adsabs/AstroCLIMB huggingface dataset:
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Broadening functions of 14 ELODIE spectra after the primary star’s signal was subtracted from the composite spectra. The broadening functions are normalized to the peak value. The blue curve is the fit to the remnant unsubtracted signal from the primary star, while the secondary star’s fit is shown in red. Observation dates and associated phase are shown in each panel.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Top: Radial velocity measurements from ELODIE (red and blue stars) and literature data vs. phase, along with the best-fit orbit model. Middle/bottom: Velocity residuals (observed minus computed) for the primary and secondary stars, respectively. Primary star measurements from Griffin & Griffin (2011) between orbital phases of −0.05 and 0.05 were removed due to likely contamination by the secondary star.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Visibility data and corresponding model fit for the PTI data on 12 Com. All data were taken in a two-week period. Circles and triangles refer to the data and model, respectively. Colors refer to different telescope pairs. The bottom plot shows the residuals between the model and data.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Visibility data and corresponding model fit for the MIRC-X data on 12 Com. The visibilities are split by observation date, where the dates are HJD−2400000. Colors refer to different telescope pairs.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Closure phase data and corresponding model fit for the MIRC-X data on 12 Com. The closure phases are split by observation date, as seen in each panel, where the dates are HJD−2400000. Colors refer to different triplets of telescopes.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Spectral energy distributions of the single giant star 31 Com and the binary 12 Com, with the photometric passbands for each point indicated with horizontal bars.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Gaia color–magnitude diagram for Coma Ber stars (black points), assuming reddening E(B −V) = 0 and distance modulus (m −M)0 = 4.67. MIST isochrones (Choi et al. 2016) are shown for 450 Myr (blue) to 600 Myr (red) with 50 Myr spacing. Thick curves on the right show allowed portions of evolution tracks (fainter and redder than the binary) for the measured mass of 12 Com A as well as ±1σ away in red, green, and blue, respectively. Corresponding positions for the secondary star (when 12 Com A’s photometry is subtracted from that of the binary) are shown on the left. The cyan box shows the required position of 12 Com A if the secondary is in the isochrones between the thick blue lines. The black box encloses the predicted positions of the secondary in the isochrones, given its mass and ±1σ uncertainties.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Top panel: spectral energy distribution of the single giant star 31 Com (orange points), with the photometric passbands for each point indicated with horizontal bars. The best-fit ATLAS9 model with T eff = 5700 K and ﹩\mathrm{log}g=3.5﹩ is shown in black, and the model predictions for each observed bandpass are shown with green points. A flux-calibrated IUE spectrum is shown in cyan. Bottom panel: relative flux residuals for each observed photometric bandpass.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: MIST (dashed lines; Choi et al. 2016) and PARSEC v1.2 (solid lines; Bressan et al. 2012) isochrones with Z = 0.0152 and E(B −V) = 0. The horizontal lines are the model positions of the primary star (assuming 2.64M ⊙) in each isochrone. Left: HR diagram for Coma Ber stars. The isochrones have ages of 520 (green), 540 (red), and 560 (black) Myr. Right: Gaia color–magnitude diagram for Coma Ber stars. The isochrones have ages of 500–560 Myr in 20 Myr increments. The large topmost red point shows the combined light of 12 Com. Smaller red points show known binary systems.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Evolutionary tracks (MESA) for a 2.64 M⊙ star (blue curve) with [Fe/H] = 0.07. The combined photometry for 12 Com is shown with a red dot, using a distance of 87.0 ± 0.2 pc and reddening E(B −V) = 0.00 (E(BP −RP) = 0.0022). The photometric position of 31 Com is shown with a blue point. The dark orange curve shows the allowed regions for the giant to exist based on photometric considerations (ages 531–535 Myr for giant branch, 554–634 Myr for red clump). Evolution tracks for masses at ±1σ (±0.07 M ⊙) are shown with gray/light orange curves.
Paper: Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
Authors: Rex Lam, Eric L. Sandquist, Gail H. Schaefer, Christopher D. Farrington, John D. Monnier, Narsireddy Anugu, Cyprien Lanthermann, Robert Klement, Jacob Ennis, Benjamin R. Setterholm, Tyler Gardner, Stefan Kraus, Claire L. Davies, Jerome A. Orosz
Figure caption: Mass–radius comparison of 12 Com A with MIST isochrones (Choi et al. 2016) showing only the subgiant and red giant branch phases.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Δv sys − ΔK  p  diagrams for the retrieved planet spectrum. The nominal and retrieved velocities are indicated by the dashed and solid green lines, respectively. The top row shows all molecules, while the subsequent four rows show the contribution of individual species. 12CO dominates the detection, while the other species show relatively weak features at the expected velocity of WASP-33b. The detection strength is estimated by dividing the computed log-likelihood map by the standard deviation taken after masking K  p  < 50 km s−1 and below/above the 10th/90th percentiles in order to reduce the impact of the PCA-induced feature near K  p  = 0 km s−1 and the planet peak itself. Figure 4 provides a better quantitative estimate of detection strength.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Cross correlation vs. planet velocity and exposure number for varying numbers of removed principal components. Data processing was identical as for the retrievals at the best-fit planet velocity, including negative injection before PCA. The S/N is estimated by dividing by the variance for v pl − v sys > 0, which does not overlap with the planet track. The lower panels show the summed CCF in the planet rest frame. Without PCA, the cross-correlation space is dominated by the time-varying fringe associated with transmissive optics in KPIC. PCA almost completely eliminates this effect, enabling a clear detection of the planet signal. Removing between 2 and 10 PCs has a negligible impact on the planet detection. We choose to remove four PCs, as visual inspection shows significant fringing and telluric contributions even in the third and fourth components (see Figure 3).
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Data processing steps for one order. The top panel shows the raw data time series for one order, with evident tellurics and frame-to-frame variations in total flux. The second panel shows the data after scaling, dividing by a median spectrum, and masking values differing from the median by >8% (approximately 10 times the median absolute deviation). Telluric and stellar features are effectively removed at this step, but a time-varying fringe pattern is clearly visible. The third panel shows data after removing the first four principal components. Occasionally weak temporally fixed features persist after PCA. The fourth panel shows the data after a second median division to remove any such features and masking values differing from the median by >4% (approximately 6 times the median absolute deviation).
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Example of the omitted principal components for the 2.44–2.49 μm NIRSPEC order shown in Figure 2. The impact of time-varying fringing and telluric absorption is clear throughout the first 4 principal components. A telluric feature can be seen near pixel 1500, where the PCA is correcting variations from our baseline PSG model. Amplitudes are relative to the continuum-normalized spectrum, with a 0.1 offset added to successive principal components.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Normalized planet spectrum including H− opacity (dotted blue) and without (black) over the wavelength range of a single NIRSPEC order corresponding to the CO band head. The ratio of the spectrum without H− to the spectrum with H− is plotted in orange. Over the short bandpasses of the NIRSPEC orders, H− is effectively achromatic, reducing line strengths by ∼10% relative to the continuum. As the continuum is removed during the detrending, the overall scaling parameter should account for the impact of H−, explaining the weak constraints using a free-retrieval approach and justifying the omission of H− opacity.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Observed orbital geometry of the WASP-33 system. The diagram is drawn to scale with the planet orbit face-on and observed orbital phases shaded by the observation date. The ellipticity of the star is neglected, and the planet’s motion is drawn clockwise to reflect the retrograde orbit. The 2021 November 21 observations probe dayside thermal emission and provide a planet-free stellar spectrum during eclipse. The 2021 November 22 observations targeted the afternoon/dusk region but suffered from poor conditions and are therefore omitted from analysis.
Paper: FX UMa: A New Heartbeat Binary System with Linear and Nonlinear Tidal Oscillations and δ Sct Pulsations
Authors: Kun Wang, 坤 王, Anbing Ren, 安炳 任, Mads Fredslund Andersen, Frank Grundahl, Tao Chen, 涛 陈, Pere L. Pallé
Figure caption: RVs of both component stars of FX UMa as a function of phase. The blue solid lines represent the theoretical RV curves for the both components, derived by using the rvfit code (Iglesias-Marzoa et al. 2015). The red dotted–dashed lines represent the best-fitting models from the PHOEBE that were constrained by both LC and RV observations, which will be described in Section 3. The yellow dashed line in the top panel shows the systemic velocity of v  γ  = −9.475 km s−1. The residuals from the best-fit model are presented in the bottom two panels.
Paper: FX UMa: A New Heartbeat Binary System with Linear and Nonlinear Tidal Oscillations and δ Sct Pulsations
Authors: Kun Wang, 坤 王, Anbing Ren, 安炳 任, Mads Fredslund Andersen, Frank Grundahl, Tao Chen, 涛 陈, Pere L. Pallé
Figure caption: One observed SONG spectrum (middle, BJD = 2458814.512091, ϕ = 0.909) and the disentangled spectra from FDBinary for the two components in FX UMa (upper and lower). The zoom panel shows a small portion of these spectra to better see the details. The besting-fitting theoretical spectra for the two stars, obtained by the iSpec code, are shown as the red solid lines. The spectra of the stars 1 and 2 have been shifted vertically by +0.3 and -0.3, respectively, for comparison purposes.
Paper: FX UMa: A New Heartbeat Binary System with Linear and Nonlinear Tidal Oscillations and δ Sct Pulsations
Authors: Kun Wang, 坤 王, Anbing Ren, 安炳 任, Mads Fredslund Andersen, Frank Grundahl, Tao Chen, 涛 陈, Pere L. Pallé
Figure caption: BF plots for FX UMa. Each panel stands for one spectroscopic observation, for which the double-rotational profile fit to the normalized smoothed BF are plotted. The central position of each BF, corresponding to the radial velocity of each component of FX UMa, is marked by the blue vertical line.
Paper: FX UMa: A New Heartbeat Binary System with Linear and Nonlinear Tidal Oscillations and δ Sct Pulsations
Authors: Kun Wang, 坤 王, Anbing Ren, 安炳 任, Mads Fredslund Andersen, Frank Grundahl, Tao Chen, 涛 陈, Pere L. Pallé
Figure caption: The full 2 minute TESS light curve of FX UMa from sectors 14, 20, and 40. The zoom panel is a closer view of a selected region of the light curve.
Paper: FX UMa: A New Heartbeat Binary System with Linear and Nonlinear Tidal Oscillations and δ Sct Pulsations
Authors: Kun Wang, 坤 王, Anbing Ren, 安炳 任, Mads Fredslund Andersen, Frank Grundahl, Tao Chen, 涛 陈, Pere L. Pallé
Figure caption: The top panel shows the phased TESS light curve of FX UMa with the best-fitting model superimposed. The unbinned and binned light residuals are presented in the middle and bottom panels, respectively.
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: The HD 1160 b orbital parameter corner plots using observable-based priors (left) and uniform priors (right). For this plot, both priors had only astrometry measurements. For observable priors, the columns represent, respectively, the period (P; in years), the eccentricity (e), the epoch of periastron passage (T 0; in years), the inclination (i; in degrees), longitude of ascending node (Ω; in degrees), and argument of periapsis (ω; in degrees). For uniform priors, the columns represent, respectively, the semimajor axis (a; in astronomical unit), the eccentricity (e), the inclination (i; in degrees), the argument of periapsis (ω; in degrees), the longitude of ascending node (Ω; in degrees), the epoch of periastron passage (τ), the distance of the system (π; in milliarcseconds), and the system mass (M; in M ⊙).
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: The semimajor axis plotted against the eccentricity of the companions. Semimajor axis values are calculated from the 68th percentile of our orbital fits. Error bars on the eccentricity represent the 68th percentile of the orbital fit. The blue dots represent “planets,” or objects under 15 M  J , while red dots represent “brown dwarfs,” or objects with masses above 15 M  J . Green dots are “boundary” objects: intermediate-mass objects that could be in either distribution. In orange, we plot the separation cutoff where we split our sample between “Close” and “Wide” separations.
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: The bar plot of how many successful tries (i.e., true parameters are within 1σ of posterior distribution) we obtain as a function of eccentricity for observable and uniform priors. For 15% of the orbital period in coverage, all of the eccentricity values from 0.1–0.9 have over 68 of the 100 trials considered successful.
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: Comparison of “planet” vs. “brown dwarf” distributions for different combinations of intermediate-mass objects: for our highest ﹩{ \mathcal P }﹩ case (i.e., most similar distributions) and lowest ﹩{ \mathcal P }﹩ case (i.e., most different distributions).
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: The mass of the companions plotted against the eccentricity of the companions. Mass estimates are from the literature, while eccentricity estimates are from this work. Error bars on the eccentricity represent the 68th percentile of the orbital fit. The blue dots represent “planets,” or objects under 15 M  J , while red dots represent “brown dwarfs,” or objects with masses above 15 M  J . Green dots are “boundary” objects: intermediate-mass objects that could be in either distribution.
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: The inferred orbital coverage of each object in the sample, calculated as a fraction of the astrometric coverage and the period fit, plotted against the eccentricity of the object. This is from the real data used in our sample. Most of the sources have less than 10% orbital period coverage, with four objects presenting less than 1% period coverage.
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: The “close” vs. “wide” separation companion populations, with the split happening at 30 au. The two distributions are consistent with each other, with a ﹩{ \mathcal P }﹩ of 0.85.
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: Uniform priors corner plot for HD 1160 b with two RV points added.