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1. Transient Triplet Metallopnictinidenes M–Pn (M = Pd ^II , Pt ^II ; Pn = P, As, Sb): Characterization and Dimerization

   https://doi.org/10.1021/jacs.4c16830  

   Neben, Marc C; Wegerich, Nils; Al_Said, Tarek A; Thompson, Richard R; Demeshko, Serhiy; Dollberg, Kevin; Tkach, Igor; Van_Trieste, Gerard P; Verplancke, Hendrik; von_Hänisch, Carsten; et al (February 2025, Journal of the American Chemical Society)
2. First Detections of PN, PO, and PO ⁺ toward a Shocked Low-mass Starless Core

   https://doi.org/10.3847/2041-8213/add344  

   Scibelli, Samantha; Megías, Andrés; Jiménez-Serra, Izaskun; Shirley, Yancy; Bergner, Jennifer; Ferrer_Asensio, Judit; Garrod, Robin T; Bonfand, Mélisse; Pokorny-Yadav, Anissa (May 2025, The Astrophysical Journal Letters)

   Abstract Phosphorus is a key element that plays an essential role in biological processes important for living organisms on Earth. The origin and connection of phosphorus-bearing molecules to early solar system objects and star-forming molecular clouds is therefore of great interest, yet there are limited observations throughout different stages of low-mass (M < a few solar masses) star formation. Observations from the Yebes 40 m and IRAM 30 m telescopes detect for the first time in the 7 mm, 3 mm, and 2 mm bands multiple transitions of PN and PO, as well as a single transition of PO⁺, toward a low-mass starless core. The presence of PN, PO, and PO⁺is kinematically correlated with bright SiO(1–0) emission. Our results reveal not only that shocks are the main driver of releasing phosphorus from dust grains and into the gas phase but that the emission originates from gas not affiliated with the shock itself but quiescent gas that has been shocked in the recent past. From radiative transfer calculations, the PO/PN abundance ratio is found to be $3.1_{-0.6}^{+0.4}$, consistent with other high-mass and low-mass star-forming regions. This first detection of PO⁺toward any low-mass star-forming region reveals a PO⁺/PO ratio of $0.0115_{-0.0009}^{+0.0008}$, a factor of 10 lower than previously determined from observations of a Galactic center molecular cloud, suggesting its formation can occur under more standard Galactic cosmic-ray ionization rates. These results motivate the need for additional observations that can better disentangle the physical mechanisms and chemical drivers of this precursor of prebiotic chemistry. 

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3. Layered and Cubic Semiconductors A Ga M ′ Q ₄ ( A ⁺ = K ⁺ , Rb ⁺ , Cs ⁺ , Tl ⁺ ; M ′ ⁴⁺ = Ge ⁴⁺ , Sn ⁴⁺ ; Q ^2– = S ^2– , Se ^2– ) and High Third-Harmonic Generation

   https://doi.org/10.1021/jacs.0c08638  

   Friedrich, Daniel; Byun, Hye Ryung; Hao, Shiqiang; Patel, Shane; Wolverton, Chris; Jang, Joon Ik; Kanatzidis, Mercouri G. (October 2020, Journal of the American Chemical Society)

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4. Phosphorescence in Mn ⁴⁺ -Doped R ⁺ / R ²⁺ Germanates ( R ⁺ = Na ⁺ or K ⁺ , R ²⁺ = Sr ²⁺ )

   https://doi.org/10.1021/acs.inorgchem.2c01364  

   Novikov, Sergei A.; Lu, Yimin; Zhang, Weiguo; Halasyamani, P. Shiv; Hariyani, Shruti; Brgoch, Jakoah; Klepov, Vladislav V.; zur Loye, Hans-Conrad; Mozharivskyj, Yurij (June 2022, Inorganic Chemistry)
5. Spectroscopic study of the 4 f ⁷ 6 s ^{2 8} S 7/2∘−4 f ⁷ ( ⁸ S ^∘ )6 s 6 p ( ¹ P ^∘ ) ⁸ P _9/2 transition in neutral europium-151 and europium-153: absolute frequency and hyperfine structure

   https://doi.org/10.1364/JOSAB.467968  

   Herd, M_T; Maruko, C.; Herzog, M_M; Brand, A.; Cannon, G.; Duah, B.; Hollin, N.; Karani, T.; Wallace, A.; Whitmore, M.; et al (September 2022, Journal of the Optical Society of America B)

   We report on spectroscopic measurements on the $4f^{7}6s^2{}^8{S}_{7/2}^{\circ <\#comment/>}\to <\#comment/>4f^7{(}^8{S}^{\circ <\#comment/>}\left)6s6p{(}^1{P}^{\circ <\#comment/>}\right){}^8{P}_{9/2}$transition in neutral europium-151 and europium-153 at 459.4 nm. The center of gravity frequencies for the 151 and 153 isotopes, reported for the first time in this paper, to our knowledge, were found to be 652,389,757.16(34) MHz and 652,386,593.2(5) MHz, respectively. The hyperfine coefficients for the $6s6p{(}^1{P}^{\circ <\#comment/>}){}^8{P}_{9/2}$state were found to be $\mathrm{A}\left(151\right)=-<\#comment/>228.84\left(2\right)\mathrm{M}\mathrm{H}\mathrm{z}$, $\mathrm{B}\left(151\right)=226.9\left(5\right)\mathrm{M}\mathrm{H}\mathrm{z}$and $\mathrm{A}\left(153\right)=-<\#comment/>101.87\left(6\right)\mathrm{M}\mathrm{H}\mathrm{z}$, $\mathrm{B}\left(153\right)=575.4\left(1.5\right)\mathrm{M}\mathrm{H}\mathrm{z}$, which all agree with previously published results except for A(153), which shows a small discrepancy. The isotope shift is found to be 3163.8(6) MHz, which also has a discrepancy with previously published results. 

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