adsabs/AstroCLIMB huggingface dataset:
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Time evolution of four estimates of the semimajor axis (lower panels) and the eccentricity (upper panels) for Nix (left panels) and Hydra (right panels) for calculations with f  H  = 1.1. Other satellites have their nominal masses. The legends in the lower panels map colors to each estimate. The upper panels use the same color scheme as the lower panels. In each panel, estimates derived from the restricted three-body theory yield the best results for a and e.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: As in Figure 7, for model Pluto–Charon satellite systems with a factor f  N,H  times the nominal mass for either Nix (f  N  > 1, purple dots) or Hydra (f  H  > 1, orange dots) and nominal masses for the other satellites. Blue dots indicate lifetimes of systems with the nominal masses for all satellites and one or more ejections. Orange stars indicate systems with f  H  > 1, where Kerberos has e and ı much larger than derived from HST observations. For completeness, we include blue (orange) triangles to represent the range of lifetimes for eight (one) ongoing calculations with the nominal masses for all four satellites (with the nominal masses for Styx, Nix, and Kerberos, and f  H  times the nominal mass for Hydra), where the system parameters still match orbital fits to HST observations. More massive satellite systems have shorter lifetimes.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Time variation of e free and ı for Kerberos (lower panel, from the calculation shown in the lower panel of Figure 2) and Styx (upper panel, from the calculation shown in the upper panel of Figure 2). In the lower panel, the orbital inclination of Kerberos is approximately constant for nearly 2 Gyr and then rises abruptly just before Kerberos is ejected. In the upper panel, the inclination of Styx begins to rise when e reaches a maximum level and then finds a plateau as e returns to a stable value. Once e rises again, ı drops; Styx is then ejected.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Lifetime of model Pluto–Charon satellite systems as a function of the mass ratio f for different f  S,K . The legend indicates the adopted mass ratio f  S  = f  K  for the masses of Styx and Kerberos relative to their nominal masses. For each calculation, Nix and Hydra have their nominal masses multiplied by the factor f; Styx and Kerberos have their nominal masses multiplied by f*f  S,K . For f = 1.5–2, lifetimes for systems with larger mass ratios for Styx and Kerberos (e.g., f  S,K  = 2 or 3) have shorter lifetimes.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Lifetime of model Pluto–Charon satellite systems as a function of the mass ratio factor f. Satellites have masses f times larger than the nominal masses listed in Table 1. Black dots indicate lifetimes for systems with ejections of either Styx or Kerberos. Gray triangles represent current lifetimes for eight ongoing calculations with f = 1.0, which we include for completeness. Some points have been adjusted vertically or horizontally for clarity. More massive satellite systems typically have shorter lifetimes.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Expanded view of the time evolution of the barycentric distance for Styx and Nix from the top panel of Figure 2, where f  H  = 1.1. Other satellites have their nominal masses. The light tan curve shows the orbit of Nix. For the orbit of Styx, the dark purple curve plots r  gc ; q and Q are shown for the basic geometric model (light green), the geometric solution from the restricted three-body problem (blue), and for the model for e free (light purple). The basic geometric values have a larger excursion in the orbit than values derived from the restricted three-body problem.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Ejection diagram for calculations with f  N  > 1 (lower panel) and f  H  > 1; other satellites have their nominal masses. Letters on the y-axis correspond to the satellites, with “S” for Styx, “N” for Nix, “K” for Kerberos, and “H” for Hydra. Nix is never ejected. Hydra ejections only occur in very massive systems. Kerberos is usually ejected when Hydra is massive. A massive Nix ejects either Styx or Kerberos roughly half of the time.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Cumulative distribution of the fractional time delay between the time when ı first rises above 0.01 and the time of ejection. In systems where Kerberos is ejected (orange curve), ı typically becomes larger than 0.01 just prior to ejection. When Styx is ejected, ı is often large well before ejection.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: The results of our standard Doppler cross-correlation analysis for our combined data sets, using models with the T-P profile from Figure 3. The left panel shows the cross-correlation map, where the planet’s radial velocity trail is visible as a curved diagonal line starting from the upper left to the lower right. The stellar pulsations are also visible. The region between the white horizontal lines is not included in our later analysis, so as to avoid regions where the pulsations and planetary signal begin to overlap. The center panel shows the same cross-correlation map shifted to the planet’s velocity, where the planetary signal now forms a straight vertical line. The right panel shows the K p−v sys map, where we have avoided summing over the orbital phases contaminated by stellar pulsations. The black lines intersect at the map’s peak (K p = 222.1 km s−1 and v sys = −6.5 km s−1), which has a S/N of 9.0.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: The conditional (2D) and marginalized (1D) likelihood distributions for our combined ESPaDOnS and HDS results, using models with the T-P profile from Figure 3. The dotted lines shown the median values for each distribution, with the exception of C, which shows the lower limit estimated from the 84th percentile of the distribution.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: Comparison of our recovered phase offset (top) and day–night contrast (bottom) to their injected values for each simulation, plotted as the difference between the recovered and injected values. For the phase offset we use the median of the marginalized distribution ±1σ, while for the contrast we use only the lower limit, taken as the 84th percentile of the bounded distribution. On the x-axis we label the simulations as they appear in Table 3. The light blue, white, and dark purple points show the results for injected models with phase offsets of θ = −12.°8, 0°, and +28.°7, respectively. The injected contrast is kept at C = 0.99 in all cases.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: An example of the planetary emission model with ﹩{\mathrm{log}}_{10}\mathrm{VMR}=-4﹩, to which different filtering methods have been applied. In the top panel we have only convolved the model to the resolution of the ESPaDOnS data and calculated the planet-star flux ratio. In the center panel we have additionally applied a minimum window filter with a window of 4 Å to remove the planetary continuum. In the bottom panel we have instead applied a high-pass Butterworth filter to the model from the top panel, which better accounts for the effect of SYSREM on the planetary signal.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: The conditional (2D) and marginalized (1D) likelihood distributions for our simulation ESP750, with an injected phase offset of 28.°7. The dotted lines shown the median values for each distribution, with the exception of C, which shows the lower limit estimated from the 84th percentile, and log10VMR, which shows the peak, since these distributions are non-Gaussian. The solid lines indicate the injected value for each parameter.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: The data reduction process as described in Section 3, applied to a single order from our second night of observations with ESPaDOnS. (a): the raw data following the initial reduction pipeline at the telescope. (b): results of cosmic ray and blaze correction. (c): resulting spectra after four iterations of SYSREM (Section 3.1). (d): the standard deviation of each data point in the reduced spectra.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: An example of the model Fe I emission spectra we use in our analysis with ﹩{\mathrm{log}}_{10}\mathrm{VMR}=-4.0﹩ (left) and our calculated T-P profile (right).
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: Orbital phases covered during our observations of WASP-33b (Table 1). The ESPaDOnS and HDS observations are shown in dark purple and light blue, respectively, and we have shifted the lines radially so that observations with overlapping phases are distinguishable. The gray shaded region indicates the portion of the phase curve we exclude from our analysis due to contamination from stellar pulsations (see Section 5.1).
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: Incident flux received by the planet vs. planet radius. Planets discovered by TESS are marked by stars, while those discovered by different instruments are marked by points. TOI-2184b is the star outlined in pink, with the estimated main-sequence position shown by the pink point connected with a dashed line. The vertical dashed line shows the Demory & Seager (2011) threshold for inflation.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: Planet mass vs. planet radius for confirmed Jovian exoplanets. Confirmed planets discovered by TESS are shown as black points while planets discovered by other telescopes are shown in gray. The colored lines show models by Freedman et al. (2014). These models do not account for planetary inflation, which explains the large radii of the many planets which fall above these curves. TOI-2184b is marked by the red star, and the shaded regions represent the 1 and 2σ confidence intervals.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: One-page vetting summary for TOI-2184b used to identify the transit signal.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: Light curve of TOI-2184 folded at a period of 6.90683 ± 0.00009 days. The detrended photometry is shown in gray with the binned photometry overplotted in blue. The fit transit model is the solid black line in the top panel, and the bottom panel shows the residuals between the light curve and transit model. The slightly positive out-of-transit values in the residuals are a remnant of the trend seen in Figure 3.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: Phase-folded radial velocity (RV) measurements of TOI-2184. The bottom panel is the residuals after subtracting the median RV model from the data. The solid black line shows the best fit to the RV. The blue lines each represent a single realization of the model drawn from the sampled posterior distribution, with 500 samples shown in total.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: Posterior distributions and correlations between parameters in our orbital model. The bimodal distribution for the argument of periastron ω is due to the uncertainty in whether the planet is approaching or receding from periastron crossing during transit.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: All time-series observations of TOI-2184b used in this analysis, including photometry and radial velocity (RV) measurements, plotted over time. The observations have independent y-axes: photometry plotted in normalized flux units on the left y-axis and RV plotting in m s−1 on the right y-axis.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: The H−K s and K s−W4 color excess for stars showing different types of line profiles and accretion properties (left) and their distribution (center, right). Stars marked in circles are those with the same accretion status in their multiple observations. The three stars marked in squares and numbered are stars that change accretion statuses in different observations. The gray dotted lines in the left and right panels indicate an area within which the H−K s colors are consistent with the photosphere. In the center and the right panel, dashed lines indicate the median of each group.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: Examples of the different types of He I λ10830 line profiles found in this survey. We identify stars with profiles with types as in the upper row as accreting stars, whereas those in the lower row we describe as non-accretors. The horizontal lines show the level of uncertainty from the continuum. The red dashed lines specify the flux at 1σ  t  from the continuum, and the solid green lines are at 3σ  t . Only (absorption/emission) features where their extrema are greater than 3σ  t  away from the continuum are considered detections.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: The velocities at feature minima compared to freefall velocities v ff,∞ for an observation showing types r, br, and b. The marker sizes scale with the stars’ masses.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: Our targets plotted in the accretion indicator–disk indicator space. The vertical lines in the left column are White & Basri’s (2003) thresholds of accretors for spectral types K5 (3 Å), M2.5 (10 Å), and M5.5 (20 Å). In the right column, the vertical lines are the thresholds of accretors adopted by White & Basri (2003; 270  km s−1) and Jayawardhana et al. (2006; 200  km s−1), respectively. The shaded regions correspond to the photospheric colors for stars of spectral types K0–M5 from Pecaut & Mamajek (2013). See Section 2.1 for the selection criteria applied in each stellar association.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: The W3 and W4 color excess for stars showing different types of line profiles and accretion properties. Stars marked in circles are those with the same accretion status in their multiple observations. The three stars marked in squares and numbered are stars that change accretion statuses in different observations. The stars marked with numbers 1, 2, and 3 are CVSO 1295, CVSO 248, and ESO-Hα 553, respectively.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: Distribution of the absolute EWs of the redshifted, blueshifted, and central absorption, and the emission components in the line profiles (Table 4).
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: Profile of He I λ10830 in CVSO 1545 as an example showing different features in the line. The black vertical lines show the velocities of the edges of each feature, and the colored vertical lines show the extrema. The shaded regions show the area of which the EWs were calculated. The horizontal lines have the same meaning as in Figure 2.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: Profiles of the He I λ10830 line for stars with more than one observation. The epoch of the observations is indicated. Lines show uncertainties in the continuum, as in Figure 2.
Paper: A Census of the Low Accretors. I. The Catalog
Authors: Thanawuth Thanathibodee, Nuria Calvet, Jesús Hernández, Karina Maucó, César Briceño
Figure caption: Theoretical HR diagram of our samples classified as accretors (Acc) and non-accretors (nAcc). The isochrones and evolutionary tracks are from the MIST tracks.
Paper: A Pilot Radio Search for Magnetic Activity in Directly Imaged Exoplanets
Authors: Y. Cendes, P. K. G. Williams, E. Berger
Figure caption: VLA C-band images of the 51 Eri system from 2018 March 2 (left) and 2021 February 2 (right) spanning 8″ on a side. Also shown are the positions of 51 Eri (green circle) and its known directly imaged exoplanet 51 Eri b (blue circle) based on positional information from Maire et al. (2019). We detect a radio source in the field (white circle, left), at a location that is outside of the field of the high-contrast direct-imaging instruments. The follow-up observations indicate that this source did not move as expected if it was associated with the 51 Eri system (white circle, right).
Paper: A Pilot Radio Search for Magnetic Activity in Directly Imaged Exoplanets
Authors: Y. Cendes, P. K. G. Williams, E. Berger
Figure caption: Radio spectral luminosity upper limits for the exoplanets in our survey (red triangles) compared to observations of UCDs plotted against spectral type (circles: flares; squares: quiescent; triangles: upper limits; lines connect flaring and quiescent emission from a single UCD), and constraining upper limits for exoplanets at GHz frequencies. The detected UCDs have been slightly shifted in spectral type for clarity. Data for UCDs are from Pineda et al. (2017), Kao et al. (2019), and references therein, and for the exoplanet upper limits from Bastian et al. (2000), Stroe et al. (2012), and Lazio et al. (2010).