adsabs/AstroCLIMB huggingface dataset:
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Confidence that a simulated Earth-like planet (a = 0.74 au, e = 0.21) is within the star’s HZ (both periastron and apastron within the HZ boundaries), increases with additional epochs of relative astrometry. Top left: Posterior probability on this simulated planet’s HZ status as a function of observing epoch. Green points represent the fraction of orbits from the fit posterior that are always between the inner and outer boundary of the HZ; red points either cross these boundaries, are closer to the star than the inner edge of the HZ, or are further than the outer edge of the HZ. For these simulated observations of this planet, only by epoch 4 is the probability that the planet is fully within its star’s HZ 100%. The number of epochs required to confidently establish a planet as being fully within the HZ depends on the orbital geometry and the timing of the relative astrometric observations. Top right: Observed sky-projected positions of the planet (blue points), true orbit (red), and orbital fit posteriors: HZ-consistent orbits (green) and orbits extending beyond the HZ (gray). Bottom panels: Corresponding 3D star–planet separations, with optimistic HZ boundaries in red, observational epochs (dashed vertical lines) in gray, and the latest epoch highlighted in blue. Note by epoch 4, all remaining orbits are fully within the HZ boundaries
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: Same as Figure 15, but for a non-HZ planet at large angular separation (a = 2.45, e = 0.43). Top left: Posterior probability on this simulated planet’s HZ status as a function of observing epoch. The large projected separations quickly rule out HZ-compatible orbits within 2–3 epochs, even with the planet undetectable in the first two epochs. Top right: Observed sky-projected positions (blue), true orbit (red), and posterior orbits: HZ-consistent (green) and inconsistent (gray). Bottom panels: 3D star–planet separations relative to optimistic HZ boundaries (red), with observational epochs (gray dashed lines) and the latest epoch in blue. By epoch 4, all remaining solutions lie outside the HZ.
Paper: Requirements for Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory
Authors: Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan
Figure caption: High-confidence characterization of HZ planets requires substantially more observational time than initial identification. The plot shows the cumulative number of confirmed HZ planets vs. observational epochs at 68% confidence (solid blue) and 95% confidence (dashed orange) levels, out of 29 true HZ planets in our 98-system sample. A planet is classified as HZ when the specified percentage of its fitted orbits lie within the optimistic HZ boundaries.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Retrieval results for the J-band spectrum with the model including cloud opacity. The top panel is the observed spectrum of HR 7672 B and the full model with 95% credible intervals. The second panel shows the leakage of the host star’s light (dark gray), that is the scaled spectrum of the observed host star, HR 7672 A, retrieved telluric transmittance (light gray), and the brown dwarf’s spectrum model (pink). Prominent FeH line positions are indicated by vertical green lines. The third panel shows the spectrum of HR 7672 B, which was corrected by dividing by the telluric lines and subtracting the scaled HR 7672 A’s spectrum (black dots). The pink lines in the third panel also represent the retrieved brown dwarf model. Other colored lines represent models excluding specific molecules; specifically, the orange lines correspond to models without H2O, and the green lines to models without FeH. The bottom panel shows residuals.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: The observed J- and H-band spectra of HR 7672 B. The top panels of each figure show the telluric transmittance created by the LBLRTM (S. A. Clough et al. 2005) for reference. The bottom three panels show the spectra of HR 7672 A, HR 7672 B, and the speckle halo light, with each combining two frames. The last spectrum was obtained from the speckle halo fiber during the observation of HR 7672 B. The gray dots in the third panel are uncertainties at each data point. Wavelength ranges used for our retrieval are highlighted in pink. The mean uncertainties within these ranges are 7.8 × 10−4 for the J band and 8.1 × 10−4 for the H band, respectively. These uncertainties are expressed as relative values with respect to the flux normalized by the blaze function. In the J band, green dashed lines are the wavelengths of K I doublets, and the orange dashed line is at the absorption of Na I. In the H band, wavelength regions in the red dashed line exhibit pronounced long-period noise.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Comparison of the spectra of HR 7672 A and B was performed to assess light leakage from the host star in HR 7672 B’s spectrum. Panels (a)–(c) display the spectra around the strong absorption lines from the host star, as indicated by vertical colored lines, following the wavelengths referenced in J. T. Rayner et al. (2009). Note that only the barycentric velocity correction for each observation date was applied; the radial velocity correction was not applied, so the wavelengths in the figure are slightly shifted from the expected line positions.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: The example of spectra of order 64 (in the H band) observed on the same date. The blue line is the spectrum of κ And b, the orange line is the FLAT spectrum scaled by a factor of 0.04 for comparison, the green line is the spectrum from speckle halo fiber of the κ And b observation, and the red line is the spectrum of κ And b with shifting trace line by 40 pixels. See the text for details.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Heatmap of the H-band spectrum of κ And b, shown across spectral orders and pixels within each order. The color gradually changes in accordance with the normalized flux. The left panel is the spectrum obtained from the science fiber, while the right panel is the spectrum obtained from the speckle halo fiber. The periodic noise appears prominently especially from orders 61 to 66, and they look similar in both fibers.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Image of HR 7672 observed by SCExAO internal fast IR detector (C-RED2) on 2021 June 7 (ID: S21A-062, PI: H. Kawahara). HR 7672 B in a green circle is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩7 away from the host star.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Comparison of fluxes in the J, H, and Ks bands. The black dots represent the observed flux, while the red and purple dots correspond to the fluxes calculated from our model—red represents the cloudy model, and purple represents the clear sky model. The J-band values from our model are derived from predictions and their 95% credible intervals. For the H and Ks bands, we plot the values derived using the median parameters of the posterior distribution as filled circles, and 100 random samples from the posterior distributions as translucent circles. The blue triangles represent fluxes computed from the Sonora Diamondback models.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Mean combined spectra from the speckle halo fiber in order 64 observed on different dates. From top to bottom: June 6, 7, 22, and 24 for HR 7672 B, and June 24 for κ And b. The colored points are selected by rejecting both edges of the order and clipping outliers beyond 4σ.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Periodograms of spectra in order 64 of the speckle halo fiber observed on different dates, corresponding to the spectra in Figure 17.
Paper: Unveiling the Atmosphere of HR 7672 B from the Near-infrared High-resolution Spectrum Using REACH/Subaru
Authors: Yui Kasagi, Yui Kawashima, Hajime Kawahara, Takayuki Kotani, Kento Masuda, Kyohoon Ahn, Olivier Guyon, Teruyuki Hirano, Nemanja Jovanovic, Masayuki Kuzuhara, Julien Lozi, Motohide Tamura, Taichi Uyama, Sebastien Vievard, Kenta Yoneta
Figure caption: Cross-correlation analysis demonstrating the detection of FeH in the J-band spectrum in panel (a) and the detection of H2O in the H-band spectrum in panel (b). The vertical black dashed line shows the rest frame of the brown dwarf.
Paper: A New Approach to Compiling Exoatmospheric Target Lists and Quantifying the Ground-based Resources Needed to Vet Them
Authors: Jennifer A. Burt, Robert T. Zellem, David R. Ciardi, Shubham Kanodia, Geoffrey Bryden, Tiffany Kataria, Kyle A. Pearson, Jessie L. Christiansen, Charles Beichman, B. J. Fulton, Mark Swain
Figure caption: Left: the 5843 known planets and TESS/Kepler planet candidates that meet all of the selection criteria (summarized in Figure 2) spread across the equilibrium temperature and planet radii bins standardized in B. J. Hord et al. (2024). Larger planets dominate the population, but thousands of sub-Neptune-sized planets are present in this initial list. Right: host stars for these same known planets and TESS/Kepler planet candidates. Bold purple dashed lines denote the mean V- and H-band magnitudes, while the thinner purple dashed lines denote the first and third quartiles in each magnitude distribution.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A New Approach to Compiling Exoatmospheric Target Lists and Quantifying the Ground-based Resources Needed to Vet Them
Authors: Jennifer A. Burt, Robert T. Zellem, David R. Ciardi, Shubham Kanodia, Geoffrey Bryden, Tiffany Kataria, Kyle A. Pearson, Jessie L. Christiansen, Charles Beichman, B. J. Fulton, Mark Swain
Figure caption: Left: two-dimensional input sample set with the 917 confirmed planets that meet our inclusion criteria of having published mass and radius measurements at the 50% or better level. Background color shows the corresponding joint probability distribution f(m, r), where blue is a higher probability and yellow is lower. Right: conditional mass distribution f(m∣r) for the joint mass–radius distribution for an example set of planet radii. The vertical dashed lines denote the expected mass value, while the curve shows the probability density function for each radius.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A New Approach to Compiling Exoatmospheric Target Lists and Quantifying the Ground-based Resources Needed to Vet Them
Authors: Jennifer A. Burt, Robert T. Zellem, David R. Ciardi, Shubham Kanodia, Geoffrey Bryden, Tiffany Kataria, Kyle A. Pearson, Jessie L. Christiansen, Charles Beichman, B. J. Fulton, Mark Swain
Figure caption: Visual summary of the target list assembly process, starting from a list of confirmed transiting planets downloaded from the Exoplanet Archive and the lists of TESS and Kepler Objects of Interest (TOIs/KOIs) that have not yet been found to be false positives via ground- and space-based follow-up observing efforts.
Paper: A New Approach to Compiling Exoatmospheric Target Lists and Quantifying the Ground-based Resources Needed to Vet Them
Authors: Jennifer A. Burt, Robert T. Zellem, David R. Ciardi, Shubham Kanodia, Geoffrey Bryden, Tiffany Kataria, Kyle A. Pearson, Jessie L. Christiansen, Charles Beichman, B. J. Fulton, Mark Swain
Figure caption: Comparison of the overall planet mass acquisition rate (top left) and midsurvey populations of planet masses using three different target prioritization schemes: a FOM ranking (green line and top right grid), an RV Efficient ranking (pink line, and bottom left grid), and a Homogeneous Spread ranking (gold line, and bottom right grid). Upon completion of the full 105 night survey on Keck, all survey designs converge and provide requisite masses for all planets on the target list (top left). However, the order in which planet masses are acquired varies, and after 25 nights, the populations of planets with newly measured masses within each survey (top right and bottom row) are quite different. Selecting a survey design that enables, for example, the early mission science priorities of the Ariel science team can ensure high-quality science even if the full RV survey is not completed before Ariel begins returning data.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Root mean square of the residuals as a function of the bin size of the broadband and spectroscopic light curves. Left: rms curves computed from the residuals of the fits to the NRS1 white light curves extracted using Eureka! (blue), Tiberius (red), and exoTEDRF (green). The colored dashed lines represent the expected 1/﹩\sqrt{N}﹩ trend of Poisson noise considering the fitted light-curve scatter. The black dashed line corresponds to the Poisson noise trend assuming the errors returned by the jwst pipeline. The three reductions show different scatters at the temporal resolution of the data but reach the same noise floor for bin sizes of >30–40 minutes. Center left: normalized rms curves (black lines) for all exoTEDRF spectroscopic light curves from the NRS1 detector. The red dashed line corresponds to the Poisson noise trend. Center right: same as left for the NRS2 white light curves from the three independent reductions. Right: normalized rms curves for all exoTEDRF spectroscopic light curves from the NRS2 detector.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Constraints from the atmospheric retrieval considering the fictitious species X as the background gas and including an offset δNRS1,2,. Left: joint constraints on the water mole fraction and effective surface pressure, where color represents the normalized probability density. The 1σ, 1.5σ, and 2σ probability contours are indicated by the full and dashed black lines for the retrievals assuming no TLS and with constrained TLS, respectively. Middle: joint constraints on the water mole fraction and background gas MMW (μX). The 1.5σ and 2σ probability contours are indicated by the full and dashed black lines for the retrievals assuming no TLS and with constrained TLS, respectively. Beyond water mole fractions of 90%, the background MMW is unconstrained as the global MMW is dominated by that of H2O. Below that, the 1.5σ and 2σ confidence regions are confined to a given range of MMW values, as global MMWs that are too low/high would result in water absorption features that are too large/small compared to the tentative feature. Right: joint constraints on the background gas MMW and effective surface pressure.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Top row: comparison between the transmission spectra obtained from the Tiberius (red) and exoTEDRF (green) reductions (left), and the Eureka! (blue) and exoTEDRF reductions (right). Middle row: residuals between the Tiberius and exoTEDRF transmission spectra (left), and the Eureka! and exoTEDRF transmission spectra (right). The error bars for the residuals are computed by summing the error bars of the two spectra in quadrature. The mean values of the residuals, normalized by their error bars, are indicated in the panels. The Tiberius and exoTEDRF spectra show great consistency across the full wavelength range, with residuals well centered around zero. As for the Eureka! spectrum, it is generally consistent with exoTEDRF over the NRS1 detector, but there is a significant deviation from zero at wavelengths past 4.5 μm between the two reductions. Bottom row: transit depth errors for the three spectra.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Left column: logarithm of the absolute values of the covariance matrices computed from the residuals of the 51 NRS1 spectroscopic light-curve fits for the Tiberius (top), exoTEDRF (middle), and Eureka! (bottom) reductions. Right column: maximum-normalized covariance curves for all individual spectral bins of the NRS1 detector. The Eureka! reduction shows significant covariance between neighboring spectral bins (away from the diagonal), contrary to the Tiberius and exoTEDRF reductions.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Constraints on the water mole fraction and effective surface pressure from the free-chemistry retrieval without TLS and including an offset δNRS1,2. Color represents the normalized posterior probability density from the retrieval assuming no TLS effect, and the full black lines indicate the 1σ, 1.5σ, and 2σ confidence intervals. The dashed lines represent those same confidence intervals for the retrieval where we assume as a prior the TLS parameter constraints from the retrieval on TOI-270 d.