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Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Fe/Mg- and Fe/Si-based CMF as a function of iron metallicity ZFe,*/ZFe,⊙ and for four different photospheric stellar parameter sources. We plot the low-density exoplanets Kepler-36 b and Kepler-105 c as black-bordered blue squares and 55 Cnc e and WASP-47 e as black-bordered green squares. We plot the super-Mercury exoplanet Kepler-107 c as a gray diamond. We plot all other exoplanets as black-bordered open circles. To evaluate the impact of stellar iron metallicity and therefore iron mass fraction on terrestrial exoplanet CMF, we use the Monte Carlo procedure described in the text to calculate Kendall’s τ coefficients and fit linear models to these data after excluding exoplanets inconsistent with pure-rock compositions (i.e., negative CMFs). We plot the linear models that result from our Monte Carlo simulations as blue or green lines and indicate their 16th–84th quantile uncertainty regions with blue or green polygons. We also report in the legend of each panel the numerical values of Kendall’s τ coefficients, slopes, and intercepts, as well as their uncertainties. Left: for the relationship between ZFe,*/ZFe,⊙ and Fe/Mg-based CMF, we find both positive and negative correlations and slopes for which zero is excluded from the 0.1–99.9 interquantile ranges of the Monte Carlo−inferred parameter distributions (corresponding to the 3σ range of a Gaussian) only for abundances based on J. M. Brewer et al. (2016) and J. M. Brewer & D. A. Fischer (2018). Middle left: for the relationship between ZFe,*/ZFe,⊙ and Fe/Si-based CMF, we find both positive and negative correlations and slopes for which zero is only excluded from the 0.1–99.9 interquantile ranges of the Monte Carlo−inferred parameter distributions only for abundances based on J. M. Brewer et al. (2016) and J. M. Brewer & D. A. Fischer (2018). Middle right: for the relationship between ZMg,*/ZMg,⊙ and Fe/Mg-based CMF, we find both positive and negative correlations and slopes for which zero is excluded from the 0.1–99.9 interquantile ranges of the Monte Carlo−inferred parameter distributions (corresponding to the 3σ range of a Gaussian) only for abundances based on J. M. Brewer et al. (2016) and J. M. Brewer & D. A. Fischer (2018). Right: for the relationship between ZMg,*/ZMg,⊙ and Fe/Si-based CMF, we find both positive and negative correlations and slopes for which zero is excluded from the 0.1–99.9 interquantile range of the Monte Carlo−inferred parameter distributions only for abundances based on J. M. Brewer et al. (2016) and J. M. Brewer & D. A. Fischer (2018). We conclude that the relationships between ZFe,*/ZFe,⊙, ZMg,*/ZMg,⊙, and Fe/(Mg,Si)-based CMF are not straightforward and merit further study.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Mass–radius-based CMF as a function of iron metallicity ZFe,*/ZFe,⊙ for four different photospheric stellar parameter sources. We plot the low-density exoplanets Kepler-36 b and Kepler-105 c as black-bordered blue squares and 55 Cnc e and WASP-47 e as black-bordered green squares. We plot the super-Mercury exoplanet Kepler-107 c as a gray diamond. We plot all other exoplanets as black-bordered open circles. To evaluate the impact of stellar iron metallicity and therefore iron mass fraction on terrestrial exoplanet CMF, we use the Monte Carlo procedure described in the text to calculate Kendall’s τ coefficients and fit linear models to these data after excluding exoplanets inconsistent with pure-rock compositions (i.e., negative CMFs). We plot the linear models that result from our Monte Carlo simulations as blue or green lines and indicate their 16th−84th quantile uncertainty regions with blue or green polygons. We also report in the legend of each panel the numerical values of Kendall’s τ coefficients, slopes, and intercepts, as well as their uncertainties. For the relationship between ZFe,*/ZFe,⊙ and mass–radius-based CMF, depicted by the blue lines, we find positive correlations and slopes for which zero is not excluded from the 2nd−98th interquantile ranges of the Monte Carlo−inferred parameter distributions (corresponding to the 2σ range of a Gaussian). If we exclude exoplanets with Mercury-like CMFs, then the significances of the correlations and slopes of the relationships depicted by the green lines are diminished. We conclude that the relationship between ZFe,*/ZFe,⊙ and mass–radius-based CMF is positive but not especially statistically significant given our sample.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Mass–radius-based CMF as a function of magnesium metallicity ZMg,*/ZMg,⊙ for four different photospheric stellar parameter sources. We plot the low-density exoplanets Kepler-36 b and Kepler-105 c as blue squares and 55 Cnc e and WASP-47 e as green squares. We plot the super-Mercury exoplanet Kepler-107 c as a gray diamond. We plot all other exoplanets as open circles. To evaluate the impact of stellar magnesium metallicity and therefore magnesium mass fraction on terrestrial exoplanet CMF, we use the Monte Carlo procedure described in the text to calculate Kendall’s τ coefficients and fit linear models to these data after excluding exoplanets inconsistent with pure-rock compositions (i.e., negative CMFs). We plot the linear models that result from our Monte Carlo simulations as blue or green lines and indicate their 16th−84th quantile uncertainty regions with blue or green polygons. We also report in the legend of each panel the numerical values of Kendall’s τ coefficients, slopes, and intercepts, as well as their uncertainties. For the relationship between ZMg,*/ZMg,⊙ and mass–radius-based CMF, depicted by the blue lines, we find positive correlations and slopes for which zero is not excluded from the 2nd−98th interquantile range of the Monte Carlo−inferred parameter distributions (corresponding to the 2σ range of a Gaussian). If we exclude exoplanets with Mercury-like CMFs, then the significances of the correlations and slopes of the relationships depicted by the green lines are diminished. We conclude that the relationship between ZMg,*/ZMg,⊙ and mass–radius-based CMF is positive but not especially statistically significant given our sample.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Mean CMFs for all three subsamples in our overall sample. In all three subsamples, the mean CMF of the population of terrestrial exoplanets in or likely formerly in mean motion resonances is about 3σ lower than the mean CMF of the other exoplanets in our sample. Likewise, the population of USP exoplanets orbiting metal-rich stars with multiple giant exoplanet companions has a mean CMF about 6σ lower than the mean CMF of the other exoplanets in our sample. It is inconsistent with a 100% rock composition. These observations confirm that the populations of both terrestrial exoplanets that are in or likely formerly in mean motion resonances and USP exoplanets orbiting metal-rich stars with multiple giant exoplanet companions are qualitatively different from the rest of the exoplanets in our sample. Resonant configurations suggest migration inward from more distant formation locations, so we attribute the low CMFs of terrestrial exoplanets in or formerly in mean motion resonances to the incorporation and retention of water in their interiors during their formation. We propose that the population of USP exoplanets orbiting very metal-rich stars with multiple giant exoplanet companions are the remnant cores of tidally disrupted mini-Neptunes, and we associate their low densities with the presence of significant hydrogen, helium, water, and/or other volatiles in their interiors.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Expected Doppler semiamplitude imparted on a solar-mass host star by a super-Earth with orbital period P = 2 days and Rp = 1.6 R⊕ as a function of CMF superimposed on the S. S. Brems et al. (2019) relationship between stellar age and radial velocity jitter. The solid blue line is the maximum likelihood S. S. Brems et al. (2019) relationship, while the light-blue polygon is the 16th–84th interquantile range; the horizontal black lines indicate the Doppler semiamplitudes imparted by the hypothesized super-Earths. We find that while high-CMF super-Earths can be detected in the presence of radial velocity jitter at all ages, low-CMF super-Earths can only be detected orbiting host stars with ages in excess of 5 Gyr. This observational bias against the detection of low-CMF terrestrial exoplanets orbiting young stars can easily explain the statistically significant inverse correlation identified by A. Weeks et al. (2025) between host star age and either the logarithm of planet density or iron mass fraction.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Comparison of posterior probability density functions for the occurrence of Mercury-like planets Θmerc in the solar system and in our sample of terrestrial exoplanets. Our inference of the occurrence of Mercury-like planets in the solar system ﹩{{\rm{\Theta }}}_{\,\rm{merc,ss}\,}=0.2{5}_{-0.16}^{+0.24}﹩ is consistent with the occurrence of super-Mercuries in the terrestrial exoplanet population ﹩{{\rm{\Theta }}}_{\,\rm{merc,exo}\,}=0.0{4}_{-0.03}^{+0.05}﹩. The probability that our super-Mercury occurrence inference is consistent with the value Θmerc,exo ≈ 0.2 put forward by V. Adibekyan et al. (2021) and C. T. Unterborn et al. (2023) is about 1% (equivalent to 2.3σ assuming Gaussian statistics).
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Top: relationship between host star age and exoplanet density. Unlike A. Weeks et al. (2025), we find no statistically significant inverse correlation between host star age and either exoplanet density or its logarithm. Bottom: relationship between host star age and exoplanet CMF. Like A. Weeks et al. (2025), we find a statistically significant inverse correlation between host star age and planetary CMF. Unlike A. Weeks et al. (2025), we attribute this inverse correlation to an observational bias: exoplanets in the super-Earth radius range with low CMFs will only yield Doppler-based mass inferences if they orbit quiescent and therefore very old stars.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Comparison between JWST-MIRI and Spitzer-IRS spectra of BP Tau. Top: the red line shows the Spitzer-IRS spectra (R ∼ 60–100). Dashed blue lines show the full wavelength coverage of the JWST-MIRI at its full resolving power(R ∼ 1600–3400); the solid blue line shows JWST-MIRI spectra convolved to the IRS resolution. Bottom: difference between IRS and the continuum of the JWST-MIRI spectra (black solid line). The gray solid line marks a difference equal to 0; dashed gray lines mark a difference of ±0.05 (5%).
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Distribution of the SS summary statistics for the distinct clusters identified by the VAE model from the GALFA-H I data set. The top left and right panels correspond to power and sparsity, while the bottom panels correspond to filamentarity, as specified by Equations (7)–(9). The morphological interpretations behind each coefficient shows a consistent picture where cluster 0 describes a sparse, filamentary CNM, cluster 1 describes a diffuse WNM, and cluster 2 corresponds to the noise component. The qualitative scale-dependent behavior of each cluster is also consistent with the simulation results in Figure 2.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Spectral distribution of the total H I emission and the SS+VAE decomposed CNM and WNM components for sightlines with a minimal level of predicted CNM content of 1019 cm−2. Left: Spectral distribution of the total, CNM, and WNM components for a sample sightline at (R.A., decl.) = (155﹩\mathop{.}\limits^{^\circ }﹩5, 24﹩\mathop{.}\limits^{^\circ }﹩1). Right: the histogram of the FWHM distribution for total, CNM, and WNM emission over all sightlines. The red dashed line marks the typical limit of FWHM <7 km s−1 adopted in Gaussian decomposition of CNM components. Here, 92% of CNM sightlines have FWHM <7 km s−1 while 95% of WNM sightlines have FWHM >7 km s−1.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: The SS+VAE CNM and WNM maps over the same continuous 19° × 51° footprint as in Figure 9. The red, green, and blue colors correspond to velocity channels between −3 < v < 40 km s−1, −15 < v < −3 km s−1, and −40 < v < −15 km s−1, respectively.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Comparing the LOS-integrated CNM column density prediction by the SS+VAE model vs. the M20 map for select regions. From left to right are the original image, the M20 CNM, the SS+VAE CNM, and the correlation between the two CNM maps. The white line indicates one-to-one correspondence.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Image realizations synthesized from the SS coefficient clusters identified by the VAE model from the GALFA-H I data set. The images are initialized to Gaussian random noise. The top, middle, and bottom rows correspond to the clusters that describe the CNM, WNM, and noise, respectively.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Comparing the LOS-integrated CNM column density prediction by the SS+VAE model vs. the M20 map for a continuous 19° × 51° footprint between ﹩152\mathop{.}\limits^{^\circ }3\lt {\rm{R}}.{\rm{A}}.\lt 203\mathop{.}\limits^{^\circ }5﹩ and ﹩7\mathop{.}\limits^{^\circ }8\lt \mathrm{decl}\lt 27\mathop{.}\limits^{^\circ }0﹩. The SS+VAE CNM map is stitched together from ﹩256^{\prime} \times 256^{\prime} ﹩ patches, applying weighted average in overlapping regions. The SS+VAE map shows continuous large-scale features and is highly correlated with the M20 map, with a Pearson coefficient of 0.76 in the footprint shown.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: Result of SS+VAE phase separation for a example sightline centered at (R.A. = 137°, decl. = 14°) across different velocity channels. Each column from left to right corresponds to the original image, and the decomposed CNM, WNM, and noise components respectively. The decomposed components show morphological features consistent with what we expect for each phase.
Paper: Neutral Gas Phase Distribution from H I Morphology: Phase Separation with Scattering Spectra and Variational Autoencoders
Authors: Minjie Lei, S. E. Clark, Rudy Morel, E. Allys, Iryna S. Butsky, Caleb Redshaw, Drummond B. Fielding
Figure caption: GALFA-H I denoising result shown for a 17° × 17° region at v = 18 km s−1, spanning 185﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3 < R.A. < 202﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4 and 8﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9 < decl. < 26﹩\mathop{.}\limits^{\unicode{x000b0}}﹩0. The left and middle panels show the original GALFA-H I emission map and the SS+VAE denoised map, respectively. The right panel compares the power spectra of the original and denoised maps.
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: A three-color NIRCam composite image of the JWST field of view of M83, using the F115W (blue), F187N continuum-subtracted (green), and F335M continuum-subtracted (red). The white circles represent informed environmental regions as a function of galactocentric distance: the center, the bar, the end of the bar, and the outer regions. The light-blue circles have been obtained by dividing the galaxy into bins containing the same numbers of combined eYSCs and oYSCs. In this second division, we exclude the center (inner blue circle) and define the bar, the leading inner-bar region, the trailing outer-bar region, and the outer region (see Section 5.3).
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: A three-color composite (panel (A)) of a giant star-forming complex in M83 (4﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 × 8﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 corresponding to a 105 × 195 pc): the green channel transmits the continuum-subtracted 3.3 μm PAH  map (also shown in panel (B)); red: continuum-subtracted Paα map (panel (C))); blue: HST/F555W (panel (D))). Different classes of identified star clusters are overplotted as circles of a five-pixel radius (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩28 corresponding to 6.4 pc), with eYSCI in red, eYSCII in yellow, 3.3 μm PAH peaks in green, and YSCs (younger than 10 Myr) in cyan. In the 3.3 μm PAH map, eYSCI and 3.3 μm PAH peak systems appear to have compact emission. The eYSCII sit in regions where 3.3 μm PAH emission is significant, but they are not associated with a compact morphology. In panel (C), eYSCI and eYSCII are clearly associated with compact Paα emission, while a compact counterpart is not seen in any of the 3.3 μm PAH peaks. In panel (D), optical YSCs with ages ≤10 Myr are associated with strong continuum emission, while that is not always the case with eYSCs, suggesting that the latter are significantly more reddened.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: The total mass of solids in the NC region at 2 Myr as a function of turbulent alpha and the maximum pebble relative velocity ﹩{v}_{{\rm{\max }}}﹩, assuming that pebble size is set by ﹩{v}_{{\rm{\max }}}﹩. The barrier is located at 5 au.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: The total mass of solids in the NC region at 2 My as a function of turbulent alpha and the maximum pebble relative velocity ﹩{v}_{{\rm{\max }}}﹩, assuming that pebble size is set by ﹩{v}_{{\rm{\max }}}﹩. Here, the barrier is located at 3 au.
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: A three-color HST composite of the FEAST JWST FOV. The mosaic shows the HST/F336W (blue), HST/F438W (green), and HST/F657N (red) bands. Different populations of star clusters are overplotted as circles, with eYSCI in red, eYSCII in yellow, 3.3 μm PAH peaks in blue, and oYSCs (younger than 10 Myr) in cyan. We note that eYSCs are closely located along dusty lanes, while YSCs are cospatial with the regions with the strongest near-UV radiation.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: The total mass of solids in the NC region at 2 Myr as a function of turbulent alpha and the maximum pebble relative velocity ﹩{v}_{{\rm{\max }}}﹩, assuming that pebble size is set by ﹩{v}_{{\rm{\max }}}﹩. The barrier is located at 10 au.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: Solid-to-gas volume density ratio for the 4 simulations shown in Figure 3.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: The total mass of solids in the NC region at 2 Myr as a function of turbulent alpha and the pebble radius R, assuming that R is fixed. The barrier is located at 5 au.