adsabs/AstroCLIMB huggingface dataset:
Paper: The MKID Pipeline: A Data Reduction and Analysis Pipeline for UVOIR MKID Data
Authors: Sarah Steiger, John I. Bailey, Nicholas Zobrist, Noah Swimmer, Rupert Dodkins, Kristina K. Davis, Benjamin A. Mazin
Figure caption: Left-hand panel: MEC Image of the HIP 109427 system with each dither position color-coded by its order in the sequence. The image of the HIP 109427 (behind a coronagraph), satellite spots, and stellar companion are shown in gray scale to be able to better see the frame boundaries. Right-hand panel: Exposure coverage footprint for the same data set. Here, bright regions have more effective exposure time than darker regions. Current dithering scripts for MEC enforce a rectangular dithering pattern leading to a non-uniform footprint, but future work will optimize this pattern for maximal uniform coverage.
Paper: The MKID Pipeline: A Data Reduction and Analysis Pipeline for UVOIR MKID Data
Authors: Sarah Steiger, John I. Bailey, Nicholas Zobrist, Noah Swimmer, Rupert Dodkins, Kristina K. Davis, Benjamin A. Mazin
Figure caption: Block diagram of the MKID Pipeline depicting implementation details.
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Eccentricity distributions for our suite of simulations. Left panel: cumulative frequency of planet eccentricity for pre- and postinstability planets for the high-mass sample (runs 1–8) and the low-mass sample (run 9). Thicker gray lines represent Rayleigh distributions with scale factors 0.02 and 0.05. Right panel: median system eccentricity as a function of multiplicity, with the same colors as the left panel. Multiplicities are shifted slightly for clarity. Red crosses mark the power law (Equation (51)) from He et al. (2020).
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Evolution of orbital elements during a typical simulation of capture into a resonant chain. Here, the planet parameters are those of run 1 (see Table 2). Migration and eccentricity damping proceeded from t = 0 to t = 100 kyr, at which point t  m  and t  e  increase exponentially, representing gas disk removal. At t =110 kyr, both timescales are set to infinity.
Paper: New CCD Astrometric Observations of Himalia Using Gaia DR2 in 2015–2021
Authors: Y. J. Shang, Q. Y. Peng, Z. J. Zheng, A. Vienne, B. F. Guo, F. R. Lin, Y. Chen
Figure caption: (O − C) residuals of the positional offsets with regard to JPL ephemeris (JUP344+DE441) for Himalia taken by different telescopes during 2015 and 2021. The dark squares are for observations with 1 m telescope from Kunming Station, the red ones for 2.4 m from Yaoan Station and the blue ones for 0.8 m from Lijiang Station in each direction. And the two red dash lines represent mean (O − C)s in each panel.
Paper: New CCD Astrometric Observations of Himalia Using Gaia DR2 in 2015–2021
Authors: Y. J. Shang, Q. Y. Peng, Z. J. Zheng, A. Vienne, B. F. Guo, F. R. Lin, Y. Chen
Figure caption: Typical GD patterns derived from a Johnson I-type filter from observations of M35 taken with 1 m telescope at Kunming Station and NGC6633 taken with 2.4 m telescope at Lijiang Station on two nights. At the top of each panel, the observational date, the median and maximum GD values are listed in units of pixels. A factor of 200 is used to exaggerate the magnitude of each GD vector.
Paper: New CCD Astrometric Observations of Himalia Using Gaia DR2 in 2015–2021
Authors: Y. J. Shang, Q. Y. Peng, Z. J. Zheng, A. Vienne, B. F. Guo, F. R. Lin, Y. Chen
Figure caption: (O − C) residuals of Himalia with different processing techniques. The left and right panels show the results with regard to JD in R.A. and decl., respectively. The black, red, and blue squares represent (O − C) residuals using classical two-dimension Gaussian-fit, double Gaussian-fit, and ePSF-subtracted techniques, respectively.
Paper: New CCD Astrometric Observations of Himalia Using Gaia DR2 in 2015–2021
Authors: Y. J. Shang, Q. Y. Peng, Z. J. Zheng, A. Vienne, B. F. Guo, F. R. Lin, Y. Chen
Figure caption: (O − C) residuals of Himalia in decl. with respect to R.A. The dark squares represent the (O − C) residuals for IMCCE and the red points for JPL.
Paper: New CCD Astrometric Observations of Himalia Using Gaia DR2 in 2015–2021
Authors: Y. J. Shang, Q. Y. Peng, Z. J. Zheng, A. Vienne, B. F. Guo, F. R. Lin, Y. Chen
Figure caption: Comparison of dispersion of (O − C) residuals of Himalia in decl. with respect to R.A. before and after precision premium (pp).
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: Eccentricity as a function of semimajor axis for confirmed WJ systems. Multiplanet systems with an outer WJ and a smaller, inner companion are shown with blue circles, whereas all other WJs are plotted with gray diamonds. The yellow star denotes TOI-1670 c. Systems with a similar configuration as TOI-1670 all have low eccentricities, suggesting a gentle formation pathway. Planet orbital parameters were assembled from exoplanet.eu (Schneider et al. 2011) and the NASA Exoplanet Archive (Akeson et al. 2013; NASA Exoplanet Archive 2021) as of 2021 June.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Range and distribution of effective temperature (T eff) and surface gravity (﹩\mathrm{log}g﹩) of target exoplanet host stars.
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: Posterior distributions of fitted parameters for TOI-1670 b and c derived from joint global fit of RVs and light curves.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Mean offset between empirically determined LDCs (through TESS transiting exoplanet light curves) and the theoretically derived LDCs when using a quadratic law. The different colors of the bars represent the different methodologies to compute theoretical LDCs, from LDC tables/codes (Section 2.3.1; orange) and SPAM LDCs (described in Section 2.3.2; blue). The x-axis shows the various origins of these theoretical LDCs: Espinoza & Jordán (2015, EJ15) and Claret (2017, C17). The additional suffix for this latter work (q and r) represents two different sets of assumptions used by Claret (2017) to obtain these LDCs (see text for details). The top panel shows the offset for the u 2 coefficient, while the bottom panel shows the offset for the u 1 coefficient of the quadratic law.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: (Left) Phase-folded light curve for the systematics-removed WASP-62b system with data taken by TESS combining the observations of all sectors (top left plot; blue data points) and the residuals from the best-fit model (bottom left plot). The white circles with black error bars are binned data points in 2 minute intervals in this phased light curve. (Right) PSD of the residuals of the best fit, which does not show any significant signal on the frequencies relevant to the transit event. Dashed lines from top to bottom show where 99.9%, 99%, and 90% of the PSD of simulated Gaussian noise with the same properties at those of the error bars on our data falls; the observed PSD of the residuals falling below these lines suggests it is consistent with that of white Gaussian noise.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Transit light curves (top; black data points are original data, white points are binned data, and blue curves are the best-fit light curves) and transit depths (bottom; blue points with error bars) on each sector for one of our best constrained targets in this work: WASP-62b. As can be seen in the bottom plot, the retrieved transit depths are consistent between sectors, and they converge to a value (﹩{{\rm{12,341}}}_{-33}^{+32}﹩ ppm; gray band representing this 68% credibility band) that is in agreement with the literature value (12,210 ± 66 ppm).
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the time of transit center (t  c ) calculated using juliet with its corresponding literature values. The observed values and the values from the literature are on the y- and x-axis, respectively, in the upper panel, while the lower panel shows the residuals between those two values.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the scaled semimajor axis (a/R *) calculated using juliet with its corresponding literature values. The observed values and the values from the literature are on the y- and x-axis, respectively, in the upper panel, while the lower panel shows the residuals between those two values.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Corner plot of various retrieved parameters for the WASP-62b system.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: The LDCs extracted for our best-precision targets (the ones spanning data in multiple sectors) compared to their theoretical predictions (blue for ATLAS models, red for PHOENIX). As can be seen, a clear offset is observed for the u 2 LDC. The bands show the uncertainties in the mean offset, with red and blue representing the PHOENIX and ATLAS models. The method to compute theoretical LDCs is the one from Espinoza & Jordán (2015).
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Temperature variation of offsets in u 1 and u 2 when, theoretically, LDCs are calculated using code provided by Espinoza & Jordán (2015). The dashed–dotted lines show the best-fit model to the residuals.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the planet-to-star radius ratio (R  p /R *) calculated using juliet with its corresponding literature values. The observed values and the values from the literature are on the y- and x-axis, respectively, in the upper panel, while the lower panel shows the residuals between those two values.
Paper: A Census of Stars and Disks in Corona Australis 
Authors: T. L. Esplin, K. L. Luhman
Figure caption: Proper motion offsets vs. parallax for candidate young low-mass stars near Corona Australis from Figure 3 (left). We have applied a GMM to these data, which consists of two clustered components (red circles and blue pluses) and a noise population (black points). The 2σ ellipses for the two model components are shown. The spatial distribution of the members of the components are plotted in the right panel. The large overlap of the two components suggests that they comprise a single non-Gaussian population rather than two distinct populations. Extinction from the Corona Australis cloud is displayed in the diagram on the right (gray scale; Dobashi et al. 2013).
Paper: A Census of Stars and Disks in Corona Australis 
Authors: T. L. Esplin, K. L. Luhman
Figure caption: Proper motions (top two rows) and proper motion offsets (bottom two rows) vs. parallax based on Gaia EDR3 for two samples of candidate members of Corona Australis from Galli et al. (2020). The offsets are computed relative to the proper motions expected for the positions and parallaxes assuming the median space velocity of known members. The contour levels are set at 10%, 50%, and 80% of the maximum densities. The bimodal nature of the candidates in μ  α  is a reflection of projection effects, which are minimized in the proper motion offsets.
Paper: A Census of Stars and Disks in Corona Australis 
Authors: T. L. Esplin, K. L. Luhman
Figure caption:                       ﹩{M}_{{G}_{\mathrm{RP}}}﹩ vs. G BP − G RP for Gaia EDR3 sources near Corona Australis with 5.5 < π < 8.5 mas. The single star sequence of the Tuc-Hor association is indicated (45 Myr; Bell et al. 2015) by the solid line. The spectral types that correspond to these colors for young stars are marked (Luhman 2021a).
Paper: A Census of Stars and Disks in Corona Australis 
Authors: T. L. Esplin, K. L. Luhman
Figure caption: Space velocities for two samples of candidate members of Corona Australis from Galli et al. (2020) that have measurements of parallaxes and radial velocities.
Paper: A Census of Stars and Disks in Corona Australis 
Authors: T. L. Esplin, K. L. Luhman
Figure caption: Spatial distribution of the adopted members of Corona Australis (Table 1).
Paper: Two Massive Jupiters in Eccentric Orbits from the TESS Full-frame Images
Authors: Mma Ikwut-Ukwa, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Asma Ali, Katya Bunten, B. Scott Gaudi, David W. Latham, Steve B. Howell, Chelsea X. Huang, Allyson Bieryla, Karen A. Collins, Theron W. Carmichael, Markus Rabus, Jason D. Eastman, Kevin I. Collins, Thiam-Guan Tan, Richard P. Schwarz, Gordon Myers, Chris Stockdale, John F. Kielkopf, Don J. Radford, Ryan J. Oelkers, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Jennifer Burt, R. Paul Butler, Michael L. Calkins, Jeffrey D. Crane, Crystal L. Gnilka, Gilbert A. Esquerdo, William Fong, Laura Kreidberg, Jessica Mink, David R. Rodriguez, Joshua E. Schlieder, Stephen Shectman, Avi Shporer, Johanna Teske, Eric B. Ting, Jesus Noel Villaseñor, Daniel A. Yahalomi
Figure caption: The (left) Speckle interferometric observations for TOI-558 and TOI-559 of the two targets from the Southern Astrophysical Research Telescope (SOAR). The autocorrelation function is shown inset the contrast curve from SOAR. The (right) Gemini South Zorro and Gemini North ‘Alopeke speckle imaging 5σ contrast curves are shown along with the reconstructed images (embedded) of TOI-558 and TOI-559.
Paper: Two Massive Jupiters in Eccentric Orbits from the TESS Full-frame Images
Authors: Mma Ikwut-Ukwa, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Asma Ali, Katya Bunten, B. Scott Gaudi, David W. Latham, Steve B. Howell, Chelsea X. Huang, Allyson Bieryla, Karen A. Collins, Theron W. Carmichael, Markus Rabus, Jason D. Eastman, Kevin I. Collins, Thiam-Guan Tan, Richard P. Schwarz, Gordon Myers, Chris Stockdale, John F. Kielkopf, Don J. Radford, Ryan J. Oelkers, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Jennifer Burt, R. Paul Butler, Michael L. Calkins, Jeffrey D. Crane, Crystal L. Gnilka, Gilbert A. Esquerdo, William Fong, Laura Kreidberg, Jessica Mink, David R. Rodriguez, Joshua E. Schlieder, Stephen Shectman, Avi Shporer, Johanna Teske, Eric B. Ting, Jesus Noel Villaseñor, Daniel A. Yahalomi
Figure caption: The two-sample Kolmogorov–Smirnov (K–S) and Anderson–Darling (A–D) tests applied to the short-period (P < 10 days) giant planet (M  p  > 0.4 M J) population split at orbital periods ranging from 1 to 9 days. The x-axis is the period at which the population is split into two samples, and the y-axis is the resulting p-value. Tidal forces influence the distribution at short periods, possibly shaping the broad minimum between ∼1.5 and 4 days, while the minimum at ∼9 days is likely due to the small sample size at longer periods. The remaining minimum at ∼5.3 days has no obvious explanation, not showing significant dependence on the lower mass limit chosen for the sample, and could indicate a true break between two distributions.
Paper: Two Massive Jupiters in Eccentric Orbits from the TESS Full-frame Images
Authors: Mma Ikwut-Ukwa, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Asma Ali, Katya Bunten, B. Scott Gaudi, David W. Latham, Steve B. Howell, Chelsea X. Huang, Allyson Bieryla, Karen A. Collins, Theron W. Carmichael, Markus Rabus, Jason D. Eastman, Kevin I. Collins, Thiam-Guan Tan, Richard P. Schwarz, Gordon Myers, Chris Stockdale, John F. Kielkopf, Don J. Radford, Ryan J. Oelkers, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Jennifer Burt, R. Paul Butler, Michael L. Calkins, Jeffrey D. Crane, Crystal L. Gnilka, Gilbert A. Esquerdo, William Fong, Laura Kreidberg, Jessica Mink, David R. Rodriguez, Joshua E. Schlieder, Stephen Shectman, Avi Shporer, Johanna Teske, Eric B. Ting, Jesus Noel Villaseñor, Daniel A. Yahalomi
Figure caption: (Top) The radial velocity observations over time for (left) TOI-558 b from PFS and (right) TOI-559 b from CHIRON. The RVs phase-folded to the best-fit periods are shown above. The EXOFASTv2 model fit is shown in red.
Paper: Two Massive Jupiters in Eccentric Orbits from the TESS Full-frame Images
Authors: Mma Ikwut-Ukwa, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Asma Ali, Katya Bunten, B. Scott Gaudi, David W. Latham, Steve B. Howell, Chelsea X. Huang, Allyson Bieryla, Karen A. Collins, Theron W. Carmichael, Markus Rabus, Jason D. Eastman, Kevin I. Collins, Thiam-Guan Tan, Richard P. Schwarz, Gordon Myers, Chris Stockdale, John F. Kielkopf, Don J. Radford, Ryan J. Oelkers, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Jennifer Burt, R. Paul Butler, Michael L. Calkins, Jeffrey D. Crane, Crystal L. Gnilka, Gilbert A. Esquerdo, William Fong, Laura Kreidberg, Jessica Mink, David R. Rodriguez, Joshua E. Schlieder, Stephen Shectman, Avi Shporer, Johanna Teske, Eric B. Ting, Jesus Noel Villaseñor, Daniel A. Yahalomi
Figure caption: The mass distributions (solid) and cumulative mass distributions (dashed) of all known hot Jupiters with measured masses >0.4  M J, split at the position of the K–S p-value valley from Figure 6 (P ≈ 5.2 days) into two samples. We include 311 planets with periods less than ∼5.2 days and 42 with periods between ∼5.2 and 10 days.
Paper: Two Massive Jupiters in Eccentric Orbits from the TESS Full-frame Images
Authors: Mma Ikwut-Ukwa, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Asma Ali, Katya Bunten, B. Scott Gaudi, David W. Latham, Steve B. Howell, Chelsea X. Huang, Allyson Bieryla, Karen A. Collins, Theron W. Carmichael, Markus Rabus, Jason D. Eastman, Kevin I. Collins, Thiam-Guan Tan, Richard P. Schwarz, Gordon Myers, Chris Stockdale, John F. Kielkopf, Don J. Radford, Ryan J. Oelkers, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Jennifer Burt, R. Paul Butler, Michael L. Calkins, Jeffrey D. Crane, Crystal L. Gnilka, Gilbert A. Esquerdo, William Fong, Laura Kreidberg, Jessica Mink, David R. Rodriguez, Joshua E. Schlieder, Stephen Shectman, Avi Shporer, Johanna Teske, Eric B. Ting, Jesus Noel Villaseñor, Daniel A. Yahalomi
Figure caption: The phase-folded and detrended transit light curves for (left) TOI-558 and (right) TOI-559 from TESS and the TFOP working group. The solid colored lines correspond to the best-fit model from our global fit (see Section 3).(The data used to create this figure are available.)
Paper: Two Massive Jupiters in Eccentric Orbits from the TESS Full-frame Images
Authors: Mma Ikwut-Ukwa, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Asma Ali, Katya Bunten, B. Scott Gaudi, David W. Latham, Steve B. Howell, Chelsea X. Huang, Allyson Bieryla, Karen A. Collins, Theron W. Carmichael, Markus Rabus, Jason D. Eastman, Kevin I. Collins, Thiam-Guan Tan, Richard P. Schwarz, Gordon Myers, Chris Stockdale, John F. Kielkopf, Don J. Radford, Ryan J. Oelkers, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Jennifer Burt, R. Paul Butler, Michael L. Calkins, Jeffrey D. Crane, Crystal L. Gnilka, Gilbert A. Esquerdo, William Fong, Laura Kreidberg, Jessica Mink, David R. Rodriguez, Joshua E. Schlieder, Stephen Shectman, Avi Shporer, Johanna Teske, Eric B. Ting, Jesus Noel Villaseñor, Daniel A. Yahalomi
Figure caption: The population of transiting giant planets with periods less than 15 days and mass >0.4  M J, shown as a function of orbital period versus planet mass, as of UT 2020 November 1. Color and size indicate 1σ detection of orbital eccentricity; planets shown in gray do not have significant eccentricity.
Paper: Two Massive Jupiters in Eccentric Orbits from the TESS Full-frame Images
Authors: Mma Ikwut-Ukwa, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Asma Ali, Katya Bunten, B. Scott Gaudi, David W. Latham, Steve B. Howell, Chelsea X. Huang, Allyson Bieryla, Karen A. Collins, Theron W. Carmichael, Markus Rabus, Jason D. Eastman, Kevin I. Collins, Thiam-Guan Tan, Richard P. Schwarz, Gordon Myers, Chris Stockdale, John F. Kielkopf, Don J. Radford, Ryan J. Oelkers, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Jennifer Burt, R. Paul Butler, Michael L. Calkins, Jeffrey D. Crane, Crystal L. Gnilka, Gilbert A. Esquerdo, William Fong, Laura Kreidberg, Jessica Mink, David R. Rodriguez, Joshua E. Schlieder, Stephen Shectman, Avi Shporer, Johanna Teske, Eric B. Ting, Jesus Noel Villaseñor, Daniel A. Yahalomi
Figure caption: The full corrected light curves from TESS. The discovery light curves (left) extracted from the full-frame images are at a 30 minute cadence, from Sectors 2 and 3 for TOI-558 and Sector 4 for TOI-559, corrected using the quaternions following the description in Section 2.1. The additional light curves (right) extracted by the SPOC pipeline are at 2 minute cadence from Sectors 29–31 of the first extended mission (see Section 2.1), corrected with the PDC module. These are not the flattened light curves used for the global fitting.