adsabs/AstroCLIMB huggingface dataset:
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: How starry computes the flux from a body in reflected light, tracking each of the linear transformations from the input map (far right) to the output (far left). The label below each map denotes the reference frame, while the label above each map denotes the basis in which the map is represented. Arrows indicate linear operations and are labeled accordingly. The upper branch corresponds to the occulted case (Equation (A18)), while the lower branch corresponds to the case where the body is unocculted (Equation (A20)). See text for details.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Four additional families of occultations in reflected light, involving rare triple (cases 11 and 12, top) and quadruple (cases 13 and 14, bottom) intersections between the limb of the occultor and the terminator of the occulted body. All four cases involve integration over two disjoint regions (bounded by the orange curves in the figure). The insets next to each case show a zoomed-in version of four such regions. See text for more details.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Examples of the spectral binning used to define the science requirements for tiers 1 (top) and 2 (bottom) of the Ariel survey. The reduction in resolution for these tiers is a result of postprocessing; so, for reference, the native spectral resolution at which all observations are taken is also shown. The error bars were computed using ArielRad, and the atmospheric forward models were computed using TauREx 3 (Al-Refaie et al. 2021b). The top panel is a free chemistry model, while the TauREx GGChem plug-in is used for the bottom panel (Woitke et al. 2018; Al-Refaie et al. 2021a). Random Gaussian scatter has been added to each spectrum based on the magnitude of the spectral uncertainties. Ariel’s instruments operate simultaneously; therefore, the complete wavelength coverage (0.5–7.8 μm) is provided in a single observation.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Sky locations of potential Ariel tier 1 targets. First panel: currently known planets; second panel: tier 1 targets from the predicted targets of B18; third panel: tier 1 targets from the predicted targets of B20; fourth panel: potential tier 1 targets from the current TPCs. The sky coverage of Ariel, which offers large continuous viewing zones at the ecliptic poles, was determined using the Terminus code (Edwards & Stotesbury 2021). Ariel’s continuous viewing zones have been heavily studied by the TESS mission, leading to many candidates within them.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Histograms of the properties of the host stars within the potential Ariel Tier 1 Catalog. Ariel will probe planets around a range of stellar types out to around 1000 pc from the Earth. The host star could be as faint as T mag ∼ 14.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Histograms of the properties of the planets within the potential Ariel Tier 1 Catalog. While the periods of the planets that can be studied are general constrained to <20 days, in terms of planet temperature and radii, the targets will be highly diverse.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Temperature and radius distribution of known planets, including those found by TESS (left), and these known planets in addition to the current TPCs (right) for M (top), K (middle), and G (bottom) stars that are suitable for tier 1 study with Ariel.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Temperature and radius distribution of known planets, including those found by TESS (left), and these known planets in addition to the current TPCs (right) for F (top) and A (bottom) stars that are suitable for tier 1 study with Ariel.
Paper: The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System
Authors: Billy Edwards, Giovanna Tinetti
Figure caption: Planets suitable for study in tiers 1 (top) and 2 (bottom). For lines marked by “Known + B18” and “Known + B20,” we do not include any confirmed detections made by TESS. “Known” and “Known + TPCs” both include confirmed planets from the TESS mission.
Paper: An ALMA Search for High-albedo Objects Among the Midsized Jupiter Trojan Population
Authors: Anna M. Simpson, Michael E. Brown, Madeline J. Schemel, Bryan J. Butler
Figure caption: Diameter plotted against albedo for all objects modeled, with the three calibrators shown in red. Lines of constant absolute magnitude (Equation (2)) are plotted in gray for values of absolute magnitude between 10 and 12. While it appears that diameter and albedo are anticorrelated, this apparent trend is driven mostly by the fact that for a given value of absolute magnitude, albedo, and diameter can only fall along the indicated line. Because of the limited range of absolute magnitudes observed, it is unknown if small low albedo objects exists, though from the WISE data it is clear that large high-albedo objects do not.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Distribution of Galactic velocity dispersions for a sample of aligned hot Jupiter host stars with smaller-than-median fractional convective envelope masses after simulating the effect of binarity across Monte Carlo realizations. The binary companions are placed at 40 au to reveal the upper limit of the effect of binarity on the Galactic velocity dispersion of the sample, and because a companion at a smaller separation can suppress the formation of giant planets (e.g., Kraus et al. 2012). The mass of the companion is chosen such that the companion is 4 magnitudes fainter than the median primary star in this sample in accordance with the fact that these stars have not been detected as double-lined spectroscopic binaries. Across 10,000 iterations, the median increase in the Galactic velocity dispersion due to binarity is 0.34 km s−1, and the maximum increase is 2.1 km s−1. As the Galactic velocity dispersions of the hosts of misaligned hot Jupiters are larger than those of the hosts of aligned hot Jupiters by ∼7.2 km s−1 for stars without convective envelopes and ∼4.6 km s−1 for stars with convective envelopes, we argue that unresolved binarity cannot explain the Galactic velocity dispersion offsets we observed.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Stellar age distributions of the host stars in misaligned systems (orange) and the host stars in aligned systems (blue) across 1000 Monte Carlo realizations of the sample. Solid lines indicate the median stellar age of each sample. Dotted lines indicate the 16th and 84th percentiles of the stellar age distributions. The misaligned and aligned populations have consistent age distributions. The stellar age inferences from isochrones are not precise enough to reproduce the relative age differences implied by the Galactic velocity dispersion analysis. Top: systems in which the host star has smaller-than-median fractional convective envelope mass. Bottom: systems in which the host star has larger-than-median fractional convective envelope mass.
Paper: Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Authors: Jacob H. Hamer, Kevin C. Schlaufman
Figure caption: Stellar mass distributions of the host stars in misaligned systems (orange) and the host stars in aligned systems (blue) across 1000 Monte Carlo realizations of the sample. As the mass distribution is consistent between the hosts of misaligned systems and hosts of aligned systems, the difference in the Galactic velocity dispersions of the two samples is not related to stellar mass. Top: systems in which the host star has smaller-than-median fractional convective envelope mass. Bottom: systems in which the host star has larger-than-median fractional convective envelope mass.
Paper: Precise Positions of Five Major Uranian Satellites During 2008–2014 Based on Gaia EDR3 
Authors: H. Y. Zhang, R. C. Qiao, Y. Yu, D. Yan, X. Cheng, K. Tang, Y. D. Mao
Figure caption: The original observed images (a), preprocessed observation images (b), and the enlarged view of the observation target area (c). The preprocessing method is as described in the paper (Zhang et al. 2021). This image was obtained on 2011 September 24th.
Paper: Precise Positions of Five Major Uranian Satellites During 2008–2014 Based on Gaia EDR3 
Authors: H. Y. Zhang, R. C. Qiao, Y. Yu, D. Yan, X. Cheng, K. Tang, Y. D. Mao
Figure caption: Schematic representation of the grayscale values for the region where the target star is located. The left panel is a drawing of a local region in Figure 1(a), and the right panel is a local region of Figure 1(b). In the figures, the x- and y-axes represent the measurement coordinate of CCD image, and the z-axis represents the gray value of each pixel.
Paper: Precise Positions of Five Major Uranian Satellites During 2008–2014 Based on Gaia EDR3 
Authors: H. Y. Zhang, R. C. Qiao, Y. Yu, D. Yan, X. Cheng, K. Tang, Y. D. Mao
Figure caption: Offsets (O–C) vs. time of the major Uranian satellites in R.A. and decl. for the seven successive periods of observation from 2008 to 2014. Offsets are computed from the comparison of our observations to the ephemerides DE431 for Uranus and Lainey et al. (2015) for satellites.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: The top two panels show the raw TESS light curves from year 1 and year 3. TESS 2-minute cadences are plotted in gray, and the in-transit points for each planet are colored according to the legend. The spline model is shown in black. The middle two panels show the flattened light curves after removal of the spline, and the best-fit EXOFASTv2 model is plotted for each planet. The bottom panels show the phase-folded transits and residuals for each planet. Colored circles indicate binned data, and the colored lines are the best-fit EXOFASTv2 models. TESS observed a portion of 44 transits of TOI-712 b, 7 transits of TOI-712 c, and 4 transits of TOI-712 d.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: The 5σ contrast curves of TOI-712, observed by the SOAR speckle imager in the I band (purple) and the Zorro speckle imager at 562 nm (blue) and 832 nm (pink). Zorro at 832 nm achieves contrast ratios better than 5 mag at 0.″1, 7 mag at 0.″5, and nearly 8 mag at 1.″2. An eclipsing binary would have to be within 7 mag to produce an event as deep as TOI-712 b.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Twelve ground-based follow-up transits with EXOFASTv2 best-fit models of TOI-712 b (purple lines) and TOI-712 c (pink lines). Labels indicate the instrument, the filter, and the date of observation (see Table 1).
Paper: Ωbar in NGC 5597 from Very Large Array H I 21 cm Observations
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Left: VLA B-configuration H I 21 cm rotation curve of NGC 5597 after several iterations utilizing the task GAL in AIPS. The final fitted systemic heliocentric velocity is V sys−helio = 2698 km s−1. Right: the angular velocity of the H I 21 cm gas, Ωgas (filled pentagons), Ωgas − κ(R)/2 (open circles), Ωgas + κ(R)/2 (open triangles), Ωgas + κ(R)/4 (open squares), where κ(R) is the epicycle frequency. The angular velocity pattern of a stellar bar, Ωbar, is equal to the angular velocity of the gas, Ωgas, in the epicycle approximation at corotation. Our estimation of ﹩{a}_{\mathrm{bar}}^{r-\mathrm{ma}}\sim 20^{\prime\prime} ﹩ (∼3.74 kpc) in NGC 5597 (see Section 3.1.5) as the corotation radius would result in Ωgas ∼ 15.3 km s−1 kpc−1; therefore, Ωbar ∼ 15.3 km s−1 kpc−1 (the constant horizontal line). This Ωbar value crosses Ωgas + κ(R)/4 at a radius R Om=4 ∼ 6.73 kpc, and Ωgas + κ(R)/2 at a radius R OLR ∼ 11.25 kpc.
Paper: Ωbar in NGC 5597 from Very Large Array H I 21 cm Observations
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Left panel: innermost optical red, filter 8040 Å, continuum image of the stellar bar in NGC 5597 in gray scale and in contours, extracted from Figure 2 (Garcia-Barreto et al. 1996). The image had not been calibrated in intensity scale, thus the gray-scale stretch is in relative units proportional to noise from 2.8σ to 40σ, where 1σ = 45 in arbitrary units, and the contours are at 34, 36, 40, 44, 48, 52, 56, 62, 70, 80, 100, 200, 300, 600, and 900 × 1σ, showing the extent of the boxy isophotal contours before a contour with azimuthal extensions. Boxy isophotes delineate a structure straddling the nucleus elongated in P.A. ∼ 52° EofN. Right panel: one-dimensional slice with intensity versus angular distance at P.A. ∼ 52° EofN. Notice the lack of dust lanes.
Paper: Ωbar in NGC 5597 from Very Large Array H I 21 cm Observations
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Left panel: innermost optical blue, 103aO, continuum image of the stellar bar in NGC 5597 in gray scale and in contours, extracted from Figure 1 (Diaz-Hernández et al. 2009). The image had not been calibrated in intensity scale, thus the gray-scale stretch is in relative units proportional to noise from 1.5σ to 39σ, where 1σ = 90 in arbitrary units, and the contours are at 15, 20, 30, 35, 40, 50, 60, 80, 95, 107, and 111.5 × 1σ, showing the extent of the boxy isophotal contours before a contour with azimuthal extensions. Boxy isophotes delineate a structure straddling the nucleus elongated in P.A. ∼ 52° EofN. Right panel: one-dimensional slice with intensity versus angular distance at P.A. ∼ 52° EofN. Notice the lack of dust lanes.
Paper: Ωbar in NGC 5597 from Very Large Array H I 21 cm Observations
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: VLA B-configuration H I 21 cm spectrum of NGC 5597. The heliocentric systemic velocity, fitted by the task GAL in AIPS, is V sys−helio = 2698 km s−1, and the widths at 50% and 20% of the peak are ΔV 50% ∼ 211.40 km s−1 and ΔV 20% ∼ 239.25 km s−1, respectively. Comparing the flux density scale to previous Parkes (64 m) and Green Bank (91m) single dish radio telescope spectra is very difficult because their beams included both disk galaxies NGC 5595 and NGC 5597 (Mathewson et al. 1992; Springob et al. 2005). The shape of the VLA spectrum looks very similar to that of Nançay’s, which has an elongated beam of ﹩\sim 3\buildrel{\,\prime}\over{.} 6﹩ east–west ﹩\times \,22^{\prime} ﹩ north–south at FWHM (Paturel et al. 2003).
Paper: Ωbar in NGC 5597 from Very Large Array H I 21 cm Observations
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: VLA B-configuration H I 21 cm integrated intensity over velocity, Moment 0, image of NGC 5597 in contours superposed on the same image in gray scale. Contours are 3, 35, 50, 70, 100, 125,150,175, 200, 250, and 270 /times 1σ ∼ 0.3 mJy beam−1 km s−1. The gray scale ranges from 3σ to 200σ. The synthesized beam (∼7.″1 × 4.″2 at FWHM) is shown in the lower left corner.
Paper: A Tendency Toward Alignment in Single-star Warm-Jupiter Systems
Authors: Malena Rice, Songhu Wang, Xian-Yu Wang, Guđmundur Stefánsson, Howard Isaacson, Andrew W. Howard, Sarah E. Logsdon, Heidi Schweiker, Fei Dai, Casey Brinkman, Steven Giacalone, Rae Holcomb
Figure caption: Significance with which warm Jupiters in single-star systems are more aligned than analogous hot Jupiters, considering three segmentations. Each panel shows the result of 30,000 iterations in which we sample N WJ random ∣λ∣ values without replacement from the set of hot-Jupiter systems. The resulting distribution of misaligned hot-Jupiter draws is shown in blue, in comparison with the number of misaligned warm-Jupiter systems that have been observed (purple). The number of samples, N WJ, is determined by the number of observed warm Jupiters in each segmentation. Left: the full population of warm Jupiters (N WJ = 12) compared with the full population of hot Jupiters. Center: the full population of warm Jupiters (N WJ = 12) compared with the population of hot Jupiters orbiting hot stars. Right: the population of warm and hot Jupiters orbiting cool stars (N WJ = 10).
Paper: A Tendency Toward Alignment in Single-star Warm-Jupiter Systems
Authors: Malena Rice, Songhu Wang, Xian-Yu Wang, Guđmundur Stefánsson, Howard Isaacson, Andrew W. Howard, Sarah E. Logsdon, Heidi Schweiker, Fei Dai, Casey Brinkman, Steven Giacalone, Rae Holcomb
Figure caption: Comparison of the summed sky-projected misalignments, ∑∣λ∣, in warm-Jupiter (purple) vs. hot-Jupiter (blue) systems. The three segmentations shown are the same as those in Figure 4; however, here we compare the distribution of summed sky-projected spin–orbit angles ∑∣λ∣, without assigning a label of “aligned” or “misaligned” to each system. Each distribution includes 30,000 draws, where each draw consists of N WJ summed ∣λ∣ measurements (N WJ = 12 in the left and middle panels, and N WJ = 10 in the right panel). Each sampled ∣λ∣ value was allowed to vary about a Gaussian distribution characterized by its measured error bars.
Paper: A Tendency Toward Alignment in Single-star Warm-Jupiter Systems
Authors: Malena Rice, Songhu Wang, Xian-Yu Wang, Guđmundur Stefánsson, Howard Isaacson, Andrew W. Howard, Sarah E. Logsdon, Heidi Schweiker, Fei Dai, Casey Brinkman, Steven Giacalone, Rae Holcomb
Figure caption: Sky-projected spin–orbit angles ∣λ∣ as a function of the system age. Warm-Jupiter systems (purple) are aligned irrespective of their age, consistent with a quiescent formation mechanism. By contrast, hot-Jupiter systems (blue) are more commonly misaligned at young system ages. We emphasize that most observed misalignments are found in hot-star systems, such that the apparent trend with age may instead indicate a trend with T eff.
Paper: A Tendency Toward Alignment in Single-star Warm-Jupiter Systems
Authors: Malena Rice, Songhu Wang, Xian-Yu Wang, Guđmundur Stefánsson, Howard Isaacson, Andrew W. Howard, Sarah E. Logsdon, Heidi Schweiker, Fei Dai, Casey Brinkman, Steven Giacalone, Rae Holcomb
Figure caption: Measured ∣λ∣ values as a function of the dimensionless tidal parameter ﹩\xi ={({M}_{{pl}}/{M}_{* })}^{-2}{(a/{R}_{* })}^{6}﹩, which is used as a proxy for the tidal realignment timescale. For clarity, we divide the full sample into hot-star (triangles; T eff ≥ 6100 K) and cool-star (circles; T eff < 6100 K) systems; the same color scheme is applied to both panels. Warm Jupiters have comparatively long tidal realignment timescales, suggesting a primordial origin of their aligned orbits.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: WISE and 2MASS color–color diagram toward B5. (a) WISE (W1–W2) vs. (W2–W3) color–color diagram to identify Class I and Class II objects by adopting the classification criteria given by Koenig & Leisawitz (2014). The black dots with their respective error bars have photometric quality flags “AAA” and “AAB.” The inset shows a zoom-in of all the targets that lie close to the boundary of Class II objects. (b) 2MASS (H − Ks ) vs. (J − H) color–color diagram. The intrinsic loci of dwarfs and giants are each marked with a black curve (Bessell & Brett 1988), whereas those of classical T Tauri stars are represented by the dashed red line (Meyer et al. 1997). All the data points are transformed to the CIT system (Carpenter 2001). The dashed lines represent the reddening direction from the tips of the giants, dwarfs, and T Tauri loci, respectively. The Class I and Class II sources identified in panel (a) are labeled and plotted here with the same symbols. The inset shows a zoom-in of all the targets that lie close to the dwarf and main-sequence loci.