adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: A schematic illustrating the “Linear Motion Parameter” γ, i.e., the angle between the relative 2D position and velocity vectors of the TOI and its comoving stellar companion in the sky plane. Because the transiting planet must follow a nearly edge-on orbit, γ will favor different values depending on the mutual inclination between the orbits of the planet and companion. In the well-aligned case of small mutual inclination, the companion will likely also have an edge-on orbit, with γ near 0° or 180°. In the misaligned case of large mutual inclination, the binary orbit will tend to be face-on with γ near 90°.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The differential position (red), differential velocity (blue), and individual velocity vectors (black) in the sky plane for one of the 155 binary TOI systems used in our alignment analysis (TOI-1473), derived from the equatorial coordinates (R.A. and decl.) and proper motions in the R.A. (μα) and decl. (μδ) directions. The velocity vectors are in units of mas yr−1, while the position vector is in units of mas/100 for easier visualization. The position and velocity vector scatter is derived from sampling the covariance matrix for 100 iterations and is represented by the clouds of gray dots. The zoomed-in inset displays how γ is measured. The expected orbital velocity (mas yr−1) assuming circular orbits is shown for comparison and represented by the length of the black line in the lower left corner.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The eccentricity distribution model derived by Tokovinin & Kiyaeva (2016; black dashed) and the eccentricity distributions from Hwang et al. (2021) for binary separations in the ranges of ∼30–300 au (red), ∼300–1000 au (orange), and ∼1000–3000 au (blue). The Tokovinin & Kiyaeva (2016) model is in good agreement with the Hwang et al. (2021) distributions in this binary separation regime of ∼30–3000 au.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The left panel displays the normalized histogram of angles γ between the differential position and velocity vectors in the sky plane for the 512 TICv8 CTL targets in our comparison sample that pass our γerr < 5° cut (gray). The right panel displays the theoretical γ distributions corresponding to an isotropic distribution of α with circular orbits (blue) or eccentric orbits (gray). The red distribution corresponds to the case of mutual inclination α between the transiting planet and companion agreeing within 10°. Note that the planetless comparison sample shows a rather uniform distribution of γ as one would expect for an isotropic distribution that also accounts for orbital eccentricities.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The right panel displays the scatter plot of binary separations and angles γ between the 2D differential position and velocity vectors for the TOI (blue) and confirmed planet (red) systems that harbor close-in giant planets (P < 10 days and RP > 4 R⊕). The left panel displays the binary separations and γ for the Kepler-like (Rp ≤ 4 R⊕ and a < 1 au) TOI and confirmed planet systems. The γ distribution histograms are provided in the background of all plots and scaled for easier visualization. We also show the best-fit theoretical γ distributions derived from HBM (gray).
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The minimum orbital distances of the close-in giant progenitors, with arrows representing the upper limit, vs. the 2D projected separation between the planet host and comoving companion in a Kozai–Lidov formation scenario. The progenitors must initially have large enough orbital periods to ensure that Kozai–Lidov oscillations induced by the comoving companion are not suppressed by GR precession. The right y-axis denotes the Kozai–Lidov timescale for the comoving binaries at their observed 2D separations. We assumed a fixed eccentricity of 0.5 for the comoving binary and fixed masses of 1 and 0.3 M⊙ for the planet host and the comoving binary, respectively. These assumptions permit a one-to-one correspondence between the left and right axes. We highlight and label the planets that have both large stellar obliquities λ and mutual inclinations γ in red.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The distributions of angles γ and normalized relative motion ﹩{\mu }^{{\prime} }﹩ for the TOI and confirmed planet systems that harbor close-in giant planets (P < 10 days and RP > 4 R⊕; right panel) and those with Kepler-like architectures (Rp ≤ 4 R⊕ and a < 1 au; left panel). The γ and ﹩{\mu }^{{\prime} }﹩ distributions appear uncorrelated.
Paper: Stellar Companions to TESS Objects of Interest: A Test of Planet–Companion Alignment
Authors: Aida Behmard, Fei Dai, and Andrew W. Howard
Figure caption: The sky-projected stellar obliquity λ and γ angles for the subset of 20 close-in giant planet systems in our sample with published λ values. We overplot the histogram of all close-in giants in our sample and scale it for easier visualization (blue). Close-in giants that are misaligned with respect to their host star (red region, λ > 30°) are often also misaligned with respect to their comoving companion (blue, 40 < γ < 140°).
Paper: Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No Evidence for Temporal Variation of the Spin–Orbit Angle
Authors: Keduse Worku, Songhu Wang, Jennifer Burt, Malena Rice, Xian-Yu Wang, Yong-Hao Wang, Steven S. Vogt, R. Paul Butler, Brett Addison, Brad Holden, Xi-Yan Peng, Zhen-Yu Wu, Xu Zhou, Hui-Gen Liu, Hui Zhang, Ji-Lin Zhou, and Gregory Laughlin
Figure caption: Phased light curve of XO-3b including 33 literature transits provided by previous works (Johns-Krull et al. 2008; Winn et al. 2008, 2009; Bonomo et al. 2017) and 12 new transits collected in this work. To estimate the system parameters, these light curves were simultaneously fitted with the radial-velocity measurements (Figure 3) as described in detail in Section 4. The orange solid line represents the best-fitting model to all of the data, and the residuals are plotted below.
Paper: Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No Evidence for Temporal Variation of the Spin–Orbit Angle
Authors: Keduse Worku, Songhu Wang, Jennifer Burt, Malena Rice, Xian-Yu Wang, Yong-Hao Wang, Steven S. Vogt, R. Paul Butler, Brett Addison, Brad Holden, Xi-Yan Peng, Zhen-Yu Wu, Xu Zhou, Hui-Gen Liu, Hui Zhang, Ji-Lin Zhou, and Gregory Laughlin
Figure caption: Light curves of XO-3b transits, obtained from the literature and as part of this work. The best-fitting models are overplotted as solid red lines in the left panel. The residuals are displayed in the right panel. Both light curves and residuals are sorted by observation date for clarity.
Paper: Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No Evidence for Temporal Variation of the Spin–Orbit Angle
Authors: Keduse Worku, Songhu Wang, Jennifer Burt, Malena Rice, Xian-Yu Wang, Yong-Hao Wang, Steven S. Vogt, R. Paul Butler, Brett Addison, Brad Holden, Xi-Yan Peng, Zhen-Yu Wu, Xu Zhou, Hui-Gen Liu, Hui Zhang, Ji-Lin Zhou, and Gregory Laughlin
Figure caption: The radial-velocity measurements of XO-3 from previous works (Hirano et al. 2011; Hébrard et al. 2008; Johns-Krull et al. 2008; Winn et al. 2009; Knutson et al. 2014; Bonomo et al. 2017; Garai et al. 2017) and from this work, marked as different colors and shown as a function of orbital phase. The best-fitting Keplerian orbit model (solid red line) is determined from the joint fitting of RVs and light curves. The residuals of the best fit, with an rms scatter σ = 267.90 m s−1, are shown in the bottom panel.
Paper: Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No Evidence for Temporal Variation of the Spin–Orbit Angle
Authors: Keduse Worku, Songhu Wang, Jennifer Burt, Malena Rice, Xian-Yu Wang, Yong-Hao Wang, Steven S. Vogt, R. Paul Butler, Brett Addison, Brad Holden, Xi-Yan Peng, Zhen-Yu Wu, Xu Zhou, Hui-Gen Liu, Hui Zhang, Ji-Lin Zhou, and Gregory Laughlin
Figure caption: Observed minus calculated midtransit times (O − C) for XO-3b, according to the updated linear ephemeris. The (O − C) = 0 reference is represented by a red solid line, and the red dashed line indicates the propagation of ±1σ errors of the updated linear ephemeris.
Paper: Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No Evidence for Temporal Variation of the Spin–Orbit Angle
Authors: Keduse Worku, Songhu Wang, Jennifer Burt, Malena Rice, Xian-Yu Wang, Yong-Hao Wang, Steven S. Vogt, R. Paul Butler, Brett Addison, Brad Holden, Xi-Yan Peng, Zhen-Yu Wu, Xu Zhou, Hui-Gen Liu, Hui Zhang, Ji-Lin Zhou, and Gregory Laughlin
Figure caption: A top-down view of the XO-3 system. Initial orbits of 300 test particles are evenly distributed over 1.3–7.5 mutual Hill radii with XO-3b. Orbits remaining after a 106 yr integration are shown in blue. All orbits lying within 3.5 mutual Hill radii of XO-3b have been destabilized. Among the unstable particles, 80% collide with XO-3 (red), and, as a consequence of XO-3b’s large mass, 20% are ejected (green).
Paper: Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No Evidence for Temporal Variation of the Spin–Orbit Angle
Authors: Keduse Worku, Songhu Wang, Jennifer Burt, Malena Rice, Xian-Yu Wang, Yong-Hao Wang, Steven S. Vogt, R. Paul Butler, Brett Addison, Brad Holden, Xi-Yan Peng, Zhen-Yu Wu, Xu Zhou, Hui-Gen Liu, Hui Zhang, Ji-Lin Zhou, and Gregory Laughlin
Figure caption: Left: phased transit light curves before the R-M measurement conducted by Hébrard et al. (2008). Right: phased transit light curves after the R-M measurement conducted by Winn et al. (2009). The best-fitting model for each data set is overplotted as a solid orange line. The two transit profiles are in good agreement.
Paper: Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No Evidence for Temporal Variation of the Spin–Orbit Angle
Authors: Keduse Worku, Songhu Wang, Jennifer Burt, Malena Rice, Xian-Yu Wang, Yong-Hao Wang, Steven S. Vogt, R. Paul Butler, Brett Addison, Brad Holden, Xi-Yan Peng, Zhen-Yu Wu, Xu Zhou, Hui-Gen Liu, Hui Zhang, Ji-Lin Zhou, and Gregory Laughlin
Figure caption: Spectroscopic radial velocities of XO-3 from Hébrard et al. (2008; left), Winn et al. (2009; center), and Hirano et al. (2011; right) as a function of orbital phase (minutes from midtransit), coupled with the best-fitting R-M models (red dashed line). The rms of the residuals from the three works, from left to right, is 40, 18, and 23 m s−1.
Paper: Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge
Authors: Kyeongsoo Hong, Jae Woo Lee, Jang-Ho Park, Hye-Young Kim, Chung-Uk Lee, Hyoun-Woo Kim, Dong-Jin Kim, and Cheongho Han
Figure caption: Comparison of the period change rates between ours and those of Pietrukowicz et al. (2017).
Paper: Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge
Authors: Kyeongsoo Hong, Jae Woo Lee, Jang-Ho Park, Hye-Young Kim, Chung-Uk Lee, Hyoun-Woo Kim, Dong-Jin Kim, and Cheongho Han
Figure caption: O–C diagrams of four CEBs, which have the highest decreasing (upper panels) and increasing (lower panels) period change rates in our samples, respectively.
Paper: Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge
Authors: Kyeongsoo Hong, Jae Woo Lee, Jang-Ho Park, Hye-Young Kim, Chung-Uk Lee, Hyoun-Woo Kim, Dong-Jin Kim, and Cheongho Han
Figure caption: I light curves of four CEBs. The blue and red circles represent the OGLE-III and OGLE-IV observations, respectively. In the left panels, the light curves were plotted using the linear ephemeris taken from the OGLE EBs catalog of Soszyński et al. (2016). In the right panels, the light curves were phased with the quadratic ephemeris determined in this study.
Paper: Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge
Authors: Kyeongsoo Hong, Jae Woo Lee, Jang-Ho Park, Hye-Young Kim, Chung-Uk Lee, Hyoun-Woo Kim, Dong-Jin Kim, and Cheongho Han
Figure caption: Histogram of the outer orbital periods (P2) of the 411 triple candidates.
Paper: Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge
Authors: Kyeongsoo Hong, Jae Woo Lee, Jang-Ho Park, Hye-Young Kim, Chung-Uk Lee, Hyoun-Woo Kim, Dong-Jin Kim, and Cheongho Han
Figure caption: Outer triple period (P2) vs. the inner binary period (P1) for the 411 triple star candidates (black circles) found in this study. The gray circles represent the 992 triple star candidates in the Galactic Bulge taken from Hajdu et al. (2019). The horizontal black, sloped blue (a typical outer eccentricity of e2 = 0.35) and green (e2 = 0.0) lines are boundaries of the regions where the amplitudes of the LTTE and dynamical effect may exceed ∼50 s or greater in amplitude to be detectable. These limits were calculated using the Equations (8) and (12) in the paper of Borkovits et al. (2016), where the parameters are adopted as mA = mB = mC = 1 M⊙, i2 = 60°, and ω2 = 90°. The dynamically unstable regions for outer eccentricities (e2) of 0.0 (cyan region) and 0.35 (orange region) were calculated using the equation (27) given in the paper by Borkovits et al. (2015), which is rewritten from the expression of Mardling & Aarseth (2001).
Paper: Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge
Authors: Kyeongsoo Hong, Jae Woo Lee, Jang-Ho Park, Hye-Young Kim, Chung-Uk Lee, Hyoun-Woo Kim, Dong-Jin Kim, and Cheongho Han
Figure caption: The histogram of the orbital period (upper panel) and the period change rate vs. the orbital-period diagram (lower panel) of the 13,820 CEBs. In the upper panel, the blue and red bars are represent the CEBs with the decreasing and increasing period change rates, respectively. In the lower panel, the black and red circles represent the 13,716 CEBs with parabolic variations and 104 CEBs with parabolic plus sinusoidal variations, respectively.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux
Authors: Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, and Bill Wohler
Figure caption: A TESS Sector 11 image colored by flux (see color bar) on top of a DSS image (gray scale). The red circle indicates TOI 1227, and the red box indicates the TESS aperture used for Sector 11 (the aperture varied between sectors). The TESS point-spread function in this region has an FWHM of approximately 1.9 TESS pixels. The large TESS point-spread function combined with a faint source meant that there were high levels of contamination around TOI 1227.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux
Authors: Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, and Bill Wohler
Figure caption: Goodman spectrum of TOI 1227 (black) and a template M5V dwarf from Kesseli et al. (2017). Because of extinction around TOI 1227 and imperfect flux calibration from Goodman, we fit out a second-order polynomial on the Goodman spectrum to better match the template. The Goodman spectrum is also higher resolution than the template (R of 5880 vs. 2000). The inset highlights the Li λ6708 line, which is absent in the spectrum of older stars like the template, but strong in TOI 1227’s spectrum.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux
Authors: Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, and Bill Wohler
Figure caption: Detection limits from the Zorro speckle imager for TOI 1227. Detection limits from the two narrowband filters (5620 Å and 8320 Å) are shown in blue and red, respectively. The inset shows the narrowband 8320 Å, reconstructed image.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux
Authors: Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, and Bill Wohler
Figure caption: Galactic heliocentric (XYZ) coordinates of 108 stars within the B subgroup of LCC (purple hexagons; Kerr et al. 2021), the A0 population of the Crux Moving Group (gray squares; Goldman et al. 2018), or stars identified using the FriendFinder algorithm restricted to ﹩{V}_{\tan ,\mathrm{off}}\lt 1﹩ km s−1 and within 10 pc of TOI 1227 (blue circles; Tofflemire et al. 2021). The planet host, TOI 1227, is marked with a red cross and is in all three lists. The significant overlap between these three selections reaffirms that these are all the same population, just selected using slightly different methods. For reference, we included a green circle that includes most of the known ϵ Cha members, highlighting that ϵ Cha is a separate and more compact population.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux
Authors: Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, and Bill Wohler
Figure caption: Galactic coordinates (l, b) of stars around TOI 1227, with arrows indicating the direction and magnitude of the proper motion for each star. Likely members of Musca (Section 3.1) are colored by their BP − RP color. All stars within 10 pc of TOI 1227 (excluding candidate members) are shown as gray arrows. TOI 1227 is thicker with a black outline.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux
Authors: Andrew W. Mann, Mackenna L. Wood, Stephen P. Schmidt, Madyson G. Barber, James E. Owen, Benjamin M. Tofflemire, Elisabeth R. Newton, Eric E. Mamajek, Jonathan L. Bush, Gregory N. Mace, Adam L. Kraus, Pa Chia Thao, Andrew Vanderburg, Joe Llama, Christopher M. Johns-Krull, L. Prato, Asa G. Stahl, Shih-Yun Tang, Matthew J. Fields, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Jacob Kamler, Richard P. Schwarz, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Dylan A. Owens, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Marshall C. Johnson, Reilly P. Milburn, Aaron C. Rizzuto, Samuel N. Quinn, Ronan Kerr, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Natalia M. Guerrero, Avi Shporer, Joshua E. Schlieder, Brian McLean, and Bill Wohler
Figure caption: CMD of stars in Musca (stars associated with TOI 1227), with symbols by the selection method or reference. We removed stars with poor astrometric fits from Gaia (RUWE > 1.5; Gaia Collaboration et al. 2021). TOI 1227 is marked as a red cross and lands within the tight sequence. The blue line indicates an empirical main sequence for reference (Pecaut & Mamajek 2013).