adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Authors: Lisa Dang, Taylor J. Bell, Ying (Zoe) Shu, Nicolas B. Cowan, Jacob L. Bean, Drake Deming, Eliza M.-R. Kempton, Megan Weiner Mansfield, Emily Rauscher, Vivien Parmentier, Alexandra Rochon, Kevin B. Stevenson, Mark Swain, Laura Kreidberg, Tiffany Kataria, Jean-Michel Désert, Robert Zellem, Jonathan J. Fortney, Nikole K. Lewis, Michael Line, Caroline Morley, Adam Showman
Figure caption: Top: trends in phase curves, similar to Figure 5, for different model selection strategies. The top plot corresponds to a uniform analysis using BLISS, and the middle plot is calculated using the phase-curve models preferred by the BIC. Bottom: trends in Bond albedo and heat recirculation efficiency for different model selection strategies. The left plot is calculated from a uniform analysis using BLISS, and the right plot is calculated using the phase-curve models preferred by the BIC. The fewer unphysical negative albedos in the bottom left panel is a testament to our visual inspection.
Paper: A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Authors: Lisa Dang, Taylor J. Bell, Ying (Zoe) Shu, Nicolas B. Cowan, Jacob L. Bean, Drake Deming, Eliza M.-R. Kempton, Megan Weiner Mansfield, Emily Rauscher, Vivien Parmentier, Alexandra Rochon, Kevin B. Stevenson, Mark Swain, Laura Kreidberg, Tiffany Kataria, Jean-Michel Désert, Robert Zellem, Jonathan J. Fortney, Nikole K. Lewis, Michael Line, Caroline Morley, Adam Showman
Figure caption: Inferred Bond albedo, A B, and heat recirculation efficiency, ε, from our sample of 4.5 μm Spitzer phase curves. Each contour represents the 1σ confidence region estimates for each planet, and contour colors, corresponding to the colors in Figure 1, represent the irradiation temperature T irr.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: A simple cartoon of the dust disks in the PDS 70 system. Left image: continuum image from 2024 (same data as lower-left panel of Figure 9) fit to two CPDs around each planet (red circles). Right image: two CPDs (radius ∼1 Hill sphere) are shown with bright starlight from A scattered off of the front edge of each CPD as observed.
Paper: A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Authors: Lisa Dang, Taylor J. Bell, Ying (Zoe) Shu, Nicolas B. Cowan, Jacob L. Bean, Drake Deming, Eliza M.-R. Kempton, Megan Weiner Mansfield, Emily Rauscher, Vivien Parmentier, Alexandra Rochon, Kevin B. Stevenson, Mark Swain, Laura Kreidberg, Tiffany Kataria, Jean-Michel Désert, Robert Zellem, Jonathan J. Fortney, Nikole K. Lewis, Michael Line, Caroline Morley, Adam Showman
Figure caption: Preferred detrended 4.5 μm Spitzer phase curves of hot Jupiters on circular orbits ordered by increasing levels of irradiation temperatures. The line represents the best astrophysical model, observations are binned for a total of 50 bins, and the error bars represent the scatter of each bin.
Paper: A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Authors: Lisa Dang, Taylor J. Bell, Ying (Zoe) Shu, Nicolas B. Cowan, Jacob L. Bean, Drake Deming, Eliza M.-R. Kempton, Megan Weiner Mansfield, Emily Rauscher, Vivien Parmentier, Alexandra Rochon, Kevin B. Stevenson, Mark Swain, Laura Kreidberg, Tiffany Kataria, Jean-Michel Désert, Robert Zellem, Jonathan J. Fortney, Nikole K. Lewis, Michael Line, Caroline Morley, Adam Showman
Figure caption: A comprehensive overview of all SPCA fits of the 4.5 μm full-orbit phase curve of WASP-52b. Each subplot displays the best-fit astrophysical model compared to the corrected Spitzer photometry with different detector models. Each column indicates the detector model used where Poly# means a 2D polynomial of order #, PLD Ord# indicates the PLD order, and 3 × 3 or 5 × 5 indicates the pixel stamp size used for PLD. The rows indicate the phase variation model used (sinusoid of order 1 or 2) and whether the detector model also included a linear model with PSF width (σ  x , σ  y ) as inputs. The ΔBIC from the preferred solution of each fit is indicated in each box, and the opacity of the background of each box reflects fit preference (darker is better). The dayside and nightside temperatures inferred from each fit are displayed. Here, the observations are quite noisy and the resulting phase curve retrieved is highly dependent on the selection of model. Since the lowest-BIC model (yellow box) seems unphysical with a nightside emission as high as the dayside emission, we inspected the highest-BIC models and chose the one that looked physically plausible (green box).
Paper: The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites 
Authors: Robert A. Jacobson, Ryan S. Park
Figure caption: Pole orientation.
Paper: The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites 
Authors: Robert A. Jacobson, Ryan S. Park
Figure caption: Uranus orbit formal uncertainties.
Paper: The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites 
Authors: Robert A. Jacobson, Ryan S. Park
Figure caption: Encounter Doppler residuals.
Paper: The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites 
Authors: Robert A. Jacobson, Ryan S. Park
Figure caption: Optical residuals.
Paper: The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites 
Authors: Robert A. Jacobson, Ryan S. Park
Figure caption: Pole decl.
Paper: The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites 
Authors: Robert A. Jacobson, Ryan S. Park
Figure caption: Ring Radius Residuals.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Masses and periods of exoplanets orbiting FGK dwarfs with (red) and without (blue) other known planetary companions in the same system. The gray dashed box highlights exoplanets with masses and periods similar to HD 86728b (5 M                      ﹩{}_{\oplus }\lt {m}_{p}\sin i\lt 15\ ﹩                      M ⊕; 20 days < P < 50 days). We differentiate between planets for which the true mass is known (e.g., transiting planets) and planets for which there exists a mass-inclination degeneracy. The former are shown as squares and the latter as circles. HD 86728b is in the minority of planets in this region without known siblings. The small red and blue markers indicate planets that fall outside the defined mass–period space or that orbit non-FGK host stars.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Sensitivity of the existing NEID and CLS RVs to additional exoplanets in the HD 86728 system, as calculated via Fisher information. The solid, dashed, and dotted red lines show the limits at which the RV semi-amplitude could be measured to 10σ, 5σ, and 3σ precision, respectively. We note that these limits are calculated assuming white noise variability dominates the stellar RV signal for the observed timescales and cadences, in accordance with our adopted planet fit. Known companions to exoplanets highlighted in Figure 9 are shown as open red circles; most of these lie above the expected 10σ sensitivity limits, and all lie above the 3σ limit.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: NEID RVs for the four nights with multiple visits: 2021 February 11, 2021 February 28, 2021 March 3, and 2021 March 6. We show the raw RVs as closed circles and the SCALPELS v ⊥ values as open diamonds. Velocities are plotted relative to the first measurement taken on each night. On each of these nights, the RV signal changes by ∼1 m s−1 between visits separated by multiple hours.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: NEID RVs and activity indicator measurements for HD 86728 (left). Vertical lines mark the boundaries between NEID’s 6 month observing semesters. The GLS periodograms are shown to the right of each time series. We indicate the period of the detected RV signal with a green vertical line and Earth’s orbital period with a gray vertical line, and the 0.1% false alarm level with a horizontal dashed line. Periodograms are computed separately for the NEID RVs obtained during Run 1 (light blue) and Run 2 (dark blue). The pink points (left) and lines (right) show the pre-telluric correction Na I and Hα indicators, and the black points and lines show the post-correction indicators.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Orbital parameter posteriors for HD 86728b. We show the posteriors for each fit to the raw RVs (left) and to the SCALPELS v ⊥ (right). The 2D histograms include 1σ, 2σ, and 3σ contours. The best-fit parameter values and ±1σ uncertainties are listed for our preferred models, which are the NEID + CLS fit with a GP for the raw NEID RVs, and the NEID + CLS fit without a GP to the SCALPELS v ⊥ time series.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: SCALPELS decomposition of the NEID RVs. We show the shape-driven velocity component, v ∥, and the corresponding GLS periodogram in the upper left and right, respectively. The lower panels show the shift-driven velocity component, v ⊥, and GLS periodogram. The 31 day RV signal is isolated almost entirely to the shift-driven component. The shape-driven component is dominated by a 1 yr signal that closely resembles that seen in the BIS. This signal is not seen in the raw RVs.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: HIRES, APF, and Lick RVs and HIRES SHK measurements for HD 86728. The GLS periodograms are shown to the right of each time series. As in Figure 1, we indicate the period of the detected RV signal with a green vertical line and Earth’s orbital period with a gray vertical line, and the 0.1% false alarm level with a horizontal dashed line.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: BF periodograms of NEID RVs following noise decorrelation with Agatha. The upper panel shows the results of the best-fit Agatha model for the raw RVs (single moving average term with BIS as the only noise proxy), and the lower panel shows the results of the best-fit Agatha model for the SCALPELS shift-driven RVs (single moving average term with no noise proxies).
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Phase-folded RVs for HD 86728 (top) and residuals to the best-fit orbital solution for the combined data set (bottom). The best-fit model and 3σ uncertainties are shown in black and gray, respectively. We bin the CLS RVs by orbital phase to show that they are consistent with the fit. The NEID RVs and model fit shown here are based on the SCALPELS v ⊥ measurements.
Paper: The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728
Authors: Arvind F. Gupta, Jacob K. Luhn, Jason T. Wright, Suvrath Mahadevan, Paul Robertson, Daniel M. Krolikowski, Eric B. Ford, Caleb I. Cañas, Samuel Halverson, Andrea S. J. Lin, Shubham Kanodia, Evan Fitzmaurice, Christian Gilbertson, Chad F. Bender, Cullen H. Blake, Jiayin Dong, Mark R. Giovinazzi, Sarah E. Logsdon, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: Complete RV time series for HD 86728. The NEID data are shown as light (Run 1) and dark (Run 2) blue circles, the APF data are shown as red squares, HIRES as orange hexagons, and Lick as purple diamonds. We also show the best-fit model (black), and in the lower panel we show the residuals to this model.
Paper: The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites 
Authors: Robert A. Jacobson, Ryan S. Park
Figure caption: Pole R.A.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Comparison of CMDs derived from clustering results using DBSCAN, HDBSCAN, and FFC algorithms. From top to bottom, the heliocentric distances (R) of the clusters represent within 1 kpc, between 1 and 2 kpc, larger than 2 kpc, and about 63 kpc for the dwarf galaxy Bootes I. N is the number of star members in a star cluster.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Galactic distribution of our cluster sample, along with one dwarf galaxy Bootes I (red pentagram).
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Example of applying GMM to classify clusters from three overlapping clusters. From left to right, the panels show CMDs, positions in α and δ, vector point diagrams, and ϖ as a function of G magnitude. The color bar indicates the probability of stars being members of the cluster.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Process of configuring FFC into the pyUPMASK pipeline framework.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: Nearby sources contaminating the TOI-6038 A aperture. Left: TPF-shaped heat map with the pixel-by-pixel flux fraction from TOI-6038 A in S58. The red grid is the SPOC aperture. The pixel scale is 21″ pixel−1. The two sources that most contribute to the aperture flux (Star 1: TIC 194736419 and Star 2: TIC 194736424) are highlighted in purple and green, respectively. Disk areas scale with the emitted fluxes. Right: flux contributions to the SPOC aperture from the target and most contaminant stars. These plots were generated through TESS-cont (A. Castro-González et al. 2024b).
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: De-trended and normalized TESS LCs of TOI-6038 A from S18 and S58 are shown with green and blue points, respectively. The full LC is displayed in the upper panel, while the phase-folded LC from both sectors is shown in the lower panel, with pink dots representing 20 minute binned data points. The black solid line in both panels represents the best-fit transit model for TOI-6038 A b (see Section 3.6).
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: Left: normalized TESS-SPOC PDCSAP LC from S58, shown with gray points (full LC) and blue points (with transits removed). The pink dots represent 120 minute binned data points, while the solid black line shows the best-fit sinusoidal signal. Right: GLS periodogram of the LC. The vertical pink line marks the most significant period (9.29 ± 0.25 days), and the horizontal dashed blue lines indicate the 0.1% false alarm probability (FAP) level.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: 5σ contrast curve in the V band for TOI-6038 A, obtained using the speckle imager on the PRL 2.5 m telescope. The speckle ACF is shown as an inset. No stellar companions are detected.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of multiplanet systems (including two-planet systems) with hot Jupiters (P < 10 days), ordered by the period of the second planet in the system, to illustrate the distribution of companions. In this sample, this is always the hot Jupiter, in systems with nearby smaller companions, and always the distant Jovian companion, in systems that have them (except WASP-47). Only WASP-148 has a nearby warm-Jupiter companion.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of all exoplanet systems with N ≥ 3 inner planets that meet the criteria of closely spaced peas-in-a-pod systems, plotted using the same format as Figure 1. 232 systems are shown (80% of all systems with N ≥ 3 inner planets), ordered by the period of the innermost planet, from bottom to top. Six systems have distant Jovian companions, including one with two Jupiters. The shortest-period planet is Kepler-42 c. The longest-period non-Jupiter is τ Cet f.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of warm-Jupiter systems (with and without gaps), ordered by period of the innermost planet within each category. This figure includes all systems in Figure 9 that have warm Jupiters, but is extended by systems with only three inner planets that also have warm Jupiters. These systems show significantly more variation even within each category than do the peas-in-a-pod systems.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of the subset of systems with N ≥ 4 inner planets plus a wide gap with a period ratio >5, ordered by a location-specific metric of “gap period.” This figure shows the relative abundance of inner-gap, middle-gap, and outer-gap systems in a population with commensurable numbers of inner planets.