adsabs/AstroCLIMB huggingface dataset:
Paper:  Gaspery: Optimized Scheduling of Radial Velocity Follow-up Observations for Active Host Stars
Authors: Christopher Lam, Megan Bedell, Lily L. Zhao, Arvind F. Gupta, Sarah A. Ballard
Figure caption: The uncertainty on the planet RV semi-amplitude, σ  K , as a function of the number of observations of a single AU Mic b-like planet transiting an AU Mic-like star, under a white noise regime (blue) and correlated noise regime (orange). We fix the observing cadence at one observation per night, every night. For reference, we overlay the Fisher information-derived σ  K  curves against the analytic ﹩\sqrt{2/{\rm{N}}}﹩ relation between the number of observations and σ  K  (green).
Paper:  Gaspery: Optimized Scheduling of Radial Velocity Follow-up Observations for Active Host Stars
Authors: Christopher Lam, Megan Bedell, Lily L. Zhao, Arvind F. Gupta, Sarah A. Ballard
Figure caption: Sensitivity map for a given fixed budget of 30 observations of an AU Mic b-like planet around an AU Mic-like star. The x-axis denotes the number of consecutive days of observation, and the y-axis denotes the number of consecutive days not observing. Strategies are outlined in red if they finish outside the 2023A NEID observing season. The color bar is normalized to a log scale in order to better illustrate differences among strategies.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Emissivity plots showing the line formation region of C IV λ λ 5802-12 (in red), and C III λ5696 (in blue) in the model atmosphere.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Radiative acceleration (Γrad, in violet) and electron-scattering (or Thomson-scattering) acceleration (Γelec, in maroon), relative to the gravitational acceleration in the stratified layers of the atmospheric model, are shown.
Paper:  Gaspery: Optimized Scheduling of Radial Velocity Follow-up Observations for Active Host Stars
Authors: Christopher Lam, Megan Bedell, Lily L. Zhao, Arvind F. Gupta, Sarah A. Ballard
Figure caption: MCMC fits for the stellar, planet, and combined signals for three different observing strategies. Blue curves depict the best-fit inferred signals; light red curves illustrate the “ground truth” signals from which the training (black points) and validation (red points) sets are drawn. The MCMC model is fit only on the training data, which follows the observing strategy. The shorter subplots show the corresponding residuals for each strategy. The first set of two rows corresponds to a strategy of observing once per night every night (first row in Table 2). The second two rows correspond to a strategy of observing once per night every other night (second row in Table 2). The last two rows correspond to a strategy of observing once per night every five nights (fourth row in Table 2).
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Clusters in the UV-bright arm of NGC 1614. Left: BVI HST color image with clusters identified by the magenta circles. Middle: NUV – B vs. V − I color–color diagram of clusters brighter than m  V  ≤ 23 shown in black. The median color of these clusters is shown as the magenta diamond. An A  V  = 1.0 reddening vector is shown in the upper right corner. Right: age–mass diagram of clusters within the UV-bright arm. The vertical dashed lines are at 25 and 250 Myr.
Paper: uGMRT Survey of EXoplanets Around M-dwarfs (GS-EXAM): Radio Observations of GJ 1151
Authors: Mayank Narang, Manoj Puravankara, H. K. Vedantham, C. H. Ishwara-Chandra, Ayanabha De, Himanshu Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya, B. Shridharan, Vinod C. Pathak, Mihir Tripathi
Figure caption: The uGMRT image (blue contours) of the GJ 1151 field at 218 MHz overlaid on the ZTF zg band image (epoch J2021.17). The red circle marks the position of GJ 1151 at the time of observations (epoch J2021.21), and the green circle marks the position of the radio source detected with LOFAR (epoch J2014.454). The rms achieved for each of the observations are mentioned in the top-left corner. The contours plotted are 5, 7, and 10 × σ. The beam is shown as a cyan ellipse at the bottom-left corner.
Paper: uGMRT Survey of EXoplanets Around M-dwarfs (GS-EXAM): Radio Observations of GJ 1151
Authors: Mayank Narang, Manoj Puravankara, H. K. Vedantham, C. H. Ishwara-Chandra, Ayanabha De, Himanshu Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya, B. Shridharan, Vinod C. Pathak, Mihir Tripathi
Figure caption: The uGMRT image (blue contours) of the GJ 1151 field at 400 MHz overlaid on the ZTF zg band image (epoch J2021.17). The red circle marks the position of GJ 1151 at the time of observations (epoch J2021.21), and the green circle marks the position of the radio source detected with LOFAR (epoch J2014.454). The rms achieved for each of the observations are mentioned in the top-left corner. The contours plotted are 5, 7, 10, 15, 30, and 50 × σ. The beam is shown as a cyan ellipse at the bottom-left corner.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: The posterior probability distributions for the lens system physical parameters: planetary companion mass (upper left), host mass (upper right), 2D projected separation (lower left), and lens distance (lower right). The vertical black line shows the median of the probability distribution for each parameter. The central 68% of each distributions is shown in dark blue, with the remaining central 95% shown in light blue.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: The mass–distance relation for MB07192L with constraints from the lens flux measurement in HST V (blue), HST I (green), and Keck K (red). Dashed lines show the 1σ error bars for each passband. The solid teal region shows the mass–distance relation calculated using the microlensing parallax measurement (π E), and the solid brown region shows the mass–distance relation calculated using the angular Einstein radius measurement (θ E).
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Comparison of model parameter distributions from the light-curve photometry only (light gray) and light-curve photometry plus HST/Keck imaging constraints (black). The two cases shown are for the s < 1, u 0 < 0 model. The constraints from the high-resolution imaging are tightened most for the north and east components of the microlensing parallax (π E,N, π E,E) as well as the source radius crossing time (t *). The median values given in the title headings (above each histogram) are for the constrained light curve and imaging model. All other model parameters give consistent distributions between the two cases.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Top left: the 2023 HST I-band stack image created from two individual exposures from the Snapshot Program. The target is indicated with a yellow box. Top right: zoomed image of the target, with the two points indicating the best-fit positions for the two stars from the multi-star PSF fitting. We note the unrelated neighbor star has moved closer to the target(s) by ∼1 pixel between the 2012 and 2023 HST data. Bottom left: the residual image from a single-star PSF fit, showing a strong signal of the blended lens (source). Bottom right: residual image for the simultaneous two-star PSF fit, showing a smoother subtraction with Poisson noise remaining as well as systematics due to the less characterized PSF model. The color bar represents the pixel intensity (counts) seen in the top-right and bottom-left/bottom-right panels.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Left: the MCMC distribution for π E from the light-curve modeling without any constraint from the high-resolution imaging. Right: the MCMC distribution for π E from the light-curve modeling with the inclusion of high-resolution imaging constraints. The color bar represents the χ 2 differences from the best-fit light-curve model. The two components of the relative proper motion that were measured by HST and Keck allow the north component, π E,N, to be tightly constrained.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Similar to Figure 4, but for the HST near-IR passbands (F125W − J band, F160W − H band). The purple and orange points indicate the inferred source and lens colors and magnitudes, respectively, with associated uncertainties. MIST isochrones for the observed bulge population (black curve) and foreground disk population (gray curve) are shown.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Spectral energy distribution measurements for the source (red) and lens (blue) for MB07192 in the V, I, and K bands. The model spectra for the source star (solid line) and lens star (dashed line) are from Kurucz et al. (1993) while the absorption law of Wang et al. (2019) is adopted.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: (a) Top: damping timescales for our toy model, calculated using Equations (1) and (2), as a function of stellar age, with τ  a  in black and τ  λ  in blue. Middle: model for the evolution of orbital period, P (shown by the black line). Bottom: model for the evolution of obliquity, λ (shown by the blue line). These models were computed assuming that the damping efficiency is the same for both parameters. The red region indicates the runaway inspiral regime. (b) Same as panel (a), but with different efficiencies for the damping of P and λ, prescribed by the tidal quality factor ﹩{Q}_{\star }^{{\prime} }﹩. This model has a difference in effective tidal quality factor of ﹩\delta \mathrm{log}{Q}_{\star }^{{\prime} }=4﹩.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Distribution of hot Jupiter obliquities as a function of stellar effective temperature, T eff. Blue points indicate cool (<6250 K) hosts, and red points indicate hot (>6250 K) hosts. The vertical dashed black line marks the Kraft break. Subgiant hosts are marked by large circles with black outlines, and all other points are main-sequence hosts. The distributions on the far right of the plot show the kernel densities of each sample, corresponding to color. The black line shows a model for the post-main-sequence realignment of a hot Jupiter. This model shows a possible pathway from the hot, misaligned population to the observed cool, well-aligned population.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: H-R diagram of stars hosting planets with measured sky-projected obliquities. Main-sequence host stars are marked by circles, while subgiant hosts are shown as stars. The color of each point indicates the sky-projected obliquity, λ. Dotted black lines show our stellar evolution models fit to each of our host stars and trace back to their ZAMS location.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Measurement of the Doppler shadow signal for TOI-1181 b from line profile residuals in the HIRES spectra. The horizontal dotted line marks the ingress and egress of the transit; the vertical dotted line indicates approximately the rotational broadening of the star (﹩v\sin i﹩). The planetary shadow is a diagonal pattern moving from the blueshifted to the redshifted part of the stellar disk. This is consistent with a well-aligned orbit seen in the RM measurement.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Regions of expected realignment given different values of ﹩\delta \mathrm{log}{Q}_{\star }^{{\prime} }﹩. The x-axis shows the initial orbital period of the planet (at ZAMS), and the y-axis shows the planet mass. Inside the shaded contours, realignment without engulfment is expected. Below the contours λ is not damped efficiently enough to realign, and above the contours the planet enters runaway inspiral.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Planet radius vs. incident flux received for planets drawn from the literature (circles) and planets in our sample (stars). The color bar indicates planet mass, and the dotted vertical line shows the empirical threshold above which planet inflation is observed.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Fractional stellar radius, R CZ/R ⋆, as a function of stellar age. On the y-axis, 0 represents the center of the star and 1 is its surface. The dashed line shows when the star was above the Kraft break (≥6250 K), and the solid line shows when the star was below the Kraft break (<6250 K). The shaded regions show the range of estimated stellar ages from isoclassify.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Same as Figure 5, but for TOI-6029 b.