adsabs/AstroCLIMB huggingface dataset:
Paper: KIC 9028474: A Long-period Eclipsing Binary on a Highly Eccentric Orbit
Authors: Orkun Özdarcan
Figure caption: Long-cadence light curve (upper panel) of KIC 9028474. The very high eccentricity is easily noticeable from very short time interval between deep and shallow eclipses. The lower panel shows closer view of successive eclipses for a portion of the whole light curve.
Paper: KIC 9028474: A Long-period Eclipsing Binary on a Highly Eccentric Orbit
Authors: Orkun Özdarcan
Figure caption: Broadening functions (small open circles) of two APOGEE spectra obtained in the close vicinity of the orbital quadratures. Gaussian fits for the primary (P) and the secondary (S) components are shown in continuous (blue and red) lines. The orbital phase (ϕ) of each observation is shown just above each panel.
Paper: KIC 9028474: A Long-period Eclipsing Binary on a Highly Eccentric Orbit
Authors: Orkun Özdarcan
Figure caption: Positions of the components in ﹩\mathrm{log}{T}_{\mathrm{eff}}\mbox{--}\mathrm{log}L/{L}_{\odot }﹩ plane. Three different isochrones for log age 9.5, 9.7, and 9.8 are also plotted with continuous curves. Dashed curves show evolutionary tracks for different masses. Each track is labeled with its corresponding mass in the solar unit.
Paper: Prospects from TESS and Gaia to Constrain the Flatness of Planetary Systems
Authors: Juan I. Espinoza-Retamal, Wei Zhu, Cristobal Petrovich
Figure caption: Uncertainty in inclination as a function of the number of RV data taken for 3 fixed systems. Left: A system detectable with only astrometry and with the inclination well constrained (﹩{\sigma }_{\cos i}^{\mathrm{astro}}\approx 0.003﹩). Center: A system detectable with astrometry but with the inclination not well constrained (﹩{\sigma }_{\cos i}^{\mathrm{astro}}\approx 0.45﹩). Right: A system not detectable with only astrometry (﹩{\sigma }_{\cos i}^{\mathrm{astro}}\approx 1.5﹩). Different colors represent different precisions for the instrument used to measure the RV. The black dashed line corresponds to the analytic limit in Equation (10) reachable in each case.
Paper: Prospects from TESS and Gaia to Constrain the Flatness of Planetary Systems
Authors: Juan I. Espinoza-Retamal, Wei Zhu, Cristobal Petrovich
Figure caption: Left: Histogram of the number of cold Jupiters that should have the inclination well constrained as a function of the size of the inner planet. Right: Scatter plot of stellar distance vs. stellar effective temperature of all TOIs. The color represents the probability of having the inclination of the cold Jupiter well constrained.
Paper: Prospects from TESS and Gaia to Constrain the Flatness of Planetary Systems
Authors: Juan I. Espinoza-Retamal, Wei Zhu, Cristobal Petrovich
Figure caption: Left: Histogram of the number of cold Jupiters that should be detected as a function of the size of the inner planet. Right: Scatter plot of stellar distance vs. stellar effective temperature of all TOIs. Color represents the probability of detecting the cold Jupiter.
Paper: Prospects from TESS and Gaia to Constrain the Flatness of Planetary Systems
Authors: Juan I. Espinoza-Retamal, Wei Zhu, Cristobal Petrovich
Figure caption: Random cumulative distribution for the absolute value of the cosine of the inclination of the cold Jupiter generated assuming that the mutual inclination follows a Rayleigh distribution with σ = 5° and 20°, and Uniform.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: CD-27 for our nine epochs of imaging data, excluding the two GPI epochs. Along the top row are the initial reduced images, the middle row displays the model created using a PSF star, and the bottom row shows the results of the PSF fitting and subtraction of the model. The best-fit orbit (white) is displayed on the reduced images. The labels at the top of each column indicate the epoch, while those at the bottom of the reduced image list the instrument and filter.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: Model fluxes of stars Aa and Ab (top panel) and B (middle panel), and the flux ratio of the resolved pair AaAb and B (bottom panel) as a function of wavelength from the Padova evolutionary model for 100 samples drawn from our MCMC analysis. The red squares represent the flux ratio between the two components measured in the Keck/NIRC2 images taken on 2020 July 24.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: The χ 2 reported in the Gaia DR3 catalog for the fit to the astrometric measurements of CD-27 (red point) compared to stars of a range of magnitudes. CD-27 has a χ 2 larger than 99.5% of stars within 0.1 mag. This is consistent with the variability of CD-27 biasing the Gaia DR2 5-parameter fit, casting doubt on the accuracy of the parallax.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: GPI NRM images of CD-27 (left), a model constructed from the calibrator star HD 153318 (middle), and the residual of the two (right) for the 2018 August 15 (top) and 2019 August 5 (bottom) epochs.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: Astrometric measurements (symbols) and a hundred orbits randomly sampled from the MCMC posterior distributions (gray curves) showing the separation (first row) and position angle (third row) as a function of time. The second and fourth rows show the corresponding residuals relative to the median orbit.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: APO/ARCES spectra of CD-27 from 2021 June 20, showing the deep Li λ6707.79 line. Also plotted for comparison is the older K3 star HIP 23311, which has no significant lithium absorption. While the CD-27 spectrum is a composite of multiple stars of varying spectral types on the slit, the strong lithium absorption is compelling evidence for a young (≲100 Myr) age for the system.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: Comparison of the measured photometry and mass of the two resolved components of the CD-27 system (red circles) to four sets of theoretical models, as well as GJ 3305 A/B (gray diamonds) from Montet et al. (2015) and V343 Nor Aa/Ab (gray squares) from Nielsen et al. (2016). For the plotted isochrones, colors corresponds to different models, and line styles correspond to ages.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: Best-fit visual orbit of the CD-27 system found using orbitize!. Different symbols and colors show the observations taken by the various instruments, while the color bar shows the relative position of the visible components over time.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: The cross-correlation function between one observed spectrum of CD-27 and the spectrum of HIP 41277, a single star with a similar spectral type, is shown in black and has a single peak. For all ARCES observations of CD-27, the cross-correlation yields similar results. Cross-correlation functions between a simulated binary and HIP 41277 are shown as colored curves. The different colors represent different delta RVs between A and B. For each panel, we apply a different ﹩v\sin i﹩ to the components of the simulated binary. Each cross-correlation function is recentered at zero to better compare each curve. Two peaks are visible for larger delta RVs (≳30 km s−1) when ﹩v\sin i=13\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩. The largest delta RV that produces a single peak matching the CD-27 cross-correlation function corresponds to an orbit of Ab around Aa with a semimajor axis larger than 0.04 au.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: The pink hatched regions indicate mass−separation combinations that are not allowed for Ab. On the left, the semimajor axis is limited by the maximum possible RV (∼25 km s−1) of Aa induced by Ab over a range of Ab masses. The range of predicted Ab masses is highlighted in yellow. On the right, the lack of a detectable wobble in the astrometric measurements allows us to draw a conservative upper limit of ∼1.6 au for the subsystem semimajor axis from the largest separation residual (∼2 mas) and dynamical arguments.
Paper: A Lithium Depletion Age for the Carina Association
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Benjamin M. Tofflemire, Adam L. Kraus
Figure caption: CMD of stars selected for fitting (blue circles) compared to PARSECv1.2 models. The green lines are 200 random samples from our MCMC analysis, and the two dashed lines are the 30 and 40 Myr isochrones for comparison. Points are shaded based on the probability that they are part of the main population or the outlier population.
Paper: A Lithium Depletion Age for the Carina Association
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Benjamin M. Tofflemire, Adam L. Kraus
Figure caption: Example equivalent width measurement. The pseudocontinuum, shown in orange, is a linear fit of the spectrum in the regions on either side of the line edges. The EW is calculated using a trapezoidal sum between the spectrum and the pseudocontinuum fit.
Paper: A Lithium Depletion Age for the Carina Association
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Benjamin M. Tofflemire, Adam L. Kraus
Figure caption: CMD of Carina members, overplotted with members of three benchmark associations, β Pictoris (24 Myr), Tuc-Hor (40 Myr), and Pleiades (112 Myr). Membership lists for benchmark associations are generated using BANYAN Σ with the same parameters as described in Section 2. High-probability members with RUWE < 1.2 are shown for benchmark associations. Observed members of Carina (see Table 1) are indicated with stars.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: Covariance between the system age and parallax, and the masses of the three components derived from the MCMC analysis using the Padova PARSEC evolutionary model with a flat prior on the parallax.
Paper: A Lithium Depletion Age for the Carina Association
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Benjamin M. Tofflemire, Adam L. Kraus
Figure caption: Reduced SOAR/Goodman spectra of all observed Carina members, overplotted with a Li-free M-dwarf template (gray; Bochanski et al. 2007). The wavelength of the Li 6707.8 Å line is marked with a vertical dashed line. Four of these stars show either no detectable Li, or have EW(Li) < 200 mÅ, and are thus Li-poor, while the other 11 have EW(Li) > 200 mÅ, and are Li-rich.
Paper: CD –27°11535: Evidence for a Triple System in the β Pictoris Moving Group
Authors: Andrew D. Thomas, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, Bruce Macintosh, Jeffrey Chilcote, Paul Kalas, Jason J. Wang, Sarah Blunt, Alexandra Greenbaum, Quinn M. Konopacky, Michael J. Ireland, Peter Tuthill, Kimberly Ward-Duong, Lea A. Hirsch, Ian Czekala, Franck Marchis, Christian Marois, Max A. Millar-Blanchaer, William Roberson, Adam Smith, Hannah Gallamore, Jessica Klusmeyer
Figure caption: Corner plot of orbital parameters from the orbitize! fit. Uniform 2D Gaussians indicate convergence.
Paper: A Lithium Depletion Age for the Carina Association
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Benjamin M. Tofflemire, Adam L. Kraus
Figure caption: Lithium measurements of Carina members. (Left) Fraction of initial Li abundance as a function of Gaia B  P  − R  P , overplotted with the DSEP magnetic models (Feiden 2016, DSEP mag). Equivalent widths of association members were converted to Li/Li0 using the curve of growth from Zapatero Osorio et al. (2002) for T eff < 4000 K and from Soderblom & Mayor (1993) for T eff > 4000 K. (Right) Lithium equivalent widths for Carina members, taken from our observations and Riedel et al. (2017), Schneider et al. (2019), are shown as teal dots plotted on top of the observed Li Sequences of the Beta Pictoris Moving Group (24 Myr, red; Binks & Jeffries 2014), Tucana-Horologium Young Association (40 Myr, orange; Kraus et al. 2014), and the Pleiades (112 Myr, yellow; Bouvier et al. 2018).
Paper: A Lithium Depletion Age for the Carina Association
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Benjamin M. Tofflemire, Adam L. Kraus
Figure caption: The lithium depletion boundary of Carina. Li-rich stars (EW(Li) > 200 mÅ) are shown as teal dots, and Li-poor (EW(Li) < 200 mÅ) ones as red x’s. Black horizontal lines are drawn through the brightest Li-rich star and the faintest Li-poor one, and labeled with the corresponding age using the DSEP magnetic model. The LDB at 30, 40, and 50 Myr for each model is shown as colored lines, where the color indicates the model, and the line style indicates the age. The right side axis shows the stellar mass corresponding to the given magnitude at 40 Myr.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: The magnetic field intensity profiles averaged over each DD campaign.
Paper: Detecting Multiplanetary Systems with Gravitational Microlensing and the Roman Space Telescope
Authors: Hossein Fatheddin, Sedighe Sajadian
Figure caption: Light curves of four different microlensing events. In each figure the triple and binary models and their difference are illustrated. The magnification map on the top right of each light curve corresponds to the configurations of the lenses and the path of the souce star where there is a second planet (the red curve), whereas the maginfication map at the bottom represents the binary system configuration (the dashed black curve).
Paper: Detecting Multiplanetary Systems with Gravitational Microlensing and the Roman Space Telescope
Authors: Hossein Fatheddin, Sedighe Sajadian
Figure caption: Visualizations of statisctical distributions of the parameters used in the simulated data set and the results. The red curve shows the detected multiplanetary systems with low sensitivity and the green curve shows the ones with high sensitivity.
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: The full posterior distributions (corner plots) of the Proterozoic-Earth-like scenario with 1% of modern Earth’s O2. The different cases explore a combination of different wavelength bands used for the retrieval process. The black lines in the corner plots refer to the true value used to simulate the data.
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: The full posterior distributions (corner plots) of the Proterozoic-Earth-like scenario with 0.1% of modern Earth’s O2. The different cases explore a combination of different wavelength bands used for the retrieval process. The black lines in the corner plots refer to the true value used to simulate the data.
Paper: Centimeter-sized Grains in the Compact Dust Ring around Very-low-mass Star CIDA 1
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto, Yuka Terada
Figure caption: The VLA images (color) show the CIDA 1 ring overlaid with the ALMA Band 7 data (dashed ellipses; r = 0.″16; i = 37.°4; P.A. = 10.°8; Pinilla et al. 2021). Panels (a)–(d) depict the Q-band (40–48 GHz), Ka-band (29–37 GHz), Ku-band (12–18 GHz), and X-band (8–12 GHz) images, respectively. The stellar position is marked by a black star, corresponding to the ICRS coordinate of (4h14m17.ˢ62395, 28d6m9.ˢ11174). The proper motion (pmRA =8.285 mas yr−1, pmDEC = − 23.607 mas yr−1; Gaia Collaboration et al. 2016, 2022) has been corrected. The synthesized beams are illustrated as white ellipses in the lower left corner. VLA FITS images shown in this figure are available as data behind the figure.(The data used to create this figure are available.)
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: N2 (left) and CO (right) retrieved partial pressures comparing the 0.2–1.8 μm to the 0.2–1.1 μm wavelength ranges. Figure 9(a) presents our N2 abundances for our 0.2–1.8 μm N2-dominated retrievals in red and our 0.2–1.1 μm N2-dominated retrievals in yellow. Both N2-dominated retrievals have an N2 abundance true value of 78% of the total atmosphere. Vertical lines show N2's true value using the same color code. Similarly, Figure 9(b) presents our CO abundances for our 0.2–1.8 μm CO-dominated retrievals in blue and our 0.2–1.1 μm CO-dominated retrievals in cyan. Both CO-dominated retrievals have a CO abundance true value of 78% of the total atmosphere. Vertical lines show CO’s true value using the same color code. Without extended wavelength coverage, our model is unable to differentiate N2 from CO and they share similar abundances that fall outside of their true value.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Posterior distributions of our nominal partial pressure retrieval with all retrieved parameters. We retrieved on a wavelength-dependent resolution R = 7, 140, 70 at wavelength ranges 0.2–0.4, 0.4–1.0, 1.0–1.8 μm with an assumed S/N of 20 at all wavelengths. The parameters’ true values are plotted with light blue lines. The cells off the diagonal are the covariant 2D posterior distributions of their axial posteriors shown with their normal distribution 1σ, 2σ, and 3σ contours. The diagonal parameter posteriors are also plotted with dashed lines (left to right) that mark the 16%, 50%, and 84% quantiles.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: The same retrieval and results as Figure 3 except gas values are represented by volume mixing ratios (VMRs) rather than partial pressures. In addition to presenting the atmospheric gases with their VMR values, the surface pressure is also included with respective correlations in the bottom row.