adsabs/AstroCLIMB huggingface dataset:
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Histogram of diagnostic statistics (standard deviation, minimum, Kolmogorov–Smirnov statistic, and scintillation timescale fit) of detected hits and events throughout all GC and GP observations.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Best candidates from the direction filter, which passed initial manual inspection.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: The yellow scatter plot in the background shows all the Gaia DR3 optical sources within 500 pc. The foreground scatter plot is for 3 GHz sources in our total sample. The three categories and stars with high proper motion (PM > 0.″5 yr−1) are shown with different markers. The black line corresponds to a fit for the MS sources in the CMD (Equation (1)). The blue lines represent the tolerance on M  G  = ±1.5 for the MS sources.
Paper: Clouds in Partial Atmospheres of Lava Planets and Where to Find Them
Authors: T. Giang Nguyen, Nicolas B. Cowan, Lisa Dang
Figure caption: Top: the absorption cross section of SiO (S. N. Yurchenko et al. 2022). The blue, green, and red show the UV, visible, and IR ranges. Bottom: the normalized flux of each star using close analogs.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: Median brightness temperatures at 3 GHz of giant, pre-MS, and different MS spectral types. Quartiles 1 and 3 have been shown using error bars that represent the central scatter around the median. Coherent and incoherent emissions can be distinguished by the T  b  = 1012 K (M. Gudel 2002) line.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: The Gaia CMD for 207 of the 391 confirmed radio sources that were also found in SIMBAD by a 2.″5-radius query. Different object types have been represented using different shapes.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: Variation of peak flux density with spectral types. White points and bold boxes inside the violins show the median and interquartile range, while the violin edges represent the distribution. SE VLASS images are mostly sensitive to the area above the shaded region (F peak > 5σ). The blue dashed line shows extrapolated median flux variation for late M types.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: Sources varying by more than the uncertainty in flux measurement (﹩\delta {F}_{\mathrm{peak}}=\sqrt{\delta {F}_{1}^{2}+\delta {F}_{2}^{2}}﹩) are denoted by blue; otherwise, by red. The dashed lines indicate different values of β.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: Distance distribution of the entire sample. The solid blue line represents the distribution of distances to all the sources. The cumulative distribution function is shown in red.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: Variable (β > 0.2) and quiescent (β < 0.2) sources are denoted by red and black circles, respectively. The black line is a linear fit.
Paper: Lunar Farside Samples Returned by Chang’E-6 Mission: Significance for Understanding the South Pole-Aitken Basin Stratigraphic History
Authors: Xing Wang, James W. Head, Wenhao Zhao, Yuan Chen, Qin Zhou, Jiaming Zhu, Bo Wu, Jianjun Liu, Chunlai Li
Figure caption: Lithologic identifications of different geological units in the Apollo basin. Corresponding mineral abundances of each point are from MI-derived lunar mineralogy data (M. Lemelin et al. 2015). Ternary diagrams are after D. Stöffler et al. (1980).
Paper: Lunar Farside Samples Returned by Chang’E-6 Mission: Significance for Understanding the South Pole-Aitken Basin Stratigraphic History
Authors: Xing Wang, James W. Head, Wenhao Zhao, Yuan Chen, Qin Zhou, Jiaming Zhu, Bo Wu, Jianjun Liu, Chunlai Li
Figure caption: Schematic cross-sectional diagrams of SPA basin structure, (a) pre- and (b) post-Apollo/Schrödinger events. The horizontal scale of the diagrams corresponds to the actual topographic scale. The stratigraphy in the SPA basin center is referenced to Figure 12 in X. Wang et al. (2024a).
Paper: Lunar Farside Samples Returned by Chang’E-6 Mission: Significance for Understanding the South Pole-Aitken Basin Stratigraphic History
Authors: Xing Wang, James W. Head, Wenhao Zhao, Yuan Chen, Qin Zhou, Jiaming Zhu, Bo Wu, Jianjun Liu, Chunlai Li
Figure caption: Spectral features of different geological units in the Apollo basin. (a) shows the smoothed M3 spectra, and their corresponding continuum-removed spectra are present in (b), with an offset of 0.15 between each spectrum. (c) Comparison of band centers between the extracted spectra and the spectra of natural and synthetic pyroxene, the latter points are from D. Liu et al. (2022). The data shown in panel (c) are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Lunar Farside Samples Returned by Chang’E-6 Mission: Significance for Understanding the South Pole-Aitken Basin Stratigraphic History
Authors: Xing Wang, James W. Head, Wenhao Zhao, Yuan Chen, Qin Zhou, Jiaming Zhu, Bo Wu, Jianjun Liu, Chunlai Li
Figure caption: Topography, crustal thickness, and Th abundance variations of the AA’ profile. The AA’ line is marked in Figures 3(b), (d), and (e).
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: The known outer satellites of the giant planets where Neptunians are blue diamonds, Uranians are magenta triangles, Saturnians are green squares, and Jovians are red circles. Symbol size is proportional to the log of the diameter of the satellite. Semimajor axis and inclination are the mean osculating orbital elements from this work for Uranus and Neptune, from R. Jacobson et al. (2022) for Saturn, and M. Brozovic & R. Jacobson (2017) for Jupiter with updates from new discoveries at Jupiter and Saturn reported in S. Sheppard et al. (2018, 2023) and E. Ashton et al. (2020, 2021, 2022) shown at ssd.jpl.nasa.gov/sats/elem. The newly discovered Uranus and Neptune satellites reported here are shown as filled solid symbols while already known satellites are shown by open symbols. As seen here, all known outer satellites have semimajor axes less than 0.5 Hill radii. Dynamical families are identified by the largest member. The new Uranian satellite S/2023 U1 has a similar orbit as Caliban and Stephano, making this the first group of three or more satellites known at Uranus. The new Neptunian S/2021 N1 has a similar distant retrograde orbit as Neso and Psamathe, while the new S/2002 N5 has a similar prograde orbit as Sao and Laomedeia, making both of these the first known groups of three or more satellites at Neptune.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Area searched around Uranus in 2021. Known outer Uranus satellite positions are shown as open square symbols for 2021 December 2. Uranus is at the center of the field shown by the filled circle. The large dotted circle is the field of view of HSC on Subaru and the smaller dotted circles are the fields imaged with IMACS on Magellan (see Table 1). The southeast quadrant has two, mostly overlapping, fields since this area was reimaged in 2021 December with IMACS as the 2021 October observations had poor seeing. All known outer satellites of Uranus were detected. The newly discovered Uranus satellite S/2023 U1 is shown by a filled star.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: The efficiency of searching the Subaru 2021 September 7 data for Neptune satellites. We would expect to find over 75% of satellites within the field of view of HSC at 27.2 mag in the r band, which we take as the limiting magnitude of this one night. Table 1 shows all the detection efficiencies for the various nights of observations at Uranus and Neptune.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Area searched around Uranus in 2023. Known outer Uranus satellite positions are shown as open square symbols for 2023 November 4. The dotted circle is the field of view imaged with IMACS on Magellan on three different nights in 2023 November and December with Uranus placed at the center of the field (see Table 1). The newly discovered Uranus satellite S/2023 U1 is shown by a filled star. The Magellan observations of 2023 had six of the nine known outer satellites of Uranus easily detected with only the most distant satellites outside the field of view undetected.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Area searched around Neptune in 2021. Known outer Neptune satellite positions are shown as open square symbols for 2021 September 7. Neptune is at the center of the field shown by the filled circle. The large dotted circle is the field of view of HSC on Subaru. The smaller dotted circles are the fields imaged with IMACS on Magellan that went to a depth beyond 26.5 mag taken on 2021 September 3 and October 6 (see Table 1). All known outer satellites of Neptune were detected. The newly discovered Neptune satellites S/2021 N1 (near far east edge) and S/2002 N5 (near Neptune) are shown by filled stars.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: DTARPS-S planet occurrence as a function of planet radius and orbital period. The occurrence rates are given as percentages. Cell color indicates planet occurrence per logarithmic unit area. Note that the bin sizes are not constant. White cells have unreliable DTARPS-S occurrence rates because the injected recall is less than 10%. Text annotations in each cell list occurrence statistics: upper left—the number of DTARPS-S candidates, n cands,cell, at the bottom of each cell the RF classifier recall rate, r RF,cell, and the vetting recall rate, S CP,cell. Cells for which the global vetting recall value was used are marked with an asterisk.
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Three observables are required to constrain a planet obliquity. (a) ﹩v\sin {i}_{\mathrm{planet}}﹩: high-resolution spectroscopy can resolve individual spectral lines to probe rotational line broadening, which yields a projected equatorial velocity (﹩v\sin {i}_{\mathrm{planet}}﹩; M. L. Bryan et al. 2018, 2020, 2021). (b) P rot: time-resolved photometry can monitor variability due to cloud patchiness or longitudinal bands, similar to those seen on Jupiter (Y. Zhou et al. 2020, 2022), in order to constrain the rotation period. (a) and (b) can be combined to constrain the planet spin-axis inclination (i planet) along our LOS. (c) i orbit: astrometric measurements over a sufficiently long baseline can resolve orbital motion and allow fits to constrain the orbital inclination (M. L. Bryan et al. 2020; M. M. Nguyen et al. 2021; T. J. Dupuy et al. 2023, and references therein).
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Top: observed spectrum of VHS 1256 b over the wavelength range with a higher SNR (≳20), with portions of order 6 (left) and 5 (right) highlighted. Middle: zoomed-in panels with 1σ errors overplotted in gray, and the fiducial model atmosphere broadened to the best-fit projected equatorial velocity overplotted in orange. Although the model atmosphere underestimates the absorption line depths, this does not affect our rotational broadening measurement. We discuss this further in Section 3.1. Bottom: same as the middle panels, but additionally doubling the equivalent width of the model atmosphere line profiles. We find model assumptions contributing to line-depth mismatch do not significantly impact our measured vsini.
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Posterior distribution of spin-axis inclination i  p  for VHS 1256 b with the correct method (green, following Equation (6), and with incorrect Monte Carlo sampling (red, following Equation (5)). The correct method yields i  p  = 90° ± 18°. These distributions are compared to a random inclination distribution (black), which is a uniform distribution in ﹩\cos {i}_{p}﹩.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Occurrence rates from DTARPS-S candidates (left panel) and from D. C. Hsu et al. (2019; right panel) using the same bins and color scheme for easy comparison.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Occurrence rates from DTARPS-S candidates (red) and from D. C. Hsu et al. (2019; black) marginalized over planetary radii for orbital periods less than 8 days (left) and marginalized over orbital periods for radii between 4 and 16 R ⊕ (right).
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Data CCF (in black) of the observed spectrum cross correlated with the model atmosphere broadened to the instrumental resolution, with 1σ jackknife errors shaded in gray. Model CCFs (in color) of the model atmosphere broadened to the instrumental resolution cross correlated with that same model additionally broadened by a series of projected equatorial velocities (0, 5, 8.7 (best fit), 15, and 20 km s−1).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Plot of fractional transit depth and host star brightness for DTARPS-S stars. The gray points are 7743 objects from the DTARPS-S Analysis List of Paper I and the red points are 462 objects from the DTARPS-S candidates catalog of Paper II. Blue circles are the subset of astronomical Confirmed Planets from the NASA Exoplanet Archive.
Paper: Searching for GEMS: TOI-6383Ab, a Giant Planet Transiting an M3-dwarf Star in a Binary System 
Authors: Lia Marta Bernabò, Shubham Kanodia, Caleb I. Cañas, William D. Cochran, Szilárd Csizmadia, Suvrath Mahadevan, Gudhmundur Stefánsson, Arvind F. Gupta, Andrew Monson, Henry A. Kobulnicky, Alexander K. Larsen, Ethan G. Cotter, Alexina Birkholz, Tera N. Swaby, Gregory Zeimann, Chad F. Bender, Scott A. Diddams, Jessica E. Libby-Roberts, Andrea S. J. Lin, Joe P. Ninan, Heike Rauer, Varghese Reji, Paul Robertson, Arpita Roy, Christian Schwab
Figure caption: Top plot: mass–radius plane of all known transiting GEMS (colored in the foreground, with error bars) and known planets around F, G, and K stars (in transparency in the background), with planets colored by host star mass. TOI-6383Ab and the similar TOI-5205 b are circled. We also plot the density contours for 0.3 g cm−3, 1 g cm−3, and 3 g cm−3. NGTS-1 b has an imprecise estimate of the radius (the large error bar is clearly visible in the top part of the plot) to due its grazing transit. Bottom plot: orbital period vs. planet radius, colored by planetary equilibrium temperature. TOI-1899b is highlighted because of its long orbital period (∼29 days) with respect to the other GEMS.
Paper: Searching for GEMS: TOI-6383Ab, a Giant Planet Transiting an M3-dwarf Star in a Binary System 
Authors: Lia Marta Bernabò, Shubham Kanodia, Caleb I. Cañas, William D. Cochran, Szilárd Csizmadia, Suvrath Mahadevan, Gudhmundur Stefánsson, Arvind F. Gupta, Andrew Monson, Henry A. Kobulnicky, Alexander K. Larsen, Ethan G. Cotter, Alexina Birkholz, Tera N. Swaby, Gregory Zeimann, Chad F. Bender, Scott A. Diddams, Jessica E. Libby-Roberts, Andrea S. J. Lin, Joe P. Ninan, Heike Rauer, Varghese Reji, Paul Robertson, Arpita Roy, Christian Schwab
Figure caption: TESS and RBO light curves fitted by exoplanet jointly with RVs, with a focus on the transit region. Time is subtracted from the transit mid-time for each light curve. In all plots, the detrended data are in gray, and the model and 16%–84% confidence levels are in blue (for TESS transits) and red (for ground-based transits). In each upper plot, the point at x = −0.05 represents the median uncertainty in the photometric data.
Paper: Searching for GEMS: TOI-6383Ab, a Giant Planet Transiting an M3-dwarf Star in a Binary System 
Authors: Lia Marta Bernabò, Shubham Kanodia, Caleb I. Cañas, William D. Cochran, Szilárd Csizmadia, Suvrath Mahadevan, Gudhmundur Stefánsson, Arvind F. Gupta, Andrew Monson, Henry A. Kobulnicky, Alexander K. Larsen, Ethan G. Cotter, Alexina Birkholz, Tera N. Swaby, Gregory Zeimann, Chad F. Bender, Scott A. Diddams, Jessica E. Libby-Roberts, Andrea S. J. Lin, Joe P. Ninan, Heike Rauer, Varghese Reji, Paul Robertson, Arpita Roy, Christian Schwab
Figure caption: Left: time series of the HPF RV data and their residuals after subtracting the best-fitting model. The best-fitting model derived from the RV–photometry joint fit is plotted in blue and the 16%–84% confidence interval is in light blue. We show data binned by night in green. Residuals of the fit are plotted in the bottom plot below the time series. Right: phase-folded HPF RV curve of TOI-6383.
Paper: Searching for GEMS: TOI-6383Ab, a Giant Planet Transiting an M3-dwarf Star in a Binary System 
Authors: Lia Marta Bernabò, Shubham Kanodia, Caleb I. Cañas, William D. Cochran, Szilárd Csizmadia, Suvrath Mahadevan, Gudhmundur Stefánsson, Arvind F. Gupta, Andrew Monson, Henry A. Kobulnicky, Alexander K. Larsen, Ethan G. Cotter, Alexina Birkholz, Tera N. Swaby, Gregory Zeimann, Chad F. Bender, Scott A. Diddams, Jessica E. Libby-Roberts, Andrea S. J. Lin, Joe P. Ninan, Heike Rauer, Varghese Reji, Paul Robertson, Arpita Roy, Christian Schwab
Figure caption: Reconstructed NESSI speckle images and 5σ contrast curves for TOI-6383A. Observations were taken simultaneously in the r′ filter with the blue camera (upper left inset image) and the z′ filter with the red camera (upper right inset image). The contrast curves indicate the limiting magnitude difference at which bound or background sources could be detected for separations between 0.″2 and 1.″2. Note that the stellar companion falls outside the field of view.
Paper: Searching for GEMS: TOI-6383Ab, a Giant Planet Transiting an M3-dwarf Star in a Binary System 
Authors: Lia Marta Bernabò, Shubham Kanodia, Caleb I. Cañas, William D. Cochran, Szilárd Csizmadia, Suvrath Mahadevan, Gudhmundur Stefánsson, Arvind F. Gupta, Andrew Monson, Henry A. Kobulnicky, Alexander K. Larsen, Ethan G. Cotter, Alexina Birkholz, Tera N. Swaby, Gregory Zeimann, Chad F. Bender, Scott A. Diddams, Jessica E. Libby-Roberts, Andrea S. J. Lin, Joe P. Ninan, Heike Rauer, Varghese Reji, Paul Robertson, Arpita Roy, Christian Schwab
Figure caption: Comparison of the LRS-2 spectra with the empirical templates from pyHammer. The observed LRS-2-B spectra after response and telluric correction are plotted in red. Empirical templates of M3, M4, and M5 stars are also shown. The summed square errors (SSE) are reported in the legend. Along with the residuals (bottom part of the Figure), they show that the M3-4 stellar spectra are the best-matching ones.
Paper: Searching for GEMS: TOI-6383Ab, a Giant Planet Transiting an M3-dwarf Star in a Binary System 
Authors: Lia Marta Bernabò, Shubham Kanodia, Caleb I. Cañas, William D. Cochran, Szilárd Csizmadia, Suvrath Mahadevan, Gudhmundur Stefánsson, Arvind F. Gupta, Andrew Monson, Henry A. Kobulnicky, Alexander K. Larsen, Ethan G. Cotter, Alexina Birkholz, Tera N. Swaby, Gregory Zeimann, Chad F. Bender, Scott A. Diddams, Jessica E. Libby-Roberts, Andrea S. J. Lin, Joe P. Ninan, Heike Rauer, Varghese Reji, Paul Robertson, Arpita Roy, Christian Schwab
Figure caption: Transiting GEMS (colored) and FGK (in gray) stellar mass vs. the planet-to-star mass ratio, colored by planetary equilibrium temperature. GEMS discovered by the Searching for GEMS survey are circled in black. GEMS in a stellar binary system are represented with a squared marker and labeled with their name. TOI-4201b and HATS-76b correspond to the two higher-mass ratios in the plot, clearly visible on the top right.
Paper: Searching for GEMS: TOI-6383Ab, a Giant Planet Transiting an M3-dwarf Star in a Binary System 
Authors: Lia Marta Bernabò, Shubham Kanodia, Caleb I. Cañas, William D. Cochran, Szilárd Csizmadia, Suvrath Mahadevan, Gudhmundur Stefánsson, Arvind F. Gupta, Andrew Monson, Henry A. Kobulnicky, Alexander K. Larsen, Ethan G. Cotter, Alexina Birkholz, Tera N. Swaby, Gregory Zeimann, Chad F. Bender, Scott A. Diddams, Jessica E. Libby-Roberts, Andrea S. J. Lin, Joe P. Ninan, Heike Rauer, Varghese Reji, Paul Robertson, Arpita Roy, Christian Schwab
Figure caption: TESS transits observed in Sectors 19 and 59 excluding masked data points, modeled with GP. The exposure times are 1800 s and 200 s, respectively.