adsabs/AstroCLIMB huggingface dataset:
Paper: Spectroscopically Resolved Partial Phase Curve of the Rapid Heating and Cooling of the Highly Eccentric Hot Jupiter HAT-P-2b with WFC3
Authors: Bob Jacobs, Jean-Michel Désert, Nikole Lewis, Ryan C. Challener, L. C. Mayorga, Zoë L. de Beurs, Vivien Parmentier, Kevin B. Stevenson, Julien de Wit, Saugata Barat, Jonathan Fortney, Tiffany Kataria, Michael Line
Figure caption: Spectral difference between two Kurucz stellar spectra of HAT-P-2 with a 0.5 K difference in effective temperature. Suppose that the hotter stellar spectrum is the observed in-eclipse spectrum and that the cooler spectrum is the out-of-eclipse spectrum. If we perform a common-mode method on this, the resultant Fp/Fs is shown on the right axis, with the best-fit blackbody being a dashed line. Note also that in this case the Paβ deviation (see Section 6.4) is measured to be 10 ppm. All wavelength bins contain five wavelength pixel columns. The δPa in this figure therefore corresponds to the dark-red bin in Figure 12.
Paper: Spectroscopically Resolved Partial Phase Curve of the Rapid Heating and Cooling of the Highly Eccentric Hot Jupiter HAT-P-2b with WFC3
Authors: Bob Jacobs, Jean-Michel Désert, Nikole Lewis, Ryan C. Challener, L. C. Mayorga, Zoë L. de Beurs, Vivien Parmentier, Kevin B. Stevenson, Julien de Wit, Saugata Barat, Jonathan Fortney, Tiffany Kataria, Michael Line
Figure caption: Corner−corner plot of the parameters retrieved from HAT-P-2b's white light curve.
Paper: Spectroscopically Resolved Partial Phase Curve of the Rapid Heating and Cooling of the Highly Eccentric Hot Jupiter HAT-P-2b with WFC3
Authors: Bob Jacobs, Jean-Michel Désert, Nikole Lewis, Ryan C. Challener, L. C. Mayorga, Zoë L. de Beurs, Vivien Parmentier, Kevin B. Stevenson, Julien de Wit, Saugata Barat, Jonathan Fortney, Tiffany Kataria, Michael Line
Figure caption: Corner−corner plot of the free-chemistry retrieval of the secondary eclipse spectrum. The reference radius at 0.01 bars (Rp,ref) is in Jupiter radii, ΔTi are the temperature changes between the layers listed in Section 3.3, and the abundances of the fitted molecular species are in log(volume mixing ratio).
Paper: Spectroscopically Resolved Partial Phase Curve of the Rapid Heating and Cooling of the Highly Eccentric Hot Jupiter HAT-P-2b with WFC3
Authors: Bob Jacobs, Jean-Michel Désert, Nikole Lewis, Ryan C. Challener, L. C. Mayorga, Zoë L. de Beurs, Vivien Parmentier, Kevin B. Stevenson, Julien de Wit, Saugata Barat, Jonathan Fortney, Tiffany Kataria, Michael Line
Figure caption: Best-fit TP profiles (aquamarine green) of the 1D free-chemistry retrievals of the four phase-resolved emission spectra of HAT-P-2b with the corresponding contribution functions. As a reference, the TP profiles and the τ = 0.5 contribution functions are shown for the 1D time-stepping forward models.
Paper: Structural Parameters of the Thin Disk Population from Evolved Stars in the Solar Neighborhood
Authors: Sedanur İyisan, Selçuk Bilir, Özgecan Önal Taş, Olcay Plevne
Figure caption: V-band extinction A∞(V) values from the dust maps of E. F. Schlafly & D. P. Finkbeiner (2011; upper panel) and the distance between Sun and stars reduced Ad(V) values (lower panel).
Paper: Spectroscopically Resolved Partial Phase Curve of the Rapid Heating and Cooling of the Highly Eccentric Hot Jupiter HAT-P-2b with WFC3
Authors: Bob Jacobs, Jean-Michel Désert, Nikole Lewis, Ryan C. Challener, L. C. Mayorga, Zoë L. de Beurs, Vivien Parmentier, Kevin B. Stevenson, Julien de Wit, Saugata Barat, Jonathan Fortney, Tiffany Kataria, Michael Line
Figure caption: Comparison of the secondary eclipse and transmission spectra from previous studies to the ones presented in this study. Purple spectra denote spectra from this work, and cyan spectra are from Q. Changeat et al. (2022) and B. Edwards et al. (2023).
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: Summary of the pipeline implemented in COSMIC. Based on the telescope's observational intent, the data will either flow from the hardware to the calibration pipeline or from the hardware to the search pipeline on the GPUs. The postprocessing step, which will be described later in this work, is a separate data flow and does not happen in real time. A more detailed depiction of the process can be found in Figures 3 and 8 of C. D. Tremblay et al. (2024).
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: Example calibration plots from the AC tuning generated by plotting the phases prior to the calibration being applied. In (a), the overall grade is <0.2, (b) has a score of 0.639, and (c) has a score of 0.991. A score greater than 0.6 is considered a “good” calibration, as this represents a score prior to the correction to the FPGA. Therefore, it shows the ease with which a solution can be found more than the actual solution. The red vertical strips indicate 1 MHz channels that are flagged as containing RFI signals during the calibration run.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: The plot above shows the power over time for the frequency channel containing the peak intensity of the W51 6.7 GHz methanol maser emission. The shape of the line is expected to correspond to the antenna's primary beam response. As a comparison, the power response of coherent and incoherent beams (multiplied by a factor of 10 to improve visibility) is plotted, along with their ratio. The ratio is ideally expected to equal the number of antennas used in the summation, which was 21 in this test. Imperfect calibration reduces the ratio away from the ideal value. The high scatter of the ratios away from the peak is due to large errors from small, noisy values.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: Histogram showing the number of frequencies per frequency window that have high kurtosis, implying high levels of RFI. The edges at 2–2.5 GHz and 3–3.5 GHz show significant RFI. Therefore, for VLASS, the central frequency range of 2.5–3.5 GHz was processed and searched.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: Example of a time-averaged power spectrum in the 2348.5–2380.5 MHz band. The transparent red regions mark the locations where CRICKETS detected RFI. The fine-frequency spikes in time-averaged power are a result of RFI. We know this to be true because these data come from observations of the calibration source 3C 286. The sinc-like pattern at the bottom of the plot is a result of the PFB process, which is a necessary step in COSMIC's signal processing procedures. This will be discussed further in Section 3.4.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: Percentage of frequencies flagged per filterbank file. Each dark red rectangle represents a filterbank file. Each dark blue rectangle represents a frequency range within the S band for which we did not have data.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: Calibration results for 2 months of operation. The colors of the bubbles represent the grade of the calibration, where the higher value is a lower SNR across the phase and the size of the bubble represents the number of times the source was observed. As can be seen, the calibration is good most of the time.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: A plot of all the coordinates of targeted stars during VLASS recordings from 2023 March 25 to 2023 June 15. All recorded data of scientific quality that are contained with the COSMIC database for Epoch 3.1 are represented here.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: A plot of the SNR vs. observing frequency showing all of the hits found in the observations toward Voyager detected by SETICORE.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: Top: distribution of detected signals by the real-time pipeline before any filtering for RFI. Bottom: number of channels flagged with high kurtosis per frequency bin. When the two plots are compared, there are frequency ranges where there are not many flagged channels but a large number of hits.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: A plot in galactic coordinates of all the coordinates currently in the database observed from 2023 March 29 to 2024 July 14. The orange points represent data from frequencies below 4 GHz, and the blue points are from data collected above 4 GHz.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: A plot showing the distribution of EIRP values calculated for each of the 511 sources evaluated during this work. The values range from 1011 to 1016 W, providing some of the lowest values for technosignatures to date.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: An example of the dynamic spectra from a single field in which the incoherent sum contained the main signal but the coherent beams each have a faint trace of the signal, indicating that it is not likely an astronomical source of emission. All sources chosen are within the FWHM of the primary beam.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: A flow diagram showing the logic behind the ARTISTIC pipeline that can be applied to any set of observations.
Paper: COSMIC’s Large-scale Search for Technosignatures during the VLA Sky Survey: Survey Description and First Results
Authors: C. D. Tremblay, J. Sofair, L. Steffes, T. Myburgh, D. Czech, P. B. Demorest, R. A. Donnachie, A. W. Pollak, M. Ruzindana, Siemion A. P. V., S. S. Varghese, S. Z. Sheikh
Figure caption: A histogram demonstrating the signals detected at each frequency for each beam. This shows that many of the signals are in similar frequency ranges and at a similar number of detected signals per frequency.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: [Eu/Mg] vs. [Mg/H] for Sgr stars (black open/filled dots) in comparison with the GSE stars from X. Ou et al. (2024; blue dots). Stars in the Sgr streams are marked. We also include measurements from C. J. Hansen et al. (2018; red diamonds), with Ca as a proxy for Mg.
Paper: Evolution of Massive Red Galaxies in Clusters from z = 1.0 to z = 0.3
Authors: Yen-Ting Lin, Kai-Feng Chen, Tsung-Chi Chen, Chen-Yu Chuang, Masamune Oguri
Figure caption: Illustration of our method. Panels (a) is a sketch of the richness-mass (N–M) relation measured at two different redshifts, at e.g., z = 1 (green) and z = 0.3 (black); the line and shaded regions represent relations and the associated uncertainties. Panel (b) is an example merger tree; the size and the color of the circles represent the mass and specific star formation rate of the halos. For our method, merger trees from a dark matter-only simulation are sufficient. We shall use panels (b), (c) and (d) to demonstrate our approach. Briefly speaking, one starts from a real cluster at high-z (step 1 in panel (c)); using the measured N–M relation at that redshift (e.g., green line in panel (a)), one infers a corresponding halo mass (step 2 in panel (c)), and try to find the closest halo in terms of mass at that redshift (step 2 in panel (b)). For a real cluster at low-z (step 3 in panel (d)), we use the low-z N–M relation to find the most appropriate mass (step 4 in panel (d)), then search for the best matched halo at that redshift (step 4 in panel (b)). This way, one can “connect” two observed clusters at the two cosmic epochs and study how the galaxy populations evolve (step 5). Panel (b) is generated courtesy of the IllustrisTNG collaboration (D. Nelson et al. 2019).
Paper: Evolution of Massive Red Galaxies in Clusters from z = 1.0 to z = 0.3
Authors: Yen-Ting Lin, Kai-Feng Chen, Tsung-Chi Chen, Chen-Yu Chuang, Masamune Oguri
Figure caption: Redshift evolution of total stellar mass contained in red member galaxies, for three sets of clusters whose z = 0.3 masses lie in the ranges ﹩\mathrm{log}{M}_{200m}/({h}^{-1}\,{M}_{\odot })=14.2-14.4﹩ (blue squares), 14.4–14.6 (green triangles), and ≥14.6 (red solid points). For each set, the points from lower left to upper right show how Mstar,tot evolves with redshift. In other words, the x-axis not only shows the cluster mass, but can also be regarded as the arrow of time (for a given cluster set). The offset of three sets of data points reflects the true halo masses derived from the merger trees (i.e., not artificially adjusted for clarity of presentation).
Paper: Evolution of Massive Red Galaxies in Clusters from z = 1.0 to z = 0.3
Authors: Yen-Ting Lin, Kai-Feng Chen, Tsung-Chi Chen, Chen-Yu Chuang, Masamune Oguri
Figure caption: Illustration of how our method can be used to derive mass–observable relations at different redshifts. From top to bottom, we show example best fits to the Mstar,tot–M200m, Mbcg–M200m, and N–M200m relations at z ≈ 0.95 (black dashed line) and z ≈ 0.42 (pale red dashed line). For the values of the slopes, please refer to Table 1. Here we simply note that the slopes of both Mstar,tot–M200m and N–M200m appear to be invariant with respect to redshift.
Paper: Evolution of Massive Red Galaxies in Clusters from z = 1.0 to z = 0.3
Authors: Yen-Ting Lin, Kai-Feng Chen, Tsung-Chi Chen, Chen-Yu Chuang, Masamune Oguri
Figure caption: Similar to Figure 4, but for the stellar mass assembly history of BCGs. There appears to be a halt in BCG stellar mass growth at z ≲ 0.6. It is also seen that the BCGs in the high cluster mass bin do not experience much growth from z = 0.99 to z = 0.3.
Paper: Evolution of Massive Red Galaxies in Clusters from z = 1.0 to z = 0.3
Authors: Yen-Ting Lin, Kai-Feng Chen, Tsung-Chi Chen, Chen-Yu Chuang, Masamune Oguri
Figure caption: Similar to Figure 4, but for BCG-to-total stellar mass ratio. For a given cluster mass bin, the ratio decreases with time, because of the dramatic differences in the rates of growth between Mbcg and Mstar,tot. Also, at a given redshift, the BCG dominance decreases with cluster mass.
Paper: Evolution of Massive Red Galaxies in Clusters from z = 1.0 to z = 0.3
Authors: Yen-Ting Lin, Kai-Feng Chen, Tsung-Chi Chen, Chen-Yu Chuang, Masamune Oguri
Figure caption: Probability density and cumulative distribution of ﹩{\mathrm{log}}_{10}({M}_{200m})﹩ for various richness and redshift.
Paper: Evolution of Massive Red Galaxies in Clusters from z = 1.0 to z = 0.3
Authors: Yen-Ting Lin, Kai-Feng Chen, Tsung-Chi Chen, Chen-Yu Chuang, Masamune Oguri
Figure caption: Probability density of richness for different mass and redshift ranges.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Stacked TESS light curves for TOI-1266 b (top row) and c (bottom row) for the prime mission (left column), extended mission (middle column), and second extended mission (right column). Individual transits are stacked by their best-fit midtimes, with the total number of transits per mission noted, and 100 random draws from the transit model posteriors shown in blue.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Planetary equilibrium temperature vs. tidal heat flux per unit mass, adapted from Figure 5 of D. Z. Seligman et al. (2024), showing the most promising rocky planets for tidal volcanism. Heat fluxes are normalized by the uncertain tidal quality parameters, point sizes are scaled by planet size, and color indicates the ratio of tidal heat flux to insolation flux. TOI-1266b has an estimated tidal heat flux nearly equal to its insolation flux. If TOI-1266 c has a damped free eccentricity of 0.001, then it falls outside of this plot (Heating/Mass/﹩\Im ({\tilde{k}}_{2})\simeq 1{0}^{-8}﹩, ﹩{\dot{E}}_{{\rm{Heat}}}/{\dot{E}}_{{\rm{Iso}}}/\Im ({\tilde{k}}_{2})\simeq 5\times 1{0}^{-5}﹩).
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: The tidal heat flux per unit mass of TOI-1266 b (top) and c (bottom) calculated with a wide range of possible Q (100–10000) and k2 (0.01–0.8) values, with e values drawn from the TTV+RV joint posterior distribution (red). Tidal heat fluxes with eb drawn from the higher-eccentricity peak where ed is small and where Q/k2 is  >1200 such that the eccentricity damping timescale is  >2 Gyr for TOI-1266 b are shown in blue. For both planets, the lower bound on heat flux is set by the post-damping eccentricity equilibrium e  ≃  0.0001.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Mass–radius diagram for TOI-1266 b (triangle) and c (square), with updated measurements from this work (blue markers) compared to C24 (gray markers). Filled circles represent all small (<3 R⊕) planets orbiting M dwarfs (T* < 3900 K) with masses and radii measured to better than 3σ, based on the NASA Exoplanet Archive list of confirmed planets as of 2024 August 23. The predicted equilibrium temperatures of the planets are indicated by the point color. For comparison, we also plot Earth-like water-rich mass–radius curves from A. Aguichine et al. (2021) and pure iron, Earth-like, and rocky iso-density curves from L. Zeng et al. (2016).