adsabs/AstroCLIMB huggingface dataset:
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Photometric MDFs for the NE shelf (red histogram, left panel), W shelf (magenta histogram, middle panel), and SE shelf (blue histogram, right panel) compared to the GSS (green hatched histograms) and the smooth halo (gray filled histograms). Each stream/shelf sample consists of stars classified as M31 members (Section 3.1, 5.1) that probably belong to a given tidal feature (p sub > 0.5;  Section 3.2.2, 5.2). The smooth halo sample is made from M31 members in SPLASH halo fields spanning 12–33 kpc (Gilbert et al. 2012) with p sub < 0.2. We determined [Fe/H]phot for the smooth halo, GSS, W shelf, and SE shelf homogeneously with the NE shelf (Section 2.2). The median [Fe/H]phot for each sample is shown as arrows (Table 5). The NE shelf has the same metallicity as the GSS and the SE shelf and is distinct from the smooth halo. The median [Fe/H]phot of the W shelf MDF is lower owing to contamination by metal-poor halo stars but shares a similar MDF peak.
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Same as Figure 5, except for the W shelf. We excluded the innermost spectroscopic field targeting the W shelf (Figure 1) from the analysis in Section 5 owing to contamination from NGC 205 (F12). We separated the W shelf fields into radial zones similar to those utilized by F12 for the velocity distribution modeling (Section 3.2).
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: The four Spitzer 3.6 and 4.5 μm secondary eclipse light curves of WASP-29b (black points), binned in intervals of 10 minutes, with the best-fit eclipse model plotted in red. The corresponding residuals are shown beneath earch light curve. Only the second observation at 4.5 μm shows a robust eclipse detection.
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: Corner plot from the preferred PLATON atmospheric retrieval of the WASP-80b transmission spectrum.
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: A full compilation of systematics-corrected spectroscopic light curves (colored points) derived from the STIS G430L and STIS G750L observations of WASP-29b transits. The black curves show the best-fit transit models, while the corresponding residuals are plotted in the right panels. The light curves from the two STIS G430L visits are shown separately.
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: Corner plot from the preferred PLATON atmospheric retrieval of the WASP-29b transmission spectrum, where the two Spitzer transit depths were excluded.
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: Similar to Figure 6, but for the six WASP-80b secondary eclipse observations.
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: Same as Figure A1, but for the WFC3 G141 observation of WASP-80b.
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: Same as Figure A1, but for the WFC3 G141 observation of WASP-29b.
Paper: The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b
Authors: Ian Wong, Yayaati Chachan, Heather A. Knutson, Gregory W. Henry, Danica Adams, Tiffany Kataria, Björn Benneke, Peter Gao, Drake Deming, Mercedes López-Morales, David K. Sing, Munazza K. Alam, Gilda E. Ballester, Joanna K. Barstow, Lars A. Buchhave, Leonardo A. dos Santos, Guangwei Fu, Antonio García Muñoz, Ryan J. MacDonald, Thomas Mikal-Evans, Jorge Sanz-Forcada, Hannah R. Wakeford
Figure caption: Same as Figure A1, but for the STIS observations of WASP-80b.
Paper: Speckle Interferometry at SOAR in 2021
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Dependence of the rms residuals of calibrators on the separation. Plus signs and squares correspond to radial Δρ and tangential ρΔθ residuals, respectively, and the dashed line is a linear fit to both.
Paper: Speckle Interferometry at SOAR in 2021
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Dependence of the difference between SOAR and Gaia positions in separation (top) and angle (bottom) on the separation. In the top plot, the dashed line is a linear fit and the solid line is a scale factor.
Paper: Reduced Variations in Earth’s and Mars’ Orbital Inclination and Earth’s Obliquity from 58 to 48 Myr ago due to Solar System Chaos
Authors: Richard E. Zeebe
Figure caption: Time-series analysis of ﹩q=\sin (I/2)\cos {\rm{\Omega }}﹩ for Earth and Mars (see text) to extract solar system s modes from ZB18a. Int = Interval, ﹩{ \mathcal F }﹩ = Fast-Fourier Transform (FFT). The arrows in (d) indicate the nodes (reduced amplitude; see Figure 4). The vertical dashed lines in (e)–(h) indicate the frequencies of the s modes (see Zeebe 2017).
Paper: Reduced Variations in Earth’s and Mars’ Orbital Inclination and Earth’s Obliquity from 58 to 48 Myr ago due to Solar System Chaos
Authors: Richard E. Zeebe
Figure caption: Time-series analysis of ﹩k=e\cos (\varpi )﹩ for Earth and Mars (see text) to extract solar system g modes from ZB18a. Int=Interval, ﹩{ \mathcal F }﹩=Fast-Fourier Transform (FFT). The vertical dashed lines in (e)–(h) indicate the frequencies of the g modes (see Zeebe 2017).
Paper: Reduced Variations in Earth’s and Mars’ Orbital Inclination and Earth’s Obliquity from 58 to 48 Myr ago due to Solar System Chaos
Authors: Richard E. Zeebe
Figure caption: Mars’ obliquity calculated using our spin vector integration with orbital solution ZB18a and two different values for the precession constant (see Equation (7)). (a) Ψ0M = 7.″6083 + 0.″0021 yr−1 and (b) Ψ0M = 7.″6083 − 0.″0021 yr−1 (Konopliv et al. 2016). Arrows indicate nodes in obliquity (reduced variation) with a period of ∼2.4 Myr that are absent from ∼58 to 48 Ma.
Paper: Reduced Variations in Earth’s and Mars’ Orbital Inclination and Earth’s Obliquity from 58 to 48 Myr ago due to Solar System Chaos
Authors: Richard E. Zeebe
Figure caption: Reconstruction of Earth’s and Mars’ q using only key eigenmodes (see Equation (17)). The reconstructed time series correspond to Figure 6a–d from the full solar system integration (solution ZB18a).
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: Visualization of an SGL probe opposite α Cen. The Sun is at the origin in our coordinate system, and Earth’s orbit lies on the xy plane. The probe is indicated in green and its outgoing beams for various dish sizes in gray (see Section 1.2).
Paper: Constraining the Planet Occurrence Rate around Halo Stars of Potentially Extragalactic Origin
Authors: Stephanie Yoshida, Samuel Grunblatt, Adrian M. Price-Whelan
Figure caption: Left: a color–magnitude diagram showing the absolute Gaia m  G  magnitudes and B p -R p  colors of stars in our sample. Our color and magnitude cuts correspond to the dashed lines. Further cuts were made based on stellar radius to focus on stars where transits are detectable, indicated by the red points. Right: a Toomre diagram of red-giant stars in the Milky Way’s halo and thick disk as a function of rotational and vertical velocity. The selection was made following the cuts in Grunblatt et al. (2021). Stars included in our injection-recovery test are shown as red points.
Paper: Constraining the Planet Occurrence Rate around Halo Stars of Potentially Extragalactic Origin
Authors: Stephanie Yoshida, Samuel Grunblatt, Adrian M. Price-Whelan
Figure caption: Left: the transit signals injected into the observed halo stars as a period by radius plot. The blue indicates the targets recovered and the orange indicates the targets that were not successfully recovered. The gap down the middle is from the masked period range of 12.5–17 days. Right: the recovery rate of the transits as a function of planet period and radius. Completeness is highest for largest and shortest-period planets.
Paper: Constraining the Planet Occurrence Rate around Halo Stars of Potentially Extragalactic Origin
Authors: Stephanie Yoshida, Samuel Grunblatt, Adrian M. Price-Whelan
Figure caption: Left: TIC455692967's light curve prior to the injection-recovery test. The target’s flux is consistent throughout observation showing no indication of planetary transits. Right: TIC455692967's light curve following the injection of a 0.62 R  J  transit signal with a period of 6.26 days. The injected planet transit can be seen at a phase of 1 day in this figure indicated by the red arrow.
Paper: Constraining the Planet Occurrence Rate around Halo Stars of Potentially Extragalactic Origin
Authors: Stephanie Yoshida, Samuel Grunblatt, Adrian M. Price-Whelan
Figure caption: Far left: the recovery rate of the transits as a function of orbital period. Sensitivity to planet detection decreases as period increases. Left: the recovery rate of the transits as a function of planet radii. Sensitivity to planet detection increases as the planet radius increases. Right: the recovery rate of the transits as a function of stellar radius. The sensitivity has a negative correlation across all stellar radii sampled. Far right: the number of stars per stellar radius–there is an excess of large stars in the sample.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Left panels: estimated 6 GHz luminosity over decades-long timescales of all QSOs considered in our time-domain analysis. The top row shows the curves of the 14 RLQs examined, the middle row shows the 27 RIQs, and the bottom row shows the 29 RQQs. The left column shows the resultant curves assuming a steep spectral index (α = −0.7) in converting FIRST and VLASS flux densities to our 6 GHz observing frequency, while the right column shows the resultant curves assuming a flat spectral index (α = 0.0). FIRST observations span 1993–2004; all 2010–2011 points reflect data from Kellermann et al. (2016); for the RQQs, the 2019 data points represent flux densities from this paper; the 2017–2019 data points for the RIQs and RLQs reflect data from preliminary “Quick Look” images from Epoch 1 of VLASS, and the 2019 data points for the RQQs are from the A-configuration observations in this paper. Right panels: preferred results selected on their best-fit spectral index from the χ 2 analysis. Sources not well suited by either choice of spectral index are shown with thick lines (two in panel (c) and three in panel (e)) and discussed further in Section 5.4.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Spectral indices between 3 and 6 GHz compared to spectral indices between 1.4 and 3 GHz for the RL, RI, and RQ classes of QSOs. The dashed line illustrates where the two spectral indices are equal, i.e., a constant power law across 1.4–6 GHz. Data at 6 GHz are from targeted VLA observations presented in Kimball et al. (2011b), 3 GHz data are from VLASS, and 1.4 GHz data are from FIRST. Several RQ and RI sources are not detected in FIRST or VLASS, as shown by the lower/upper-limit symbols (rightward-pointing for FIRST nondetections; upward- and leftward-pointing for VLASS nondetections). Two RQQs (J1425+0803 and J1617+0638) are omitted from this figure, as they are nondetections in both FIRST and VLASS, so we cannot obtain meaningful estimates of spectral indices at this frequency range. Median error bars for each radio-loudness class are shown; the large errors primarily result from the high flux density uncertainties in the early Quick Look images from VLASS (see discussion in Section 5.1 and Lacy et al. 2020). Star symbols denote three RIQs and two RQQs that are highlighted in the discussion of Section 5.4.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Top: distribution of ﹩\mathrm{log}({S}_{{\rm{A}}}/{S}_{{\rm{C}}}﹩) (see text) for the RQQ sample. Magenta dotted lines mark ±1σ offsets from 0 (where σ is the standard deviation of the sigma-clipped main distribution). As discussed in Section 4.3, the excess of sources < − σ compared to those > + σ suggests the presence of radio emission below the surface brightness sensitivity of our follow-up observations. Bottom: marginal distributions of ﹩\mathrm{log}({S}_{{\rm{A}}}/{S}_{{\rm{C}}})﹩ for sources that appear unresolved in our 0.″33 scale images (solid blue; median ﹩\mathrm{log}({S}_{{\rm{A}}}/{S}_{{\rm{C}}})\approx -0.15﹩) and those that have been resolved (dashed orange; median ﹩\mathrm{log}({S}_{{\rm{A}}}/{S}_{{\rm{C}}})\approx 0.0043﹩), plotted as the fractional total from each class. Median error bars of ﹩\mathrm{log}({S}_{{\rm{A}}}/{S}_{{\rm{C}}})﹩ for each class of object are shown for reference.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: The two outlier RQ sources discussed in Section 5.4. The first column shows the FIRST image (Becker et al. 1995; Helfand et al. 2015); the second column shows the source in the VLA’s C configuration (Kimball et al. 2011b; Kellermann et al. 2016); the third column displays the source’s “Quick Look” image from the VLASS (Lacy et al. 2020); the fourth column contains the A-configuration images from the observations presented in this paper. The resolution element (synthesized beam) is shown in the lower left corner for each image. Note that images in the different columns were observed at different times and frequencies. The color bar maps the source flux density at 6 GHz for each image assuming α = −0.7; the choice of spectral index is discussed in the text in Section 5.2–5.4. See panel (a) of Table 4 for a summary of each of the contributing surveys.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption:                          ﹩\mathrm{Log}({S}_{{\rm{A}}}/{S}_{{\rm{C}}})﹩ as a function of S C. The lower left quadrant exclusively contains unresolved RQQs, consistent with an interpretation that these sources have subgalactic radio emission that is too faint to be detected in our A-configuration observations (see text of Section 4.3). Marginal distributions for unresolved and resolved sources are shown on the top and right axes (blue solid: unresolved; orange dashed: resolved; black dotted: nondetections).
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: The five sources in this figure are those whose observations over multiple epochs clearly suggest that they are variable rather than having spectral index values of α ∼ −0.7, 0 that are suitable for the bulk of the QSO population analyzed in this section. Instead, we solved for α as a free parameter while attempting to fit the light curves to a constant power law. The results shown here correspond to the “best” α value for each source; see text of Section 5.4.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: The three RIQs discussed in Section 5.4. The panel layout follows that of the first three columns of Figure 12. All images are on the same color scale. Assumption of spectral index α = −0.7 or 0 yields a conclusion that all three sources increased and then decreased in flux density over a similar timescale; we suggest that the likelier explanation is that these QSOs have radio spectra peaked at >3 GHz.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: The final transmission spectra of WASP-96b, which include the combined FORS2 and IMACS data (purple) and the G102 (green) and G141 (pink) data, both from Yip et al. (2021). Best-fit PLATON retrieval models that include stellar activity (gray), scatters (gold), and a clear atmosphere (red) are also plotted, with the 1σ confidence interval shaded in the same colors. Because the optical offsets were slightly different for each of the three models, what is shown here is the mean depth where the true offsets were ﹩{0.00476}_{-.00039}^{+.00040}﹩, ﹩{0.00414}_{-.00035}^{+.00036}﹩, and ﹩{0.00467}_{-.00034}^{+.00039}﹩ for the activity, scatters, and clear models, respectively. As can be seen in Table 7, the model with the highest evidence is one with scatters; however, no model has sufficiently strong evidence to favor it over another.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: The H2O-J indices (color-coded squares) defined by Stevenson (2016) relative to the planetary surface gravities and equilibrium temperatures. Other planets with surface gravities and effective temperatures obtained from  TEPCat  are plotted as green circles for context. We also plot the dividing line in T  equ -log10(g) phase space that Stevenson (2016) proposed delineates between cloudy and clear planets. Those authors say H2O-J indices greater than 2 indicate atmospheres that are likely completely clear, and indices less than 1 are greatly obscured by clouds. The only planets with indices greater than 2 are HAT-P-11b (2.5 ± 0.5), WASP-96 (2.4 ± 0.7), and WASP-17b (2.3 ± 0.9). WASP-96 (star) is shown to be one of the clearest observed planets, both through this index and in the optical, yet it sits very close to the dividing line. The data in this table were produced in Alam et al. (2020).
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Same as Figure 9, but with Exoretrievals. In this figure, the optical (combined FORS2 and IMACS), G102, and G141 observations are cyan, white, and red, respectively. Again, the evidence of each plotted model (activity—gray, scatters—green, and clear—purple) are indistinguishable from each other, but the clear atmosphere has the highest evidence. The offset with each fit were 0.00554 ± .00031, 0.00558 ± .00034, and ﹩{0.00547}_{-.00032}^{+.00031}﹩ for the activity, scatters, and clear models, respectively.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Observed mass–metallicity trend for transiting exoplanets. The bulk of the data were acquired from Wakeford & Dalba (2020)                      , but we added HAT-P-32b (Alam et al. 2020), WASP-17b (PLATON run with data from Sing et al. 2016), WASP-62b (using Na abundance from Alam et al. (2021) as a proxy), WASP-94b (Ahrer et al. 2022), and WASP-96 (this work, magenta star). The dashed black line corresponds to a linear fit in log–log space to the solar system points (black dots). We highlight the clear planets with magenta, and all other planets are gray.