adsabs/AstroCLIMB huggingface dataset:
Paper: JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-776 b
Authors: Lili Alderson, Sarah E. Moran, Nicole L. Wallack, Natasha E. Batalha, Nicholas F. Wogan, Anne Dattilo, Hannah R. Wakeford, Jea Adams Redai, Munazza K. Alam, Artyom Aguichine, Natalie M. Batalha, Anna Gagnebin, Peter Gao, James Kirk, Mercedes López-Morales, Annabella Meech, Johanna Teske, Angie Wolfgang
Figure caption: 2D light curves for ExoTiC-JEDI and Eureka! for Visit 1 and Visit 2. Columns show the data (left), models (middle), and residuals (right) at R ∼ 200, the resolution plotted in Figure 2 and used in the modeling and interpretation. The white vertical stripe in the ExoTiC-JEDI Visit 1 data corresponds to the observed HGA move, where 15 integrations were removed from the time series. The Eureka! reduction elected not to manually remove any integrations surrounding the HGA move, instead relying on light-curve level outlier rejection.
Paper: Ground-based Reconnaissance Observations of 21 Exoplanet Atmospheres with the Exoplanet Transmission Spectroscopy Imager
Authors: Ryan J. Oelkers, Luke M. Schmidt, Erika Cook, Mary Anne Limbach, D. L. DePoy, J. L. Marshall, Jimmy Ardoin, Mitchell Barry, Evan Batteas, Alexandra Boone, Brant Conway, Silvana Delgado Adrande, John D. Dixon, Enrique Gonzalez-Vega, Alexandra Guajardo, Landon Holcomb, Christian Lambert, Shravan Menon, Divya Mishra, Jacob Purcell, Zachary Reed, Nathan Sala, Noah Siebersma, Nhu Ngoc Ton, Raenessa M. L. Walker, Z. Franklin Wang, Kaitlin Webber
Figure caption: Left: a comparison of the difference in brightness between the target star and comparison star and the ratio of the out-of-transit precision measured for 330 light curves observed on 22 separate nights using both the comparison star method (σCOMP) and the CMI method (σCMI). On average, we find the CMI method improves light-curve precision by a factor of ~1.5 for comparison stars within 1 mag of the target star or brighter. We only found the comparison star method to improve the precision on seven out of 330 light curves. Right: the achieved dispersion in the light curve of WASP-33 b observed on 2022 September 8 when using the CMI method (black; σ = 3 × 10−4) and when using a traditional comparison star method (red; σ = 3 × 10−3). We find a factor of 10 improvement in out-of-transit precision quality when using the CMI method for this light curve.
Paper: Ground-based Reconnaissance Observations of 21 Exoplanet Atmospheres with the Exoplanet Transmission Spectroscopy Imager
Authors: Ryan J. Oelkers, Luke M. Schmidt, Erika Cook, Mary Anne Limbach, D. L. DePoy, J. L. Marshall, Jimmy Ardoin, Mitchell Barry, Evan Batteas, Alexandra Boone, Brant Conway, Silvana Delgado Adrande, John D. Dixon, Enrique Gonzalez-Vega, Alexandra Guajardo, Landon Holcomb, Christian Lambert, Shravan Menon, Divya Mishra, Jacob Purcell, Zachary Reed, Nathan Sala, Noah Siebersma, Nhu Ngoc Ton, Raenessa M. L. Walker, Z. Franklin Wang, Kaitlin Webber
Figure caption: A visual comparison of the transmission spectra measured with ETSI on separate nights. The final combined spectra are shown as a black line and the spectra for each night are shown as colored lines (red, orange, and blue). The spectra are ordered from large p-values on the top left to smaller p-values on the bottom right. All exoplanets with multiple observations of their transmission spectra have large p-values (p ≥ 0.31) indicating there no exoplanets with statistically dissimilar observations even though the transmission spectra were measured days, weeks, months, and even years apart.
Paper: Ground-based Reconnaissance Observations of 21 Exoplanet Atmospheres with the Exoplanet Transmission Spectroscopy Imager
Authors: Ryan J. Oelkers, Luke M. Schmidt, Erika Cook, Mary Anne Limbach, D. L. DePoy, J. L. Marshall, Jimmy Ardoin, Mitchell Barry, Evan Batteas, Alexandra Boone, Brant Conway, Silvana Delgado Adrande, John D. Dixon, Enrique Gonzalez-Vega, Alexandra Guajardo, Landon Holcomb, Christian Lambert, Shravan Menon, Divya Mishra, Jacob Purcell, Zachary Reed, Nathan Sala, Noah Siebersma, Nhu Ngoc Ton, Raenessa M. L. Walker, Z. Franklin Wang, Kaitlin Webber
Figure caption: Left: the white light curves of KELT-9 b for observations taken across three nights. Right: the white light curves of WASP-77 A b for observations taken across two nights.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Top: best-fit spectra from the petitRADTRANS (pRT) and ATMO retrievals fitting only the JWST/NIRSpec G395H spectrum. Bottom: best-fit spectra from petitRADTRANS fitting the entire 0.2–5.1 μm HST+JWST spectrum. Black points show the spectrum with the offsets fitted in the free-chemistry retrieval, while gray points show the spectrum with the offsets corresponding to the chemical equilibrium retrieval. While the self-consistent PHOENIX radiative-convective equilibrium model shows the correct features, it underpredicts the NUV absorption and overpredicts the magnitude of the IR features. The flexibility of the retrievals allows them to fit the data well (i.e., χ2/N < 1.2).
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Top: transmission spectrum of WASP-178b from the FIREFLy and transitspectroscopy reductions. Middle: Transit depth difference between the FIREFLy and transitspectroscopy reductions, in units of the transit depth uncertainty. Solid lines show a second order polynomial fit to NRS1 and NRS2. Bottom: the FIREFLy reduction compared to two versions of the transit spectrum of ultra-hot Jupiter WASP-121b from C. Gapp et al. (2025), after normalizing to each planet’s equilibrium scale height and taking a 15-point moving average. The points with error bars indicate the average measurement uncertainty.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Graphical representation of the elemental ratios inferred from the retrievals listed in Table 3 in the style of S. Gandhi et al (2023) Figure 3. Redder colors represent retrievals assuming chemical equilibrium, while bluer colors represent free-chemistry retrievals. Measurements with square markers retrieve on only the JWST data, while circular markers are measurements from retrievals of the full-spectrum data set. In black we show our preferred constraints, the evidence-weighted measurements from all HST+JWST retrievals, dominated by the 3TP chemical equilibrium model in pink.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Abundance profiles for H2O, CO, SiO, and CO2 (clockwise from upper left) from the various retrieval scenarios. The abundance profile for WASP-121b from the ATMO chemical equilibrium retrieval is shown for comparison. Also shown are the normalized contribution functions (black) from the pRT chemical equilibrium retrieval, showing approximately where in the atmosphere each molecule is being measured. For SiO, the solid black contribution function shows where the 4.1 μm feature probes, while the dashed line shows where the NUV feature probes. The profile for the ATMO chemical equilibrium retrieval of SiO (dashed yellow) represents the 1σ upper limit.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Temperature profiles from various retrieval scenarios and the PHOENIX 1D radiative-convective equilibrium model. Top: retrievals using only the JWST NIRSpec observations. Bottom: retrievals using both the HST and JWST observations. Dotted lines indicate relevant contribution function profiles. While the shape of the retrieved temperature profile greatly varies, JWST+HST retrievals converge on a 1 mbar temperature around 3200 K. While this is much hotter than the planet’s equilibrium temperature of ∼2450 K (C. Hellier et al. 2019; R. Rodrìguez Martìnez et al. 2020), this may indicate that the transmission spectrum probes a temperature inversion.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Retrieved posteriors for the full-spectrum HST+JWST retrieval under chemical equilibrium and with the three-parameter temperature structure from T. Guillot (2010). Elemental ratios are represented relative to solar, data offsets are in parts per million, the planet radius Rp is in units of Jupiter radii, the temperature is in kelvin, γ is unitless, and κIR is in square centimeters per gram.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: White light-curve fits to the FIREFLy-reduced JWST/NIRSpec G395H data for NRS1 (left) and NRS2 (right). The top panel shows the fit to the raw data, normalized to the out-of-transit baseline. The bottom panel shows the resulting residuals to the fit. While the NRS1 light curve is fit with a linear slope in time, the NRS2 light curve is not. Significant red noise was not detected in the Allan deviation.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Isothermal transmission spectra at 1200 K (left) and 2500 K (right) at a range of metallicities from the forward models of J. M. Goyal et al. (2018). The spectra are all normalized to 1.0 at 4.0 μm to compare feature sizes and shapes. While the H2O feature at 1200 K becomes larger with metallicity before decreasing, at 2500 K the magnitude of H2O monotonically decreases with metallicity.
Paper: Refractory and Volatile Species in the UV-to-IR Transmission Spectrum of Ultra-hot Jupiter WASP-178b with HST and JWST
Authors: Joshua D. Lothringer, Katherine A. Bennett, David K. Sing, Brian Kehoe-Seamons, Zafar Rustamkulov, Henrique Reggiani, Kevin C. Schlaufman, Patrick McCreery, Seti Norris, Peter Hauschildt, Ceiligh Cacho-Negrete, Amélie Gressier, Néstor Espinoza, Cyril Gapp, Thomas M. Evans-Soma, Kevin B. Stevenson, Hannah Wakeford, Neale Gibson, Jamie Wilson, Nikolay Nikolov
Figure caption: Posterior distribution from the stellar characterization in Section 2. Our analysis improves the precision on the fundamental stellar parameters, most significantly the age, which we constrain to be ﹩14{0}_{-80}^{+100}﹩ Myr.
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Data products at several stages of the reduction process for the NIRISS/SOSS eclipse observation of WASP-80 b. (a) Last group of the 113th integration, after superbias subtraction. (b) 1/f noise in frame (a). (c) Integration 113 after ramp fitting and flat field correction. (d) Final calibrated frame after background subtraction and bad pixels interpolation. The full and dashed lines represent the center and edges, respectively, of the aperture boxes used to extract the first (red) and second (blue) orders. The top trace is a contaminant from another star.
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Top: eclipse spectrum of WASP-80 b. The black points with the 1-σ vertical error bars show the NIRISS/SOSS spectrum obtained with the supreme-SPOON reduction pipeline, and the blue points show the spectrum obtained with the additional reduction, shifted by 0.01 μm for clarity. The bins from the order 2 trace are the first 2 points of this spectrum, and the other bins come from the order 1 trace. The HST/WFC3 data points from B. Jacobs et al. (2023) are shown in orange, as well as the first part (2.42–2.81 μm) of the JWST/NIRCam spectrum from T. J. Bell et al. (2023), in pink, binned down to the NIRISS/SOSS resolution. Bottom: The difference in SOSS spectra between the supreme-SPOON and other pipeline is shown in dark blue, where the vertical error bars represent the maximum ones of the two reductions for each bin. The difference between the SOSS supreme-SPOON and NIRCam spectra is shown in dark pink, where the vertical error bars represent the square root of the sum of the squares of the individual error bars.
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Top: median model (blue) along with the 1σ and 2σ confidence intervals from the SCARLET chemical equilibrium retrieval to the secondary eclipse spectrum of WASP-80 b (black). The inclusion of a reflected light geometric albedo in this retrieval leads to a contribution from reflected light of ∼30 ppm to explain the data at short wavelengths. For comparison, we show 1D self-consistent models, assuming Bond albedo values of 0 (red) and 0.25 (orange), produced with SCARLET for an atmospheric metallicity of 6 times solar and carbon-to-oxygen ratio of 0.35. We show in green the 1σ confidence region of the best-fit model to the NIRCam secondary eclipse spectrum (purple, binned down to the NIRISS/SOSS resolution) as presented in T. J. Bell et al. (2023). Bottom: cross sections of water (blue), methane (brown), carbon dioxide (green), carbon monoxide (red), and ammonia (purple); the species considered in the free chemistry retrieval over the NIRISS/SOSS wavelength range. The cross sections, shown at a fixed resolving power of R = 100, are computed at a temperature of 800 K and pressure of 10 mbar, roughly corresponding to the photospheric conditions of WASP-80 b. Increasing cross sections correspond to stronger absorption and, thus, lower thermal emission.
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Top: raw NIRISS/SOSS order 1 (0.85–2.83 μm) white-light curve with 1σ error bars (gray), representing the standard deviation on the out-of-eclipse data points and its temporally binned points (black). The best-fit model, including the eclipse and the systematics, is overlapped in red. Second: systematics removed from the white-light curve. The linear systematics model from Equation (2) is shown in turquoise, and the remaining correlated noise modeled with the GP, along with its 1σ confidence interval, is shown in purple. Third: detrended order 1 white-light curve (gray, binned points in black) once the systematics of the second panel are removed from the data of the top panel along with the eclipse model (red). The error bars represent the best-fit scatter parameter (σ = 102.9 ppm). As more easily seen on the binned points, the error bars seem overestimated, as expected from our Allan variance plot from Figure B4, which is explained by potential remaining correlated noise at the integration level. Bottom: residuals to the best-fit model and their rms value (based on the gray unbinned points).
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Equilibrium temperature as a function of the Bond albedo, AB, and the recirculation factor, f. Since WASP-80 b is a warm gas giant, it is expected to distribute its energy at least uniformly across its dayside (f = 2) or, at best, across its entire surface (f = 1). The retrieved dayside brightness temperature is plotted in black. The median value is shown by a solid line, the 1σ confidence region is delimited by dashed–dotted lines, the 2σ region by dashed lines, and the 3σ region by dotted lines. The gray dashed lines represent the technically possible 1σ limits on AB (0.113 < AB < 0.691), while the white dashed lines show the more realistic 1σ limits on AB (0.148 ≲ AB ≲ 0.383), which cover the possible values for q. Our measured dayside brightness temperature is consistent with full heat redistribution.
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Left: median temperature profile from the chemical equilibrium retrieval, along with its 1 and 2σ confidence regions. Our constraints show a slight preference for a noninverted profile over the photosphere (P = 10−1–10−2 bar). The temperature profiles from the 1D self-consistent models, shown in red (AB = 0) and orange (AB = 0.25), are consistent within 1σ of our measured profile. Center: constraint on the brightness temperature (TB = ﹩{811}_{-70}^{+69}﹩ K) as measured from the samples of the thermal emission spectra obtained from the retrieval. The equilibrium temperature of WASP-80 b (Teq = 824 ± 19 K) assuming a Bond albedo of 0 and full heat redistribution (f = 1) is shown for comparison. Right: constraint on the reflected light geometric albedo (﹩{A}_{{\rm{g}}}=0.20{4}_{-0.056}^{+0.051}﹩), which is constrained to 3.6σ above 0. Our measured reflected light geometric albedo is consistent with the 3σ upper limit from HST (Ag < 0.33, B. Jacobs et al. 2023).
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Reflected light models of WASP-80 b for a variety of cloud species produced with PICASO and VIRGA, considering a Bond albedo of 0.25. The full and dashed lines correspond to models with sedimentation efficiencies fsed of 0.1 and 3, respectively. The models are compared to our measured secondary eclipse spectrum (black and white points, binned by a factor of 2) for wavelengths below 1.6 μm, where the contribution from thermal emission is minimal, as shown by the pink dotted line. The short-wavelength spectrum is best explained by either chromium (Cr), intermediate-sedimentation sodium sulfide (Na2S), potassium chloride (KCl), or low-sedimentation zinc sulfide (ZnS) clouds.
Paper: A Moderate Albedo from Reflecting Aerosols on the Dayside of WASP-80 b Revealed by JWST/NIRISS Eclipse Spectroscopy
Authors: Kim Morel, Louis-Philippe Coulombe, Jason F. Rowe, David Lafrenière, Loïc Albert, Étienne Artigau, Nicolas B. Cowan, Lisa Dang, Michael Radica, Jake Taylor, Caroline Piaulet-Ghorayeb, Pierre-Alexis Roy, Björn Benneke, Antoine Darveau-Bernier, Stefan Pelletier, René Doyon, Doug Johnstone, Adam B. Langeveld, Romain Allart, Laura Flagg, Jake D. Turner
Figure caption: Haze (tholin and soot) models from B. Jacobs et al. (2023) for two metallicities: [M/H] = 0 (solid) and [M/H] = 1 (dashed). The various formation rates are shown in cool colors for the tholins and in warm colors for the soots. The haze models are compared to the NIRISS/SOSS eclipse spectrum of WASP-80 b. If the aerosols are hazes, they could consist of soots or tholins, with formation rates for tholins most likely lower than 10−11.5 g cm−2 s−1.