adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Left: CMD of sources within 35 pc and 3 km s−1 of TOI-1224. Points are color-coded by their velocity difference, and TOI-1224 is denoted as a pink star. Targets with a high RUWE (more likely to be binaries) are denoted as squares. Right: RVs of candidate members of MELANGE-5 compared to the value predicted assuming they have identical UVW to TOI-1224. RV data are extracted from Gaia DR3 and archival sources. The excess of points around zero is far above what is possible by chance and is far narrower than the velocity distribution of all solar neighborhood stars. Stars closer to zero RV difference are also statistically closer in tangential velocity. The excess of sources below (but near) zero may be due to uncertainties in TOI-1224’s velocity, with TOI-1224 landing slightly off-center of the association, or coincident alignment with other groups (see Section 4) or Galactic motions.
Paper: Investigation of Galactic Supernova Remnants and their Environment in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25 Using Radio Surveys
Authors: Tian-Xian Luo, Ping Zhou, Hao-Ning He
Figure caption: Blue: the histogram of distances of all known pulsars within 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25. Orange: the histogram of distances of known pulsars within the sky area covered by the molecular bubble, which is denoted as a green circle in Figure 4.
Paper: Investigation of Galactic Supernova Remnants and their Environment in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25 Using Radio Surveys
Authors: Tian-Xian Luo, Ping Zhou, Hao-Ning He
Figure caption: The THOR+VGPS continuum image (red) and the SuperCOSMOS Hα image (cyan). A yellow × sign denotes the potential pulsar of G29.38+0.10. The white dashed line shows the length of the Hα structure. The white dotted line shows the approximate position of the radio shell.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Detection limits from the speckle images of TOI-1224. The subpanel in the top right shows the narrowband 8320 Å reconstructed image.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Rotation periods of MELANGE-5 compared to rotation periods of benchmark open clusters. MELANGE-5 members are represented by red stars, and the shade indicates the quality of the rotation, with darker red (0) representing a clearly observed rotation in the light curve and lighter red (1) representing a questionable period. MELANGE-5 falls above the 120 Myr clusters and slightly below the 300 Myr clusters. The gray lines are the “mean” empirical isochrones fitted by Bouma et al. (2023) with ascending time intervals of 100 Myr, 200 Myr, and so on. The astrophysical scatter about these mean lines sets the empirical precision limit for this age-dating method.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: The TESS Sector 1 light curve (green points) is binned to 5 minute intervals and is overplotted with a GP for the stellar variability (black line). Only ttransit of planet b is modeled here. The transit times of the two planets are marked in pink for TOI-1224 b and purple for TOI-1224 c. Bottom: phase-folded light curve of planet b after the best-fit stellar variability model has been removed taken in filters TESS, z, and g  p . Data for TESS and z are binned into 10 and 5 minute bins, with the best-fit transit model illustrated by a black line.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: CMD of members of Theia 424 from Kounkel et al. (2020) compared to PARSECv1.2 solar metallicity models using a mixture model (Section 4.1.3). The green lines are 100 random draws from the fit posterior, and individual points are shaded by the probability that they are part of the main (single-star single-aged) population. The group is well described by a ≃90 Myr isochrone (black dashed line) with a visible binary sequence above and a small number of field interlopers below.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Lithium EWs of candidate members of MELANGE-5 as a function of Gaia color. The top axis shows the approximate T eff for reference. Points are color-coded based on their RV. Non- or weak detections are shown as arrows. Targets with RVs within 5 km s−1 of the predicted value are outlined in red. The predicted 200 Myr sequence from EAGLES is shaded.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: SED of TOI-1224 (red points) compared to the best-fit template spectra (black) and BT-SETTL model (blue). Horizontal errors on the observed photometry approximate the filter width. The synthetic photometry used to compare to the observed photometry is shown as green points. The bottom panel shows the residual in units of standard deviations.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: The spatial spread and velocity spread of MELANGE-5 (green) compared to the nearby associations, Crius 221 (purple), Theia 424 (pink), and Volans-Carina (yellow). The top row shows the galactic position (X, Y, and Z), and the bottom row shows the velocities (U, V, and W) for each population. MELANGE-5 (∼200 Myr) overlaps with Crius 221 (∼100 Myr) but does not intersect with Theia 424 or Volans-Carina. The position of TOI-1224 is marked with a green cross.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Posteriors from the MCMC fit for the parameters, period (P), planet-to-star radius ratio (R  P /R *), and impact parameter (b) for planet b (left) and planet c (right). Planet b was fit using MISTTBORN, and planet c was fit using juliet to account for the TTVs. In the histogram, the dashed lines indicate the 16th and 84th percentiles. Figure made with corner.py (Foreman-Mackey 2016).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Example CMD of MELANGE-5 (black circles) fit using a mixture model. Each point is shaded by the probability of being part of the primary population (the single-star single-aged group). The green lines are 100 random draws from the Markov chain Monte Carlo (MCMC) posterior. For reference, we included 400 and 150 Myr isochrones.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Stellar density from SED fitting (blue) compared to the stellar density from the transit fit (orange) assuming the eccentricity is 0. This is consistent with a low or zero eccentricity for TOI-1224 b, which is common for (older) multiplanet systems (Van Eylen et al. 2019).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Young (< 1 Gyr), transiting, multiplanetary systems that are members of a known association or a cluster as a function of its period (days). The leftmost circle in each row represents the host star, with the size of the marker proportional to the stellar radius and colored by its effective temperature (T eff). The circles to the right represent the planets in each system, with the size of the marker proportional to the planetary radius and colored by its equilibrium temperature (T eq). The systems are sorted in order of their age, with the youngest systems at the top and the oldest at the bottom. Data for these planets are listed in Table 9. TOI-1224 follows the intrasystem uniformity pattern (Weiss et al. 2018), as both planets, b and c, share comparable sizes.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Contour of all planets discovered by Kepler and K2 as a function of planet radius (R ⊕) and orbital period (days). Young (<700 Myr) transiting systems are colored by their approximate age in log space, derived from their respective host cluster or association. TOI-1224 b and c are outlined as stars and fall within the distribution of mature planets. These two planets stand out as rare finds within the age range of ∼200 Myr. Planet properties from NASA Exoplanet Science Institute (2020).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Phase-folded light curve of TOI-1224 c taken with TESS (green), ASTEP R (blue), LCO z  s  (red), and LCO g  p  (yellow). Transit numbers 0, 19, 58, 81, 85, 89, and 103 are arranged from top to bottom and offset for clarity. The best-fit transit model is overlaid as a black line. Circular points are data binned into 1.5 minute intervals.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Observed minus calculated (O − C) mid-transit times as a function of time for TOI-1224 c in minutes taken with TESS (green), ASTEP R (purple), LCO z  s  (red), and LCO g  p  (yellow). The gray dashed horizontal line represents a linear ephemeris.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: Injection/recovery test for TOI-1224. Each point represents an injected planet, with red points indicating an injected planet we failed to recover, while blue points are ones we recovered successfully. Only 20% of the injected planets are shown for clarity. The background is color-coded by the overall completeness in a given bin. Interestingly, the completeness right around the inner planet is only ≃20%.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association
Authors: Pa Chia Thao, Andrew W. Mann, Madyson G. Barber, Adam L. Kraus, Benjamin M. Tofflemire, Jonathan L. Bush, Mackenna L. Wood, Karen A. Collins, Andrew Vanderburg, Samuel N. Quinn, George Zhou, Elisabeth R. Newton, Carl Ziegler, Nicholas Law, Khalid Barkaoui, Francisco J. Pozuelos, Mathilde Timmermans, Michaël Gillon, Emmanuël Jehin, Richard P. Schwarz, Tianjun Gan, Avi Shporer, Keith Horne, Ramotholo Sefako, Olga Suarez, Djamel Mekarnia, Tristan Guillot, Lyu Abe, Amaury H. M. J. Triaud, Don J. Radford, Ana Isabel Lopez Murillo, George R. Ricker, Joshua N. Winn, Jon M. Jenkins, Luke G. Bouma, Michael Fausnaugh, Natalia M. Guerrero, Michelle Kunimoto
Figure caption: TESS image around TOI-1224 from Sector 13. The red region shows the aperture used for extracting the light curve. Points indicate other sources detected from Gaia scaled in size by their contrast. Other than TOI-1224, only a single Gaia source is within the aperture, and it is too faint to reproduce the transits. Figure made with tpfplotter (Aller et al. 2020).
Paper: Climbing the Cliffs: Classifying Young Stellar Objects in the Cosmic Cliffs JWST Data Using a Probabilistic Random Forest
Authors: B. L. Crompvoets, J. Di Francesco, H. Teimoorinia, T. Preibisch
Figure caption: The spectral indices for the YSOs which form the basis for our training set (maroon), an example of how the EVT method (dotted black line) or SMOTE method (solid black line) of data augmentation can cause variation in spectral index, and the full range of spectral indices throughout the entire SPICY catalog (gray), normalized for comparison. Gray dashed lines indicate the typical cuts in spectral index applied to separate classes (e.g., Dunham et al. 2015; Kuhn et al. 2021). The associated class labels are also marked above their respective regions (Class II ≡  “C II”).
Paper: Climbing the Cliffs: Classifying Young Stellar Objects in the Cosmic Cliffs JWST Data Using a Probabilistic Random Forest
Authors: B. L. Crompvoets, J. Di Francesco, H. Teimoorinia, T. Preibisch
Figure caption: The region of NGC 3324 imaged by JWST. Stiff peaks along the Gum 31 H II region are formed by stellar winds originating from the massive stars in NGC 3324. This color image is made from six NIRCam filters: F444W (red), F335M (orange), F470N (yellow), F200W (green), F187N (cyan), and F090W (blue). Image credit: NASA, ESA, CSA, and STScI.
Paper: Climbing the Cliffs: Classifying Young Stellar Objects in the Cosmic Cliffs JWST Data Using a Probabilistic Random Forest
Authors: B. L. Crompvoets, J. Di Francesco, H. Teimoorinia, T. Preibisch
Figure caption: A comparison of the F1 scores for the validation set of the PRF (solid red line), an RF filled via copulas (blue dashed line), and an RF filled with thermal noise (purple dashed line) as a function of the amount of missing data.
Paper: Climbing the Cliffs: Classifying Young Stellar Objects in the Cosmic Cliffs JWST Data Using a Probabilistic Random Forest
Authors: B. L. Crompvoets, J. Di Francesco, H. Teimoorinia, T. Preibisch
Figure caption: All cYSOs in this region matched to JWST sources from Preibisch et al. (2014, black X’s), Ohlendorf et al. (2013, black circles), Kuhn et al. (2021, black squares), Reiter et al. (2022, black hexagons), and with our own cYSOs marked in varying shades of red based on their probability of being a YSO.