adsabs/AstroCLIMB huggingface dataset:
Paper: Uncertainty of Line-of-sight Velocity Measurements of Faint Stars from Low- and Medium-resolution Optical Spectra
Authors: László Dobos, Alexander S. Szalay, Tamás Budavári, Evan N. Kirby, Robert H. Lupton, Rosemary F. G. Wyse
Figure caption: The dependence of the ratio of Equation (40) of Hatzes & Cochran (1992) to empirical measurements of σ(v los) based on our simulations, plotted as a function of the effective line number per resolution element as defined in Equation (45) for the arm configurations B (blue dots), R (red dots), and MR (black dots). Correcting the formula in Equation (40) using n eff can account for a factor of 10 change in the uncertainty of the line-of-sight velocity as a function of spectral type. The black line is not a fit but rather the function ﹩0.6\cdot {n}_{\mathrm{eff}}^{-3/4}﹩. The outlier point is an M giant, see Section 7.2 for discussion.
Paper: Uncertainty of Line-of-sight Velocity Measurements of Faint Stars from Low- and Medium-resolution Optical Spectra
Authors: László Dobos, Alexander S. Szalay, Tamás Budavári, Evan N. Kirby, Robert H. Lupton, Rosemary F. G. Wyse
Figure caption: Comparison of σ(v los) predictors of Hatzes & Cochran (1992, dashed black line, see Equation (40)) and Bouchy et al. (2001, solid black line, see Equation (41)) compared to our results from repeated simulations (blue lines) for a low-metallicity K giant with T eff = 4000 K. The multiple blue lines indicate different logarithmic binning of Δv los to calculate σ(v los). The red line is a linear fit to the logarithm of the data with a slope of −0.95, very close to the theoretical value of −1.
Paper: Uncertainty of Line-of-sight Velocity Measurements of Faint Stars from Low- and Medium-resolution Optical Spectra
Authors: László Dobos, Alexander S. Szalay, Tamás Budavári, Evan N. Kirby, Robert H. Lupton, Rosemary F. G. Wyse
Figure caption: Dependence of the effective line number N eff on the atmospheric parameters in four different projections, calculated for the MR arm. In this wavelength range, the effective number of lines depends primarily on metallicity and temperature and only secondarily on surface gravity, as it can be seen in the top two panels and and bottom left one, respectively. While the depth of the hydrogen lines grows with temperature in the range we tested, the roughly inverse relation between T eff and N eff suggests that the calcium and iron lines play a more significant role.
Paper: Uncertainty of Line-of-sight Velocity Measurements of Faint Stars from Low- and Medium-resolution Optical Spectra
Authors: László Dobos, Alexander S. Szalay, Tamás Budavári, Evan N. Kirby, Robert H. Lupton, Rosemary F. G. Wyse
Figure caption: The distribution of the correlation coefficient of v los and the atmospheric parameters (left three panels), and the coefficient of multiple correlation (rightmost panel), calculated from the Monte Carlo sampling of all realizations of all spectral types. According to these, the covariance of v los with the template parameters is minimal on average.
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: We show the transmission spectrum for the nominal Eureka! reduction (detailed in Section 3.1) and the ExoTiC-JEDI and Aesop reductions (left to right) compared to the fitting results of the three highest-likelihood nonphysical models. The three highest-likelihood nonphysical models are consistent between reductions. In all panels, the solid colored line indicates the median fit from the samples, the dark shaded region is the 68th percentile region (1σ), and the light shaded region is the 99th percentile region. The Bayes factor, as defined by the difference in evidence, for each of the nonphysical models prefers the step function model in all three reductions.
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: Results from interior structure modeling with smint. Left panel: ﹩{f}_{\mathrm{core}}^{{\prime} }﹩, ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩, T eq, and M  p  for TOI-836c using the model from Aguichine et al. (2021). Middle panel: f env, M  p , age, and S inc for TOI-836c using the model from Lopez & Fortney (2014). Right panel: ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ and M  p  for K2-18b using the model from Zeng et al. (2016).
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: Mass–radius diagram of small planets colored by bulk water mass fraction (left) and bulk H2–He mass fraction (right). We show the sub-Neptunes with JWST observations (TOI-836c, GJ 1214b, and K2-18b) as stars and planets from the NASA Exoplanet Archive with mass errors of <20% and radius errors of <5% as circles. Zeng et al. (2016) curves are used for the Earth-like and 50% liquid water compositions. Aguichine et al. (2021) curves are used for the 50% and 100% steam water composition and are shown for T eq = 600 K and an Earth-like core. Lopez & Fortney (2014) curves are used for the 1%, 2%, and 5% H2–He composition and are shown for T eq = 600 K and an age of 5 Gyr. For each planet, the bulk volatile content (H2O or H2–He) has been determined with the method described in the Appendix.
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: We show the transmission spectrum for each reduction in the top panel and the differences between the reductions (in units of sigma) in the bottom panel. All three of our reductions agree per point, at the ﹩\unicode{x0007E}﹩2σ level or better, with a median difference of 6 ppm.
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: The posteriors for the time (T 0 in minutes from the predicted midtransit time of 59991.7252 BMJD), the a/R *, and the inclination from the fits to our white-light curves of our Eureka! reduction including 13 engineering parameters in our systematic model are shown in colors. The corresponding posteriors from the fits without the engineering parameters are shown in gray and outlined in their respective detector colors. The posteriors for the fits without the engineering parameters are identical to those shown in Figure 2. The T 0 values are more in agreement between NRS1 and NRS2 when we include engineering parameters.
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: We show the transmission spectrum for the nominal Eureka! case (as detailed in Section 3.1) along with four example models depicting 10×, 150×, and 1000× solar metallicity, as well as a 100% H2O model. In the legend, we also show the χ 2/N and the corresponding σ at which the model can be confidently ruled out. In panel (b) we show the full parameter space of opaque pressure level and metallicity. Here the color scale of the heatmap similarly indicates at what σ each model can be confidently ruled out. Ultimately, we are unable to rule out metallicities > 175× solar (log[M/H] > 2.2).
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: Results from our CARMA modeling of TOI-836c. The curves show the cumulative nadir optical depth at a wavelength of 4 μm for different haze production rates and assuming purely reflective haze optical properties (solid lines) and tholin haze optical properties (dashed lines). The vertical dotted line shows which nadir optical depth gives a slant optical depth of 1 for a 100× solar-metallicity atmosphere following Fortney et al. (2005), with a mean molecular weight of 4.25 g mol−1.
Paper: JWST COMPASS: A NIRSpec/G395H Transmission Spectrum of the Sub-Neptune TOI-836c
Authors: Nicole L. Wallack, Natasha E. Batalha, Lili Alderson, Nicholas Scarsdale, Jea I. Adams Redai, Artyom Aguichine, Munazza K. Alam, Peter Gao, Angie Wolfgang, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan
Figure caption: We show the transmission spectrum for the nominal Eureka! case (detailed in Section 3.1) and the spectrum where we utilize a 13-engineering-parameter systematic noise model. We show the differences between the nominal spectrum and the spectrum that included engineering parameters (in units of sigma) in the bottom panel. The two spectra agree per point at the 2.3σ level or better with a median difference of 17 ppm.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Top: normalized TESS photometry for each of our systems, phase-folded to the orbital periods of the planets. Raw TESS photometry is marked by gray points, and binned photometry is marked by blue points. The median of the posterior transit model is shown by the black line. Bottom: residuals between observations and the best-fit transit model.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Top: observations of the RM effect for each of our targets. Data from Keck/HIRES and Keck/KPF are shown as red and blue points, respectively, and the line shows our model fit. Bottom: residuals between observations and the best-fit RM model.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Top: RV measurements for each of our systems, phase-folded to the orbital periods of the planets. Keck/HIRES observations are shown as red points, and Keck/KPF observations are marked by blue points. The black line shows the best-fit orbital model to the system, including the RM signal. Bottom: residuals between observations and the best-fit RV model.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Left column: contrast (in Δmag units) at 0.″2 (solid blue/red circle) and 0.″4 (open blue/red circle) plotted as a function of host star W1/R magnitude for all targets in the sample. The corresponding best-fit lines are plotted as blue/red solid and dashed lines. Negative slopes of the best-fit line indicate decreasing sensitivity for fainter stars. See Section 6.3 for a discussion of the discrepancies in the data with the best-fit line for the brighter targets. Right column: difference in contrast (in Δmag units) at 0.″2 (solid blue/red circle) and 0.″4 (open blue/red circle) achieved by Super-RDI (sRDI) and ADI as a function of host star W1/R magnitude for all targets in the sample. A gray dashed line marks zero difference corresponding to both techniques achieving the same sensitivity level. Super-RDI shows an improvement over ADI for the majority of fainter targets at both separations, while the reverse is true for brighter targets.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: A common proper motion test based on three epochs of relative astrometry between 2MASS J0602-1634 and the candidate companion CC1. The left panels show the predicted relative motion of a stationary background source in separation (top; black solid line) and PA (bottom; black solid line) based on the first epoch of relative astrometry (light purple circles). Gray shaded regions represent 1σ and 2σ uncertainties. The predicted positions at 2017.04 and 2017.85 are plotted as an open square and an open triangle, respectively. The light pink squares and green triangles represent our measurements at the respective epochs. The separation and PA measurements for the 2017.04 and 2017.85 epoch detections are consistent with the predicted background tracks within uncertainties. The right panel shows the same background track comparison but in ΔR.A. and Δdecl. space instead of separation and PA.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Left: 5σ Super-RDI and ADI contrast curves for 2M0602-1634 for each observation epoch. The point-source detection (“CC1”) is marked with a star. Right: final PSF-subtracted images of 2M0602-1634 obtained with Super-RDI and ADI for each observation epoch. North is up and east is to the left. The two images and the color bars are depicted in linear scale in normalized analog to digital units and have been smoothed using a Gaussian kernel with a 1.5 pixel standard deviation (40% of the width of the instrumental PSF) to average out high-frequency noise.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Left: final PSF-subtracted images of LO Peg obtained with Super-RDI. North is up and east is to the left. The image and color bar are depicted in linear scale in normalized analog to digital units and have been smoothed using a Gaussian kernel with a 1.5 pixel standard deviation (40% of the width of the instrumental PSF) to average out high-frequency noise. Right: P.A. of individual frames obtained across the entire observation sequence. Presented as insets are three representative derotated preprocessed frames (north is up and east is to the left) in the sequence showing that the point source in our final PSF-subtracted image rotates across the sequence as expected for a speckle.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Previously known companions detected with Super-RDI in Keck/NIRC2 ﹩L^{\prime} ﹩ observations. The final PSF-subtracted images of 2MASS J0122-2439 (one epoch; left) and 2MASS J2351+3127 (two epochs; right) are presented above. White arrows point to the detected companions. North is up and east is to the left. All three images and the color bars are depicted in linear scale in analog to digital units and have been smoothed using a Gaussian kernel with a 1.5 pixel standard deviation (40% of the width of the instrumental PSF) to average out high-frequency noise.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Left: difference in contrast (units of Δmag) achieved between annular ADI with a rotation gap criterion of 0.1 FWHM (aADI 0.1) and annular ADI with no rotation gap criterion (aADI 0) as a function of separation (units of arcseconds). A black dashed line marks zero difference and corresponds to both strategies achieving the same sensitivity level. Gray curves correspond to individual targets in the sample and the green curve corresponds to the median computed across all targets. Right: same as the left panel but presenting the difference in contrast achieved between full-frame ADI (fADI) and annular ADI (aADI). The best-performing strategy varies depending on the individual target.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Median difference in Super-RDI (sRDI) and ADI contrast (units of Δmag) as a function of separation (units of arcseconds) for observations sorted into four ΔP.A. bins (units of degrees). A horizontal gray dashed line marks zero difference and corresponds to both techniques achieving the same sensitivity level. Positive differences indicate better Super-RDI performance and negative differences indicate better ADI performance. Vertical dashed lines mark the separations at which 1 FWHM rotation is achieved for the median ΔP.A. value of targets in each bin. The step-like feature at ≈0.″9 is discussed in Section 6.1.
Paper: The Components of Cepheid Systems: The FN Vel System 
Authors: Nancy Remage Evans, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Charles Proffitt, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: The Cepheid mass as a function of inclination and the mass of the companion. The lines show the relation for the range of companion masses M 2 in Table 4: 3.89 M ⊙: blue; 4.09 M ⊙: red; 4.31 M ⊙: green. The maximum value of the Cepheid mass M 1 is listed above the curves for the companion masses M 2.
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: The incidence of adjacent pairs near first-order resonances (−0.015 ≤ Δ ≤ 0.03) as a function of planet radii. The boundaries of the radius bins are strategically placed at (1) Earths and sub-Earths (R  p  < 1R ⊕;  25/99; 25.3% ± 4.4%); (2) super-Earths (1R ⊕ ≤ R  p  < 1.5R ⊕;  51/353; 14.4% ± 1.9%); (3) planets in the radius gap identified by B. J. Fulton et al. (2017; 1.5R ⊕ ≤ R  p  < 1.9R ⊕;  32/270; 11.9% ± 2.0%); (4) sub-Neptunes (1.9R ⊕ ≤ R  p  < 2.5R ⊕;  54/376; 14.4% ± 1.8%); (5) Neptunes (2.5R ⊕ ≤ R  p  < 4R ⊕;  72/446; 16.1% ± 1.7%); (6) sub-Saturns (4R ⊕ ≤ R  p  < 8R ⊕;  22/111; 19.8% ± 3.8%); and (7) Jupiters (R  p  ≥ 8R ⊕;  10/64; 15.6% ± 4.5%). Planets within the radius gap have the lowest chance of being near first-order resonances.