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Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Posterior distributions of stellar inclination for stars hosting hot Jupiters in our sample. Shaded regions show the 68% and 95% credible intervals.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Results from our HBM of the underlying stellar inclination distributions for hot Jupiters (orange) and warm Jupiters (blue). Thin lines in the background show randomly sampled distributions from the α and β hyperparameter posteriors, which represent the shape parameters of the beta distribution. The thick orange and blue curves display the median inferred underlying i * distribution among all hot and warm Jupiter host stars below the Kraft break, respectively. Solid lines represent a truncated Gaussian hyperprior while the dashed lines represent a log-uniform hyperprior. The lower panel displays the residuals of hot Jupiter host stars subtracted from stars harboring warm Jupiters. The two underlying i * distributions are mutually consistent when modeled with the beta distribution, irrespective of the different hyperpriors we tested.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Stellar properties for the hot Jupiter (orange) and warm Jupiter (blue) samples as a function of scaled orbital distance, a/R *. Marginalized histograms of each parameter are shown on the right. From top to bottom panels, projected rotational velocities, stellar radii, rotation periods, and ages are plotted as a function of a/R *. In general the hot and warm Jupiter samples show similar characteristics, but hot Jupiters have a broader spread of ages compared to warm Jupiter hosts, which are typically <5 Gyr. We note that K2-281 does not have a reported age and was therefore not included in the bottom panel.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption:  ψ as a function of i * for all systems with measurements in our sample (Albrecht et al. 2022; Johnson et al. 2022). We find stars that are most likely misaligned in i * space are also most likely misaligned in ψ space. This generates a lower limit on the inferred misalignment. The dashed line corresponds to minimum misaligned obliquities and represents the case where λ = 0, so cos(ψ) = sin(i *). Any departure from 0 will increase ψ for a given i *. The dashed curve corresponds to minimum misaligned obliquities and represents the case where λ = 0, so cos(ψ) = sin(i *).
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption:                          ﹩v\sin i﹩ plotted as a function of v eq for all systems below the Kraft break in our sample. The dashed line represents where our measured v eq values are in agreement with the adopted ﹩v\sin i﹩ values. The gray shaded area corresponds to an unphysical region in which the projected rotational velocity is larger than the equatorial velocity. All stars have ﹩v\sin i﹩ values that are within 2σ of their equatorial velocities. Values to the upper left of the 1:1 line represent misaligned stellar obliquities.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Posterior distributions of stellar inclination for stars hosting warm Jupiters in our sample. Shaded regions show the 68% and 95% credible intervals. The ﹩\sin {i}_{* }﹩ isotropic prior distribution is shown for comparison in the bottom right panel.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Results from our HBM test focusing on scaled orbital distance as a potential bias. Underlying stellar inclination distributions with an a/R * cut at 10 for hot and warm Jupiter host stars are displayed. See Figure 8 for details.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Results from our HBM test focusing on age as a potential bias. Underlying stellar inclination distributions for hot and warm Jupiter host stars younger than 6 Gyr are displayed. See Figure 8 for details.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption:  i * posterior distributions for the 25 hot Jupiter (a/R * < 20; top panel) and 22 warm Jupiter (a/R * > 20; bottom panel) host stars below the Kraft break. These i * posterior distributions are then used as individual likelihood functions in ePop!.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Top: i * as a function of stellar effective temperature for all stars in our sample. Bottom: cos(i *) as a function of stellar effective temperature for all stars in our sample. The gray dashed line marks the transition region above and below the Kraft break at T eff ∼ 6200 K.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Joint posterior distributions of the beta distribution parameters, α and β, in our HBM. Top left: the hot Jupiter sample modeled with a truncated Gaussian hyperprior. Top right: the warm Jupiter sample modeled with a truncated Gaussian hyperprior. Bottom left: the hot Jupiter sample modeled with a log-uniform hyperprior. Bottom right: the warm Jupiter sample modeled with a log-uniform hyperprior.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Normalized Kepler light curves and GLS periodograms for Kepler-9, Kepler-27, Kepler-28, Kepler-30, and Kepler-51. The strongest periodogram peak is marked with a gray dashed vertical line. The light curves are phased to the period corresponding to the peak and shown in the right panel with the median binned phases displayed in cyan dots.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Normalized TESS and Kepler light curves and GLS periodograms for K2-281, K2-329, TOI-1227, TOI-4562, and V1298 Tau.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Normalized Kepler light curves and GLS periodograms for Kepler-52, Kepler-63, Kepler-75, Kepler-289, Kepler-447, and Kepler-468.
Paper: Signs of Similar Stellar Obliquity Distributions for Hot and Warm Jupiters Orbiting Cool Stars
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Erik Petigura, Vighnesh Nagpal, Sarah Blunt
Figure caption: Normalized Kepler light curves and GLS periodograms for Kepler-470, Kepler-486, Kepler-539, Kepler-1654, K2-77, and K2-139.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: An example UDG candidate with a plausible NSC (SMDG 0004118+163159, the second galaxy with what we will classify as an NSC in our R.A.-ordered catalog) with several nearby contaminating sources is presented in the left panel. The mask in the right panel highlights most of the visible nearby sources with the central object shaded in gray, indicating that it is unmasked for the final model fitting but would be masked in the initial model fitting (see text for details).
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: The distribution of normalized radial offsets between S 1 and N 1,PSF, r  p /r  e . Solid blue lines represent the data; the blue dotted lines show the models for the central Gaussian and background that together, modulated by the radial completeness, combine to produce the red dashed line. In the left panel, the background is assumed to follow the S 1 profile, while in the right panel, it is assumed to be randomly distributed on the sky. The models fit the data indistinguishably well, demonstrating that we cannot differentiate between the two background scenarios at the current time and that our conclusions are insensitive to this choice.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: The distribution of host galaxy colors, (g − r)UDG from Table 3, and apparent magnitudes for systems with unresolved sources with r  p /r  e  < 0.10 (NSCs; filled circles) and r  p /r  e  > 0.38 (non-NSCs; open circles). The right panel shows the normalized distributions in color of these two populations (the filled histogram represents NSCs; the unfilled blue solid line represents non-NSCs), as well as that for the full SMUDGes sample (represented by the dashed red line).
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: NSC stellar mass vs. host galaxy stellar mass. Stellar masses are calculated assuming a fixed stellar mass-to-light ratio of 1.8 M ⊙/L ⊙. The solid line and shaded region represent the relationship and its uncertainty presented by Neumayer et al. (2020). The heavy dotted line represents a normalized 1:1 relation where M NSC = 0.019M HOST. The thinner dotted line corresponds to M NSC = 0.1M HOST and represents the upper limit on the NSC mass fraction. Red stars represent UDGs. Blue dots represent the galaxies that do not meet the UDG physical size criterion.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: Absolute magnitude of NSCs, for SMUDGes with estimated distances, across redshift. Systems that are UDGs (r  e  ≥ 1.5  kpc; filled blue circles) and non-UDGs (r  e  < 1.5  kpc; open red circles) are plotted. The curves designate completeness limits corresponding to the three incompleteness fractions shown in Figure 6. We also include a vertical line that indicates the redshift beyond which any object in the SMUDGes catalog would satisfy the size criterion for UDGs, and the redshifts corresponding to the Virgo and Coma clusters.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: NSC detection limits in the r band determined for 100 single Sérsic SMUDGes images as a function of r-band central surface brightness, μ 0,r . Points represent the brightest simulated point source that was not recovered as an NSC by our procedure. Horizontal lines mark where we reach the corresponding incompleteness percentage. The three labeled values correspond to limiting magnitudes of r PSF of 23.2, 24.1, and 24.9 mag.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: Mosaic of galaxies with extreme NSC mass fractions. The top row presents the five galaxies in our sample with the largest NSC mass fraction. The bottom row presents the five UDGs (r  e  ≥ 1.5 kpc) with the largest NSC mass fraction. Images span slightly over an arcminute on a side with north at the top and east to the left. These are drawn from the Legacy Surveys online viewer. Object labels are included at the top of each panel.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: Distribution of n and r  e  for S 2 components when two components are statistically favored over a single component, but no statistically significant difference exists between competing multicomponent models. The box highlights the parameter region where, after visual examination, we reclassify systems as having unresolved sources.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: Mosaic of the first 21 SMUDGes sources in R.A. that have an identified NSC. Images span slightly over an arcminute on a side with north at the top and east to the left. These are drawn from the Legacy Surveys online viewer (https://www.legacysurvey.org/viewer). Object labels are included at the top of each panel.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: Model and residual images for SMDG 0004118+163159. Left to right: the original image, single Sérsic model, residual image using the single Sérsic model, Sérsic + PSF model, and residual image using the Sérsic + PSF model. The need for a central unresolved source is evident when comparing the residual images.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Difference between the surface brightness of the SW and NE sides of the disk. Asymmetric peaks or clumps are detected with MIRI between 40 and 100 au, with both the peak positions and brightnesses varying significantly between 15 and 23 μm. The dashed lines show the Gaussian fit used to estimate the central location of the brightest peak in the asymmetry at each wavelength. Shaded gray areas correspond to 3σ ranges. Color-coded shaded areas correspond to the results from prior observations at 10–12 μm. No significant variation between the SW and NE sides is seen in the NIRCam data for this range of separations.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Left: β as a function of grain size for Ballering et al. (2016) best-fit composition (dotted red) and other compositions/porosities. Our dynamic model requires high β and larger grains, consistent with fluffy refractory organic material. Right: normalized SEDs for the best-fit Ballering et al. (2016) halo component for the main disk (red), as well as three highly porous compositions. Only fluffy organic refractory material can produce a bluer mid-infrared color (higher ratio of F1550C/F2300C) than the Ballering et al. (2016) composition. The solid, dashed, and dotted lines indicate different particle size ranges and/or locations, as labeled in gray.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: False color image generated from the F1550C (15.5 μm, cyan) and F2300C (23 μm, red) images. At these wavelengths, the main disk is redder, while the secondary disk, cat’s tail, and extended nebulosity are bluer. Several linear striations or tendrils just above the cat’s tail are clearly seen, and are consistently blue. As noted in the text, deconvolution of the F1550C data is challenging and leaves residual artifacts along the 4QPM boundaries, as marked.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Synthetic 23 μm thermal emission image of a two-component “toy” steady-state collision point model with β = 0.7 blowout grains and without external forcing (e.g., ISM drag), as discussed in Section 5.1. The left panel shows the projected view oriented the same as Figure 4, and the right panel shows a face-on view looking down onto the disk from the NW. Invoking preferential production of β ∼ 0.7 via porous silicates can produce a cat’s tail–like stream of material, but which seems to be at odds with the surface brightness profile, color, and crook of the cat’s tail.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Orientation of the secondary disk for the steady-state model and our favored sporadic dust production model, which each require a slightly different inclination of the secondary disk. Note that the difference in assumed orientation is for the secondary disk only; in both cases the main disk orientation remains nearly edge on with the NW side nearer to us, as has been inferred from the brightness asymmetry attributed to forward scattering (e.g., Golimowski et al. 2006; Milli et al. 2014; Millar-Blanchaer et al. 2015). The rotation of both disks (main and secondary) is such that the SW side’s orbital motion is toward us, unambiguously known from radial velocity observations of the CO gas (Dent et al. 2014) and the planet β Pic b (Snellen et al. 2014).
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: The MIRI coronagraphy data in F1550C and F2300C (15.5 and 23 μm, respectively) presented with a linear stretch and scaled by the projected distance from the star squared. This stretch better visually emphasizes (a) the brightness asymmetry between the two sides, and (b) the presence of localized peaks or clumps of brightness particularly to the SW. The white arrows indicate the estimated clump locations from the Gaussian fitting shown in Figure 6, at 55.5 ± 3.9 au for F1550C, and 63.4 ± 2.9 au for F2300C. The cyan annotations C1–C4 indicate the angular separations of the clumps reported in ground-based VLT/NEAR 12 μm data (Skaf et al. 2023). Both C1 and C2 are clearly detected in the MIRI F1550C data.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Left: orbital trajectories of grains from a collision point as a function of β (inspired from Figure 1 of Krivov 2010). Middle: steady-state collision point model with β < 2 producing an eccentric disk of dust and a fan of blowout grains. Right: collision point model with periodic dust production events at 100 yr intervals. Individual dust production events leads to curved streams of material that travel outward while forming a spiral, with bound grains eventually populating the main disk.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Cat’s tail surface brightness in both MIRI filters. The left panel shows the contrast with the main disk, where the cat’s tail at 15.5 μm (black line) is consistently brighter, sometimes closer to two orders of magnitude. The right panel shows the surface brightness of the cat’s tail, which is higher at 23 μm (gray line) and decreases constantly with distance to the star. The red shaded area marks the beginning of the cat’s tail feature.