adsabs/AstroCLIMB huggingface dataset:
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Frequency (solid and dotted–dashed) and damping time (dashed and dotted) of the f-mode calculated with and without Cowling approximation for the QMC-RMF3 EOS. The damping time of g-modes in Figure 5 is plotted as the blue region for comparison. The bottom of the blue region corresponds to the lowest-order g-mode.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Same as Figure 5 but for the IUFSU EOS (panel (a)) and the IOPB-I EOS (panel (b)).
Paper: Cold Gas in a Post-starburst Pair in the z ∼ 1.4 HeavyMetal Survey: Major Mergers as a Pathway to Retain Gas in Quenched Galaxies
Authors: Katherine A. Suess, Aliza G. Beverage, Mariska Kriek, Justin S. Spilker, Rachel Bezanson, Vincenzo R. D'Onofrio, Jenny E. Greene, Jamie Lin, Yuanze Luo, Desika Narayanan, Imad Pasha, Sedona H. Price, David J. Setton, Margaret E. Verrico, Yunchong Zhang
Figure caption: UVJ diagram for our sample of young post-starburst galaxies at z ∼ 1.4 (red stars; red circle for HM1-214340 and red circle with black outline for serendipitously observed UVISTA-214345) as well as existing measurements of molecular gas in quiescent galaxies at z > 1 (M. T. Sargent et al. 2015; R. Bezanson et al. 2019; S. Belli et al. 2021; C. C. Williams et al. 2021; A. Zanella et al. 2023) and z ∼ 0.7 (SQuIGG﹩\overrightarrow{L}﹩E; R. Bezanson et al. 2022). UVJ colors for SQuIGG﹩\overrightarrow{L}﹩E galaxies are extrapolated from their best-fit SED models (K. A. Suess et al. 2022b). The gray contours show the distribution of 1 < z < 1.5 galaxies from 3D-HST (R. E. Skelton et al. 2014). With the exception of one of the A. Zanella et al. (2023) objects, most previous measurements of gas in quiescent galaxies at z > 1 have targeted older systems (≳1 Gyr old from the S. Belli et al. 2019 relation). Our sample (filled red stars; selected from the full HeavyMetal sample in open red stars) focuses on the youngest quiescent galaxies, where most existing measurements are at z < 1 (R. Bezanson et al. 2022).
Paper: Cold Gas in a Post-starburst Pair in the z ∼ 1.4 HeavyMetal Survey: Major Mergers as a Pathway to Retain Gas in Quenched Galaxies
Authors: Katherine A. Suess, Aliza G. Beverage, Mariska Kriek, Justin S. Spilker, Rachel Bezanson, Vincenzo R. D'Onofrio, Jenny E. Greene, Jamie Lin, Yuanze Luo, Desika Narayanan, Imad Pasha, Sedona H. Price, David J. Setton, Margaret E. Verrico, Yunchong Zhang
Figure caption: Top center/right: LRIS and MOSFIRE spectra of UVISTA-214340 (blue) and UVISTA-214345 (red). Left: SEDs, SFHs, and best-fit Prospector models to UVISTA-214340 and UVISTA-214345. Bottom center: CO(2–1) spectrum and moment-0 map of our detection. Bottom right: ALMA contours (3σ, 4σ, 5σ) overlaid on the F814W image of the region. Both galaxies are spectroscopically confirmed massive post-starburst galaxies at the same redshift, likely in the early stages of a near-equal-mass merger. The ALMA observations show ∼109.74M⊙ of molecular gas contained in the system; as described in the text, the majority of this gas is likely associated with UVISTA-214345, but our spatial resolution is too coarse to conclusively determine whether some gas is also associated with HM1-214340 or one of the small clumps apparent in F814W.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Real (solid) and imaginary (dashed) parts of the difference between the dynamical and equilibrium sound speed squared, ﹩{\rm{Re}}[{c}_{{\rm{dy}}}^{2}-{c}_{{\rm{eq}}}^{2}]﹩ and ﹩{\rm{Im}}[{c}_{{\rm{dy}}}^{2}]﹩, as functions of the baryon number density nB at fixed values of the entropy per baryon, S = 0.3 kB (thin) and S = 0.4 kB (thick). Results are shown for the QMC-RMF3 EOS at an oscillation frequency f = 100 Hz (blue) and for the IUFSU EOS at f = 30 Hz (orange). The density regions where ﹩{\rm{Re}}[{c}_{{\rm{dy}}}^{2}-{c}_{{\rm{eq}}}^{2}]\gt {\rm{Im}}[{c}_{{\rm{dy}}}^{2}]﹩ can support local g-mode oscillations, whereas regions dominated by the imaginary part indicate strong damping and therefore the mode propagation is suppressed.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Temperature profiles at fixed entropy per baryon for three (QMC-RMF3, IUFSU, and IOPB-I) EOSs. These profiles are obtained by solving the equations of motion numerically in weak chemical equilibrium and at finite temperatures. At each density point, the entropy is calculated for several temperature points and then linearly interpolated in order to apply a root-finding algorithm to determine the desired constant entropy profile.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Left panel: the differences between the adiabatic and equilibrium sound speed squared ﹩{c}_{{\rm{ad}}}^{2}-{c}_{{\rm{eq}}}^{2}﹩ around beta equilibrium xeq (nB, T), as a function of the baryon density for various fixed-temperature profiles T = [0,  3,  5,  7] MeV for the QMC-RMF3 EOS. Right panel: the beta equilibration relaxation rate γ as a function of nB for fixed-temperature profiles T = [3,  5,  7] MeV. The dotted lines follow the exact definition in Equation (7). The solid lines include finite-temperature effects in the beta reaction rate λn↔p, but approximate the susceptibility ﹩\left.(\partial \delta \mu /\partial \delta x\right){| }_{{n}_{{\rm{B}}},S}﹩ using its zero-temperature value.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: g1-mode frequency as a function of NS mass at fixed entropy per baryon S = 0.2 kB (top), S = 0.3 kB (middle), and S = 0.4 kB (bottom). The real (thick solid lines) and imaginary (dotted–dashed lines) parts of the frequency are shown, and the thin solid line refers to the cold adiabatic g-mode frequency in the absence of viscosity, which has no imaginary part. Results for three different EOSs are shown, and the calculations were performed within the Cowling approximation.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Isothermal (red, dashed) vs. constant specific entropy (blue) adiabatic speed of sound ﹩{c}_{{\rm{ad}}}^{2}﹩ and their difference for the QMC-RMF3 EOS at a temperature of T = 6 MeV. Even at temperatures in the upper range that we consider in this paper, the difference between the isothermal and the constant specific entropy ﹩{c}_{{\rm{ad}}}^{2}﹩ is negligible, especially at larger densities.
Paper: Suppression of Composition g-modes in Chemically Equilibrating Warm Neutron Stars
Authors: Tianqi Zhao, Peter B. Rau, Alexander Haber, Steven P. Harris, Constantinos Constantinou, Sophia Han
Figure caption: Imaginary part of the radial displacement field ξr(r) for the fundamental g1-mode (left panels) and first overtone g2-mode (right panels) as a function of the temperature, for three different EOSs: QMC-RMF3 (top row), IUFSU (middle row), and IOPB-I (bottom row).
Paper: Nitrogen-bearing Species on Trans-Neptunian Objects Revealed by JWST/DiSCo-TNOs
Authors: S. Cryan, R. Brunetto, A. Guilbert-Lepoutre, N. Pinilla-Alonso, E. Hénault, B. J. Holler, Y. Pendleton, D. Cruikshank, J. Stansberry, J. P. Emery, L. T. McClure, J. Licandro, V. Lorenzi, T. G. Müller, N. Peixinho, B. Harvison, C. Schambeau, M. T. Bannister, A. C. de Souza-Feliciano, M. N. de Prá
Figure caption: (Left) From top to bottom, representative spectra of five object classes: Double-Dip, Cliff1, Cliff2–CC, Cliff2-Ecc TNOs and the centaur. (Right) Four Gaussian components fit to each spectrum between 4.35 and 4.75 µm: 13CO2 (at 4.38 µm), a 4.5 µm feature, a 4.62 µm feature, and CO (at 4.68 µm). Vertical lines indicate the absorption bands that were targeted by our fitting procedure, as well as those used for band area comparison in the left panel. Spectra are shifted in the y-direction for clarity.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Adapted Figure 4 from Y. Zheng et al. (2024) showing column densities (N) for low ions (H I, C II, and Si III) as a function of normalized impact parameter (b/R200c). The column density results from the M+M sample are shown as 2D probability density histograms with the brightest cells showing a greater probability at a given b/R200c. The median of all simulated columns as a function of b/R200c is shown as a solid line with two shaded regions representing the 16th–84th (1σ) and 5th–95th percentiles (2σ). Observed column densities are shown as points, where each marker is attributed to a certain observational paper (legend shown at the bottom of the figure). Open markers are nondetections and are treated as upper limits, while filled markers are detections; filled markers with upward arrows are saturations and are treated as lower limits. Black bars are intervals provided in N. Mishra et al. (2024) that show the observationally constrained range (upper and lower limits) of column densities for saturated systems. Each column shows all simulated and observational data for the CGM around galaxies within a given stellar mass bin (denoted at the top). From left to right, the three stellar mass bins (and the number of simulated galaxies in each bin) are as follows: M* = 106.0−7.5 M⊙ (N = 19), M* = 107.5−8.5 M⊙ (N = 29), and M* = 108.5−9.5 M⊙ (N = 16). We find the M+M sample reproduces the majority of existing column density observations for the low ions included in this work (see also Table 1).
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Total halo metal retention for each halo. The horizontal axis shows the fraction of metals retained in the disk (gas and stars), defined by ﹩{r}_{\,{{\rm{\Sigma }}}_{\,\rm{HI}\,}}﹩. The vertical axis shows the fraction of metals retained in all gas beyond the disk (extended CGM and disk–CGM interface) out to R200c. Galaxies are differentiated by simulation suite by marker type (i.e., Marvel, circles; Massive, diamonds) and color-coded by stellar mass. If a halo lies in the lower-right gray region, then the disk holds more metals than the CGM; the reverse is true in the upper-left white region. The solid gray lines denote the fraction of metals lost relative to the metal mass predicted by the star formation history. For example, if a halo lies on the 40% line, then 40% of the metals are not accounted for and are likely outside of the halo. With decreasing stellar mass, dwarf galaxies are less effective at retaining metals in their disk and more effective at losing metals from their halo; however, the CGM metal retention tends to remain within 0.1–0.45.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Same as Figure 4 (adapted Figure 4 from Y. Zheng et al. 2024) now showing column densities for higher ions (Si IV, C IV, and O VI). We find the M+M sample reproduces the majority of existing Si IV column density observations, while the simulations tend to underpredict C IV and O VI column densities (see Section 6.1 for further discussion).
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Luminosity–metallicity relation (Fe/H vs. LV; left) and galaxy specific star formation rates (sSFR vs. M*; right). Red circles represent galaxies from the Marvel suite, and blue diamond markers represent the Marvelous Massive suite; median values of both suites are shown as solid lines. Left panel: shown is the logarithm of the mean stellar metallicity relative to solar abundance. Error bars on simulated points show the 16th–84th percentile range of the simulated stellar metallicity distribution. Open-faced pentagon markers are observational data from A. W. McConnachie (2012), and open-faced square markers are observational data from the Local Volume Database (A. B. Pace 2025). Right panel: sSFR values for the M+M sample are calculated over a timescale of 100 Myr (sSFR values for individual galaxies are provided in Table 3). Open-faced markers are observations that derive star formation rates as follows: R. Bordoloi et al. (2014) use detected nebular emission lines, and C. J. Liang & H.-W. Chen (2014) use rest-frame UV absolute magnitude. I. D. Karachentsev et al. (2013) and J. C. Lee et al. (2011) values utilize far-UV magnitudes and are corrected for Galactic extinction in Y. Zheng et al. (2024) following the methods presented in their Appendix. We find adequate agreement between the M+M sample and observations, as well as similar behavior across suites.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Top panel: summary of the virial mass (blue circle), total gas mass in the halo (green square), and stellar mass (yellow star) for each galaxy in the Marvel simulation (open-faced markers) and the Marvelous Massive Dwarfs simulations (filled markers). The galaxies in the Marvelous Massive Dwarfs have slightly greater virial masses for a given virial radius than the Marvel galaxies due to the difference in cosmology (see Section 2). Bottom panel: histograms of stellar masses for the observed galaxies (Y. Zheng et al. 2024, solid black line; N. Mishra et al. 2024, dashed gray line) and histogram of stellar masses for the M+M  sample (orange). All simulated stellar masses are 0.6 of the total sum of star particle masses within a halo, as this is a better match to photometric stellar mass determinations (F. Munshi et al. 2013). All galaxies included in Y. Zheng et al. (2024) and the z < 0.3 galaxies included in N. Mishra et al. (2024) are shown in this plot. These values are also provided in Table 3 for each galaxy in the M+M sample.