adsabs/AstroCLIMB huggingface dataset:
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: RV time-series plot for the disjoint GP model with the 12.2 day prior on η  P , phased to the period of b and c, respectively, after subtracting the best-fit stellar activity model and the other planet.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Periodograms of HD 79210's white light HARPS-N radial velocities with the binary trend removed, activity indicators, and the window function. The three most significant peaks (<0.1% FAP) are marked with dashed vertical lines. Note that there are no periodic signals in the RVs with FAP < 0.01%. The 25.16 and 26.98 days signals are just offset from significant (<0.01% FAP and <0.1% FAP, respectively) peaks in the periodogram of BIS. We suspect that the RV signals correspond to these BIS signals, as BIS signals have been shown to be offset in time from RV variability (Dumusque et al. 2014; Collier Cameron et al. 2019). We suspect that the 225.54 days signal is a harmonic of the 25.16 days variability signal.
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Posterior distributions of the free parameters when fitting HD 79211’s combined HARPS-N and CARMENES RV data set with an eccentric orbit and a quasi-periodic GP kernel.
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: Histogram coloring is the same as Figure 2. Each histogram includes all planets from the NEA (gray), as well as all planets included in each of the three HZ groups (greens). Panel (A): distribution of planet period. The HZ planets peak at higher periods than those in the full catalog. Panel (B): eccentricity distribution. Only those planets with eccentricity uncertainty measurements are included in these plots. The <2R ⊕ planets tend to have more circular orbits. Panel (C): ﹩\mathrm{log}\,g﹩ distributions. The HZ planet groups skew right progressively. Panel (D): effective temperature (T eff) distributions. The <2R ⊕ planets tend to be found around stars with lower T eff. Panel (E): J distributions. The >0% HZ objects that pass through the HZ are more often found around brighter stars. Panel F: TSM distributions. HZ planets have lower TSM values than the full catalog. Note that both transiting and nontransiting planets are included in panel (F) to represent the overall exoplanet population.
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: Mass and radius histograms of the full catalog of exoplanets from the NEA (gray), planets that spend any time at all in the HZ (>0% HZ; light green), planets found to orbit in the HZ 100% of the time (100% HZ; medium green), and those <2R ⊕ that orbit in the HZ 100% of the time (Rocky-OHZ; dark green). Histogram (A) includes only those planets that have measured values for mass. Histogram (B) includes both measured values and calculated values of mass using the mass–radius relationship from Chen & Kipping (2017). Histogram (C) includes only those planets that have measured values for radius. Histogram (D) includes both measured values and calculated values of radius.
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: The most eccentric HZ planets. Top left: the most eccentric planet within the CHZ: KELT-6 c is a 3.71 ± 0.21M J planet discovered by Collins et al. (2014). With an eccentricity of 0.21, this planet’s T eq will range from 385 K at periastron to 311 K at apastron. Top middle: the most eccentric planet within the OHZ: GJ 1148 b, discovered by Haghighipour et al. (2010), is a ﹩{0.3043}_{-0.0032}^{+0.0044}﹩                          M J planet. With an eccentricity of 0.38, this planet’s T eq will range from 422 K at periastron to 283 K at apastron. Top right: the most eccentric planet to pass through the HZ: HD 20782 b, discovered by Jones et al. (2006). This ﹩{1.4878}_{-0.1066}^{+0.1045}﹩                          M J planet is the most eccentric planet found to date and has a massive variation in T eq of 1603 K at periastron to 257 K at apastron. Bottom left: the most eccentric planet ≤2 R ⊕ that passes through the OHZ, GJ 1061 d has an eccentricity of 0.58 and has a variation in T eq of 278–502 K (Dreizler et al. 2020). Bottom right: the most eccentric planet ≤2 R ⊕ that spends 100% of its orbit in the OHZ, Kepler-296 f, has an eccentricity of 0.33 and its T eq fluctuates in the range 303–427K (Rowe et al. 2014).
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: Heat maps with HZ planets (green) overlying the full catalog of known exoplanets (gray). Top left: compared to the full catalog, HZ planets tend to have longer periods and larger masses. Top right: the planet period vs. radius heat map highlights the gap between the mini-Neptune sized planets and the larger Jupiter sized planets. Middle left: longer period planets tend to have a wider distribution of eccentricity in both the full catalog and HZ planets. Middle right: so too do the larger mass planets. Bottom left: this trend of larger planets having a broader range of eccentricities is not seen in the HZ planets in the radius–eccentricity plot, but this may be due to a smaller population. Bottom right: the measured mass vs. radius plot reveals clusters of Jupiter sized planets and super-Earths in the full catalog, but not in the HZ planets.
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: Panels (A), (C), and (D) include only the planets found in the HZ that have both a measured mass and radius. Panel (B) also includes mass or radii calculations from Chen & Kipping (2017). Panels (A) and (B): the color of data points indicates the transmission spectroscopy metric (TSM) of the planet (Kempton et al. 2018). The planets with the highest TSM value in each plot are labeled. GJ 414 A b has the greatest TSM of all known transiting planets, including those without mass measurements. HD 102365 b has the greatest TSM of all HZ planets, though, like many of the planets included in panel (B), it is not known to transit. Panel (C): the color of data points indicates J, as indicated by the color bar on the right. The brightness of GJ 414 A contributed to the high TSM value. Panel (D): the color of data points indicates bulk density of the planet in g cm−3. The planets with the greatest density on the bottom left are the TRAPPIST-1 planets.
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: Heat maps of stellar effective temperature and ﹩\mathrm{log}\,g﹩. The population of >0% HZ planets spans the same distribution of T eff and ﹩\mathrm{log}\,g﹩ as the full catalog of planets, except for among the more evolved stars at the top of the plot. These stars either may not host planets in the HZ, or the properties of these stars may mean detection of any HZ planets is beyond current capabilities.
Paper: A Catalog of Habitable Zone Exoplanets
Authors: Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ravi Kopparapu, Zhexing Li, Colby Ostberg
Figure caption: Predicted RV amplitude as a function of orbital period for four groups of planets: plot (A) includes the full catalog of planets, plot (B) includes all planets with radii ≤2R ⊕, plot (C) includes the >0% HZ planets, and plot (D) includes >0% HZ planets with radii ≤2R ⊕. Planets that are missing mass measurements are denoted by an X symbol. Planets represented with a dot have mass measurements, but many would benefit from RV follow-up to refine their orbit and mass measurements. The plots are color coded by V magnitude, as indicated by the color bar on the right, with a V cutoff of 14 mag.
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Left panels: Lomb-Scargle periodograms of the light curves of TOI 560 from the SuperWASP survey in 2009–2012 from bottom to top, plotted in green as a function of period on the horizontal axis and power on the vertical axis. Right panels: phased seasonal light curves of the SuperWASP TOI 560 seasonal light curves in the same reverse annual order. The light curves are binned in phase in 0.05 increments in blue with the coadded uncertainties shown, with rotational phase on the horizontal axis and relative and normalized apparent magnitude on the vertical axis. Spot evolution is readily apparent from year to year, including some double-humped features from spots on the northern and southern hemispheres of the star.
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Top left: our 5σ contrast curves and the reconstructed speckle images observed using the Zorro speckle instrument on the Gemini South 8 m telescope. Sensitivity is quoted on the vertical axis in magnitudes relative to the host star, as a function of angular separation on the horizontal axis. Inset: a cutout of our image, centered on the target star TOI 560. Top right: same as top-left, showing the 5σ detection sensitivity and speckle autocorrelation functions from the SOAR observations. Bottom: same as the top two panels, showing our sensitivity of the Gemini/NIRI observations to companion stars, as a function of separation from the host star. No visual companions are seen anywhere in all of our high-contrast imaging data, and the star appears single.
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: SED of TOI 560 from the first of our two independent SED analyses; this analysis is particularly suited for the identification of the NUV excess. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit NextGen atmosphere model (black).
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: GALEX-Gaia color–color diagram for TOI 560 (red diamond) compared to nearby field stars detected in GALEX (black circles), members of various nearby, young associations with ages in the range 5–100 Myr (right-pointing purple triangles; see Gagné et al. 2018), and members of the Pleiades (left-pointing blue triangles; 112 ± 5 Myr; Dahm 2015; Gagné et al. 2021). TOI 560 falls on the UV-bright end of the field distribution, but on the UV-faint end of the Pleiades distribution, compared to other stars of a similar Gaia G − G RP color.
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Gaia DR3 color–magnitude diagram for TOI 560 (red diamond) compared to nearby field stars (black dots) and empirical age-dated sequences built from the members of nearby coeval associations (thick colored lines; see Gagné et al. 2021). The position of TOI 560 is consistent with an age ≈100 Myr or older, and ages of 45 Myr and younger are clearly ruled out.