adsabs/AstroCLIMB huggingface dataset:
Paper: Observations and Studies on the Transiting Systems HAT-P-36, XO-2 and WASP-76
Authors: Weilong Wang, Shenghong Gu, Xiaobin Wang, Leilei Sun, Byeong-Cheol Lee, Chi-Tai Kwok, Ho-Keung Hui, Jiangpei Dou, Yue Xiang, Dongtao Cao, Fukun Xu
Figure caption: The examples of light curve fitting for the ground-based photometry (top three panels) and TESS photometry (bottom three panels), along with the residuals. The upper black dots are observations and the blue curves represent the best-fit model in each panel. The left two panels are for HAT-P-36, the middle two panels for XO-2, and the right two panels for WASP-76.
Paper: Observations and Studies on the Transiting Systems HAT-P-36, XO-2 and WASP-76
Authors: Weilong Wang, Shenghong Gu, Xiaobin Wang, Leilei Sun, Byeong-Cheol Lee, Chi-Tai Kwok, Ho-Keung Hui, Jiangpei Dou, Yue Xiang, Dongtao Cao, Fukun Xu
Figure caption: The contour plots show the logarithm of the normalized observed TTV dispersion for each system, denoted as ﹩\mathrm{log}({\sigma }_{1}{n}_{1}{\mu }_{2}^{-1})﹩, where σ1 is the standard deviation of the observed TTVs, n1 is 2π/P1 and μ2 is m2/M*. The dashed lines represent the boundary that the perturbing objects satisfy the specific orbital configuration conditions (a2(1 − e2) > 5a1). The top panel is for the HAT-P-36 system, the middle panel for the XO-2 system, and the bottom panel for the WASP-76 system.
Paper: Observations and Studies on the Transiting Systems HAT-P-36, XO-2 and WASP-76
Authors: Weilong Wang, Shenghong Gu, Xiaobin Wang, Leilei Sun, Byeong-Cheol Lee, Chi-Tai Kwok, Ho-Keung Hui, Jiangpei Dou, Yue Xiang, Dongtao Cao, Fukun Xu
Figure caption: The best-fit results of the TTV patterns for the three systems. The blue line represents the orbital decay model, and the red line represents the apsidal precession model. The top panel is for the HAT-P-36 system, the middle panel for the XO-2 system, and the bottom panel for the WASP-76 system.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Power-law geometrical model fit to the F480M kernel phase and log kernel amplitude data of PDS 70 (images) using uniform priors on the positions of PDS 70 b and c, shown with a linear stretch in arbitrary units. With respect to the central source (yellow star), PDS 70 b is to the southeast, while PDS 70 c is directly west. The white and gray dashed contours, plotted on top of the arbitrarily colored posterior density, denote the 1σ, 2σ, and 3σ contours of the marginalized posterior of the positions of PDS 70 b and c from the Bayesian average of the posteriors of the three models. The two gray dashed circles are centered on the predicted locations of the planets at the time of the observations (J. J. Wang et al. 2021b) from whereistheplanet (J. J. Wang et al. 2021a). We mask the central region to denote the inner working angle of ~0.5λ/B = 94 mas, the diffraction limit of the data.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Log kernel amplitude data in black with the model values plotted in red (top) and the kernel phase data in black with the model kernel phases shown in red (bottom) for the two point source plus power law disk geometrical model fit to the F480M data. The error bars are the square root of the diagonal of the covariance matrices, including the estimated systematic uncertainty in the log kernel amplitudes. For both panels, the large red circles denote the values calculated with the median parameter model, and 250 random posterior samples are denoted by the small, transparent red points. The noise-normalized residuals are shown below both panels.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Squared visibility data (top) and closure phase data (bottom).
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Mean PDS 70 calints file, after bad pixel correction, using only the first 28 groups.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Corner plot showing the 1D and 2D marginalized posteriors of the companion parameters from the joint two point source plus geometrical model fits to the F480M log kernel amplitudes and kernel phases.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Evolution of the central 3 × 3 pixels as a function of the intensity in each pixel (in the linearized-ramp-level data). Each panel represents a pixel and is colored by the count rate in that pixel from the ramp fit to the entire data set. PDS 70 is shown on the left, and HD 123991 is shown on the right. The solid red line shows the evolution of the mean of the calints frames after data cleaning. Here we are plotting the calculated rate minus the rate calculated from the first 28 groups and the first 10 groups for PDS 70 and HD 123991, respectively. These rates are divided by the rate of the ramp fit using all of the groups. The orange line shows the evolution of the linearized-ramp-level data (ramp level immediately after it has undergone the linearity step, in stage 1 of the jwst pipeline). To clearly illustrate the change in rate in each pixel as a function of well depth, we are plotting the difference between groups separated by 15 groups and 5 groups for PDS 70 and HD 123991, respectively, for increasing signal. From this, we additionally subtract the difference between the 25th and 10th groups for PDS 70 and the difference between the 10th and 5th groups for HD 123991 and then normalize this quantity by the difference between the final group and one 15 and 5 groups earlier for PDS 70 and HD 123991, respectively. The vertical dashed red line shows the extent of the data that were used in our analysis.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Point-source model SNR map, within a radius of 400 mas (denoted by the gray circle), calculated from the kernel phase residuals from the two point sources plus power law geometrical model fit. The white contours denote the 1σ, 2σ, and 3σ contours from the posterior calculated with nested sampling. The gray dashed lines denote the predicted locations of PDS 70 b and c at the time of the observations (J. J. Wang et al. 2021a, 2021b). The white star denotes the position of the star. The extended white contours to the southwest of the star denote the forward-scattering side of the outer disk from the power-law model. As in Figure 3, the white dashed circle denotes the diffraction limit of the data.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Mean contrast curves calculated from the residuals of the power-law geometrical model plus two-point-source fit. The color map represents the 0σ–7σ contrast upper limits linearly from white to black. We also denote the 1σ, 3σ, and 5σ azimuthally averaged limits with the white curves. The 1σ, 2σ, and 3σ confidence intervals of the planet contrast/separation, calculated from the nested sampling posterior of the power-law model fit, are denoted by the white contours. We note that, for the signal depth of our data, the expected achievable contrast for photon-noise-dominated data is ~7.8, from Equation (10) in A. Sivaramakrishnan et al. (2023).
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Spectral fit of PDS 70 b using Drift-PHOENIX models with (dashed orange line) and without (solid green line) contribution from a CPD. Blue circles represent the IFS and GRAVITY spectra, while the photometric data points are reported with blue squares (see Section 4.3 for details). Horizontal error bars represent the effective width of the filters. The red star shows the new NIRISS F480M measurement. The thick lines are the spectra obtained from the set of parameters providing the maximum likelihood, while the thin lines report 100 samples randomly drawn from the posterior distribution.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: The correlation matrices, from left to right, of the model parameters for the Gaussian model, the Henyey–Greenstein model, and the power-law model.
Paper: The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 μm
Authors: Dori Blakely, Doug Johnstone, Gabriele Cugno, Anand Sivaramakrishnan, Peter Tuthill, Ruobing Dong, Benjamin J. S. Pope, Loïc Albert, Max Charles, Rachel A. Cooper, Matthew De Furio, Louis Desdoigts, René Doyon, Logan Francis, Alexandra Z. Greenbaum, David Lafrenière, James P. Lloyd, Michael R. Meyer, Laurent Pueyo, Shrishmoy Ray, Joel Sánchez-Bermúdez, Anthony Soulain, Deepashri Thatte, William Thompson, Thomas Vandal
Figure caption: Same as Figure 9 but for PDS 70 c.
Paper: Continuous Fragmentation of Comet 157P/Tritton
Authors: Jane Luu, David Jewitt
Figure caption: Median image from each night of observation. The green boxes show the near-comet fragments, while the white boxes show the fragment cluster B. Arrows point to Fragment C, visible on UT 2024 November 16 and 25. All panels have the same dimensions.
Paper: Continuous Fragmentation of Comet 157P/Tritton
Authors: Jane Luu, David Jewitt
Figure caption: 157P’s nightly mean H  R . The formal uncertainties are ∼0.03 mag, smaller than the size of markers. The straight line is a linear fit to our data, with the slope of 0.04 mag day−1. The error bar on the COBS point is due to the uncertainty in the filter used.
Paper: Continuous Fragmentation of Comet 157P/Tritton
Authors: Jane Luu, David Jewitt
Figure caption: 157P’s nightly photometry.
Paper: Continuous Fragmentation of Comet 157P/Tritton
Authors: Jane Luu, David Jewitt
Figure caption: Scattering cross section of 157P over time. The lines are the fits to the data using Equations (7) and (8).
Paper: Continuous Fragmentation of Comet 157P/Tritton
Authors: Jane Luu, David Jewitt
Figure caption: Motion of the brightest pixel in fragment cluster B as a function of time, in R.A. (left) and decl. (right). The x-axis is the time elapsed since the time of the first observation at UT 2022 October 7 05:46:09. The cluster changes direction and magnitude after UT November 1. The lines shown are fit to the motion over UT October 7–November 1 (dR.A./dt = −0.9 m s−1, d(decl.)/dt = 1.0 m s−1), and UT November 1–16 (dR.A./dt = 2.5 m s−1, d(decl.)/dt = 1.8 m s−1).
Paper: Continuous Fragmentation of Comet 157P/Tritton
Authors: Jane Luu, David Jewitt
Figure caption: A summed image of 157P on UT 2022 October 7, consisting of six individual 150 s exposures. Fragment A and complex B are indicated with arrows. The oblique trails are due to field stars; the small gap in each trail is due to a short break in the observations. The dotted circles show the sky annulus.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: The NIRSpec/G395H white light curves (left) for L 168-9 b from the Aesop (top), Tiberius (middle), and Eureka! (bottom) reductions for visits 1 (pink), 2 (blue), and 3 (green), compared to the best-fitting transit+systematics models (black). The residuals for each visit are shown in the right panel.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: Top: comparison of the Aesop (pink), Tiberius (blue), and Eureka! (green) reductions for visit 1 (left), visit 2 (middle), and visit 3 (right). Bottom: the combined transmission spectrum for all three visits from the Aesop and Tiberius weighted averages and the Eureka! joint fit.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: The MIRI/LRS white light curve for L168-9 b (points) compared to the best-fitting transit+systematics model (black). The residuals are shown in the bottom panel.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: Top left: the Aesop weighted-average NIRSpec/G395H transmission spectrum (black points) of L 168-9 b compared to 1D isothermal atmospheric models assuming single-gas compositions, with methane (dark pink, dashed), water (dark green, dashed), and carbon dioxide (dark blue, dashed), as well as solar composition (light green), 25× solar metallicity (light pink), and 100× solar (light blue) models extracted from the model grid generated using the analytical temperature–pressure profile from T. Guillot (2010). A flat-line model is shown in purple. The best-fitting (χ  r  = 0.76) atmospheric model is the flat-line model, consistent with either a high-altitude gray cloud deck, atmospheres with mean molecular weights greater than 4 g mol−1, or no atmosphere. The light-gray shaded region corresponds to the 1σ scatter in the data. Top right: typical size of spectral features ( ±5 atmospheric scale heights; S. Seager & D. D. Sasselov 2000) as a function of mean molecular weight (MMW) compared to the MMW of molecular hydrogen (2.3 g mol−1; gray), methane (16.0 g mol−1; pink), water (18.02 g mol−1; green), and carbon dioxide (44.01 g mol−1; blue). The transit-depth uncertainty per spectral bin as well as the scatter in the transmission spectrum far exceeds the scale height of any possible high mean molecular weight atmosphere for this planet. Bottom: the same as the top panel, except for the NIRSpec/G395H (Aesop weighted average) + MIRI/LRS transmission spectrum. A flat line best fits the near- to mid-infrared transmission spectrum (﹩{\chi }_{r}^{2}﹩ = 0.95).
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: Top: cloud-top pressure vs. atmospheric metallicity for the Aesop weighted-average NIRSpec/G395H transmission spectrum of L 168-9b, where the colored contours correspond to the significance level (in σ) to which we can rule out our forward models. The dashed black curve indicates the threshold beyond which we can rule out regions of this parameter space to >3σ confidence. Bottom: same as the top panel, but for the NIRSpec/G395H+MIRI/LRS transmission spectrum of L 168-9b.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: Left: solid lines are the predicted temperature–pressure profiles from clima for the 100 bar CO2 (pink), 100 bar H2O (blue), and 100 bar CH4 (green) atmospheric scenarios for L168-9 b, compared to the expected dayside emission temperature of a bare rock (1200 K, assuming an albedo of 0.1; black vertical dashed line). The colored dashed curves are the 15 μm emission contribution function (Equation (4) from J. D. Lothringer et al. 2018) for each atmospheric scenario. Right: simulated JWST/MIRI eclipse depths at 15 μm for three eclipse observations (points) based on each scenario. The bare-rock case is represented by a 1200 K blackbody.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: Mass–radius diagram for small planets (points) color coded by planetary equilibrium temperature compared to theoretical curves of constant composition (solid lines; L. Zeng et al. 2016). The pink dashed line represents the smallest radius a rocky planet can have due to loss of its mantle by collisional stripping by planetesimals, based on the model of R. A. Marcus et al. (2010). The measured mass and radius of L168-9 b are consistent with a Mercury-like bulk composition.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: Photoevaporation model based on J. G. Rogers & J. E. Owen (2021), adapted to the L 168-9 system for initial H/He atmospheric mass fractions of 2% (dark pink), 5% (light pink), 20% (dark blue), 30% (light blue), 50% (dark green), and 100% (light green). For a large range of potential initial atmospheric mass fractions, L 168-9 cannot retain an atmosphere beyond the first 200 Myr of its 3 Gyr lifetime.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: The transit-depth precisions achieved by each independent reduction compared to the predicted values from PandExo simulations for each individual visit and for the combined spectra from each reduction.
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: Comparison of the ExoTiC-MIRI (pink) reduction of the MIRI/LRS commissioning data compared to the CASCADE (blue) and Eureka! (green) reductions from J. Bouwman et al. (2023).