adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Relative RVs of HD 984 from HPF (top panel; this work) and HARPS (bottom panel; Grandjean et al. 2020). HPF RVs from individual exposures are shown in gray, while the final, binned measurements for each visit are shown in red. No clear trends are observed, which may in part be caused by large scatter owing to HD 984's young age and early spectral type. Nevertheless, their inclusion in the orbit fit places constraints on the radial acceleration induced by HD 984 B.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: HGCA proper motion measurements of HD 984 in R.A. (top) and decl. (bottom). Three proper motions are available from the HGCA: the individual Hipparcos and Gaia proper motions and an average proper motion from the difference in sky position between the two missions. For HD 984, the position difference proper motion is the most precise, followed by the Gaia epoch. The slope of these points indicates the time-averaged tangential (sky-plane) acceleration induced by the star’s companion.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Reduced χ 2 values from orbit fits to the ensemble of relative astrometry for HD 984 as a function of increasing astrometric jitter. An astrometric jitter of σ jit = 3.17 mas yields ﹩{\chi }_{\nu }^{2}=1.0﹩. We therefore inflate the relative astrometry uncertainties by this amount for the final joint orbit fit.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Orbit fit of HD 984 B compared to the relative astrometry (top panels), HGCA acceleration of its host star (middle panels), sky-projected orbit (bottom left), and RVs (bottom right). The gray curves show 150 randomly drawn orbits from the MCMC chains. The maximum-likelihood orbit is highlighted in black. In the RV plot, the red points are HPF RVs, while the blue points are HARPS RVs. The gray error bars in the relative astrometry plots are the inflated uncertainties, while the blue error bars are the original uncertainties. The gray error bars in the RV plot incorporate the jitter terms from the best-fit orbit (σ HARPS and σ HPF), while the blue and red error bars are the original instrumental uncertainties.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Joint posterior distributions for select parameters in the orbit fit of HD 984 B. Diagonal panels show the marginalized posteriors for each parameter. The dynamical mass of HD 984 B is 61 ± 4 M Jup, placing the companion firmly in the brown dwarf regime.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Dynamical mass of HD 984 B (top distribution) compared to inferred mass distributions for a variety of hot-start evolutionary models. Mass distributions are assembled for a given model by sampling the luminosity and age distributions of HD 984 B 106 times, and then linearly interpolating the model grid to produce a corresponding mass for each trial. For the Fernandes et al. (2019) models, the predicted mass distributions are limited to >57.6 M Jup, which is the lowest-mass track computed in their study (see Figure 13). These inferred masses are thus overestimates of the true model predictions for these two grids. The median and 68.3% confidence interval are shown for each complete distribution. Each model prediction is broadly consistent with our measured dynamical mass.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Predicted ages of HD 984 B based on the dynamical mass and luminosity for a variety of hot-start evolutionary models. Ages are inferred for a given model by sampling the luminosity and dynamical mass distributions of HD 984 B 106 times, and then linearly interpolating the model grid to produce a corresponding age for each trial. Due to the partial coverage of the Fernandes et al. (2019) grids over HD 984 B’s luminosity and mass (see Figure 13), the corresponding predicted ages are somewhat overestimated for these models. Note that there is not a strict minimum age for these two models because the inferred age is luminosity dependent. Altogether, hot-start models predict a young age of ∼50–90 Myr.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Isomass tracks from each evolutionary model considered in this study compared with HD 984 B’s age and luminosity. We adopt a linearly uniform distribution from 30–200 Myr for HD 984 B’s age and a Gaussian distribution for its luminosity. Contours of 1σ, 2σ, and 3σ are shown in blue. The color of the model tracks corresponds to their mass. The transparency and thickness of the tracks is related to the dynamical mass posterior probability density. The narrow dynamical mass distribution (61 ± 4 M Jup) means that only a few model tracks available from these grids appear thick in each panel. Note that the Fernandes et al. (2019) models only partially cover the luminosity, age, and dynamical mass of HD 984 B.
Paper: A Search for Planet Nine using the Zwicky Transient Facility Public Archive
Authors: Michael E. Brown, Konstantin Batygin
Figure caption: The V magnitude at which there is a 95% or higher probability that a moving object would be detected seven or more times in the first 3 yr of the ZTF public survey. The Mollweide equal-area projection is centered at R.A. = 180° and decl. = 0° with R.A. increasing toward the left. The path of the ecliptic and ±15° of the galactic plane are highlighted. For much of the sky a uniform limit of V ∼ 20.5 is attained, with slightly greater depth north of celestial equator. Despite the high density of stationary stars, the northern galactic plane has no worse depth than any other region of the sky. The higher density in the southern galactic plane and the lower declinations make this region the least well-covered. At high-ecliptic latitudes the small number of asteroids prevents accurate calculation of the limits.
Paper: A Search for Planet Nine using the Zwicky Transient Facility Public Archive
Authors: Michael E. Brown, Konstantin Batygin
Figure caption: An example object from our Planet Nine reference population with a current distance of 264.8 au is predicted to have been detected 50 times in the ZTF survey. (a) Seen from the Earth, these detections make three loops over the three year survey period. (b) Transformed to heliocentric coordinates at the correct assumed distance (black), the object travels in a straight line at a constant speed. With an incorrect assumed distance of 263.2 au (red) or 270.3 au (green) deviations to the straight line motion can be seen.
Paper: A Search for Planet Nine using the Zwicky Transient Facility Public Archive
Authors: Michael E. Brown, Konstantin Batygin
Figure caption: The speed in heliocentric longitude and in heliocentric latitude to travel from the first point in the orbit to each of the other 49 for our synthetic object shown in Figure 2. If the correct distance of 264.8 au is assumed, the speeds to all data points are nearly identical (black). With an incorrect assumed distance (263.2 au, red, and 270.3 au, green, as in Figure 2), the cluster of inferred speeds is larger. Our algorithm finds all clusters within the ranges of selected values of ﹩{\rm{\Delta }}\dot{\alpha }﹩ and ﹩{\rm{\Delta }}\dot{\beta }﹩ shown and would successfully identify all red (and black) detections as clustered. With the incorrect distance assumed for the green cluster, many of the points would not be identified.
Paper: A Search for Planet Nine using the Zwicky Transient Facility Public Archive
Authors: Michael E. Brown, Konstantin Batygin
Figure caption: Limits to the detection of the Planet Nine reference population in the ZTF data. Across the entire sky 91% of the brightest objects are detected. If we exclude areas south of −25° decl., 94% are detected, and if we exclude the poorly observed southern hemisphere galactic plane region, 100% of the bright objects are detected.
Paper: A Search for Planet Nine using the Zwicky Transient Facility Public Archive
Authors: Michael E. Brown, Konstantin Batygin
Figure caption: Detection limits across the Planet Nine search region determined from the search for objects from the Planet Nine reference population injected into the data stream. The geometry of the project is identical to that of Figure 1. The dark blue regions in the southern hemisphere are areas not covered by ZTF.
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Spectral energy distribution of TOI 1842. 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 Kurucz atmosphere model (black).
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Zorro speckle observations of TOI-1842 obtained at 562 and 832 nm. The lines (red: 832 nm; blue: 562 nm) represent the 5σ contrast levels reached, revealing that no companion star is detected from the diffraction limit (17 mas) out to 1.″2 within a Δ mag of 4 to 7.5. The inset shows the 832 nm reconstructed speckle image and has north up and East to the left.
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: TLS power spectra of the detrended TESS PDCSAP light curve of Sector 23 and LCOGT data. Horizontal dashed lines indicates the signal detection efficiency power level of 5.7, 7.0, and 8.3, which corresponds to the TLS false-positive rate of 10%, 1%, and 0.1%. The strongest TLS power appears at 9.57 days, the remaining significant peaks are the low-frequency harmonics of the transit signal.
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Top panel: window function power spectrum of the combined Doppler data for TOI-1842. Middle panel: GLS power spectra of the Doppler data of TOI-1842. Horizontal dashed lines indicate GLS false-positive thresholds of 10%, 1%, and 0.1%. A significant periodic signal is detected at a period of 9.34 days, which is induced by TOI-1842b. The other significant signals near ∼10.8, 7.10, and 1.12 days are aliases of the window function and the planetary signal. Bottom panel: same as above panel, but for the RV residuals of the best joint model of TOI-1842.
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Transit photometry data and model fit for TESS (blue, Sector 23), LCOGT data from SAAO (red), and CTIO (green and magenta). The transit model (black solid line) is constructed jointly with precise Doppler data as described in Section 4.2.
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Radial-velocity data and model fit for TOI-1842. Top: complete time series and joint fit model including a linear trend. Bottom: phase-folded RV data, with each of the four instruments individually highlighted (with heavier points) in each subpanel for clarity. Left to right subpanels: MINERVA-Australis Telescopes 1 (blue), 4 (red), 5 (green), and NRES/SAAO (purple).
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Planetary density as a function of orbital distance a/R * for 410 hot Jupiters. Only 37 hot Jupiters have bulk densities smaller than TOI-1842b (starred in this plot).
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Estimated atmospheric scale height vs. J magnitude for 410 giant planets (R  p  > 0.75 R J). With a scale height of 893 km, TOI-1842b is an attractive target for atmospheric characterization. Only WASP-76b (West et al. 2016) presents a larger scale height and a brighter host star.
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Incident irradiation received by TOI-1842b over the course of the host star evolution. Assuming no tidal modification of the orbit of the planet, TOI-1842b is now receiving 30% more incident irradiation (∼550 F ⊕) than it did when the host star settled on the main sequence.
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Planet radius vs. mass (in Jupiter units) for well-characterized Saturns, color coded by incident flux in terms of the flux received by Earth (F ⊕). TOI-1842b is marked as a large star. The dashed line at 1.2  R J denotes the approximate maximum radius for uninflated planets, as given by Lopez & Fortney (2016).
Paper: TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
Authors: Robert A. Wittenmyer, Jake T. Clark, Trifon Trifonov, Brett C. Addison, Duncan J. Wright, Keivan G. Stassun, Jonathan Horner, Nataliea Lowson, John Kielkopf, Stephen R. Kane, Peter Plavchan, Avi Shporer, Hui Zhang, Brendan P. Bowler, Matthew W. Mengel, Jack Okumura, Markus Rabus, Marshall C. Johnson, Daniel Harbeck, René Tronsgaard, Lars A. Buchhave, Karen A. Collins, Kevin I. Collins, Tianjun Gan, Eric L. N. Jensen, Steve B. Howell, E. Furlan, Crystal L. Gnilka, Kathryn V. Lester, Rachel A. Matson, Nicholas J. Scott, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Alexander Rudat, Elisa V. Quintana, David R. Rodriguez, Douglas A. Caldwell, Samuel N. Quinn, Zahra Essack, Luke G. Bouma
Figure caption: Relative atmospheric scale height (H/R  p  ) vs. planet mass for well-characterized Saturns. TOI-1842b is marked as a large star, and is among the most favorable targets in this mass regime.
Paper: Detection of Ongoing Mass Loss from HD 63433c, a Young Mini-Neptune
Authors: Michael Zhang, Heather A. Knutson, Lile Wang, Fei Dai, Leonardo A. dos Santos, Luca Fossati, Gregory W. Henry, David Ehrenreich, Yann Alibert, Sergio Hoyer, Thomas G. Wilson, Andrea Bonfanti
Figure caption: HST/STIS spectra for planet c (left) and planet b (center and right for the earlier and later observations). Flux increases from dark blue to yellow. The white horizontal gap represents the seven to nine orbit hiatus due to the South Atlantic Anomaly (SAA) crossing. Gaps due to Earth occultation are not shown to avoid visual distraction; the y-axis is therefore not strictly accurate because it assumes time increases uniformly from spectrum to spectrum. The horizontal dashed black lines indicate the beginning and end of the white-light transit. The region between the blue (red) vertical lines is what we define as the blue (red) wing. They correspond to [−140, −10] km s−1 and [100,200] km s−1.
Paper: Detection of Ongoing Mass Loss from HD 63433c, a Young Mini-Neptune
Authors: Michael Zhang, Heather A. Knutson, Lile Wang, Fei Dai, Leonardo A. dos Santos, Luca Fossati, Gregory W. Henry, David Ehrenreich, Yann Alibert, Sergio Hoyer, Thomas G. Wilson, Andrea Bonfanti
Figure caption: Lyα light curves for planet c (left) and b (right), in the red and blue wings, compared to the predictions from our 3D hydrodynamic model. For b, the solid circles represent the first visit, and the open circles represent the failed second visit. The error bar for each orbit is its photon noise. The gray region represents the white-light transit.