adsabs/AstroCLIMB huggingface dataset:
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: Six selected regions illustrate key aspects of the CH4 features identified in this study, as described in the main text. Line plots of the normalized ESPRESSO and UVES Titan spectra, divided by their respective best-fit backgrounds (BFBG), are shown in an inverted format to emphasize absorption strength. The telluric model is also plotted in an inverted format, with its strength scaled to fit the vertical axis. In this scale, the lowest value represents no absorption, and the highest corresponds to 100% absorption. The legend on the left side refers to the left vertical axis, while the legend on the right refers to the right axis. A key for all symbols used in the plots is provided in the top-left panel.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: Comparison of the Titan spectrum with the “background.” (Top) Regions dominated by solar lines. (Middle) Regions with minimal telluric and solar interference. (Bottom) Regions with prominent telluric O2 and H2O lines. Telluric and solar features in the Titan spectrum align with their counterparts in the background, while telluric residuals from the solar spectrum appear only in the background, without overlap in the Titan spectrum. Features not originating from Titan typically produce positive residuals, except near the wings of strong lines, where negative residuals may occur. The percentage difference between the Titan spectrum and the background, providing a measure of their variation, is calculated by summing the absolute differences and dividing by the average of the two spectra.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: An illustration of the adjusted telluric models for the solar and Titan spectra, where a 10% reduction from the best-fit model is applied to the solar spectrum and a 10% increase from the best-fit model is applied to the Titan spectrum, as described in Section 2.2. “o” and “x” markers indicate uncontaminated telluric lines used to estimate these adjustments. “o” markers represent lines with expected strength, while “x” markers denote lines with anomalous strength. The center of each “o” or “x” corresponds to the peak of the adjusted telluric model. The four regions shown were selected to clearly demonstrate both marker scenarios and to span a broad wavelength range relevant to the study.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: The best-matched telluric models for the observed telluric lines in both the solar and Titan spectra, in contrast to the adjusted models shown in Figure 3. Unlike Figure 3, where a 10% reduction and increase were applied to the best-fit models for the solar and Titan spectra, respectively, the models here represent the closest match to the observed telluric features without adjustments. The “x” and “o” markers indicate the same wavelength positions as in Figure 3, with their vertical positions adjusted to align with the peak centers of the best-fit telluric model lines. This alignment allows for a direct comparison of line depths relative to the weaker and stronger models illustrated in Figure 3.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: ESPRESSO spectrum of Titan before (top) and after (bottom) continuum normalization with RASSINE. The red curve in the top panel represents the estimated continuum level, constructed by linearly connecting the anchor points (not shown in this plot) described in the text. The average distance between anchor points is approximately 4 Å, as indicated by the label on the left edge of the top panel. The blue line in the top panel serves as a reference for telluric absorption across different wavelengths.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: Examples of CH4 features across the three categories discussed in Section 2.3. (Top) Features detected in both the adjusted and best-fit backgrounds, indicating consistent detections. (Middle) Features unique to the best-fit background, i.e., peaks found in the red spectrum but not in the green-dotted spectrum, suggesting that the improved background reveals these features, which could represent either genuine CH4 features or artifacts. (Bottom) Features unique to the adjusted background, i.e., peaks found in the green-dotted spectrum but not in the red spectrum, indicating that these features are sensitive to the choice of background and may not be robust. In each panel, the feature under discussion is marked with a vertical blue dashed line. Cyan bands represent variations across the three individual Titan spectra, and horizontal lines at y = 1 denote the background levels.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: Same spectrum as shown in Figure 1, but zoomed into 100 Å wide segments centered on selected regions: (rows 1–2) regions with moderate CH4 absorption, (rows 3–4) regions with strong absorption from both CH4 and telluric features, and (rows 5–6) regions dominated by strong CH4 absorption alone. The red solid line indicates the continuum level from Figure 1, with blue dots marking its anchor points. Orange crosses and green triangles denote the anchor points from the remaining two spectra. A red dashed line at a normalized flux of 1 marks the baseline of the normalized spectrum. The average distance between neighboring anchor points in each region is shown in the lower right corner of the corresponding panel.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: Identified CH4 features, with their relative strengths plotted against vacuum wavelengths and wavenumbers. The green line represents CH4 absorption coefficients at 100 K from E. Karkoschka & M. G. Tomasko (2010), serving as a reference for the locations and strengths of absorption bands. The left vertical axis corresponds to the relative strengths of the absorption features identified in this work, while the right vertical axis represents the absorption coefficients from E. Karkoschka & M. G. Tomasko (2010). The gray line indicates the detection threshold applied during the line identification process (5 times the local noise level). The blue line represents telluric absorption across different wavelengths. The size of the circles is proportional to the ratio of strength uncertainty to the measured strength. Vibrational band assignments, based on L. P. Giver (1978), are annotated in black text.
Paper: Identification of Likely Methane Absorption Features in the Optical Spectra of Titan
Authors: Sirinrat Sithajan, Lalita Kaewbiang, Hugh R. A. Jones, Pakakaew Rittipruk, Sukanya Meethong
Figure caption: Comparison of the Titan spectrum with the “best-fit background.” The panel structure is similar to that in Figure 4, but here the background is constructed using telluric models that best match the observed telluric lines in both the solar and Titan spectra, referred to as the “best-fit background.” In this case, negative residuals are no longer solely attributed to Titan’s absorption.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: Discovery and follow-up photometry obtained for NGTS-EB-8. Top-left panel: phase-folded photometry for the primary eclipse in each instrument, offset for clarity. Binned data in 2 minute bins for NGTS and 15 minute bins for all other instruments is shown as solid circles, with raw data shown as lower opacity points. The median best-fit allesfitter model for the High k-range model is shown as a solid line for each photometric data set. Top-right panel: phase-folded photometry for the secondary eclipse in each instrument it was observed, offset for clarity. Bottom panels: residuals for the primary and secondary eclipses in each instrument, offset for clarity. The photometric data are provided 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: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: Relative flux calibration process for the VO feature around 746 nm. Top panel: GHOST spectrum of telluric standard star in black with the continuum fit shown in blue. Middle panel: PHOENIX synthetic spectrum with Teff  =  10,000 K, ﹩\mathrm{log}g﹩  =  3.50, and [Fe/H]  =  −0.5 shown in black with the continuum fit shown in blue. Bottom panel: GHOST spectrum of NGTS-EB-8 shown in black prior to the relative flux calibration and shown in blue following the relative flux calibration.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: Distribution of radius ratios of the best-fitting templates to the GHOST spectrum of NGTS-EB-8. The median radius ratio, kmed = 0.91 is marked as a vertical dashed line. The 68% confidence interval, [0.31, 0.97], is shown as dashed–dotted lines.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: Telluric line identification for the Na I region, zoomed on the Na I feature around 819 nm. Top panel: GHOST spectrum of NGTS-EB-8 shown in black. Regions identified as telluric absorption features are highlighted in red and marked with ⊕. Bottom panel: GHOST spectrum of the telluric standard star (HIP 60985) in blue and the synthetic PHOENIX spectrum that represents an A0V star in orange.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: The CCF for the NIRPS spectrum of NGTS-EB-8 from the night of 2023 April 27 cross-correlated with the NIRPS M2 mask. The solid blue line shows the CCF. The vertical dashed–dotted pink line shows the barycentric Earth radial velocity (BERV) value that coincides with the sky emission peak. The orange and green dashed lines show the Gaussian fits for the primary and secondary component, respectively.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: CCF for the first GHOST spectrum of NGTS-EB-8 cross-correlated with the HARPS M5 mask. The solid blue line shows the median CCF. The orange and green dashed lines show the Gaussian fits for the primary and secondary component, respectively.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: ATLAS photometric data for NGTS-EB-8. o-band and c-band measurements are shown in orange and cyan, respectively.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: Normalized and stacked GHOST spectrum of NGTS-EB-8 zoomed on the Hα (left panel) and Hβ (right panel) emission features.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: Mass–radius diagrams of low-mass stars in double-lined eclipsing binary systems composed of two M dwarfs with the position of the components of NGTS-EB-8 shown for the different k-range models in each panel. In all panels, black points show stars with both mass and precision measured to better than 2%. Light-gray points show all other stars found in the literature search (see Table 7). NGTS-EB-8 A is shown as an orange star. NGTS-EB-8 B is shown as a green star. The 50 Myr and 10 Gyr isochrones from I. Baraffe et al. (2015) are plotted as dashed–dotted pink and solid blue lines, respectively. The relation from A. Schweitzer et al. (2019) is shown as a dashed orange line. The relation derived from A. W. Mann et al. (2015) and A. W. Mann et al. (2019) is shown as a dotted green line. Top-left panel: positions of NGTS-EB-8 shown as determined by the Full k-range model. Top-right panel: positions of NGTS-EB-8 shown as determined by the Middle k-range model. Bottom panel: positions of NGTS-EB-8 shown as determined by the High k-range model.
Paper: NGTS-EB-8: A Double-lined Eclipsing M+M Binary Discovered by Citizen Scientists
Authors: Sean M. O'Brien, Megan E. Schwamb, Christopher A. Watson, Louise D. Nielsen, Edward M. Bryant, Sarah L. Casewell, Matthew R. Burleigh, Lucy Fortson, Samuel Gill, Chris J. Lintott, Katlyn L. Hobbs, Ioannis Apergis, Daniel Bayliss, Jorge Fernández Fernández, Maximilian N. Günther, Faith Hawthorn, James S. Jenkins, Alicia Kendall, James McCormac, Ernst J. W. de Mooij, Toby Rodel, Suman Saha, Laura Trouille, Richard G. West, Peter J. Wheatley, Marius Constantin Agafitei, Deniz Rüzgar Apaydın, Elisabeth Baeten, Bruce Baller, Jeff Carabott, Sallyann Chesson, Sebastián Alejandro Freigeiro, Virgilio Gonano, Matthias Hanke, Pete Hermes, Avery Hildebrand, John S. Langley, See Min Lim, Leo Ryan McCarthy, Graham Mitchell, Ken O'Neill, Charles R. Pearson, Nolan Reket, Jeanne Riethmiller, Juergen Saeftel, Arttu Sainio, Charlie Steiner, Amanda Strickland, Christopher Tanner, Ivan A. Terentev, Ernest Jude P. Tiu, Sergey Y. Tumanov, Marciniak Urszula, Pia Vahlenkamp, Femke de Vroome, Paweł Wantuch, Timothy Woodruff
Figure caption: Gaia DR3 HR diagrams for all stars within 100 pc with the median fiducial tracking the main sequence in blue and the same fiducial shifted by −0.753 mag in green, corresponding to the position of unresolved binaries composed of two identical stars. NGTS-EB-8 is shown as a cyan star, and the inset shows the region zoomed in around NGTS-EB-8. Low-mass host stars of confirmed exoplanets, TOIs, and candidates identified by B23 are overplotted, colored by TFOPWG/B23 disposition. Confirmed/known planets are shown as black filled circles, (ambiguous) planetary candidates are shown as open black circles, and false positives are shown as gray circles. Binary systems hosting confirmed planets, Kepler-16 and TOI-762, are shown as lime-green filled circles.