adsabs/AstroCLIMB huggingface dataset:
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: The dynamical stability of the Earth-mass test particles distributed in the HD 63433 system, as a function of semimajor axis, a, and eccentricity, e, over the 1 Myr of our simulations. Each point in the plot shows the mean lifetime of 45 test particles that began the simulations at that particular (a, e) location, which were distributed across a variety of arguments of periastron, ω, and mean anomalies, M. The left-hand panels show the mean lifetime across the region tested, while the right-hand panels show the fraction of stable simulations in the same area. The upper row shows the results for the highest considered masses of HD63433's planets, the middle row shows the intermediate-mass solution, and the lower row shows the low-mass solution. The locations of the two known planets in the system are marked by hollow circles in the right-hand plot, along with the position of key mean-motion resonances with those planets.
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: The dynamical stability of the Earth-mass test particles distributed between the orbits of HD 21749 b and HD 21749 c, as a function of semimajor axis, a, and eccentricity, e, over the million years of our simulations. Each point in the plot shows the mean lifetime of 45 test particles that began the simulations at that particular (a, e) location, which were distributed across a variety of arguments of periastron, ω, and mean anomalies, M. The left-hand panel shows the mean lifetime across the region tested, while the right shows the fraction of stable simulations in the same area. The right-hand panel also shows the location of the two known planets in the system (denoted by hollow circles), and the location of key resonances with those planets, in the top half of the plot.
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: The dynamical stability of the Earth-mass test particles distributed between the orbits of TOI 1670 b and TOI 1670 c, as a function of semimajor axis, a, and eccentricity, e, over the 1 Myr of our simulations. Each point in the plot shows the mean lifetime of 45 test particles that began the simulations at that particular (a, e) location, which were distributed across a variety of arguments of periastron, ω, and mean anomalies, M. The left-hand panel shows the mean lifetime across the region tested, while the right shows the fraction of stable simulations in the same area. The location of the two known planets, and their mean-motion resonances, are shown in the right-hand panel.
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: The dynamical stability of the Earth-mass test particles distributed between the orbits of HD 15337 b and HD 15337 c, as a function of semimajor axis, a, and eccentricity, e, over the million years of our simulations. Each point in the plot shows the mean lifetime of 45 test particles that began the simulations at that particular (a, e) location, which were distributed across a variety of arguments of periastron, ω, and mean anomalies, M. The left-hand panel shows the mean lifetime across the region tested, while the right shows the fraction of the simulations that began at a given a-e ordinate that survived for the full simulation duration. In the right-hand panel, the semimajor axis and eccentricity of the two known planets are marked by hollow circles, with the locations of key mean-motion resonances with those planets shown in the top half of the plot. The resonances with the inner planet (HD 15337b) are shown in brown, while those with the outer planet (HD 15337c) are shown in pink.
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: The dynamical stability of the Earth-mass test particles distributed in the LTT 3780 system, as a function of semimajor axis, a, and eccentricity, e, over the 1 Myr of our simulations. Each point in the plot shows the mean lifetime of 45 test particles that began the simulations at that particular (a, e) location, which were distributed across a variety of arguments of periastron, ω, and mean anomalies, M. The left-hand panel shows the mean lifetime across the region tested, while the right shows the fraction of stable simulations in the same area, along with the location of the two known planets and their mean-motion resonances.
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: The dynamical stability of the Earth-mass test particles in the TOI 421 system, as a function of semimajor axis, a, and eccentricity, e, over the 1 Myr of our simulations. Each point in the plot shows the mean lifetime of 45 test particles that began the simulations at that particular (a, e) location, which were distributed across a variety of arguments of periastron, ω, and mean anomalies, M. The left-hand panel shows the mean lifetime across the region tested, while the right-hand panel shows the fraction of stable simulations in the same area, along with the locations of the two confirmed planets in the system, and their mean-motion resonances.
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: The dynamical stability of the Earth-mass test particles distributed in the HD 73583 system, as a function of semimajor axis, a, and eccentricity, e, over the 1 Myr of our simulations. Each point in the plot shows the mean lifetime of 45 test particles that began the simulations at that particular (a, e) location, which were distributed across a variety of arguments of periastron, ω, and mean anomalies, M. The left-hand panel shows the mean lifetime across the region tested, while the right shows the fraction of stable simulations in the same area, along with the location of the two known planets, and several of their mean-motion resonances.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: A series of zoom-in plots shows the jet outflow from Centaurus A’s central engine at various spatial scales. On the largest scales, we show the 10–100 kpc jet (B. McKinley et al. 2022) imaged with the Murchison Widefield Array. The Very Large Array image of Centaurus A shows the kiloparsec-scale jet (M. J. Hardcastle et al. 2003), and the Event Horizon Telescope image shows the jet outflow very close to the black hole (M. Janssen et al. 2021). The VLBA jet studied in this work is the intermediate region between the EHT image and the VLA image. The R  g  values shown are along the plane of the sky (not corrected for inclination angle), and are calculated using a mass of 5.5 × 107 M ⊙ (N. Neumayer 2010) and distance of 3.4  Mpc (F. P. Israel 1998).
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: A stacked 7.78 GHz naturally weighted image of Centaurus A during the eight epochs listed in Table 1. The distances are measured from the base of the jet at 7.78 GHz. We also annotate the different components detected in the approaching and receding jets, along with the choice of model component used to represent the feature. The previously detected VLBA components are named using the same names used in PAPER I/II (as C1, C2, C3, and CJ2), and the more recently launched jet components are named using the names used in TANAMI (J7 and J10). The contour levels increase as ﹩\mathrm{noise}\times {\sqrt{2}}^{n}﹩, where n = 3, 5, 7, 9,.... The restoring beam size is shown in gray at the bottom left, and the rms noise in the image is 2.7 mJy beam−1. All pixels below 3 × noise have been masked to be white for better illustration.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Astrometry and proper motion of the jet components detected along the approaching jet (top panel) and the receding jet (bottom panel). The distances of the jet components are measured from the base of the jet at 7.8 GHz (nucleus). In orange, we show data for the components obtained from the literature (PAPER I, PAPER II                      , and TANAMI), along with their errors. The black dashed line is the best-fit proper motion obtained from using our model-fit components along with the ones already published in the literature. The gray shaded area is the 68% high-density interval of our proper motion fit.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The uv coverage at the highest- and the lowest-frequency bands for the epoch BO043A, after having flagged BR, HN, MK, and SC VLBA stations. The baseline lengths are measured in megawavelengths along the east–west and north–south directions.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: The mass–metallicity relationship for giant exoplanets, adapted from D. P. Thorngren et al. (2016) and E. Nasedkin et al. (2024b) and references therein. AF Lep b from this work is indicated by a red star, while AF Lep b with the mass from M. J. Bonse et al. (2024) and metallicity from Z. Zhang et al. (2023) and K. Franson et al. (2024) is indicated by a blue star. Other planets that have metallicities estimated based partially on GRAVITY spectra and petitRADTRANS retrievals, namely β-Pictoris b (GRAVITY Collaboration et al. 2020) and the HR 8799 planets (P. Mollière et al. 2020; E. Nasedkin et al. 2024b), are indicated with black stars. The solar system gas giants, Jupiter and Saturn, are indicated with squares, with bulk abundances from T. Guillot (1999) and D. P. Thorngren et al. (2016). Note that, unlike the other error bars that only include the uncertainty on the planetary abundances, the uncertainties for AF Lep b include the uncertainty on the stellar abundances and the planetary abundances combined.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption:  petitRADTRANS retrieval examples, as described in Section 3.2.3. These three models use the EddySed cloud model with Fe, MgSiO3, and KCl clouds and the RCE-prior-constrained gradient P–T profile. The solid orange line represents a retrieval run with free chemistry and a wide (0.5R J–2.0R J) uniform prior on radius; the dashed magenta line, a run with (dis)equilibrium chemistry and the same wide uniform radius prior; the dotted dark-purple line, a run with (dis)equilibrium chemistry and a restricted (1.2R J–1.5R J) uniform radius prior following Z. Zhang et al. (2023). Each retrieval is labeled with its reduced χ 2; their associated parameters appear in Table 4, lines 13–15.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: Interpolated Exo-REM atmospheric models assuming the dynamical mass as a prior (dashed light blue) and fixing the dynamical mass and evolutionary model prediction for radius (solid dark blue). To better fit the SPHERE H1 band spectrophotometry and the Keck/NIRC2 L’ photometry, the sampler prefers unphysically small radii (high ﹩\mathrm{log}(g)﹩), higher effective temperatures, higher C/O, and lower metallicity. The GRAVITY data rule out higher-temperature models, very low and very high C/O ratios, and solar metallicities and are matched well by the model in either case.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: Model comparisons to the GRAVITY spectrum (not including additional data sets). Shown are models, numbered based on their appearance in Table 4, and the reduced χ 2 of the fit. Most models provide a reasonable fit to the spectrum, but only the cloudy Exo-REM grid and the cloudy, free chemistry petitRADTRANS retrieval result in physically plausible radii (R > 1.1R J).
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption:  P–T profiles corresponding to the retrievals shown in Figure 7. When the sampler is forced to accept solutions with R > 1.2R J, the P–T profile is forced away from RCE and into an isothermal shape. This could be indicative of missing cloud/haze opacity due to the parameterization of cloud particle sizes, as discussed in Section 4.4.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: Posterior distribution of select parameters from the orvara orbit fit visualized in Figure 3 and summarized in Table 3. Complex correlations are apparent between a and e that result in a low-probability tail of more eccentric orbits. The majority of accepted orbits are circular. The component masses are well-constrained, roughly normal distributions.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: Fraction of AF Lep b orbits consistent with stirring AF Lep’s debris disk at 46 ± 9 au (following A. J. Mustill & M. C. Wyatt 2009; T. D. Pearce et al. 2022) for the isochronal age (left; C. P. M. Bell et al. 2015) and the kinematic traceback age (right; J. Lee & I. Song 2024).
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: The posterior distribution of atmospheric parameters for the Exo-REM model fit to our observations for the case where ﹩\mathrm{log}(g)﹩ is not fixed to 3.7, but we adopt the dynamical mass as a prior and let ﹩\mathrm{log}(g)﹩, R vary. Light-blue dashed normal distributions plotted over the 1D marginalized posteriors for parallax (ϖ) and planetary mass (M) denote the adopted priors as explained in Section 3.2.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: The posterior distribution of atmospheric parameters for the Exo-REM model fit to our observations for the case where ﹩\mathrm{log}(g)﹩ is fixed to 3.7, the mass is fixed to the central value of our dynamical mass, and the resulting radius is 1.35R J. Light-blue dashed normal distributions are plotted over the 1D marginalized posteriors for parallax (ϖ) as explained in Section 3.2. Unlike Figure 11, ﹩\mathrm{log}(g)﹩ and mass are not shown, as they were not varied.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: The solar neighborhood ISO distribution, without including the volume sampling rate. The distribution of q < 5 au ISOs of Figure 3 is included as an outline for comparison—there is very little difference apart from the speed distribution.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Predicted distribution of ISOs with similar velocities to 1I and 2I in composition, age, and [M/H]. For comparison, the overall ISO population distribution in Figure 3 is also shown, in gray.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Slices through the continuous three-dimensional velocity distribution of q < 5 au ISOs, calculated with the kNN method described in Section 4.2. Slices through the Sun's velocity (U, V, W = 0, 0, 0) show a peak caused by gravitational focusing not present in other slices.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Same as Figure 3 but for ISOs with q < 1 au.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Same as Figure 3 but for ISOs with q < 30 au.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Comparison of observed (right column) and modeled (left and centered column) images of the V Cyg dust envelope in polarized intensity. The first column corresponds to the model of a spherical envelope (Section 5.2). The second column corresponds to the model of a spherical envelope and disk (Section 5.3). The third column corresponds to the model of a spherical envelope and torus (Section 5.3). The brightness units in the color scale represent polarized flux in a 20 × 20 mas pixel relative to the total flux from the star.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Noise characteristics of DPV ﹩{{ \mathcal R }}_{Q}﹩, ﹩{{ \mathcal R }}_{U}﹩ for observations at 880 nm. (a) ﹩{ \mathcal R }﹩ demodulated using the factor ﹩\cos 18\gamma ﹩. Black lines indicate the ring zones used later in Section 5.3.2 for the noise correlation analysis. (b) Two-point correlation of the noise as a function of the distance between the considered points. Different lines correspond to different ring zones (as described above). The red line shows the function ﹩\exp (-{f}_{r}/{f}_{l})﹩ at fl = 0.065fc. (c) Local standard deviation of noise as a function of the spatial frequency. (d) Spectral filter used for image reconstruction.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Differential polarimetric visibility of V Cyg. The rows correspond to observations in the 550, 625, and 880 nm bands, from top to bottom. The first four columns display the following DPV components: ∣RQ∣, ∣RU∣, ﹩{\rm{\arg }}{R}_{Q}﹩, ﹩{\rm{\arg }}{R}_{U}﹩. Spatial frequency is shown along the axes, with the displayed domain having a size of 2D/λ, where D is the telescope diameter and λ is the wavelength. The fifth column presents the image in polarized intensity, reconstructed as described in Section 4. The units of intensity are flux per 20 × 20 mas pixel, relative to the total stellar flux. Dashes indicate the orientation of the polarization plane. In all panels, north is up, east is to the left.