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1. A Massive H i -absorption-selected Galaxy at z  ≈ 2.356

   https://doi.org/10.3847/2041-8213/adb83d  

   Kaur, B; Kanekar, N; Neeleman, M; Zhu, Y; Prochaska, J X; Rafelski, M; Becker, G (March 2025, The Astrophysical Journal Letters)

   Abstract We use the Karl G. Jansky Very Large Array (VLA) and the Atacama Large Millimeter/submillimeter Array to detect CO(1–0), CO(3–2), and rest-frame 349 GHz continuum emission from an Hi-selected galaxy, DLA1020+2733g, atz ≈ 2.3568 in the field of thez= 2.3553 damped Lyαabsorber (DLA) toward QSO J1020+2733. The VLA CO(1–0) detection yields a molecular gas mass of (2.84 ± 0.42) × 10¹¹ × (α_CO/4.36)M_⊙, the largest ever measured in an Hi-selected galaxy. The DLA metallicity is +0.28 ± 0.16, from the Zniiλ2026 absorption line detected in a Keck Echellette Spectrograph and Imager spectrum. This continues the trend of high-metallicity DLAs being frequently associated with massive galaxies. We obtain a star formation rate (SFR) of ≲400M_⊙yr⁻¹from the rest-frame 349 GHz continuum emission and a relatively long molecular gas depletion timescale of ≳0.6 Gyr. The excitation of theJ= 3 rotational level is subthermal, with $r_{31}\equiv L{\prime }_{\mathrm{CO}(3-2)}/L{\prime }_{\mathrm{CO}(1-0)}=0.513\pm 0.081$, suggesting that DLA1020+2733g has a low SFR surface density. The large velocity spread of the CO lines, ≈500 km s⁻¹, and the long molecular gas depletion timescale suggest that DLA1020+2733g is likely to be a cold rotating-disk galaxy. 

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2. The RESOLVE and ECO G3 Initiative: Drivers of H i Content and X-Ray Emission in Galaxy Groups

   https://doi.org/10.3847/1538-4357/adc395  

   Hutchens, Zackary L; Kannappan, Sheila J; Hess, Kelley M; Baker, Andrew J; Sun, Ming; Carr, Derrick S; Eckert, Kathleen D; Stark, David V (May 2025, The Astrophysical Journal)

   Abstract Adding to the RESOLVE and ECO Gas in Galaxy Groups (G3) initiative, we examine possible drivers of group-integrated Hi-to-halo mass ratios (M_HI,grp/M_halo) and group X-ray emission, including group halo mass (M_halo), virialization as probed by crossing time (t_cross), presence of active galactic nuclei (AGN), and group-integrated fractional stellar mass growth rate (FSMGR_grp). G3 groups spanM_halo= 10¹¹−10^14.5M_⊙with comprehensive Higas and AGN information, which we combine with X-ray stacking of ROSAT All-Sky data. We detect hot gas emission exceeding AGN and X-ray binary backgrounds confidently forM_halo= 10^12.6−10¹⁴M_⊙and unambiguously forM_halo> 10¹⁴M_⊙, reflecting an inverse dependence ofM_HI,grp/M_haloand hot gas emission on halo mass. At fixed halo mass,M_HI,grp/M_halotransitions to greater spread belowt_cross∼ 2 Gyr. Dividing groups across this transition, lower-t_crossgroups show elevated X-ray emission compared to higher-t_crossgroups forM_halo> 10^13.3M_⊙, but this trend reverses forM_halo= 10^12.6−10^13.3M_⊙. Additionally, AGN-hosting halos belowM_halo∼ 10^12.1M_⊙exhibit a broad, ∼0.25 dex deep valley inM_HI,grp/M_halocompared to non-AGN-hosting halos with correspondingly reduced FSMGR_grp. When diluted by non-AGN-hosting halos, this valley becomes shallower and narrower, falling roughly between $M_{\mathrm{halo}}={10}^{11.5}{M}_{\odot }$and $M_{\mathrm{halo}}={10}^{12.1}{M}_{\odot }$in the overallM_HI,grp/M_halovs.M_halorelation. We may also detect a second, less easily interpreted valley atM_halo∼ 10¹³M_⊙. Neither valley matches theoretical predictions of a deeper valley located at or above $M_{\mathrm{halo}}={10}^{12.1}{M}_{\odot }$. 

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3. Onset of CN Emission in 3I/ATLAS: Evidence for Strong Carbon-chain Depletion

   https://doi.org/10.3847/2041-8213/ae1232  

   Salazar_Manzano, Luis E; Lin_林, Hsing_Wen 省文; Taylor, Aster G; Seligman, Darryl Z; Adams, Fred C; Gerdes, David W; Ruch, Thomas; Frincke, Tessa T; Napier, Kevin J (October 2025, The Astrophysical Journal Letters)

   Abstract Interstellar objects provide a direct window into the environmental conditions around stars other than the Sun. The recent discovery of 3I/ATLAS, a new interstellar comet, offers a unique opportunity to investigate the physical and chemical properties of interstellar objects and to compare them with those of comets in our own solar system. In this Letter we present the results of a 10 night spectroscopic and photometric monitoring campaign with the 2.4 m Hiltner and 1.3 m McGraw–Hill telescopes at the MDM Observatory. The campaign was conducted between August 8 and 17 while 3I/ATLAS was inbound at heliocentric distances of 3.2–2.9 au. Our observations captured the onset of optical gas activity. Nightly spectra reveal a weak CN emission feature in the coma of 3I/ATLAS, absent during the first nights but steadily strengthening thereafter. We measure a CN production rate ofQ(CN) ∼ 6 × 10²⁴s⁻¹, toward the lower end of activity observed in solar system comets. Simultaneous photometry also indicates a small but measurable increase in the coma’s radial profile and increasingr-bandAfρwith values in the order of ∼300 cm. We derived a gas-to-dust production ratio of $\log Q\left(\mathrm{CN}\right)/Af\rho \sim 22.4$. Our upper limit on the C₂-to-CN ratio ( $\log Q\left({\mathrm{C}}_2\right)/Q\left(\mathrm{CN}\right)\lesssim -0.8$) indicates that 3I/ATLAS is a strongly carbon-chain-depleted comet. Further observations of 3I/ATLAS are required to verify the apparent carbon-chain depletion and to explore whether such composition represents a recurring trait of the interstellar comet population. 

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4. A Complete Triad of Zero‐Valent 17‐Electron Monoradicals of Group 7 Elements Stabilized by m ‐Terphenyl Isocyanides

   https://doi.org/10.1002/anie.202300254  

   Salsi, Federico; Wang, Shuai; Teutloff, Christian; Busse, Marvin; Neville, Michael L.; Hagenbach, Adelheid; Bittl, Robert; Figueroa, Joshua S.; Abram, Ulrich (April 2023, Angewandte Chemie International Edition)

   Abstract The first consistent series of mononuclear 17‐electron complexes of three Group 7 elements has been isolated in crystalline form and studied by X‐ray diffraction and spectroscopic methods. The paramagnetic compounds have a composition of [M⁰(CO)(CNp‐F‐Ar^DArF2)₄] (M=Mn, Tc, Re; Ar^DArF2=2,6‐(3,5‐(CF₃)₂C₆H₃)₂C₆H₂F) and are stabilized by four sterically encumbering isocyanides, which prevent the metalloradicals from dimerization. They have a square pyramidal structure with the carbonyl ligands as apexes. The frozen‐solution EPR spectra of the rhenium and technetium compounds are clearly anisotropic with large⁹⁹Tc and^185,187Re hyperfine interactions for one component. High‐field EPR (Q band and W band) has been applied for the elucidation of the EPR parameters of the manganese(0) complex. 

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5. A rare isocyanide derived from an unprecedented neutral yttrium( ii ) bis(amide) complex

   https://doi.org/10.1039/d3sc00171g  

   Jena, Rashmi; Benner, Florian; Delano, Francis; Holmes, Daniel; McCracken, John; Demir, Selvan; Odom, Aaron L. (April 2023, Chemical Science)

   A room temperature stable Y(ii)bis(amide) has been prepared and fully characterized. The complex reacts withtert-butylisocyanide to make a rare example of a transition metal isocyanide, CN–Y(NHAr*)₂. 

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