adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Periodograms of the joint RVs (top panel); the HARPS RVs alone (second panel); the joint RV residuals to a one-planet fit for TOI-199 b (third panel); the HARPS Hα indicator (fourth panel); and the HARPS log(﹩{R}_{\mathrm{HK}}^{{\prime} }﹩) activity indicator (bottom panel). The gray solid, dashed, and dotted horizontal lines indicate false alarm probability levels of 10%, 1%, and 0.1%, respectively. The periods of the two planets are indicated with vertical orange and green lines. We note that the peak at ∼81 days is a one year alias of the ∼104 day planet.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Contrast curve and speckle auto-correlation function from the HRCam at SOAR for TOI-199. The black points and solid line indicate the 5σ contrast curve; the inset shows the speckle auto-correlation function. No nearby sources are detected.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: TESS FFI light curve for Sector 36 extracted with tesseract (blue points), ASTEP light curve (orange points), NEOSSat light curve (green points), Hazelwood light curve (red points), and fitted model to the TESS data (black line) for transit 10.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: TESS FFI light curve for Sector 32 extracted with tesseract (blue points), PEST light curve (orange points), LCO light curve (green points), and fitted model to the TESS data (black line) for transit 9.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Global diagnostics: precipitation, top of the model (100 mb) SH in volume mixing ratios (H2O/Air), surface SH in mass mixing ratios (H2O/Air), and ocean ice fraction (in percent). Lines are 120 month moving means. Note that the Kasting et al. (1993) moist greenhouse limit of 3 × 10−3 v v−1 is not reached for any run although see Figure A2. Note that to make all four cases easily comparable, we have scaled the number of years (x-axis) in Case 4 to the same as Cases 1–3. Nothing changes in Case 4 in the y-axis.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Global diagnostics: surface temperature, planetary albedo, net cloud radiative forcing, and net radiative balance. Lines are 120 month moving means. Note that to make all four cases easily comparable, we have scaled the number of years (x-axis) in Case 4 to the same as Cases 1–3. Nothing changes in Case 4 in the y-axis.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Global diagnostics: precipitation, top of the model (100mb) SH in volume mixing ratios (H2O/Air), surface SH in mass mixing ratios (H2O/Air), and ocean ice fraction (in percent). Black solid lines are 120 month moving means. The Kasting et al. (1993) moist greenhouse limit of 3 × 10−3 v v−1 is denoted by a black dashed line. Notice that Case 4 often has different x- and y-axis scaling from that of Cases 1–3.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Global diagnostics: snow+ice ice fraction, ground water amount in the first soil layer, ground albedo, and total cloud coverage. Lines are 120 month moving means. Note that to make all four cases easily comparable, we have scaled the number of years (x-axis) in Case 4 to the same as Cases 1–3. Nothing changes in Case 4 in the y-axis.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Global diagnostics: snow+ice ice fraction, ground water amount in the first soil layer, ground albedo, and total cloud coverage. Black solid lines are 120 month moving means. Notice that Case 4 often has different x- and y-axis scaling from that of Cases 1–3.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Global diagnostics: surface temperature, planetary albedo, net cloud radiative forcing, and net radiative balance. Black solid lines are 120 month moving means. Notice that Case 4 often has different x- and y-axis scaling from that of Cases 1–3.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Instellation (Flux W m−2) and eccentricity through time for Cases 1, 2, 3 (left) and Case 4 (right). Black line in upper panels is a 120 month moving mean. Note that y-axes have different scales. The x-axis scales are different in the left vs. right set of plots. See Table 1 for details.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Comparable monthly insolation patterns for Cases 1–4 at given snapshots in their eccentricity evolution. We do not include snapshots of the higher eccentricity values attained in Case 4. Insolation bar in the lower right goes from zero to 341 W m−2. Note that we plot Case 4 in the first column and Cases 1–3 in columns 2–4 to make comparisons between Cases 4 and 1 easier.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Best-fit population models and observed occurrence rates marginalized to show distributions in orbital period (left) and planet radius (right). Individual points represent occurrence rates calculated via the inverse detection efficiency method (Equation (4)), with and without accounting for reliability (black and gray points, respectively); numbers represent the number of candidates within each bin. For each method, the colored curve represents the median of the distribution of occurrence rates found by evaluating the population model with the distribution of parameter vectors; lighter filled regions denote the 1σ uncertainty envelopes. Colors represent the results of individual fitting methodologies: M1 (blue) considers only the median parameter values of planets within [0.5, 200] days, [0.5, 1.5] R ⊕ and treats all planets as fully reliable; M2 (orange) is similar to M1 but repeatedly draws planets based on their reliability and concatenates the posteriors; M3 (green) is similar to M2 but also draws each planet’s parameters from within their uncertainties, allowing for the inclusion of planets with median values outside the designated range.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Because of Kepler's poor sensitivity to habitable zone planets (around any star), the current sample does not offer evidence to support M dwarfs hosting more Earth-sized planets than FGK stars at habitable zone instellations. Top: the number of Earth-sized ([0.5, 1.5] R ⊕) Kepler planet candidates orbiting M-dwarf (solid blue), K-dwarf (dashed orange), G-dwarf (dotted–dashed green), or F-dwarf (dotted red) stars as a function of instellation. The shaded gray region denotes the regime where there are no detections of Earth-sized planets around F-type stars, such that FGKM comparisons require models and/or extrapolations. Bottom: Earth-sized planet occurrence rates calculated via the reliability-weighted inverse detection efficiency method (Equation (4)) over a continuum of habitable zone–width instellation bins. The vertical black dashed line represents the approximate point where the Petigura et al. (2022) occurrence distribution plateaus for [0.5, 0.7] M ⊕ stars, indicating the regime where comparisons between spectral types would not be affected by differences in the break points of their power-law distributions.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Posterior distributions for the ﹩{\mathrm{log}}_{10}﹩ power-law breaks in orbital period (top) and instellation (bottom) from the M3 models. Tick marks at the top of each panel represent the corresponding nonlogarithmic values. There is a bimodality in the instellation break posteriors, meaning that our model parameters are not well constrained in this dimension; this feature is discussed further in Appendix C.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Posterior distributions for the ﹩{\mathrm{log}}_{10}﹩ power-law breaks in instellation (left) and average number of planets per star (right). Gray histograms represent posteriors from the M3 models for the full sample (same as Figure 8), while the orange and blue histograms show posteriors from models fit to the warmer and cooler subsamples split at T eff ∼ 3770 K. In the left panel, tick marks on the upper edge represent the corresponding nonlogarithmic values. Both temperature bins produce a bimodality in ﹩{\mathrm{log}}_{10}{I}_{\mathrm{break}}﹩, suggesting that this feature is not attributable to two host star populations distinct in temperature, though the location of the primary peaks is opposite what one would expect from scaling the same orbital period to hotter/cooler stars. In the right panel, we cannot resolve any significant difference in the average number of Earth-sized planets between warmer and cooler M dwarfs.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Similar to Figure 6, but with evaluations in instellation (rather than orbital period) for the range of [0.2, 400] I ⊕, [0.5, 1.5] R ⊕.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: The occurrence rate of Earth-sized habitable zone planets around M dwarfs calculated in this work in orbital period (left) and instellation (right). In either dimension, we include a comparison to previous results: the modeled results of Hsu et al. (2020) calculated in orbital period, or the results of Dressing & Charbonneau (2015) calculated in instellation with the inverse detection efficiency method. Purple and green points denote calculations for optimistic and conservative habitable zone bounds, respectively. For our plotted values in orbital period, we adopted the average habitable zone bounds for the stars in our sample; different stellar effective temperature cases are considered in Table 2.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Modeled occurrence rates of Earth-sized planets around M dwarfs distributed in orbital period (left) and instellation (right), calculated by evaluating Equation (5) with the emcee-output parameter vectors from method M3 (plotted values represent median occurrence rates). Planet candidates from Figure 3 are reproduced here as points with error bars denoting their 1σ parameter uncertainties. Dashed gray lines represent the optimistic habitable zone, and solid gray lines represent the conservative habitable zone (Kopparapu et al. 2013, 2014). The three cases in orbital period represent the habitable zone bounds for the coldest (﹩{T}_{\min }\approx 2979﹩ K) and warmest (﹩{T}_{\max }\approx 4000﹩ K) stars in our sample, along with the average of the bounds for all stars in our sample.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Occurrence rates of Earth-sized planets around M dwarfs distributed in orbital period (left) and instellation (right), calculated via the reliability-weighted inverse detection efficiency method (Equation (4)). White bins with a printed occurrence of η = 0% indicate bins that are technically populated, but by a candidate(s) with a reliability of 0.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Median distance per HEALpixel for the constant number sample in GDR3: Geometric (top) and kinegeometric (middle). The linear color bar spans the full common range. The bottom panel shows the median fractional differences between these (computed on the individual stars). It uses a bilinear color bar with white at zero and diverges on different linear scales to the maximum negative and positive differences.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Median per HEALpixel of the ratio (kinegeo/geo) of the posterior widths for the constant fraction sample in GDR3. Numbers less than 1 (in orange) show where the width of the kinegeometric distance posterior is narrower than the width of the geometric distance posterior, and these are therefore statistically likely to be more accurate. We see that this is the case in most parts of the sky, but particularly so in the disk and bulge. The bilinear color bar with white at unity and diverges on different linear scales to the minimum and maximum values.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Normalized residuals for the geometric posterior distance (top left) and for the three parameters of the kinegeometric posterior (other panels), computed for all sources in mock HEALpixel 6200. The smooth red lines show the unit Gaussian for comparison.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Variation of the fractional difference between the kinegeometric and geometric distances with geometric distance for the constant fraction sample in GDR3. The color scale shows the density of stars on a log scale. The solid orange line shows the median fractional difference, and the dotted lines the 5th and 95th percentiles. The dashed pink line shows the median fractional difference for just the subset with parallax S/N less than three.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Velocity residuals—(estimated-true)—per HEALpixel for the constant number sample in the mock catalog. The top row shows the median residual (the bias); the bottom row shows the median absolute residual (the scatter). The left column is for geometric method (geometric distance times proper motion). The right column is for kinegeometric estimates. The color bars span the full common range in each of the top and bottom rows. The top row uses a bilinear color bar (separate scales for negative and positive values).
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Demonstration of how the proper motion likelihood (P(μ∣r, v), orange) combines with the velocity prior (P(v∣r), blue) to constrain the distance via Equation (A1), from a measured proper motion of 1 ± 0.25 mas yr−1. This is shown for two different velocities, 10 and 30 km s−1. The gray curve is the product of the orange and blue curves. The black dashed line is the integral in Equation (A1) computed for a continuous range of velocities. None of these functions are probability density functions in r, but all have been normalized to unit area over the range plotted.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Median transverse velocity per HEALpixel for the constant number sample in GDR3: Geometric (top) and Kinegeometric (middle). The linear color bar spans the full common range. The bottom panel shows the median differences between these (computed on the individual stars). It uses a bilinear color bar with white at zero and diverges on different linear scales to the maximum negative and positive differences
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Median performance of the geometric (blue) and kinegeometric (orange) distance estimates as a function of distance for the constant fraction sample in the mock GDR3 (solid) and mock GDR5 (dashed) catalogs. The left panel shows the fractional bias in the estimates. The right panel shows the fractional scatter. The solid lines are the same as those in Figure 7.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Median differences between the kinegeometric and geometric velocities per HEALpixel (computed on the individual stars), for the constant number sample in the mock catalog. The color bar has white at zero and diverges on different linear scales to the maximum negative and positive differences.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Top panels: the 15 × 15 pixel TESS FFI from Sectors 6 and 33. The black shaded region represents the 3 × 3 pixel custom aperture we used to conduct photometry. TOI-4201 is marked as a white star at the center. Different sizes of red circles represent different magnitudes in contrast with TOI-4201. Bottom panels: the normalized TESS light curves of TOI-4201 from Sectors 6 (left) and 33 (right) that we extracted. The red solid lines are the GP models used for detrending. The detrended light curves are shown below. The transits of TOI-4201b are marked with blue tickmarks.