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Paper: Zeeman Doppler Imaging of τ Ceti: The Weakest Magnetic Field Detected in a Sun-like Star
Authors: Federica Chiti, Oleg Kochukhov, Jennifer L. van Saders, Travis S. Metcalfe
Figure caption: Properties of the global magnetic morphologies for cool main-sequence stars obtained via ZDI. All values of Rossby numbers are calculated from the Gaia GBP–GRP color using the asteroseismic calibration of E. Corsaro et al. (2021), normalized by the solar value on this scale (Ro⊙ = 0.496). The location of τ Ceti is highlighted with an arrow and labeled. The critical Rossby number, Rocrit = 0.91 ± 0.03 (N. Saunders et al. 2024), is shown as a vertical dashed black line, with a shaded gray band representing its uncertainty. Data for τ Ceti are from this work. All other data are from J. F. Donati et al. (2008), A. Morgenthaler et al. (2012), S. V. Jeffers et al. (2014), S. Boro Saikia et al. (2015), I. A. Waite et al. (2015), S. Boro Saikia et al. (2016), J. D. do Nascimento et al. (2016), C. P. Folsom et al. (2016), S. Boro Saikia et al. (2018), C. P. Folsom et al. (2018a, 2018b), V. See et al. (2019b), C. P. Folsom et al. (2020), E. L. Brown et al. (2021), T. Willamo et al. (2022), S. Bellotti et al. (2024), T. S. Metcalfe et al. (2024), S. Bellotti et al. (2025), and T. S. Metcalfe et al. (2025).
Paper: Zeeman Doppler Imaging of τ Ceti: The Weakest Magnetic Field Detected in a Sun-like Star
Authors: Federica Chiti, Oleg Kochukhov, Jennifer L. van Saders, Travis S. Metcalfe
Figure caption: LSD profiles of τ Ceti derived from ESPaDOnS data. The Stokes I (left), V (middle), and null profile (right) are offset vertically for display purposes. The different rotational phases are shown in the Stokes I panel. Percentage mean errors on the computed LSD Stokes V profile are indicated with an error bar in the middle panel.
Paper: Zeeman Doppler Imaging of τ Ceti: The Weakest Magnetic Field Detected in a Sun-like Star
Authors: Federica Chiti, Oleg Kochukhov, Jennifer L. van Saders, Travis S. Metcalfe
Figure caption: Result of the ZDI analysis of τ Ceti. The three rectangular maps represent the surface distributions of the radial, meridional, and azimuthal magnetic field components. The color bar indicates the polarity and strength (in G) of the magnetic field. The gray shaded area at southern latitudes represents the portion of the stellar surface that remains hidden from view due to the star’s low inclination. The two vertical panels show a comparison between the observed (black) and model (red) Stokes I and V. The spectra are offset vertically, with the rotational phase indicated next to each profile.
Paper: Sub-Neptunes Are Drier than They Seem: Rethinking the Origins of Water-rich Worlds
Authors: Aaron Werlen, Caroline Dorn, Remo Burn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Envelope H2O mass fraction as a function of semimajor axis. The same data set as in Figure 1 is shown. The left panel shows planets that predominantly formed inside the water ice line; the right panel shows those that formed outside. Classification is based on the accreted H2O mass fraction, with a threshold set at 5% of the total planetary mass. The colorbar indicates the molar bulk C/O ratio. Planets formed inside the ice line are systematically depleted in carbon due to the lack of volatile ice accretion and exhibit higher envelope H2O mass fractions. In contrast, planets formed beyond the ice line retain lower H2O content despite higher bulk volatile abundances. Each pie chart shows the mean mass fraction of hydrogen in H2 (gas), H (metal), H2 (silicate), H2O (gas), and H2O (silicate), normalized to the total mean hydrogen inventory for each population. Only components contributing more than 5% are labeled. Planets that formed beyond the ice line store most hydrogen as H2 (gas) and H (metal), while those that formed inside the ice line retain a larger share of hydrogen in H (metal), H2 (silicate), and H2O (gas + silicate).
Paper: Sub-Neptunes Are Drier than They Seem: Rethinking the Origins of Water-rich Worlds
Authors: Aaron Werlen, Caroline Dorn, Remo Burn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Atmosphere–magma ocean interface (AMOI) temperature vs. AMOI pressure. The same data set as in Figure 1 is shown. The colorbar indicates the mass fraction of H2O in the envelope. The gray dashed region marks the domain where pure H2O exists in the supercritical state (Y. Yang 2007). The dashed and dotted lines indicate the H2–H2O solvus at 0.68 wt% H2 and 0.17 wt% H2, respectively. The latter corresponds to the critical composition where the solvus in pressure-composition space reaches its minimum (A. Gupta et al. 2025). Planets to the left of the solvus fall within the one-phase regime, where H2 and H2O are fully miscible. Planets to the right lie in the two-phase regime, where the two species coexist as separate phases. Most planets with high H2O gas mass fractions lie within the one-phase regime.
Paper: Sub-Neptunes Are Drier than They Seem: Rethinking the Origins of Water-rich Worlds
Authors: Aaron Werlen, Caroline Dorn, Remo Burn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Equilibrated H2O mass fraction as a function of total planet mass, using the same data set as in Figure 1. The colorbar indicates the molar bulk C/O ratio. The gray dashed lines mark the lower and upper estimates of Earth’s water mass fraction, corresponding to 1 and 11 Earth oceans (EO), respectively. This estimate agrees well with our results, suggesting that the H2O content of sub-Neptunes is broadly consistent with Earth’s upper bound. A negative correlation is visible between planet mass and H2O content for planets with high C/O ratios.
Paper: Sub-Neptunes Are Drier than They Seem: Rethinking the Origins of Water-rich Worlds
Authors: Aaron Werlen, Caroline Dorn, Remo Burn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Envelope H2O mass fraction as a function of envelope mass fraction, using the same data set as in Figure 1. The colorbar indicates the molar bulk C/O ratio. Planets with low envelope mass fractions tend to retain a higher proportion of H2O in the gas phase. Moreover, planets with low C/O ratios consistently show higher H2O content compared to their carbon-rich counterparts.
Paper: A New Subclass of Carbon-enhanced Metal-poor Stars at Extremely Low Metallicity
Authors: Young Sun Lee, 영선 이, Timothy C. Beers, Yutaka Hirai, Jihye Hong, Miji Jeong, Changmin Kim, Young Kwang Kim
Figure caption: A(C) distribution of our LR sample, as a function of [Fe/H]. The black and white scale represents the logarithmic number density. The red dots are the stars from the HR sample; the green-filled circles are CEMP-no stars classified by [Ba/Fe] < 0.0 from the HR sample. Note that stars with upper limits of [Ba/Fe] > 0 are also regarded as CEMP-no stars. The green solid line is at [C/Fe] = +0.7. The blue box is the region of interest for further consideration of our proposed Group IV (see Section 4.3 for the boundary definition). The magenta open squares and circles are the recognized single and binary CEMP-no stars, respectively. The cyan-open squares and circles represent the recognized single and binary CEMP stars from our LR sample, respectively (see the main text).
Paper: A New Subclass of Carbon-enhanced Metal-poor Stars at Extremely Low Metallicity
Authors: Young Sun Lee, 영선 이, Timothy C. Beers, Yutaka Hirai, Jihye Hong, Miji Jeong, Changmin Kim, Young Kwang Kim
Figure caption: A(C) histograms of our LR sample in different ranges of [Fe/H]. Note that we adopt the HR measurements for overlapping stars between the LR and HR samples. The metallicity range is indicated at the top right of each panel. The bin size is 0.2 dex. Ntot is the total number of stars in each metallicity interval. The red, blue, and magenta curves are fits to the A(C) histogram with a three-component Gaussian mixture model; the green line represents the sum of the three components. The separation of the three components becomes more evident as metallicity decreases. The dashed vertical lines shown in the lower panel are the divisions between the Group II and Group III stars (A(C)  = 6.74) and between the Group III and the proposed Group IV stars (A(C)  = 7.39), respectively, derived from the Gaussian mixture model.
Paper: A New Subclass of Carbon-enhanced Metal-poor Stars at Extremely Low Metallicity
Authors: Young Sun Lee, 영선 이, Timothy C. Beers, Yutaka Hirai, Jihye Hong, Miji Jeong, Changmin Kim, Young Kwang Kim
Figure caption: The Yoon–Beers diagram of the CEMP stars from our LR sample. Guided by the morphological scheme of J. Yoon et al. (2016), we identify Groups I, II, and III, as indicated by the colors of their ellipses. The magenta ellipse represents the region where the proposed new Group IV stars reside. The magnitudes of the minor axes of Group III and Group IV are set to 2σ of the Gaussian fit to the A(C) histogram in the bottom panel of Figure 5. The cyan dashed lines indicate the peak of each group, while the red solid lines are the dividing lines between the groups. Other symbols are the same as in Figure 4.
Paper: A New Subclass of Carbon-enhanced Metal-poor Stars at Extremely Low Metallicity
Authors: Young Sun Lee, 영선 이, Timothy C. Beers, Yutaka Hirai, Jihye Hong, Miji Jeong, Changmin Kim, Young Kwang Kim
Figure caption: Similar to Figure 3, but with Group IV candidates excluded (all stars in the blue box of Figure 4 are treated as Group IV). Note that brown (LR CEMP-no/CEMP) and navy (HR CEMP-no/CEMP) symbols indicate the cumulative fractions of CEMP-no stars relative to all CEMP stars for the LR and HR samples, respectively (see the main text for details).
Paper: Extreme Anisotropies in Deep Layers of an Exploding Star: Overabundance of Cr in the Northeastern Jet of Cassiopeia A
Authors: Vincenzo Sapienza, Marco Miceli, Masaomi Ono, Shigehiro Nagataki, Takashi Yoshida, Emanuele Greco, Salvatore Orlando, Fabrizio Bocchino
Figure caption: Upper-left panel: counts image of Cas A with colorbar in logarithmic scale. The yellow box highlights the zoom region for the other panel and the green circle marks the background region used for the spectral analysis. Upper-right panel: close-up view of the Chandra/ACIS flux map of Cas A in the region of the northeastern jets in the 0.7−8.0 keV band and with the dimension of a pixel of ∼0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5. Source regions of the spectral analysis (S1, S2, and S3) of the different jets are marked with colored polygons. The color scale is linear in units of photons cm−2 s−1. Lower panels: same as the upper-right panel but in the 5.5−5.8 keV band (left panel) and in the 6.3–6.9 keV band (right panel). The pixel size is ∼2″ and source regions for the detection of Cr (C1, C2, and C3) are marked with colored polygons.
Paper: Extreme Anisotropies in Deep Layers of an Exploding Star: Overabundance of Cr in the Northeastern Jet of Cassiopeia A
Authors: Vincenzo Sapienza, Marco Miceli, Masaomi Ono, Shigehiro Nagataki, Takashi Yoshida, Emanuele Greco, Salvatore Orlando, Fabrizio Bocchino
Figure caption: Left panel: Chandra/ACIS spectra extracted from the regions shown in Figure 1 (lower panels), with their corresponding best-fit model and residuals, obtained by letting the Cr abundance free to vary (solid lines for the models and central subplot for the residuals), and fixed to the solar value (dashed lines for the models and lower subplot for the residuals). The three spectra were multiplied by different scaling factors, as indicated in the figure label, to improve visibility. Right panel: Chandra/ACIS spectra extracted from the regions shown in Figure 1 (upper panels), with their corresponding best-fit model and residuals. The three spectra were multiplied by different scaling factors, as indicated in the figure label, to improve visibility.
Paper: Extreme Anisotropies in Deep Layers of an Exploding Star: Overabundance of Cr in the Northeastern Jet of Cassiopeia A
Authors: Vincenzo Sapienza, Marco Miceli, Masaomi Ono, Shigehiro Nagataki, Takashi Yoshida, Emanuele Greco, Salvatore Orlando, Fabrizio Bocchino
Figure caption: Mass fractions of Si, S, Ar, Ca, and Cr with respect to Fe in the one-dimensional CCSN nucleosynthesis model with ﹩{E}_{{\rm{\exp }}}=3\times 1{0}^{51}﹩ erg as a function of the Lagrangian mass coordinates (Mr). The shaded areas are the range (2σ confidence level) of mass fractions measured by our spectral analysis in regions S1, S2, and S3 (left, center, and right panels, respectively). The colors of shaded regions are semitransparent; overlapped areas are shown as color composites. Gray arrows and square points mark where the model and the observation match. The red and black ticks on the upper border indicate the corresponding peak densities and temperatures, respectively. The vertical dashed lines denote the transition points between the iron- and silicon-dominated regions, which approximately separate the complete Si burning via α-rich freeze-out from the incomplete Si burning with quasi-statistical equilibrium. In regions S1 and S3, the observed ranges of Ar and Ca are almost overlapped with each other.
Paper: Extreme Anisotropies in Deep Layers of an Exploding Star: Overabundance of Cr in the Northeastern Jet of Cassiopeia A
Authors: Vincenzo Sapienza, Marco Miceli, Masaomi Ono, Shigehiro Nagataki, Takashi Yoshida, Emanuele Greco, Salvatore Orlando, Fabrizio Bocchino
Figure caption: The combinations of two Lagrangian points consistent with the observed mass ratios for the region S2 are shown as shaded colors for S, Ar, Ca, and Cr. The relevant mass fractions are derived by the average of two Lagrangian points with weights recovering the observed Si/Fe ratio. The horizontal (Mr1) and vertical (Mr2) axes denote the mass coordinates of the first (inner) and the second (outer) Lagrangian points, respectively. Then, the regions in the two-dimensional grid consistent with the observed 2σ ranges are shown. The colors of shaded regions are semitransparent; overlapped areas are shown as color composites.
Paper: Unveiling Unprecedented Fine Structure in Coronal Flare Loops with the DKIST
Authors: Cole A. Tamburri, Maria D. Kazachenko, Gianna Cauzzi, Adam F. Kowalski, Ryan French, Rahul Yadav, Caroline L. Evans, Yuta Notsu, Marcel F. Corchado-Albelo, Kevin P. Reardon, Alexandra Tritschler
Figure caption: Example of fine-scale coronal strands studied in this work. (a) VBI-red Hα image from 20:12:40 UT (r0 = 12.2 cm). Yellow boxes indicate the three regions near the loop top where we investigate the coronal strand width. (b)–(d) Regions of interest for loop width determination in Section 4.1. Colored line cuts are placed perpendicular to the thin strands investigated here. (e) Intensity profiles along the coronal strands indicated by the cuts in panels (b)–(d). They can vary between ∼100 and ∼250 km in length. Dots on each profile are separated by ∼12 km. Colors indicate the corresponding features in panels (b)–(d). Red solid lines indicate a fit of the data to a function as in Equation (1), from which the FWHM loop width is determined. Dashed intensity profiles without displayed fits in red indicate the features for which the algorithm could not find a successful fit. We note the derived widths of each feature. Axis labels in panels (a)–(d) are in kilometers along the respective axes in the VBI images; in panel (e), axis labels are in kilometers along the perpendicular cuts.
Paper: Unveiling Unprecedented Fine Structure in Coronal Flare Loops with the DKIST
Authors: Cole A. Tamburri, Maria D. Kazachenko, Gianna Cauzzi, Adam F. Kowalski, Ryan French, Rahul Yadav, Caroline L. Evans, Yuta Notsu, Marcel F. Corchado-Albelo, Kevin P. Reardon, Alexandra Tritschler
Figure caption: Summary of loop widths in each of the 20 best-seeing image frames indicated in Table 1. (a) Histograms of the loop width distributions in each frame. Colors do not correspond to those in Figure 2(e). Black dotted vertical lines indicate the distribution means. The third panel in the leftmost column is the distribution corresponding to the features shown in Figure 2. Vertical red lines in the bottom panel of the leftmost column indicate the spatial resolution of DKIST/VBI and BBSO/GST. (b) Loop widths with errors for all frames studied. Alternating shaded regions indicate the features from each of the three regions in Figure 2, which are the same for all 20 frames. (c) Combined distribution of calculated widths from all 20 frames, with the mean and median of the distribution and the VBI and GST resolution limits indicated.
Paper: Evidence for Intrinsic Galaxy Alignments in Ellipticity Autocorrelations Out to 100 h−1 Mpc from SDSS Galaxies with DESI Imaging
Authors: Teppei Okumura
Figure caption: Multipole moments of the intrinsic ellipticity autocorrelation functions expanded in the standard Legendre basis, measured from SDSS LRG (left), LOWZ (middle), and CMASS (right) galaxy samples. The upper set shows the II(+) correlation multipoles, ξ+,ℓ, while the lower set shows the II(−) multipoles, ξ−,ℓ, for ℓ = 0 (monopole; circles) and ℓ = 2 (quadrupole; squares). The correlation amplitude for the LRG sample is multiplied by 1/4. The LRG results are reproduced from T. Okumura & A. Taruya (2023), while the LOWZ and CMASS measurements incorporate high-quality DESI imaging data, significantly improving the signal. The solid curves are the best-fit nonlinear model fitted using the data points enclosed by the vertical lines. The dotted curves are the linear predictions.
Paper: Evidence for Intrinsic Galaxy Alignments in Ellipticity Autocorrelations Out to 100 h−1 Mpc from SDSS Galaxies with DESI Imaging
Authors: Teppei Okumura
Figure caption: Upper panels: similar to Figure 1, but L = 4 moments of II(−) correlation functions of SDSS galaxies expanded by the associated Legendre basis, ﹩{\widetilde{\xi }}_{-,L}﹩. The solid curves are the best-fit nonlinear alignment and RSD models fitted using the data points enclosed by the vertical lines. Lower panels: same as upper panels, but the vertical axes are multiplied by r2 so that they can be directly compared to the statistics shown in Figure 1.
Paper: Evidence for Intrinsic Galaxy Alignments in Ellipticity Autocorrelations Out to 100 h−1 Mpc from SDSS Galaxies with DESI Imaging
Authors: Teppei Okumura
Figure caption: Constraints on (bKσ8, σv) from II correlation multipoles of the LOWZ sample at 6 ≤ r ≤ 100 h−1 Mpc. The contours show the 68%, 95%, and 99.7% confidence levels from inward. The dashed line represents the linear-theory prediction for velocity dispersion.
Paper: UNCOVER/MegaScience: No Evidence of Environmental Quenching in a z ∼ 2.6 Protocluster
Authors: Richard Pan, Katherine A. Suess, Danilo Marchesini, Bingjie Wang, 冰洁 王, Joel Leja, Sam E. Cutler, Katherine E. Whitaker, Rachel Bezanson, Sedona H. Price, Lukas J. Furtak, John R. Weaver, Ivo Labbé, Gabriel Brammer, Yunchong Zhang, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Karl Glazebrook, Tim B. Miller, Ikki Mitsuhashi, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Adi Zitrin
Figure caption: Top left: redshift histogram of all galaxies in the redshift range centered around cosmic noon adopting the “best” available redshift as detailed in Section 2.1. Bottom left: redshift histogram from refitting the photometry with a uniform redshift prior at zspec ± 0.1. The overdensity is centered at z ≈ 2.58 (red), while the field was selected at higher and lower redshifts. Top right: comparison of the photo-zs and spec-zs of 259 spectroscopically observed galaxies. The quiescent galaxies are shown in red, the star-forming galaxies are shown in blue, the UNCOVER objects are shown as crosses, and the ALT objects are shown as diamonds. Bottom right: residuals of the spectroscopically observed galaxies (zphot − zspec). The red and purple stripes denote the overdensity and field redshift ranges. Our σNMAD ≈ 0.010 is consistent with the σNMAD ≈ 0.015 found in K. A. Suess et al. (2024) and highlights the constraining power of the medium-band photometry.
Paper: UNCOVER/MegaScience: No Evidence of Environmental Quenching in a z ∼ 2.6 Protocluster
Authors: Richard Pan, Katherine A. Suess, Danilo Marchesini, Bingjie Wang, 冰洁 王, Joel Leja, Sam E. Cutler, Katherine E. Whitaker, Rachel Bezanson, Sedona H. Price, Lukas J. Furtak, John R. Weaver, Ivo Labbé, Gabriel Brammer, Yunchong Zhang, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Karl Glazebrook, Tim B. Miller, Ikki Mitsuhashi, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Adi Zitrin
Figure caption: Left: comparison of the formation time (﹩{t}_{50}^{\,\rm{lb}\,}﹩) and the quenching time (﹩{t}_{90}^{\,\rm{lb}\,}﹩) in three stellar mass bins: low mass (8.5 < log(M⋆/M⊙) ≤ 9.0), intermediate mass (9.0 < log(M⋆/M⊙) ≤ 10.0), and high mass (10.0 < log(M⋆/M⊙) ≤ 11.0). Middle: comparison of the Δt timescale vs. the redshift in the same stellar mass bins. Right: stacked SFHs of the protocluster and field galaxies in the same stellar mass bins. The shaded regions indicate the 1σ uncertainty, while the dashed lines indicate the median SFHs. We compare the distributions in the left and middle panels using a KS test and find them to be statistically indistinguishable. Similarly, the stacked SFHs in the right panels are consistent within 1σ demonstrating similar quenching pathways irrespective of environment.
Paper: UNCOVER/MegaScience: No Evidence of Environmental Quenching in a z ∼ 2.6 Protocluster
Authors: Richard Pan, Katherine A. Suess, Danilo Marchesini, Bingjie Wang, 冰洁 王, Joel Leja, Sam E. Cutler, Katherine E. Whitaker, Rachel Bezanson, Sedona H. Price, Lukas J. Furtak, John R. Weaver, Ivo Labbé, Gabriel Brammer, Yunchong Zhang, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Karl Glazebrook, Tim B. Miller, Ikki Mitsuhashi, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Adi Zitrin
Figure caption: We show the best-fit population models centered at the mean, μ, with a dispersion of σ. The columns are a comparison of ﹩{t}_{50}^{\,\rm{lb}\,}﹩, ﹩{t}_{90}^{\,\rm{lb}\,}﹩, and Δt, while the rows are a comparison of the different stellar mass regimes from top to bottom: low mass, intermediate mass, and high mass. The population distribution of the protocluster is in red, while the field is in purple. The overlapping area below the two distributions is in green, which roughly quantifies the similarity of the two populations. There is significant overlap between the population models of the protocluster and field, indicating similar SFH timescales between the two.
Paper: UNCOVER/MegaScience: No Evidence of Environmental Quenching in a z ∼ 2.6 Protocluster
Authors: Richard Pan, Katherine A. Suess, Danilo Marchesini, Bingjie Wang, 冰洁 王, Joel Leja, Sam E. Cutler, Katherine E. Whitaker, Rachel Bezanson, Sedona H. Price, Lukas J. Furtak, John R. Weaver, Ivo Labbé, Gabriel Brammer, Yunchong Zhang, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Karl Glazebrook, Tim B. Miller, Ikki Mitsuhashi, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Adi Zitrin
Figure caption: Mass–size relation of quiescent galaxies in the protocluster (red stars) and the field (blue plus signs), measured in the JWST NIRCam F444W. Their median mass–size are shown as red and blue circles, respectively, along with median values from S. E. Cutler et al. (2024; gray circles). We also overplot the mass–size relation from HST F160W measurements from K. V. Nedkova et al. (2021; solid black line) and S. E. Cutler et al. (2022; dotted–dashed line). We find a similarly flat mass–size relation and no significant difference between the protocluster and field populations.