adsabs/AstroCLIMB huggingface dataset:
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Slices of telluric CCF (cross-correlation between the SysRem residual spectra and the telluric model) at the expected location of the planet, K p = 164.27 km s−1 (see Section 4), for different SysRem iterations. The gray area highlights the region within S/N ± 3. SysRem #0 means before applying SysRem. The blue curves are all CCF values after applying SysRem (from SysRem #1 to #10).
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Top: the in-transit section of the left panel of Figure 7 for SysRem #1. The white solid line is the expected planetary RV path while the purple solid line is the planetary RV path corresponding to the detected K p and V rest values from Figure 9. The red area is the in-trail distribution and spans ∼±3 pixels (with 1.3 km s−1 sampling) from the expected planetary path (red solid line). The green area is the out-trail distribution. The area between the in-trail and out-trail that spans 5 km s−1 (from the black dashed lines to the blue dashed lines) is excluded from the analysis. Bottom: the histogram for both the in-trail and out-trail distributions. The vertical dashed lines show the mean of each distribution, calculated by fitting a Gaussian to the histogram and subsequently computing its mean, with colors shown by the legend.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Slices of S/N of the POKAZATEL model of H2O at K p = 164.27 km s−1 from the first half (blue curve) and second half (red curve) of the transit. S/N for the second half without frame number #44 is also shown (green curve). The vertical black dashed line corresponds to V rest retrieved from Figure 9 (V rest = 2.5 km s−1). The gray area highlights regions within S/N = ±3.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: S/N map for the POKAZATEL model. The y-axis is the semiamplitude radial velocity while the x-axis is the systemic velocity measured in the planetary rest frame V rest. The white dashed lines point to the maximum peak in the map, marked by the red cross symbol, the significance of which is indicated at the lower left corner of the map, along with the corresponding SysRem iteration The blue plus symbol marks the expected K p and V rest location of the planet.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Left panels show the chemical equilibrium model spectra generated using petitRADTRANS in planetary radius. The models shown are already broadened by the FWHM of CARMENES. The right panel shows the temperature and chemical equilibrium abundance profiles for H2O (solar C/O) and HCN (C/O = 1.2), computed using FastChem, which are used to generate the spectra in the left panels.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Welch-t σ evolution with the in-trail width. The vertical dashed line marks the location of maximum significance. Significance is evaluated at fixed values of K p and V rest taken from the location of the detected signal in the S/N map of POKAZATEL in Figure 9.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Slices of the S/N map at K p = 164.27 km s−1 for the upper panel and K p = −164.27 km s−1 for the lower panels for various injection tests with injected models shown by the legend. All injected water (POKAZATEL and HITEMP) models are injected at the detected V rest. Regions within S/N = ±3 are marked in gray. Black vertical dashed lines mark the V rest used for models in each panel.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Corner plot of the normalized likelihood ﹩{ \mathcal L }﹩ values for the fit parameters. Vertical dashed lines in the marginalized distribution panels correspond to the 16th, 50th, and 84th percentiles from left to right.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Marginalized posteriors for V rest (left), K p (middle), and α (right) using the H2O POKAZATEL model. The vertical dashed lines mark the median values that are indicated in the legend alongside the ±1σ standard deviation. For each parameter, three posteriors are given, where black indicates the case where we include frame #44 and red indicates the case where we exclude it.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: S/N evolution with η and SysRem iteration. S/N is taken at (K p, V rest) ∼ (160.0, 2.5) km s−1, which are the values retrieved from the S/N map in Figure 9.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The final spectra for each of our four test planets, with both linear detrending (with two PCs as regressors) and GP detrending (with five PCs as regressors). Note that the y-axis scale of WASP-69 b has been restricted to hide some large outliers, due to the large systematics present in the G750L data (clearly seen in the white-light curves; see Figure 3), but the full scale can be seen in Figure 23 in Appendix C.1. Also shown are past results from the literature for comparison: Wakeford et al. (2018) for WASP-39 b, Evans et al. (2018) for WASP-121 b, Estrela et al. (2021) for WASP-69 b, and Alderson et al. (2022) for WASP-17 b. Note that our results show close agreement with those for WASP-39 b, WASP-121 b (after offset; see Figure 10), and WASP-17 b but significant difference for WASP-69 b.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Our final best spectrum for each of our four test planets, shown along with models from Goyal et al. (2019). Note that, due to the general lack of features in this wavelength range, there are multiple models equally consistent with the data, but one model is shown as demonstrative of such a family of models. For WASP-39 b, WASP-121 b, and WASP-17 b, due to the similarities in our final spectra, we refer the reader to the planet-specific papers and the modeling results therein for an in-depth discussion of the specific properties of the planets’ atmospheres. For WASP-69 b, for which our final spectrum differs significantly from that in past results, we present our best-fit models specifically: a potential haze scattering slope forward model (Goyal et al. 2019) and stellar contamination model. It is impossible to confidently distinguish between these models with the quality of the data. The points in the shaded region are affected by large systematics (see Figure 5) and so are left out of the analysis.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The white-light-curve fits for each of our four planets: WASP-39 b, WASP-121 b, WASP-69 b, and WASP-17 b (top to bottom). From left to right: joint linear detrending G430L, joint GP detrending G430L, linear detrending G750L, and GP detrending G750L. All linear detrending is done with two PCs as regressors, and all GP detrending is done with five PCs as regressors. All plots of the same planet are shown on a common y-axis scale.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The spectrum of the WASP-17 b fit using different detrending methods, each with its average R  p /R  s  removed. It can be seen that the silver and red points, corresponding to linear detrending fits with 10 detrending vectors (either PCs or original vectors, respectively), have a larger variance than the rest of the points, which encompass the best-fit linear and GP detrending models (two and five PCs, respectively), as well as the two GP fits using those same 10 detrending vectors. To see these spectra in context with the rest of the tested methods, see Figure 12.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The spectroscopic light-curve fits for WASP-69 b, from G430L (two transits, phased together). The left panel shows the linear detrending using two PCs as regressors, and the right panel shows the GP detrending using five PCs as regressors. The raw data points are shown as a more transparent color version of the final detrended points for reference, and each wavelength bin is offset vertically. The beginning and end values of the wavelengths included in the bin are shown above the pretransit baseline of each spectroscopic light curve (in μm).
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The difference in R  p /R  s  between the individually fit WASP-17 b G430L transits, plotted with the error bars from the corresponding method’s joint-fit error. If the joint fit is correctly estimating the scatter in predicted outcomes given the state of the data, the errors should encompass the spread in values from each transit’s individual fit and be consistent with zero. It can be seen that, besides the first spectral point, the GP’s errors are consistent with zero throughout the spectrum but that there are multiple linear points that are inconsistent with zero. This suggests caution for using linear detrending methods to estimate the error with problematic data sets.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The extracted spectra from G430L transit 1 (red), G430L transit 2 (blue, offset vertically for comparison), and G750L (green) for WASP-39 b (top left), WASP-121 b (top right), WASP-69 b (bottom left), and WASP-17 b (bottom right). Each panel shows the entire time series of extracted spectra stacked on top of each other.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 4, but for G750L (single transit).
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: An example of our joint fit for WASP-69 b. All the priors used for this fit and their corresponding best-fit values are given in Table 2.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: A refit of the G750L spectrum of WASP-121 b, with the limb darkening fixed to that fit for in Evans et al. (2018), compared to the results from said work. Note that the absolute R  p /R  s  has been removed from all data sets, to account for any vertical offset due to differences in detrending method or system parameters. The difference in the spectra seen in Figure 6 has mostly disappeared after changing the limb darkening, showing that the choice of whether to fix to theory or fit to data can have an effect on the end result when analyzing HST data.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The combined STIS G430L and G750L spectrum of WASP-39 b (top left), WASP-121 b (top right), WASP-69 b (bottom left), and WASP-17 b (bottom right). Each color (common between planets) corresponds to a different systematics detrending technique, using either linear or GP methods and either between 1 and 10 PCs or for the 10 initial input vectors.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 11, but each spectrum has its average R  p /R  s  subtracted from it to remove any absolute R  p /R  s  offsets. This compares spectral shape rather than true R  p /R  s .
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The normalized 0−1 ln Z for each set of regressors from 1 to 10 PCs, and also for all original vectors, for G430L GP detrending. Each color corresponds to a wavelength bin. The true Δ ln Z this is detailing is given in the legend. The more bunched toward 1 a regressor set is, the better overall fit it is across all wavelength bins.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 13, but for G750L linear detrending.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 13, but for G430L linear detrending.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 13, but for G750L GP detrending.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 4, but for WASP-39 b.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 5, but for WASP-39 b.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The transit depth with the average transit depth removed for both of our analyses (GP and linear) and the analysis from Estrela et al. (2021). In the left panel the average transit depth has been removed on each instrument separately, whereas in the right panel the overall average transit depth has been removed for each reduction. In both cases, the leftover spectral shape is distinctly different within the error bars, meaning that there is more than just a vertical offset between reductions.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as the bottom left panel of Figure 6, but without a restricted y-axis scale, showing the full spectrum of WASP-69 b.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: The result of changing the aperture used for spectral extraction on the final transmission spectrum. It can be seen that the resulting spectra are broadly consistent with each other but that the median error bar (given in the legend) do change a significant amount.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 4, but for WASP-121 b.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 5, but for WASP-121 b.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 5, but for WASP-17 b.
Paper: HST SHEL: Enabling Comparative Exoplanetology with HST/STIS
Authors: Natalie H. Allen, David K. Sing, Néstor Espinoza, Richard O'Steen, Nikolay K. Nikolov, Zafar Rustamkulov, Thomas M. Evans-Soma, Lakeisha M. Ramos Rosado, Munazza K. Alam, Mercedes López-Morales, Kevin B. Stevenson, Hannah R. Wakeford, Erin M. May, Rafael Brahm, Marcelo Tala Pinto
Figure caption: Same as Figure 4, but for WASP-17 b.
Paper: Different Planetary Eccentricity-period (PEP) Distributions of Small and Giant Planets
Authors: Dolev Bashi, Tsevi Mazeh, Simchon Faigler
Figure caption: Separate PEP diagrams for the small and giant planets. Triangles and squares represent planets discovered by the transit and RV methods, respectively. Red open circles mark planets in known multiplanet systems. The open triangles in the small-planet diagram present orbits from the study of Feng et al. (2022), which did not publish some of their orbital elements, nor the RV measurements. The red dashed line in the giant-planet diagram marks our upper-envelope best-fit model, marked by a vertical dotted line, based on planets with an orbital period shorter than 100 days. The red area marks the transition region of ±δ width along the envelope (see text). Gray dashed curve and the corresponding gray region mark the expected constant angular momentum evolutionary track, given a final orbital period of 2 ≤ P final < 5 days.