show orbits drawn from the posterior, posterior density of planet position calculated at the 2021 epoch, median photometry if the planet were at that position in 2021, and photometric accuracy at those positions, i.e., the S/N of a planet if it were on an orbit that would pass through that pixel in 2021. Pixels are left blank where there are only a negligible number of samples.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Top: Confidence levels of a Gaussian distribution and empirical confidence level from the inner 1λ/D annulus of our images extrapolated to 1–10−6 using an exponential function. We increase our S/N thresholds to account for this slight deviation from Gaussian noise. Bottom: Empirical log PDF of standardized pixel intensities compared to a Gaussian model, and Gaussians scaled to cover the tails of the distribution.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Top: images from each of the five epochs. Bottom: 2D marginal position posterior at each epoch. This shows the a posteriori most likely positions for an inner planet at each epoch. Note that the posterior is calculated jointly from all images; this figure merely visualizes it at individual epochs. Even epochs where the location is poorly constrained can still contribute to the S/N of the model as a whole by reducing the space of plausible orbits and planet photometry.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Marginal posteriors of photometry and orbital elements compared between the four known planets and the inner planet model.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: The 2021 epoch before and after subtracting a model planet injected at the expected location and photometry of the single inner planet model fit to all five epochs. The area interior to 100 mas is excluded from the processing, due to detector saturation. The bottom right image shows the flux removed by the negative planet injection. The structure is more complex than the typical dark wings from ADI processing, due to the high FoV rotation and tight separation.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Flux-ratio and semimajor axis marginal posteriors for an additional outer planet between planet b and the start of the outer debris disk. The black line gives the 84th percentile flux as a function of semimajor axis. No planet is detected, and our sensitivity is not strongly dependent on any of the orbital parameters within this range of semimajor axis.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Visualization of 1500 orbit draws from the posteriors of the b, c, d, e, and inner planet models overplotted on the combined 2021 epoch. Directly modeling the photometry in our images allows us to simultaneously detect the known planets and produce orbital posteriors that agree with previous fits to extracted astrometry.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Flux-ratio and semimajor axis posteriors for an additional inner planet with a 1σ contour overplotted. The dashed lines show 16% and 84% percentile limits. The recovered photometry is consistent with that of planets c, d, and e.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Marginal photometry vs. semimajor axis for planets b, c, d, and e. All four are detected at very high significance and S/Ns greater than in any individual epoch. The scales are different between each panel.
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: Surface zonal wind speeds of Uranus and Neptune as a function of latitude. On the left panel, red points show Keck and Hubble Space telescope measurements (Hammel et al. 2005; Sromovsky & Fry 2005) and blue points show Voyager II measurements (Hammel et al. 2001). The solid line is the fit by the latter. On the right panel, red points show Hubble Space telescope measurements (Sromovsky et al. 1993) and blue points show Voyager II measurements (Limaye & Sromovsky 1991; Lindal et al. 1990). The solid line is the fit by French et al. (1998), and the orange dotted line is our fit given by Equation (18).
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Full combined image from each epoch. The top two panels consist of archival data, while the bottom three are from the new campaign. The artifacts south of the star in the 2009 image are from a chopping strategy used to subtract the thermal background. The approximate location of the inner edge of the outer debris disk is outlined in blue. These processed images are available at 10.5281/zenodo.6823071.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Stellar astrometric motion predicted at the Hipparcos and GAIA epochs for the stable four-planet V  d  solution of Goździewski & Migaszewski (2014) (blue square) and with the addition of the fifth inner candidate (colored by the semimajor axis of the candidate). The red error bars show the stellar astrometric motion at the Hipparcos and GAIA epochs as calculated by the HGCA (Brandt 2021). The black marker shows the long-term proper motion from the HGCA calculated from the difference in position between both epochs. The planets c, d, e, and the candidate f are assumed to have masses of 7 M jup, while b is assumed to have a mass of 5 M jup.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: The 85th percentile upper limit of the marginal L-band flux-ratio posterior for an additional fifth inner planet (black). The turquoise lines show the same, but after subtracting a planet model from the raw data of 2021 epoch (C in Figure 10). The gray lines show the traditional 1σ projected contrast of individual epochs from backward-rotated reductions.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: The MEGNO stability map for the coplanar “f” candidate using the parameters from Table 4, for an integration time of 0.5 Myr (left) and 1.0 Myr (right). Most of the configurations become unstable (MEGNO > 2) within this integration period.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Corner plot showing the posterior of the inner planet model applied to all epochs. Note that the angular parameters i, Ω, ω, and τ are periodic. Chains are available at 10.5281/zenodo.6823071.
Paper: Deep Orbital Search for Additional Planets in the HR 8799 System
Authors: William Thompson, Christian Marois, Clarissa R. Do Ó, Quinn Konopacky, Jean-Baptiste Ruffio, Jason Wang, Andy J. Skemer, Robert J. De Rosa, Bruce Macintosh
Figure caption: Position posterior density for the inner planet model at different epochs. The position is shown on August 15th of each year between 2009 and 2024.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: Color–magnitude diagram of Gaia EDR3 sources in the shell region. The dashed–dotted line represents the 10 Myr isochrone from the PARSEC model (Bressan et al. 2012; Marigo et al. 2017). The arrow line is the reddening vector of A v = 2 mag, and the gray dashed line parallel to it is the isomass line of 8 M ⊙. The gray dashed line perpendicular to x-axis is set to distinguish main-sequence stars from the giant branch. The blue dots represent the Gaia sources and the red-filled circles are the identified massive stars.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The massive stars identified in the shell region by using the Gaia data (see also Table 2), plotted on the 13CO intensity image. For each star, its distance and mass are labeled, while the proper motion is marked by the arrow.
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Examples of families of hyperprior eccentricity distributions randomly drawn from different hyperpriors of the beta distribution shape parameters α and β. Each panel shows a representative sample of 200 eccentricity distributions randomly drawn from a given hyperprior. The eccentricity distribution corresponding to the median (α, β) drawn from the hyperprior is highlighted in bold. The top row shows the distributions drawn from a log-uniform hyperprior with lower bound of 0.01 and upper bounds of 10, 100, and 1000 (from left to right). The middle row shows distributions drawn from uniform hyperpriors spanning ranges of [0.01, 10], [0.01, 100], and [0.01, 1000]. These have a tendency to produce progressively narrower distributions as the upper bound increases. In the third row, we show the distributions drawn from three different truncated Gaussian hyperpriors. From left to right, these hyperpriors are parameterized by: (μ, σ) = (1.0, 0.1), (μ, σ) = (1.0, 0.4), and (μ, σ) = (0.69, 1.0).
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Results of hierarchical Bayesian fitting using uniform hyperpriors for α and β on [0.01, 100] for a set of synthetic Gaussian eccentricity posteriors drawn from the RV exoplanet distribution (dashed line). The nine panels show the posteriors of population-level distributions obtained as N (sample size or number of artificial planets in the analyzed data set) and σ (width of the individual eccentricity posteriors) are varied. The thick solid curves are the median recovered distributions while the thin lines are randomly sampled distributions from the posterior. In the case of low N or high σ, the recovered distributions are preferentially narrowly peaked, a trend reminiscent of the results found for the giant planet sample in BBN20. Furthermore, we see that this trend persists across the first row, even when N increases by a factor of 10, a sign that the results are being biased by the choice of a uniform prior.
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Flowchart summarizing the forward-modeling process described in Section 5.1. We begin by assuming an underlying eccentricity distribution, from which we randomly sample N systems. Then for each system, we use a Keplerian model to simulate five evenly spaced astrometric points. Orbit fits are performed for each system using OFTI, which produce a set of N eccentricity posteriors. Finally, we use ePop! to run a hierarchical fit on this set of posteriors, producing a posterior on hyperparameters α and β, which translates to a posterior of underlying population-level eccentricity distributions.
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Visualization of the simulated forward modeled sample. In the top panel, we show the individual eccentricity posteriors (violin plots) obtained by using OFTI to perform orbit fits to the simulated astrometry for each of the 45 systems drawn from an underlying uniform population-level eccentricity distribution. In each individual violin plot, the black dot corresponds to the “true” eccentricity of the individual system, while the gray box corresponds to the interquartile range of its eccentricity posterior. On the right, we plot the histogram of true eccentricities for the simulated sample, where the thick black curve shows the underlying uniform eccentricity distribution. The bottom panel shows the analogous information for the ensemble of 45 systems drawn from an underlying RV exoplanet distribution.
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Analogous to Figure 2, but here we impose a truncated Gaussian hyperprior with μ = 0.69 and σ = 1.0 on (α, β). In contrast with the case of the uniform hyperprior seen in Figure 2, even in the case of low N or high σ, the distributions recovered are reminiscent of the underlying RV exoplanet eccentricity distribution. The preference for narrowly peaked distributions observed when imposing a uniform hyperprior disappears in this case, and the posteriors of inferred distributions approach the underlying distribution as N increases and σ decreases.
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Same as Figure 8, but for the case of an underlying RV exoplanet distribution. We once again observe that the Gaussian hyperprior consistently performs the best at each sample size, followed by the log-uniform, uniform, and log-normal hyperpriors. Note that even for large samples, the log-uniform, uniform, and log-normal hyperpriors introduce a narrow peak in the posterior distributions.
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Analogous to Figure 2, but here we impose a log-uniform hyperprior with bounds [0.01, 100] on (α, β). Similar to what we observe in Figure 3 for truncated Gaussian hyperpriors, there is no artificial preference for narrowly peaked distributions. This provides further evidence that the narrow peaks for small samples in Figure 2 for uniform hyperpriors arise from prior-driven effects.
Paper: Automatic Classification of Galaxy Morphology: A Rotationally-invariant Supervised Machine-learning Method Based on the Unsupervised Machine-learning Data Set
Authors: GuanWen Fang, Shuo Ba, Yizhou Gu, Zesen Lin, Yuejie Hou, Chenxin Qin, Chichun Zhou, Jun Xu, Yao Dai, Jie Song, Xu Kong
Figure caption: An overview of the UML data set. Left: cutouts of galaxies selected from different categories, i.e., SPH, ETD, LTD, IRR, and UNC galaxies, are shown from top to bottom. Right: the t-SNE visualization of 6000 randomly selected galaxies with different morphologies (top) and the corresponding counting distribution (bottom) in the UML data set are given.
Paper: The Impact of Bayesian Hyperpriors on the Population-level Eccentricity Distribution of Imaged Planets
Authors: Vighnesh Nagpal, Sarah Blunt, Brendan P. Bowler, Trent J. Dupuy, Eric L. Nielsen, Jason J. Wang
Figure caption: Hyperpriors imposed on both α and β for the hierarchical fitting of our forward modeled data set. We chose these distributions to test the hyperprior impact on the recovered distribution. We only plot hyperprior distributions for hyperparameter values ≤10 for ease of displaying the qualitative distinctions between the hyperpriors.