adsabs/AstroCLIMB huggingface dataset:
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Joint distribution of flattening f and projected obliquity, which we define as the angle between the ﹩\hat{{\boldsymbol{x}}}﹩ and spin angular momentum vectors, for HIP 41378 f, derived from the transit light-curve fitting using the model described in Section 2. The central panel displays the density of solutions in the joint parameter space, with darker shades indicating a higher density of allowed solutions. The marginal histograms above and to the right of the central panel show the projected distributions of f and projected obliquity, respectively. We overlay the prior probability distributions on the marginalized flattening and obliquity for comparison, using dashed gray lines. The posterior distributions highlight the range of possible planetary shapes (flattening f; lower values are more strongly preferred) and axial tilts (projected obliquity; all values are technically allowed by the model). The results suggest a wide range of possible obliquities, indicating a range of potential dynamical histories and orientations of HIP 41378 f.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Illustration of the coordinate system and rotation angles used to model the transit of an ellipsoidal planet. The observer’s line of sight aligns with the ﹩\hat{{\boldsymbol{z}}}﹩-axis, and the ﹩\hat{{\boldsymbol{y}}}﹩-axis is oriented along the horizontal transit chord; the ﹩\hat{{\boldsymbol{x}}}﹩-axis is mutually perpendicular to ﹩\hat{{\boldsymbol{y}}}﹩ and ﹩\hat{{\boldsymbol{z}}}﹩ such that the coordinate system follows the right-hand rule. The ellipsoidal planet’s orbit is described by two rotation angles: α (rotation around ﹩\hat{{\boldsymbol{x}}}﹩) and β (rotation around ﹩\hat{{\boldsymbol{y}}}﹩), which correspond to the mean anomaly and elevation angle, respectively. The orbital distance d is measured to the stellar center; though the star is spherical by assumption, we collapse its geometry to a plane for simplicity. The left panel shows the rotation of the ellipsoid by α, the middle panel illustrates rotation by β, and the right panel depicts the view of an observer. The additional angles ζ, η, and ξ are not shown, but their associated axes ﹩\hat{{\boldsymbol{x}}}^{\prime} ﹩, ﹩\hat{{\boldsymbol{y}}}^{\prime} ﹩, and ﹩\hat{{\boldsymbol{z}}}^{\prime} ﹩ are drawn as a projection.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Analog to Figure 9 of J. W. Barnes & J. J. Fortney (2003), showing the difference between the relative flux of an oblate transit model and the best-fit spherical model, for various values of orientation angle ξ and impact parameter b. The small-amplitude numerical noise visible in the plot is expected since the computations are carried out in single-precision floating-point.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Diagram of the coordinate “snapping” described in the text. The point ﹩\left({x}_{\rm{e}\,},{y}_{\,\rm{e}}\right)﹩ on the boundary of the projected ellipsoid falls outside the stellar disk, so the line integral should be carried out on the dashed purple curve instead of the solid purple curve. This point can be mapped to the point on the disk edge at the same angular displacement λ, ﹩\left({x}_{\rm{d}\,},{y}_{\,\rm{d}}\right)﹩.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Gallery of several validation tests performed against batman (L. Kreidberg 2015) showing the computed light curve (top panel) and absolute residual (bottom panel); the parameters for each test are given in the key below the plot. In the top panel, the light, solid curves are output from batman, and the dark, dashed curves are output from greenlantern, showing qualitative and quantitative agreement. The maximum absolute residual is encountered during ingress and egress and does not exceed 0.5 ppm.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Analog to Figure 4 of J. W. Barnes & J. J. Fortney (2003), showing the difference between the relative flux of an oblate transit model and the spherical counterpart of the same cross-sectional area at mid-transit and b = 0, for various values of impact parameter b. The small-amplitude numerical noise visible in the plot is expected since the computations are carried out in single-precision floating-point.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Performance of the code presented in this work, greenlantern, compared to the popular modeling code batman for spherical transits (L. Kreidberg 2015). By running on a GPU, our code achieves similar timings per sample once at least 104 samples are computed.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Joint parameter distributions when planet f is constrained to be an oblate ellipsoid with nonnegative flattening.
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: Tracking down the swiftest variations in NGC 4051: NICER light curve in the 0.3–3 keV energy range (in blue), extracted from archival observations taken between 2017 November and 2022 March (Δt = 5 s). The corresponding background count rate is plotted in red at the bottom. Bottom panels: a zoomed version of the brightest, Flare A (b), and the fastest flare, Flare B (c) (“0” corresponds to the start time of each event).
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: Power-spectral density analysis: Top: PSDs derived from the 0.3 to 3.0 keV light curves from XMM-Newton (red circles) and NICER (blue squares). The black and magenta lines represent the best-fit models for the XMM-Newton and NICER PSDs, respectively. Bottom: best-fit residuals for the XMM and NICER PSDs.
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: PSDs in the 0.3–0.5 keV range (same as Figure 2). Best-fit models are plotted in the case when αhigh is separate for the XMM and NICER PSDs.
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: Best-fit PSD parameters, i.e., normalization, high-frequency PSD slope, and bending frequency (from top to bottom), plotted as a function of energy. The weighted mean of the PSD parameters is marked by the blue dashed lines.
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: Exploring uncharted variability at high frequencies: Poisson-noise-subtracted PSDs derived from light curves obtained from NICER and XMM-Newton. Heavily binned PSD points are in green.
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: PSDs in the 1.0–3.0 keV range (same as Figure 5).
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: PSDs in the 0.7–1.0 keV range (same as Figure 5).
Paper: High-frequency Power Spectrum of Active Galactic Nucleus NGC 4051 Revealed by NICER
Authors: B. Rani, Jungeun Kim, I. Papadakis, K. C. Gendreau, M. Masterson, K. Hamaguchi, E. Kara, S.-S. Lee, R. Mushotzky
Figure caption: PSDs in the 0.5–0.7 keV range (same as Figure 5).
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Long- and short-cadence transit light-curve data for HIP 41378 f, folded with orbital period Porb = 542.08 days. The reduced long-cadence data are shown in the left panels as scattered points; the short-cadence data are shown on the right with small points, then binned to 30 minutes and plotted with large points. The solid purple curve shows a randomly drawn model from the posterior for comparison. The lower row presents the residual between the maximum likelihood model and the data. If we select the maximum likelihood model with f > 0.1, we obtain the residual shown by the dashed purple curve, which is disfavored with log-likelihood difference ﹩{\rm{\Delta }}\left(\mathrm{log}{ \mathcal L }\right)\approx -3.4﹩.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: A simple illustration of the model degeneracy present when the two semiaxes b and c are equal and the planet is not tidally locked to its host star. For a given value of μ, there is a range of flattenings f and orientation angles η that can produce an identical projection. We show here that the same projection (upper panel) can be produced by two different geometries (lower panel).
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Joint posterior of flattening and obliquity for a simulated light curve of a flattened planet with f = 0.15. For this test case, fitting with greenlantern excludes the f = 0 model. As in Figure 8, the prior probability distribution for the marginalized quantities is shown with dashed gray lines.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Contours of constant μ, as defined in Equation (A1). Along these contours, models are indistinguishable, and the Bayesian parameter posteriors are influenced only by the prior.
Paper: A Long Spin Period for a Sub-Neptune-mass Exoplanet
Authors: Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers, Andrew Vanderburg
Figure caption: Two limiting cases of tidal locking, at arbitrary scale. The solid purple ellipse is not locked to the host star (shown in yellow); the dashed purple ellipse is completely locked. These are the two cases that can currently be simulated using greenlantern.
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: The raw combined Host+SN spectrum is shown as a blue dashed line (top), followed by the host spectrum as a red dotted line extracted from rows neighboring the SN trace in Figure 2 (middle), and the host-subtracted SN spectrum is a black solid line (bottom). The black line is used for spectroscopic classification, and no obvious spectroscopic emission features are present for a redshift in the host spectrum. The NIRCam filters used here are shown in green at the bottom of the figure for reference.
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: (Left column) Full-color images (from PID 2514) using F115W+F150W (blue) F200W+F277W (green), and F356W+F444W (red), with a zoomed-out view on the top and the host of SN 2023aeax on the bottom. (Columns 2–3) Difference images created from the COSMOS-Web and PRIMER visits separated by  ∼1 yr, with the SN 2023aeax position marked with a green indicator. All images are drizzled to 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩03 pix–1, and the cutouts have the same spatial extent.
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: (a) The NIRSpec/MSA slitlet positions over SN 2023aeax for one of the dithered observations. (b), (c) The 2D- and 1D-extracted NIRSpec spectrum for SN 2023aeax. The two absorption lines primarily used for spectroscopic classification of SNe Ia are shown with dotted lines.
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: Luminosity distance measurements from the full sample of SNe Ia from D. Brout et al. (2022) extending to z = 2.22. Black points (with errors) are SNe Ia with spectroscopic classifications, while blue squares (with error) are SNe Ia with photometric classifications. The two strongly lensed SNe Ia with distance measurements are shown as purple triangles. SN 2023aeax is shown as a green star, and ΛCDM is shown as a solid red line. The width of the red line encompasses the width of the current H0 tension, with the center of the line used for reference. The black star is the distance modulus for SN 2023adsy measured in this work with photometry from J. D. R. Pierel et al. (2024a). The best-fit FlatwCDM cosmological constraints from D. Brout et al. (2022; black dashed line) and DES Collaboration et al. (2024; cyan dotted line) are also shown for comparison.
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: The photometry measured in Section 2.1 is shown as black circles with error, with (5σ) upper limits denoted by triangles. The fit to the full light curve is shown as a solid line in each filter, with the shaded region representing the BayeSN model+fitting uncertainty. The time of peak brightness is measured relative to the rest-frame B-band and is reported in Table 4, and the amplitude is set by the luminosity distance (Section 4.1).
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: The host-subtracted NIRSpec spectrum (with uncertainty) of SN 2023aeax is shown as a black solid line, with the primary features used for the preferred SN Ia classification labeled (bottom). The best-match template from NGSF is an SN Ia (blue, +52 days, bottom), and a 91T-like SN Ia subclass (green,  +82 days, second from bottom) is also shown for comparison. The best core-collapse matches are also shown, including Ib (yellow, third from top), Ic (cyan, second from top), and IIP (pink, top). A normal SN Ia is heavily favored based on the spectrum (see Table 3). All phases are rest-frame days relative to peak B-band brightness.
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: Posterior distributions for the BayeSN fitting of SN 2023aeax photometry. The dashed vertical lines correspond to the 16th, 50th, and 84th quantiles of the distribution. The parameters are V-band dust extinction, light-curve shape, time of peak B-band brightness, and distance modulus.
Paper: Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST
Authors: J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft, Y. Zenati
Figure caption: The distributions of rest-frame B − V color at peak B-band brightness, Δm15(B), and host-galaxy properties measured for the cosmological sample of SNe Ia presented in D. Brout et al. (2022). The vertical red dashed lines are the measurements for SN 2023aeax.
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
Authors: Anuroop Dasgupta, Lucas A. Cieza, Camilo González-Ruilova, Trisha Bhowmik, Prachi Chavan, Grace Batalla-Falcon, Gregory Herczeg, Dary Ruiz-Rodriguez, Jonathan P. Williams, Anibal Sierra, Simon Casassus, Octavio Guilera, Sebastian Pérez, Santiago Orcajo, P.H. Nogueira, A.S Hales, J.M. Miley, Fernando R. Rannou, Alice Zurlo
Figure caption: Histograms of the size distribution of the ∼100 brightest systems in Ophiuchus (top panels) with Gaussian fits from the scipy.optimize.curve_fit function in Python. The figures show the size distributions including individual components of close-binary (sep. < 200 au) systems (left panel) and excluding them (right panel). The middle-left panel corresponds to the disk size distribution of stars only in close-binary systems and the restricted sample of binary stars (ie., excluding the faintest secondary components). The middle-right panel presents the cumulative versions of the four distributions. The shaded regions correspond to the uncertainties in the Gaussian fits listed in Table 2. In the bottom-left panel, we plot the disk size as a function of Band 8 flux, finding essentially the same dependence as N. Hendler et al. (2020) found for Ophiuchus disks in Band 6 (size ∝ ﹩{L}_{mm}^{0.6}﹩). Close binaries are indicated as labeled. The bottom-right panel shows the disk size as a function of binary separations. The 0.1 and 0.3 ratios are indicated. The vast majority of objects fall below the 0.1 line. Some outliers are expected because these are projected (not physical) separations. Disk sizes from C. F. Manara et al. (2019) are also shown, but note that their sizes are R95% instead of the HWHM measurements we adopted for binary systems.
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
Authors: Anuroop Dasgupta, Lucas A. Cieza, Camilo González-Ruilova, Trisha Bhowmik, Prachi Chavan, Grace Batalla-Falcon, Gregory Herczeg, Dary Ruiz-Rodriguez, Jonathan P. Williams, Anibal Sierra, Simon Casassus, Octavio Guilera, Sebastian Pérez, Santiago Orcajo, P.H. Nogueira, A.S Hales, J.M. Miley, Fernando R. Rannou, Alice Zurlo
Figure caption: The left panel shows the disk radii fitted in the visibility plane (from uvmodelfit) vs. the disk radii measured in the image plane (from imfit). Both values agree within 3% across the full range. The right panel is the comparison between the R68% size estimates obtained from the Frank profiles and the HWHM values obtained from the Gaussian imfit values. The best-fit line (in red) has a slope of 0.78. Objects with inner dust cavities (transition disks) are indicated and mostly fall above the line.
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
Authors: Anuroop Dasgupta, Lucas A. Cieza, Camilo González-Ruilova, Trisha Bhowmik, Prachi Chavan, Grace Batalla-Falcon, Gregory Herczeg, Dary Ruiz-Rodriguez, Jonathan P. Williams, Anibal Sierra, Simon Casassus, Octavio Guilera, Sebastian Pérez, Santiago Orcajo, P.H. Nogueira, A.S Hales, J.M. Miley, Fernando R. Rannou, Alice Zurlo
Figure caption: The deprojected visibility profile of one of the smallest objects (ODISEA_C4_099), with an estimated HWHM size of 21 mas and a R68% of 29 mas. The visibility profile falls with baseline and is therefore not consistent with a point source. The source is ∼​​​​​​16 mJy in Band 8 and ∼5 mJy in Band 6.