adsabs/AstroCLIMB huggingface dataset:
Paper: A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916’s Dust Morphology
Authors: Jamie R. Lomax, Emily M. Levesque, John P. Wisniewski, John H. Debes
Figure caption: Cross cuts (thin black curves) of the HST/STIS BAR5 imagery in the east–west (top row) and north–south (bottom row) directions. The thickness of the colored lines around the black curves display the uncertainties on our cross cuts. The left column of cross cuts are from the imagery where the diffraction masks were allowed to cross in the center (see left side of Figure 3). The right column are cross cuts taken from the final imagery where the diffraction masks did not cross (see right side of Figure 3). Each of these cross cuts were fit by a function of the form ﹩\frac{C}{{r}^{3}}﹩ (see Section 4.1), which is displayed as a thin, dashed black curve surrounded by a gray region representing the fit’s uncertainty. Regions under the occulting bar and masked out are concealed by the gray boxes. The straight vertical dashed line at 0″ marks the location of the central star under the occulter.
Paper: A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916’s Dust Morphology
Authors: Jamie R. Lomax, Emily M. Levesque, John P. Wisniewski, John H. Debes
Figure caption: GPI H band linear polarization fraction imagery of CD -31°4916’s circumstellar material (top) and relative linear polarization intensity (bottom). The black cross in both panels represents the location of the central star, which was centered behind GPI’s coronagraph, while the solid white circle represents the inner working angle for the GPI instrument in the H band. Both panels are in the same orientation as Figure 1: north is up and east is to the left. Potential clumps of material around the central star are apparent in both images near the edge of the inner working angle of the coronagraph.
Paper: A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916’s Dust Morphology
Authors: Jamie R. Lomax, Emily M. Levesque, John P. Wisniewski, John H. Debes
Figure caption: GPI H-band unpolarized imagery of CD -31°4916’s circumstellar material. The black cross represents the location of the central star, which was centered behind GPI’s coronagraph, while the solid white circle represents the inner working angle for the GPI instrument in the H band. A clump of apparent dust is located almost directly to the south of the central 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: Spectrally averaged contributions overlaid with T–P profiles (left panel) and contribution functions (right panel). (a) Results for the mass-constrained cloudy model, showing the total opacity from the retrieval. (b) Results from panel (a), but isolating only the CIA contribution, excluding cloud opacity. The plotted wavelength range spans from the start of the J-band spectrum to the end of the H-band spectrum used in our retrieval analysis. The white background between the J and H bands corresponds to the wavelength gap not covered in our retrievals.
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 T–P profiles. The black and gray lines represent the T–P profiles derived from our retrievals using the cloudy and cloud-free models, respectively. The gray shaded region indicates the 1σ range from the retrieval in J. Wang et al. (2022), reproduced from Figure 12 of that paper. The blue solid and dashed lines show the best-fit cloud-free and cloudy models, respectively, from the Sonora Diamondback grid (C. V. Morley et al. 2024), with an effective temperature of 1800 K.
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: Contribution functions with varying g and xi while maintaining ﹩g/{x}_{i}={\rm{const.}}﹩. The atmospheric parameters used to generate all figures are based on the results from the mass-constrained retrieval with a cloudy model. Contributions from both the J- and H-band wavelength ranges used in our retrieval are shown. In the panels from left to right, the surface gravity increases. The blue represents the contribution from line opacity, the green represents that from CIA opacity, and the gray dashed line shows the total opacity from both line and CIA opacity. Note that the case with ﹩{\mathrm{log}}\,g=6.5﹩ is included, although such a high gravity is not physical for a brown dwarf.
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 retrieved T–P profile (black line) with condensation curves (colored dashed lines). The gray lines represent 100 random samples from the posterior distributions, while the gray dashed line indicates the retrieved pressure at the cloud top. References for the condensation curves: C. Helling et al. (2001) for TiO2; H. R. Wakeford et al. (2017) for Al2O3; C. Visscher et al. (2010) for Fe, MgSiO4, and MgSiO3. The metallicity is set to be Z = −0.04 according to J. Wang et al. (2022), except for TiO2, as its treatment of metallicity in C. Helling et al. (2001) is uncertain.
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: Abundances assuming thermochemical equilibrium (solid lines). We set C/O = 0.56 and [Fe/H] = −0.04 for this calculation. The retrieved 1σ values of VMRs for H2O and FeH are shown by vertical shaded regions. According to the contribution functions, we observe the atmosphere in the region around 100 < P < 101.1 bar, shown as the horizontally shaded region.
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 function (CCF) of the observed spectrum with the best-fit model (blue line). The model was Doppler-shifted by the retrieved RV, such that the CCF peak is expected to appear at 0 km s−1 (vertical dashed line). For comparison, the gray line shows the CCF of the speckle halo spectrum, simultaneously obtained from the speckle halo fiber during the HR 7672 B observation.
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 same as Figure 6, except for the H-band spectrum. Prominent H2O line positions are indicated by orange lines in the second panel.
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: Posterior distributions of the retrieval for the J- and H-band spectra when a model includes cloud opacity. Only the main parameters are shown here, excluding telluric-related ones.
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: Posterior distributions of the retrieval for the J- and H-band spectra with a clear sky model. Only the main parameters are shown here, excluding telluric-related ones.
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: Cumulative uncertainty for the mideclipse times of a future eclipse survey of our 150 object target lists, set to a nominal Ariel science start date of 2030 May 1. For all planets and planet candidates, we assume an optimistic future uncertainty on ﹩e\,{\rm{\cos }}\,\omega ﹩ of 10%. In the worst-case scenario, where no ephemerides are refreshed (black lines), there will be over 500 accumulated uncertainties for these targets by 2030. Observations by TESS’s current extended mission (EM2, red lines) and our suggested extended missions (EM3 in gold, and EM4 in green) all serve to reduce these uncertainties, and by EM4, the cumulative uncertainty falls below 240 days in both cases. Further decreasing the uncertainties for a 2030s eclipse survey will require targeted observing campaigns to either refresh the transit ephemeris close to the planned eclipse observation date or to capture one or more eclipses and determine the true eclipse epoch and spacing.
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: Cumulative uncertainty for the midtransit times of the two representative target lists at the JWST Cycle 4 start date of 2025 July 1 (left column) and a predicted Ariel start date of 2030 May 1 (right column). In the worst-case scenario, where no transit ephemerides are refreshed beyond what is currently reported in the Exoplanet Archive (black lines), there will be over 40 days of uncertainty for these targets during JWST’s Cycle 4 operations and over 90 days of uncertainty by the time Ariel begins science operations. Observations by TESS’s current extended mission (EM2, red lines) and our suggested extended missions (EM3 in gold, and EM4 in green) all decrease the total uncertainty, and by EM4 are able to bring it down to 23–29 days for Ariel.
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: Planetary radii and equilibrium temperatures of the four transmission spectroscopy planet populations described in Sections 3.1 and 3.2. The left column takes the top 750 objects from the list of viable targets as ranked by a platform-independent transmission FOM (Equation (1)), while the right column populations are assembled by iteratively passing through the grid and taking the top-ranked object in each radius/Teq bin until the target list reaches 750 objects. The top row populations select targets from the confirmed planets alone, while the bottom row populations draw from both the confirmed planets and the TESS and Kepler planet candidates.
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 select stellar and planet properties for the objects that require RV follow-up efforts from the known planets only target list (red) and the known planets + candidates target list (blue). While the known planets + candidates list contains 41% more targets that require mass measurements, a combination of those targets orbiting brighter stars, cooler (and thus lower-mass) stars, and having larger RV semiamplitudes results in the known planets + candidates RV survey still requiring less telescope time than the known planets only RV survey.
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: Distribution of the representative target lists when considering only those planets that have been previously confirmed (top plot) and confirmed planets + current TESS/Kepler planet candidates that have not yet been found to be false positives (bottom plot). Color coding indicates whether the planets require a 10σ (purple stars, reserved for eclipse targets), 5σ (red squares, for small and temperate transmission targets), or 2σ (blue triangles for large and/or hot transmission targets) mass measurement, or if they already have a sufficient mass measurement (green circles).
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: Planetary radii and equilibrium temperatures of our 150 planet representative emission spectroscopy populations, assembled following our representative target list methodology. The top plot selects targets from the known planets alone, while the bottom plot draws from both the known planets and the TESS/Kepler planet candidates. Only planets/planet candidates with an estimated eclipse depth of ≥20 ppm in the H band (1.65 μ) are considered, and those that can obtain a 10σ mass uncertainty in less than three nights of Keck time are considered. Drawing from the planet candidates produces numerous grid spaces with more than five objects present, leading to a more representative survey than what would be possible when only considering known planets.
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: Planet host star distributions for each of the representative transmission + emission spectroscopy target lists described above, following the same layout as in Figure 3. Adding in the TESS and Kepler candidate planets alongside the known planets (right plot) shifts the stellar host population to include more M stars than the known planets only lists, unsurprising given that the TESS mission was optimized to detect planets around cool, nearby stars.
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: Distribution of radii for the planets and planet candidates that still require a 10σ (top panel, reserved for eclipse targets), 5σ (second panel, for transmission targets that are both small and cool), or 2σ (third panel, for transmission targets that are either large or hot), and those that already have a sufficient mass measurement (bottom panel). Each panel includes a histogram for the mass needs distribution assuming the inclusion of both known planets and TESS/Kepler planet candidates (black outline histogram) and the use of only those planets that have already been confirmed (filled color histogram).
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 number of telescope nights required on a 10 m class telescope (blue bars) and a 3.5 m class telescope (gold bars) to obtain sufficient mass measurements for the two representative target lists based on what V-magnitude cut is used to split targets between the two facilities. The purple dashed line in each plot shows the V-magnitude split where the total number of 3.5 m nights is ∼6× the number of 10 m nights, in accordance with the Cost ∝ Diameter1.7 relation from H. P. Stahl & M. Allison (2020).
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. Left: joint constraints on the water mole fraction and effective surface pressure, where color represents the normalized probability density. The 1σ, 1.5σ, 2σ, and 3σ 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, 2σ, and 3σ 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: comparison of our measured transmission spectrum, binned at a fixed resolving power of R = 35 for visual clarity, to cloudless self-consistent models produced using SCARLET and assuming a solar carbon-to-oxygen ratio (C/O = 0.55; M. Asplund et al. 2009) and atmosphere metallicities of 1 (yellow), 100 (orange), 300 (maroon), and 1000 times solar (brown). The relatively small amplitude of the spectrum of TOI-270 b is inconsistent with any clear H2/He-rich atmosphere with atmosphere metallicities below 300 times solar. Chi-square χ2 values between the models and the full-resolution (R = 200, N = 113 data points) spectrum are shown for comparison. Bottom: comparison of TOI-270 b with 100 bar pure H2O (blue), CH4 (red), CO2 (green), and NH3 (purple) atmospheres. The rise in transit depth at the shorter wavelengths of NIRSpec G395H is best reproduced by the absorption features of water.
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: mass–radius diagram for all planets with equilibrium temperatures (AB = 0, f = 1) below 1000 K, radii below 1.6 R⊕, and masses measured at more than 20% precision. The gold star indicates the position of TOI-270 b, using our measured radius and the mass of L. Kaye et al. (2022). Isocomposition model curves from L. Zeng et al. (2016) are shown for pure iron (red), Earth-like (33% iron; brown), and pure rock (orange) scenarios. In contrast with planets that are in a similar mass range, TOI-270 b is inconsistent with an Earth-like composition at 4.4σ. While consistent with a pure-rock composition at 2.4σ, its radius is best explained by 3%–6% water by mass when considering the irradiated ocean model from A. Aguichine et al. (2021; blue line). The planet is also slightly below the 0.01% H2/He curve (light blue line), the lowest value modeled in the atmosphere models of E. D. Lopez & J. J. Fortney (2014). Bottom left: inferred water mass fraction (WMF, ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩) probability posterior distribution when assuming a log-uniform prior on the planetary iron-to-magnesium ratio to sample the core mass fraction of the interior (CMFI). Bottom right: inferred WMFs when assuming the stellar (blue) and solar (green) Fe/Mg values as priors for the CMFI.