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1. Stabilizing Ti ₃ C ₂ T _x MXene flakes in air by removing confined water

   https://doi.org/10.1073/pnas.2400084121  

   Fang, Hui; Thakur, Anupma; Zahmatkeshsaredorahi, Amirhossein; Fang, Zhenyao; Rad, Vahid; Shamsabadi, Ahmad A; Pereyra, Claudia; Soroush, Masoud; Rappe, Andrew M; Xu, Xiaoji G; et al (July 2024, Proceedings of the National Academy of Sciences)

   MXenes have demonstrated potential for various applications owing to their tunable surface chemistry and metallic conductivity. However, high temperatures can accelerate MXene film oxidation in air. Understanding the mechanisms of MXene oxidation at elevated temperatures, which is still limited, is critical in improving their thermal stability for high-temperature applications. Here, we demonstrate that Ti ${}_3$ C ${}_2$ T ${}_x$ MXene monoflakes have exceptional thermal stability at temperatures up to 600 ${}^{°}$ C in air, while multiflakes readily oxidize in air at 300 ${}^{°}$ C. Density functional theory calculations indicate that confined water between Ti ${}_3$ C ${}_2$ T ${}_x$ flakes has higher removal energy than surface water and can thus persist to higher temperatures, leading to oxidation. We demonstrate that the amount of confined water correlates with the degree of oxidation in stacked flakes. Confined water can be fully removed by vacuum annealing Ti ${}_3$ C ${}_2$ T ${}_x$ films at 600 ${}^{°}$ C, resulting in substantial stability improvement in multiflake films (can withstand 600 ${}^{°}$ C in air). These findings provide fundamental insights into the kinetics of confined water and its role in Ti ${}_3$ C ${}_2$ T ${}_x$ oxidation. This work enables the use of stable monoflake MXenes in high-temperature applications and provides guidelines for proper vacuum annealing of multiflake films to enhance their stability. 

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2. Search for heavy pseudoscalar and scalar bosons decaying to a top quark pair in proton–proton collisions at $\sqrt{s}=13\text{TeV}$

   https://doi.org/10.1088/1361-6633/ae2207  

   Collaboration, The CMS (December 2025, Reports on Progress in Physics)

   Abstract A search for pseudoscalar or scalar bosons decaying to a top quark pair ( $\text{t}\overline{\text{t}}$ ) in final states with one or two charged leptons is presented. The analyzed proton–proton collision data was recorded at $\sqrt{s}=13\text{TeV}$ by the CMS experiment at the CERN LHC and corresponds to an integrated luminosity of 138  ${\text{fb}}^{-1}$ . The invariant mass $m_{\mathrm{t}\overline{\mathrm{t}}}$ of the reconstructed $\text{t}\overline{\text{t}}$ system and variables sensitive to its spin and parity are used to discriminate against the standard model $\text{t}\overline{\text{t}}$ background. Interference between pseudoscalar or scalar boson production and the standard model $\text{t}\overline{\text{t}}$ continuum is included, leading to peak-dip structures in the $m_{\mathrm{t}\overline{\mathrm{t}}}$ distribution. An excess of the data above the background prediction, based on perturbative quantum chromodynamics (QCD) calculations, is observed near the kinematic $\text{t}\overline{\text{t}}$ production threshold, while good agreement is found for high $m_{\mathrm{t}\overline{\mathrm{t}}}$ . The data are consistent with the background prediction if the contribution from a simplified model of a color-singlet ${}^1{\text{S}}_0^{\left[1\right]}$ $\text{t}\overline{\text{t}}$ quasi-bound state ${\eta }_{\mathrm{t}}$ , inspired by nonrelativistic QCD, is added. Upper limits at 95% confidence level are set on the coupling between the pseudoscalar or scalar bosons and the top quark for boson masses in the range 365–1000 GeV, relative widths between 0.5% and 25%, and two background scenarios with or without ${\eta }_{\mathrm{t}}$ contribution. 

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3. Evidence for Environmental Effects in the z = 4.3 Protocluster Core SPT2349–56

   https://doi.org/10.3847/2041-8213/adc1c9  

   Hughes, Chayce; Hill, Ryley; Chapman, Scott C; Aravena, Manuel; Archipley, Melanie; Dike, Veronica J; Gonzalez, Anthony; Greve, Thomas R; Gururajan, Gayathri; Hayward, Chris; et al (April 2025, The Astrophysical Journal Letters)

   Abstract We present Atacama Large Millimeter/submillimeter Array observations of the [CI] 492 and 806 GHz fine-structure lines in 25 dusty star-forming galaxies (DSFGs) atz= 4.3 in the core of the SPT2349–56 protocluster. The protocluster galaxies exhibit a median $L_{\left[\text{C}\mathrm{I}\right](2-1)}^{\prime }/L_{\left[\text{C}\mathrm{I}\right](1-0)}^{\prime }$ ratio of 0.94, with an interquartile range of 0.81–1.24. These ratios are markedly different to those observed in DSFGs in the field (across a comparable redshift and 850μm flux density range), where the median is 0.55, with an interquartile range of 0.50–0.76, and we show that this difference is driven by an excess of [Ci](2–1) in the protocluster galaxies for a given 850μm flux density. Assuming local thermal equilibrium, we estimate gas excitation temperatures of $T_{\mathrm{ex}}=59.1_{-6.8}^{+8.1}$ K for our protocluster sample and $T_{\mathrm{ex}}=33.9_{-2.2}^{+2.4}$ K for the field sample. Our main interpretation of this result is that the protocluster galaxies have had their cold gas driven to their cores via close-by interactions within the dense environment, leading to an overall increase in the average gas density and excitation temperature, as well as an elevated [Ci](2–1) luminosity-to-far-infrared-luminosity ratio. 

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4. Massive Extremely High-velocity Outflow in the Quasar J164653.72+243942.2

   https://doi.org/10.3847/1538-4357/adef0d  

   Rodríguez_Hidalgo, Paola; Choi_최, Hyunseop 현섭; Hall, Patrick B; Leighly, Karen M; Flores, Liliana; Charles, Mikel M; DeFrancesco, Cora; Hlavacek-Larrondo, Julie; Perreault-Levasseur, Laurence (September 2025, The Astrophysical Journal)

   Abstract We present analysis of one of the most extreme quasar outflows found to date in our survey of extremely high-velocity outflows (EHVOs). J164653.72+243942.2 (z_em ∼ 3.04) shows variable Civλλ1548,1551 absorption at speeds larger than 0.1c, accompanied by Siiv, Nv,and Lyα, and disappearing absorption at lower speeds. We perform absorption measurements using the apparent optical depth method and SimBAL. We find the absorption to be very broad (Δv ∼  35,100 km s⁻¹in the first epoch and 13,000 km s⁻¹in the second one) and fast (v_max ∼  –50,200 km s⁻¹and −49,000 km s⁻¹, respectively). We measure large column densities ( $\log N_{\mathrm{H}}>$ 21.6 (cm⁻²)) and are able to place distance estimates for the EHVO (5 ≲ R ≲ 28 pc) and the lower-velocity outflow (7 ≲ R ≲ 540 pc). We estimate a mass outflow rate for the EHVO to be ${\dot{M}}_{\mathrm{out}}\sim 50–290M_{\odot }{\mathrm{yr}}^{-1}$ and a kinetic luminosity of $\log L_{\mathrm{KE}}\sim 46.5–47.2\left(\mathrm{erg}{\mathrm{s}}^{-1}\right)$ in both epochs. The lower-velocity component has a mass outflow rate ${\dot{M}}_{\mathrm{out}}\sim 10–790M_{\odot }{\mathrm{yr}}^{-1}$ and a kinetic luminosity of $\log L_{\mathrm{KE}}\sim 45.3–47.2\left(\mathrm{erg}{\mathrm{s}}^{-1}\right)$ . We find that J164653.72+243942.2 is not an outlier among EHVO quasars in regard to its physical properties. While its column density is lower than typical BAL values, its higher outflow velocities drive most of the mass outflow rate and kinetic luminosity. These results emphasize the crucial role of EHVOs in powering quasar feedback, and failing to account for these outflows likely leads to underestimating the feedback impact on galaxies. 

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5. JWST’s PEARLS: Temperatures of Nine Highly Magnified Stars in a Galaxy at Redshift 0.94 and Simulated Stellar Population Dependence on Stellar Metallicity and the Initial Mass Function

   https://doi.org/10.3847/1538-4357/ae1966  

   Williams, Hayley; Kelly, Patrick L; Windhorst, Rogier A; Filippenko, Alexei V; Alfred, Amruth; Broadhurst, Tom; Chen, Wenlei; Conselice, Christopher J; Cohen, Seth H; Diego, José M; et al (December 2025, The Astrophysical Journal)

   Abstract We present stellar atmosphere modeling of JWST NIRCam photometry of nine highly magnified individual stars in a single galaxy at redshiftz= 0.94 known as the Warhol arc, which is strongly lensed by the galaxy cluster MACS J0416. Seven of these transients were identified by Yan et al. The nine sources are likely red supergiants with temperaturesT_eff ≈ 4000 K. We present new long-slit spectroscopy of the Warhol arc acquired with Keck I telescope and the Large Binocular Telescope, and use these data to help constrain the arc’s oxygen abundance to be $12+\log (\mathrm{O}/\mathrm{H})=8.45\pm 0.08$ . A microlensing simulation is performed on synthetic stellar populations using a range of stellar metallicities and initial mass function (IMF) slopes. The temperature distribution of the simulated detectable stars is sensitive to the choice of stellar metallicity, and setting the stellar metallicity equal to the arc’s nebular metallicity ( $\log (Z_{*}/Z_{\odot })=-0.24$ ) produces a simulated temperature distribution that is consistent with the observations, while lower stellar metallicities ( $\log (Z_{*}/Z_{\odot })<\text{–}0.75$ ) produce simulated temperatures that are inconsistent with the observations. The expected detection rate is strongly anticorrelated with the IMF slope forα > 1.2. For the canonical IMF slopeα = 2.35, the simulation yields expected transient detection rates that agree with the observed detection rates in the Hubble Space Telescope Flashlights filters, but overpredicts the detection rate by a factor of ∼3–12 (<2σtension) in the JWST filters. The simulated detection rate is sensitive to the choice of stellar metallicity, with lower metallicities ( $\log (Z_{*}/Z_{\odot })<\text{–}0.75$ ) yielding a significantly lower simulated detection rate that further reduces the modest tension with the observations. 

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