adsabs/AstroCLIMB huggingface dataset:
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption:  ζ Gem results from Step 3. Right: ζ Gem position residuals plotted against TJD, re-determining coefficients A–F in Equations (4)–(7) while solving for η Aql parallax and proper motion. Compared to Figure 8, allowing ζ Gem to assist in determining A–F has reduced the ζ Gem rms residuals from (x, y) = (1.8, 1.6 mas) to (1.5, 1.3 mas), but left the parallax value, ϖ = 3.11 ± 0.20 mas, close to the Gaia EDR3 value. Left: reference star residuals. Compared to Figure 7, allowing the ζ Gem measurements to inform the coefficients A–F has increased the reference star residuals rms from (x, y) = (1.3, 1.2 mas) to (1.5, 1.3 mas).
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption:  η Aql results from Step 4. Right: η Aql position residuals plotted against TJD, re-determining the coefficients A–F in Equations (4)–(7) while solving for η Aql parallax and proper motion, including EDR3 priors for all stars. Compared to Figure 8, allowing η Aql to assist in determining A–F has significantly reduced the rms residuals from (x, y) = (1.8, 1.6 mas) to (0.9, 1.0 mas). Left: reference star residuals. Compared to Figure 7, including the η Aql measurements has significantly increased the reference star residuals rms from (x, y) = (1.1, 0.8 mas) to (1.9, 1.3 mas).
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption:  ζ Gem results from Step 4. Right: ζ Gem position residuals plotted against TJD, re-determining the coefficients A–F in Equations (4)–(7) while solving for ζ Gem parallax and proper motion, including EDR3 priors for all stars. Compared to Figure 8, allowing ζ Gem to assist in determining A–F has reduced the rms residuals from (x, y) = (1.8, 1.6 mas) to (1.1, 0.9 mas). Left: reference star residuals. Compared to Figure 7, including the ζ Gem priors from EDR3 has increased the reference star residuals rms from (x, y) = (1.3, 1.2 mas) to (1.5, 1.3 mas).
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: The η Aql A position residuals of Step 2 vs. the β parameter of Section 4.4.2, showing no strong correlation The lines linking the smallest and largest measured β values (while passing near the average β = 0.015) indicate what variation might be caused by an η Aql AB system with separation ρ AB = 200 mas at position angle P.A. = 45°.
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: Lomb–Scargle periodogram of the Step 2 residuals in Figure 8. ζ Gem exhibits significant power (false alarm probability (FAP) ≪ 0.001%) near one year or aliases of that period. η Aql residuals exhibit a broad peak near 133 days with FAP ∼ 0.1%.
Paper: Near-infrared Spectra of the Inflated Post-common Envelope Brown Dwarf NLTT 5306 B
Authors: Cam Buzard, Sarah L. Casewell, Joshua D. Lothringer, Geoffrey A. Blake
Figure caption: Diagram showing the center position of each of our 44 epochs. Orange points represent dayside epochs, purple points represent nightside epochs, and gray points represent observations during which NLTT 5306 B crossed quadrature and are therefore neither primarily day- or nightside. The blue arc starting at ϕ = 0 shows the average change in orbital position over a 5 minute exposure.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Substellar cooling curves derived from three independent evolutionary models given our measured masses. The top curve in each panel corresponds to ε Indi Ba, and the bottom curve corresponds to ε Indi Bb. The darker shaded region of each curve shows the 1σ range in our measured mass, and the lighter shading is the 2σ range. On each curve, the ages corresponding to T eff = 1400 K and 1200 K are marked, indicating the approximate beginning and ending of the L/T transition. Over-plotted on each panel are the 1σ and 2σ joint uncertainty contours for the age and luminosities of ε Indi Ba and Bb.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Residuals to the best-fit astrometric model for ε Indi Ba. The top panel shows the residuals in altitude, and the bottom panel shows the residuals in azimuth, both plotted as a function of altitude. Empty red circles show the rejected epochs from 3σ clipping of the azimuthal residuals. A histogram of the residuals is shown to the right of each scatter plot. Strong systematics are seen in the altitude residuals but not the azimuth ones, evident from the symmetric, roughly Gaussian distribution for the former and the altitude-dependent nonzero mean for the latter. These systematics are consistent with the magnitude expected for uncorrected ADC residual dispersion (Avila et al. 1997).
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Corner plot for the relative orbit fit MCMC chain. The parameters are angular semimajor axis ( a  ang) in mas, period (P) in years, eccentricity (e), longitude of ascending node (Ω) in degrees and inclination (i) in degrees. The posterior mean is used as the estimator for each parameter, and the errors are one standard deviation from the mean.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Root mean square residuals of the measured separations from the true separations of the PSFs in simulated data. Top panel shows the residuals in the radial direction. Bottom panel shows the residuals in the tangential direction in terms of arclength. Arclength is a better indicator of the fitting algorithm’s performance than PA, because we expect arclength residuals to be independent of radial separation, but the PA will go up at smaller separation simply due to geometry.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Relative orbit fit of ε Indi Ba and Bb. The orbit is plotted as the relative separation of Bb from Ba, where Ba is fixed at the origin. The black dots are the measured relative astrometry, the hollow dots show the beginning of each year, and the solid line is the best-fit orbit. The bottom panel shows the residuals of the separation in blue and PA in green.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Distortion correction to one of the 904 image frames from the FORS2 long-term monitoring of ε Indi B’s absolute positions. The position of ε Indi B is indicated by the yellow star while the blue dots are field stars. The red points are reference stars in the Gaia EDR3 catalog. The green lines indicate the residuals of the measured centroids from their distortion-corrected predictions based on EDR3 astrometry. Red open circles are Gaia EDR3 stars that we discard as outliers.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Top panel shows the flux ratios of ε Indi Ba over Bb in J, H, and K  s  bands measured using the joint PSF fitting method, and the flux ratios of Ba + Bb over the average of the field stars measured using aperture photometry. The bottom panel shows the flux scatter of ε Indi compared to the field stars in I band FORS2 data.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Examples of the joint moffat PSF fits to NACO data. Top panel shows an example of negligible PSF overlap. Bottom panel shows an example from the epoch with maximum overlap in NACO data.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Example fits and residuals to FORS2 images when the two components (ε Indi Ba and ε Indi Bb) are completely resolved (top panel) or strongly blended (bottom panel). In each panel, all values are normalized to the peak intensity of the model fits.
Paper: Near-infrared Spectra of the Inflated Post-common Envelope Brown Dwarf NLTT 5306 B
Authors: Cam Buzard, Sarah L. Casewell, Joshua D. Lothringer, Geoffrey A. Blake
Figure caption: NLTT 5306 B’s wavelength-dependent brightness temperatures (points, from Casewell et al. 2020a) and effective temperatures (horizontal lines). Dayside measurements are in orange and nightside measurements are in purple. The brightness temperatures, shown with squares, were calculated assuming the evolutionary model radius, and the crosses assumed the Roche lobe radius.
Paper: Near-infrared Spectra of the Inflated Post-common Envelope Brown Dwarf NLTT 5306 B
Authors: Cam Buzard, Sarah L. Casewell, Joshua D. Lothringer, Geoffrey A. Blake
Figure caption: Results of Sonora model fits. The three corner plots show Sonora fits to all of the epochs, the NLTT 5306 B dayside epochs, and the NLTT 5306 B nightside epochs, respectively. The contour plots show higher likelihood with darker colors, and the line plots the marginalized results with 68% confidence intervals. Contours are at 50, 68, and 95%. The log likelihood value used to compare each model is the average of the log likelihoods between K BD of 288 and 378 km s−1.
Paper: A Multiplanet System’s Sole Super-puff: Exploring Allowable Physical Parameters for the Cold Super-puff HIP 41378 f
Authors: Michelle Belkovski, Juliette Becker, Alex Howe, Isaac Malsky, Konstantin Batygin
Figure caption: Mass–radius relation for HIP 41378 f calculated with models varying in entropy and metallicity for a planet with an iron core. The six models plotted consist of three entropies (5.5, 6.0, or 6.5 k  b /baryon) where each entropy value was tested with a metallicity of solar (Z = 1) and 10 times solar (Z = 10). In the inset, the gray shaded box represents HIP 41378 f’s observed radius of 9.2 ± 0.1 R ⊕. Three of the six models achieved this radius by an age of 2 Gyr, serving a better idea of what core mass range HIP 41378 f may have given the entropy and metallicity values tested in those models. From left to right: Model 1 (entropy of 6.0, metallicity of 1.0), Model 2 (entropy of 6.5, metallicity of 10.0), and Model 3 (entropy of 6.5, metallicity of 1.0).
Paper: A Multiplanet System’s Sole Super-puff: Exploring Allowable Physical Parameters for the Cold Super-puff HIP 41378 f
Authors: Michelle Belkovski, Juliette Becker, Alex Howe, Isaac Malsky, Konstantin Batygin
Figure caption: The measured masses and radii for the five planets with mass and radius measurements in the HIP 41378 system. Candidate HIP 41378 g is excluded because it is detected only in the radial velocity data of Santerne et al. (2019) and no radius has been measured. For HIP 41378 d, only an upper mass limit is provided, which corresponds to the 95% credible upper limit (Santerne et al. 2019). Contour lines for a planet with solar metallicity, an age of ∼2 Gyr, 1 F ⊕, and varying envelope fractions are overlaid. The models for these lines come from Lopez et al. (2012).
Paper: A Multiplanet System’s Sole Super-puff: Exploring Allowable Physical Parameters for the Cold Super-puff HIP 41378 f
Authors: Michelle Belkovski, Juliette Becker, Alex Howe, Isaac Malsky, Konstantin Batygin
Figure caption: Bulk densities for planets where both radius and mass have been measured (the first via transit photometry, the second via either radial velocities or transit timing variations). HIP 41378 f, the main subject of analysis in this work, is marked as a pink star. Reference lines for water and Styrofoam are included. Data downloaded from NASA Exoplanet Archive on 2021 March 1.
Paper: A Multiplanet System’s Sole Super-puff: Exploring Allowable Physical Parameters for the Cold Super-puff HIP 41378 f
Authors: Michelle Belkovski, Juliette Becker, Alex Howe, Isaac Malsky, Konstantin Batygin
Figure caption: The envelope mass fractions of each planet in HIP 41378 over 2 Gyr, computed with VPLanet. While the envelope mass fractions of HIP 41378 d, HIP 41378 e, and HIP 41378 f are essentially constant over time, the values of HIP 41378 b and HIP 41378 c decrease by roughly a factor of 2 by an age of 2 Gyr.
Paper: A Multiplanet System’s Sole Super-puff: Exploring Allowable Physical Parameters for the Cold Super-puff HIP 41378 f
Authors: Michelle Belkovski, Juliette Becker, Alex Howe, Isaac Malsky, Konstantin Batygin
Figure caption: Subplots of the HIP 41378 planets’ density, envelope mass, and radius values over 2 Gyr. All planets in the system have increasing densities and decreasing radii over time. However, planets HIP 41378 b and HIP 41378 c have envelope masses that decrease by a factor of two over the simulated period.
Paper: A Multiplanet System’s Sole Super-puff: Exploring Allowable Physical Parameters for the Cold Super-puff HIP 41378 f
Authors: Michelle Belkovski, Juliette Becker, Alex Howe, Isaac Malsky, Konstantin Batygin
Figure caption: The stellar luminosity of HIP 41378 in the XUV (top panel), the XUV luminosity as a fraction of the total luminosity (middle panel), and the full bolometric luminosity (bottom panel). The XUV luminosity drives photoevaporative mass loss from the planetary envelopes.
Paper: Leveraging Space-based Data from the Nearest Solar-type Star to Better Understand Stellar Activity Signatures in Radial Velocity Data
Authors: Tamar Ervin, Samuel Halverson, Abigail Burrows, Neil Murphy, Arpita Roy, Raphaelle D. Haywood, Federica Rescigno, Chad F. Bender, Andrea S. J. Lin, Jennifer Burt, Suvrath Mahadevan
Figure caption: Comparison between SDO/HMI derived observables and NEID RV observations. Top panel: Filling factor computed from SDO/HMI magnetograms. Second panel: Unsigned magnetic flux computed from SDO/HMI magnetograms. Third/Fourth panel: Unscaled basis velocity components ﹩{\rm{\Delta }}{\hat{v}}_{\mathrm{conv}}﹩ and ﹩{\rm{\Delta }}{\hat{v}}_{\mathrm{phot}}﹩. Fifth panel: Total ΔRV model computed for the NEID observational time span (in light lavender) with the ground-based NEID RVs filtered for bad weather and cloud cover overlaid (in dark red). The average photon-limited error on the daily binned RV NEID measurements is ∼5 cm s−1. Sixth panel: Residuals between ΔRV model and ΔRV NEID from panel five. The residual rms scatter is 78 cm s−1.
Paper: Leveraging Space-based Data from the Nearest Solar-type Star to Better Understand Stellar Activity Signatures in Radial Velocity Data
Authors: Tamar Ervin, Samuel Halverson, Abigail Burrows, Neil Murphy, Arpita Roy, Raphaelle D. Haywood, Federica Rescigno, Chad F. Bender, Andrea S. J. Lin, Jennifer Burt, Suvrath Mahadevan
Figure caption: Example of corrected SDO/HMI data products during the highest activity day (largest magnetic filling factor) in our studied time frame (2021 June 30). Top left: Flattened continuum intensity after limb-darkening correction (used to identify bright and dark regions) Top right: Doppler velocity map after removal of spacecraft and solar rotational velocity. Bottom left: Unsigned magnetic flux density (∣B  r ∣). In this image, 3.25% of the Sun is covered by faculae/plage and 0.026% by sunspots, as identified by our pipeline. Bottom right: Thresholded image showing magnetically active regions identified by our algorithms. Faculae/plage regions are red, and sunspot regions are blue.
Paper: Leveraging Space-based Data from the Nearest Solar-type Star to Better Understand Stellar Activity Signatures in Radial Velocity Data
Authors: Tamar Ervin, Samuel Halverson, Abigail Burrows, Neil Murphy, Arpita Roy, Raphaelle D. Haywood, Federica Rescigno, Chad F. Bender, Andrea S. J. Lin, Jennifer Burt, Suvrath Mahadevan
Figure caption: Comparison between our pipeline-derived SDO/HMI derived velocities and observables (red) with reference calculations from Milbourne et al. (2019; blue). Correlation coefficients are shown in the upper left of each plot. First panel: Filling factor estimate, defined as the percentage of magnetically active pixels on the solar surface. The filling factor, f, for this period reflects the period of higher solar activity during which these data were taken. Second/Third panel: Comparison of unscaled velocity components ﹩{\rm{\Delta }}{\hat{v}}_{\mathrm{conv}}﹩ and ﹩{\rm{\Delta }}{\hat{v}}_{\mathrm{phot}}﹩. Fourth panel: Total ΔRV model from Milbourne et al. (2019) compared with our results, showing excellent agreement.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Isochrones from three different evolutionary models, ranging from 2 to 6 Gyr. Black and gray contours show the joint 1σ and 2σ confidence intervals of the masses and luminosities of ε Indi Ba and Bb. Because these two brown dwarfs must be coeval they should lie along a single model isochrone. The only models that pass this test are the Saumon & Marley (2008) hybrid models that predict a distinctly different mass–luminosity relation for brown dwarfs. These models have a much shallower dependence of luminosity on mass as objects cool through the L/T transition over T eff = 1400–1200 K, changing from cloudy to cloud-free atmosphere boundary conditions.
Paper: Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition
Authors: Minghan Chen, Yiting Li, Timothy D. Brandt, Trent J. Dupuy, Cátia V. Cardoso, Mark J. McCaughrean
Figure caption: Probability distributions of the difference between the model-derived substellar cooling ages (t cool) of ε Indi Ba and Bb. The dashed line shows the expectation that t cool,Bb = t cool,Ba. Only the Saumon & Marley (2008) hybrid models predict consistent, coeval ages. This is the highest-precision coevality test of brown dwarf binaries to date, and it supports previous results from brown dwarf binaries with mass errors of ≈5% (Dupuy et al. 2015; Dupuy & Liu 2017).
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: Number of planets detected as a function of spectral type (top left), planet radius (top right), orbital period (bottom left), and host star TESS magnitude (bottom right). The stacked histograms show the number of new planets detected with each major stage of the TESS mission, with PM detections in blue, new detections from EM1 in orange, and new detections from EM2 in red. The black points give the mean and standard deviation of the total (cumulative) number of planets predicted over the full 7 yr. Contrary to previous works that predict that F-type stars are the most common TESS planet hosts, we find that detections are dominated by G-type stars. Meanwhile, early mission TESS detections will be dominated by thousands of giant planets, while thousands of small super-Earth and sub-Neptune-sized planets will be increasingly detectable as the mission progresses. Later years also reveal longer-period planets. The magnitude histogram only shows planets with R  p  < 4 R ⊕ to emphasize that many of the small planets found later in the mission will be around fainter stars.
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: 4695 simulated detections from the PM (top), 8384 detections from the combined PM + EM1 (middle), and 12,521 after the full simulated 7 yr spanning the PM + EM1 + EM2 (bottom). Planets found only in the FFIs (which have cadences of 30 minutes, 10 minutes, and 200 s for the PM, EM1, and EM2, respectively) are plotted in blue, while planets found only in 2-minute observations are plotted in gray and planets found in both types of observations are plotted in orange. The most significant change between the predictions is the increased number of small and long-period planets, which both benefit from the longer baselines of reobserved stars. The block-like nature of the distributions is due to the use of discrete period−radius occurrence rate bins (Figure 3).
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: Occurrence rate grids adopted for this work, with AF, G, and K occurrence rates from Kunimoto & Matthews (2020) and M occurrence rates from Dressing & Charbonneau (2015). The number of planets per star is given in percentage (10−2), and the uncertainties show only the larger of the lower and upper uncertainties to improve readability. Bins that had no estimate or only upper limits for the occurrence rates are in gray and are assumed to be equal to 0.
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: Planet detection probability for select numbers of transits as a function of transit S/N from Hsu et al. (2019), which took into account incompleteness due to both search and vetting based on Kepler DR25 injection/recovery tests (Christiansen et al. 2020). S/N = 7.3 is marked by a dotted black line. Previous TESS simulation papers (Sullivan et al. 2015; Bouma et al. 2017; Barclay et al. 2018; Huang et al. 2018; Cooke et al. 2018; Villanueva et al. 2019; Cooke et al. 2019) have considered planets 100% detectable with S/N ≥ 7.3, which should significantly overpredict the number of low-S/N detections.
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: The 1 hr rms CDPP measurements for all ∼230,000 PM targets processed by the SPOC pipeline, in ppm as a function of TESS magnitude. Each gray dot represents a target’s rms CDPP for an individual sector. The green and blue lines show fits to the 10th and 50th percentiles of the measurements, respectively, while the red line shows the presumed pre-launch systematic limit from Sullivan et al. (2015).