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1. Atomic Transition Probabilities for Ultraviolet and Optical Lines of Tm ii *

   https://doi.org/10.3847/1538-4365/ad614f  

   Den_Hartog, E_A ; Voith, G_T ; Roederer, I_U ( August 2024 , The Astrophysical Journal Supplement Series)

   We report new branching fraction measurements for 224 ultraviolet and optical transitions of Tmii. These transitions range in wavelength (wavenumber) from 2350 to 6417 Å (42,532–15,579 cm⁻¹) and originate in 13 odd-parity and 24 even-parity upper levels. Thirty-five of the 37 levels, accounting for 213 of the 224 transitions, are studied for the first time. Branching fractions are determined for two levels studied previously for comparison to earlier results. The levels studied for the first time are high lying, ranging in energy from 35,753 to 54,989 cm⁻¹. The branching fractions are determined from emission spectra from two different high-resolution spectrometers. These are combined with radiative lifetimes reported in an earlier study to produce a set of transition probabilities and log(gf) values with accuracy ranging from 5% to 30%. Comparison is made to experimental and theoretical transition probabilities from the literature where such data exist. These new log(gf) values are used to derive an abundance from one previously unused Tmiiline in the UV spectrum of ther-process-enhanced metal-poor star HD 222925, and this abundance is consistent with previous determinations based on other Tmiilines.

    

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2. CECILIA: The Faint Emission Line Spectrum of z ∼ 2–3 Star-forming Galaxies

   https://doi.org/10.3847/2041-8213/ad07dc  

   Strom, Allison L. ; Rudie, Gwen C. ; Trainor, Ryan F. ; Brammer, Gabriel B. ; Maseda, Michael V. ; Raptis, Menelaos ; Rogers, Noah S. ; Steidel, Charles C. ; Chen 陈, Yuguang 昱光 ; Law, David R. ( November 2023 , The Astrophysical Journal Letters)

   We present the first results from Chemical Evolution Constrained Using Ionized Lines in Interstellar Aurorae (CECILIA), a Cycle 1 JWST NIRSpec/MSA program that uses ultra-deep ∼30 hr G235M/F170LP observations to target multiple electron temperature-sensitive auroral lines in the spectra of 33 galaxies atz∼ 1–3. Using a subset of 23 galaxies, we construct two ∼600 object-hour composite spectra, both with and without the stellar continuum, and use these to investigate the characteristic rest-optical (λ_rest≈ 5700–8500 Å) spectrum of star-forming galaxies at the peak epoch of cosmic star formation. Emission lines of eight different elements (H, He, N, O, Si, S, Ar, and Ni) are detected, with most of these features observed to be ≲3% the strength of Hα. We report the characteristic strength of three auroral features ([Nii]λ5756, [Siii]λ6313, and [Oii]λλ7322, 7332), as well as other semi-strong and faint emission lines, including forbidden [Niii]λλ7380, 7414 and permitted Oiλ8449, some of which have never before been observed outside of the local Universe. Using these measurements, we findT_e[Nii] = 13,630 ± 2540 K, representing the first measurement of electron temperature using [Nii] in the high-redshift Universe. We also see evidence for broad line emission with a FWHM of${536}_{-167}^{+45}$km s⁻¹; the broad component of Hαis 6.01%–28.31% the strength of the narrow component and likely arises from star-formation-driven outflows. Finally, we briefly comment on the feasibility of obtaining large samples of faint emission lines using JWST in the future.

    

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3. A Nonheme Mononuclear {FeNO} 7 Complex that Produces N 2 O in the Absence of an Exogenous Reductant

   https://doi.org/10.1002/ange.202109062  

   Dey, Aniruddha ; Gordon, Jesse B. ; Albert, Therese ; Sabuncu, Sinan ; Siegler, Maxime A. ; MacMillan, Samantha N. ; Lancaster, Kyle M. ; Moënne‐Loccoz, Pierre ; Goldberg, David P. ( August 2021 , Angewandte Chemie)

   A new nonheme iron(II) complex, Fe^II(Me₃TACN)((OSi^Ph2)₂O) (1), is reported. Reaction of1with NO_(g)gives a stable mononitrosyl complex Fe(NO)(Me₃TACN)((OSi^Ph2)₂O) (2), which was characterized by Mössbauer (δ=0.52 mm s⁻¹, |ΔE_Q|=0.80 mm s⁻¹), EPR (S=3/2), resonance Raman (RR) and Fe K‐edge X‐ray absorption spectroscopies. The data show that2is an {FeNO}⁷complex with anS=3/2 spin ground state. The RR spectrum (λ_exc=458 nm) of2combined with isotopic labeling (¹⁵N,¹⁸O) reveals ν(N‐O)=1680 cm⁻¹, which is highly activated, and is a nearly identical match to that seen for the reactive mononitrosyl intermediate in the nonheme iron enzyme FDPnor (ν(NO)=1681 cm⁻¹). Complex2reacts rapidly with H₂O in THF to produce the N‐N coupled product N₂O, providing the first example of a mononuclear nonheme iron complex that is capable of converting NO to N₂O in the absence of an exogenous reductant.

    

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4. A Nonheme Mononuclear {FeNO} 7 Complex that Produces N 2 O in the Absence of an Exogenous Reductant

   https://doi.org/10.1002/anie.202109062  

   Dey, Aniruddha ; Gordon, Jesse B. ; Albert, Therese ; Sabuncu, Sinan ; Siegler, Maxime A. ; MacMillan, Samantha N. ; Lancaster, Kyle M. ; Moënne‐Loccoz, Pierre ; Goldberg, David P. ( August 2021 , Angewandte Chemie International Edition)

   A new nonheme iron(II) complex, Fe^II(Me₃TACN)((OSi^Ph2)₂O) (1), is reported. Reaction of1with NO_(g)gives a stable mononitrosyl complex Fe(NO)(Me₃TACN)((OSi^Ph2)₂O) (2), which was characterized by Mössbauer (δ=0.52 mm s⁻¹, |ΔE_Q|=0.80 mm s⁻¹), EPR (S=3/2), resonance Raman (RR) and Fe K‐edge X‐ray absorption spectroscopies. The data show that2is an {FeNO}⁷complex with anS=3/2 spin ground state. The RR spectrum (λ_exc=458 nm) of2combined with isotopic labeling (¹⁵N,¹⁸O) reveals ν(N‐O)=1680 cm⁻¹, which is highly activated, and is a nearly identical match to that seen for the reactive mononitrosyl intermediate in the nonheme iron enzyme FDPnor (ν(NO)=1681 cm⁻¹). Complex2reacts rapidly with H₂O in THF to produce the N‐N coupled product N₂O, providing the first example of a mononuclear nonheme iron complex that is capable of converting NO to N₂O in the absence of an exogenous reductant.

    

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5. Spectroscopic Properties of the Astrochemical Molecules [Al, O, Si] x (x = 0, +1)

   https://doi.org/10.3847/1538-4357/ac92fb  

   Friskey, Jacqueline M. ; Esposito, Vincent J. ; Trabelsi, Tarek ; Francisco, Joseph S. ( October 2022 , The Astrophysical Journal)

   Aluminum and silicon are present in large quantities in the interstellar medium, making the triatomic species consisting of both elements intriguing with regard to the foundations of astrochemistry. Spectroscopic parameters have been calculated via high-level ab initio methods to assist with laboratory and observational detection of [Al, O, Si]^x(x= 0,+1). All [Al, O, Si]^x(x= 0,+1) isomers exist in the linear geometry, with linear AlOSi (X²Π) and linear AlOSi⁺(X¹Δ) being the most stable neutral and cationic species, respectively. Formation of the neutral species most likely occurs via reaction of AlO/SiO on an Si/Al dust grain surface, respectively. The cation molecules may form via ion–neutral reaction or as a consequence of photoionization. The rotational frequencies of linear AlOSi (X²Π) have been calculated using vibrationally corrected rotational constants and centrifugal distortion to lead experimental and observational radio detection. The rotational frequencies are discussed for three temperatures indicative of various astronomical environments: the central circumstellar envelope (CSE) (100 K), outer CSE (30 K), and the interstellar medium (3 K). At 100 K, the lines originating fromJ′ > 30 are the best candidates for detection via ground-based telescope. Anharmonic vibrational analysis revealed various Fermi resonances that may complicate the vibrational spectrum of linear AlOSi (X²Π). Finally, electronic spectroscopy may be the best means for laboratory detection of linear AlOSi (X²Π), due to the presence of two overlapping electronic transitions with large oscillator strengths occurring at approximately 250 nm.

    

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