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Reactive Species and Reaction Pathways for the Oxidative Cleavage of 4-Octene and Oleic Acid with H 2 O 2 over Tungsten Oxide Catalysts

The oxidative cleavage of carbon-carbon double bonds (C=C) in alkenes and fatty acids produces aldehydes and acids valued as chemical intermediates. Solid tungsten oxide catalysts are low cost, non-toxic, and selective for the oxidative cleavage of C=C bonds with hydrogen peroxide (H 2 O 2 ) and are, therefore, a promising option for continuous processes. Despite the relevance of these materials, the elementary steps involved and their sensitivity to the form of W sites present on surfaces have not been described. In this work, we combine in situ spectroscopy and rate measurements to identify significant steps in the reaction, the reactive species present on catalysts, and examine differences between the kinetics of this reaction on isolated W atoms grafted to alumina and on those exposed on crystalline WO 3 nanoparticles. Raman spectroscopy shows that W-peroxo complexes (W-(η 2 -O 2 ) formed from H 2 O 2 ) react in a kinetically relevant step to produce epoxides, which undergo hydrolysis at protic surface sites. Subsequently, the CH 3 CN solvent deprotonates diols to form alpha hydroxy ketones that react to form aldehydes and water following nucleophilic attack of H 2 O 2 . Turnover rates for oxidative cleavage, determined by in situ site titrations, on WO x -Al 2 O 3 are 75% greater than those on WO 3 at standard conditions. These differences reflect activation enthalpies (ΔH ‡ ) for oxidative cleavage of 4-octene that are much lower for the isolated WO x sites (36±3 and 60±6 kJ∙mol -1 for WO x -Al 2 O 3 and WO 3 , respectively) and correlate strongly with the difference between enthalpies of adsorption for epoxyoctane (ΔH ads,epox ), which resembles the transition state for epoxidation. The WO x -Al 2 O 3 catalysts mediate oxidative cleavage of oleic acid with H 2 O 2 following a mechanism comparable to that for 4-octene. The WO 3 materials, however, form only the epoxide and do not cleave the C-C bond or produce aldehydes and acids. These differences reflect the distinct site requirements for these reaction pathways and indicate that acid sites required for diol formation are strongly inhibited by oleic acids and epoxides on WO 3 whereas the Al 2 O 3 support provides sites competent for this reaction and increase the yield of the oxidative cleavage products.

37 INORGANIC, ORGANIC, PHYSICAL, AND ANALYTICAL CH↗

Structural and spectroscopic characterization of a Tb(IV) polyoxometalate

There has been a renaissance in high valent lanthanide chemistry, which has resulted in the first examples of tetravalent praseodymium (Pr) and terbium (Tb) in molecular systems. These feats have been achieved with tailored ligands that facilitate tetravalent lanthanide stability in non-aqueous conditions. The next step in realizing the potential of high valent lanthanide chemistry is moving towards complexes that are stable in ambient and aqueous conditions. In this investigation, we advance this paradigm by obtaining definitive evidence of Tb(IV) in a molecular system under aqueous conditions utilizing the lacunary Wells-Dawson polyoxometalate, K 10 P 2 W 17 O 61 •20H 2 O. Herein we present the single crystal structure of K 16 Tb(IV)(P 2 W 17 O 61 ) 2 •39.85H 2 O (Tb(IV)W 34 ) as well as extensive spectroscopic evidence obtained via UV–Vis-NIR, X-ray absorption near edge spectroscopy, continuous wave X-band electron paramagnetic resonance spectroscopy and SQUID magnetometry measurements to confirm the oxidation state of Tb in W 34 complexes as +4.

37 INORGANIC, ORGANIC, PHYSICAL, AND ANALYTICAL CH↗

DESI 2024 VII: cosmological constraints from the full-shape modeling of clustering measurements

We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-α forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been thoroughly validated in a series of supporting papers as summarised in [1]. We combine the full-shape information with DESI's DR1 constraints from the baryon acoustic oscillations (BAO) of these tracers. In the flat ΛCDM cosmological model, DESI (FS+BAO), combined with a baryon density prior from Big Bang Nucleosynthesis and a weak prior on the scalar spectral index, determines matter density to Ω m = 0.2962 ± 0.0095, and the amplitude of mass fluctuations to σ 8 = 0.842 ± 0.034. The addition of the cosmic microwave background (CMB) data tightens these constraints to Ω m = 0.3056 ± 0.0049 and σ 8 = 0.8121 ± 0.0053, while further addition of the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data further improves these measurements, and leads to a 0.4% determination of the Hubble constant, H 0 = (68.40 ± 0.27) km s -1 Mpc -1 . In models with a time-varying dark energy equation of state parametrised by w 0 and w a , combinations of DESI (FS+BAO) with CMB and type Ia supernovae continue to show the preference, previously found in the DESI DR1 BAO analysis, for w 0 > -1 and w a < 0 with similar levels of significance. DESI data, in combination with the CMB, improve the upper limits on the sum of the neutrino masses relative to the case when only the DR1 BAO was available, giving ∑m ν < 0.071 eV at 95% confidence. We finally constrain deviations from general relativity represented by two modified gravity parameters. DESI (FS+BAO) data alone measure the parameter that controls the clustering of massive particles, μ 0 = 0.11 +0.45 -0.54 , in agreement with the zero value predicted by general relativity. The combination of DESI with the CMB and the clustering and lensing analysis from DESY3 constrains both modified-gravity parameters, giving μ 0 = 0.04 ± 0.22 and Σ 0 = 0.044 ± 0.047, again in agreement with general relativity.

79 ASTRONOMY AND ASTROPHYSICS↗

WEST full tungsten operation with an ITER grade divertor

The mission of WEST (tungsten-W Environment in Steady-state Tokamak) is to explore long pulse operation in a full tungsten (W) environment for preparing next-step fusion devices (ITER and DEMO) with a focus on testing the ITER actively cooled W divertor in tokamak conditions. Following the successful completion of phase 1 (2016-2021), phase 2 started in December 2022 with the lower divertor made entirely of actively cooled ITER-grade tungsten mono-blocks. A boronization prior the first plasma attempt allowed for a smooth startup with the new divertor. Despite the reduced operating window due to tungsten, rapid progress has been made in long pulse operation, resulting in discharges with a pulse length of 100 s and an injected energy of around 300 MJ per discharge. Plasma startup studies were carried out with equatorial boron nitride limiters to compare them with tungsten limiters, while Ion Cyclotron Resonance Heating assisted startup was attempted. High fluence operation in attached regime, which was the main thrust of the first campaigns, already showed the progressive build up of deposits and appearance of dust, impacting the plasma operation as the plasma fluence increased. In total, the cumulated injected energy during the first campaigns reached 43 GJ and the cumulated plasma time exceeded 5 h. Demonstration of controlled X-Point Radiator regime is also reported, opening a promising route for investigating plasma exhaust and plasma-wall interaction issues in more detached regime. This paper summarises the lessons learned from the manufacturing and the first operation of the ITER-grade divertor, describing the progress achieved in optimising operation in a full W environment with a focus on long pulse operation and plasma wall interaction.

70 PLASMA PHYSICS AND FUSION TECHNOLOGY↗

The Dark Energy Survey supernova program: cosmological biases from supernova photometric classification

ABSTRACT Cosmological analyses of samples of photometrically identified type Ia supernovae (SNe Ia) depend on understanding the effects of ‘contamination’ from core-collapse and peculiar SN Ia events. We employ a rigorous analysis using the photometric classifier SuperNNova on state-of-the-art simulations of SN samples to determine cosmological biases due to such ‘non-Ia’ contamination in the Dark Energy Survey (DES) 5-yr SN sample. Depending on the non-Ia SN models used in the SuperNNova training and testing samples, contamination ranges from 0.8 to 3.5 per cent, with a classification efficiency of 97.7–99.5 per cent. Using the Bayesian Estimation Applied to Multiple Species (BEAMS) framework and its extension BBC (‘BEAMS with Bias Correction’), we produce a redshift-binned Hubble diagram marginalized over contamination and corrected for selection effects, and use it to constrain the dark energy equation-of-state, w. Assuming a flat universe with Gaussian ΩM prior of 0.311 ± 0.010, we show that biases on w are <0.008 when using SuperNNova, with systematic uncertainties associated with contamination around 10 per cent of the statistical uncertainty on w for the DES-SN sample. An alternative approach of discarding contaminants using outlier rejection techniques (e.g. Chauvenet’s criterion) in place of SuperNNova leads to biases on w that are larger but still modest (0.015–0.03). Finally, we measure biases due to contamination on w0 and wa (assuming a flat universe), and find these to be <0.009 in w0 and <0.108 in wa, 5 to 10 times smaller than the statistical uncertainties for the DES-SN sample.

79 ASTRONOMY AND ASTROPHYSICS↗

Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory

We present the cosmological implications from final measurements of clustering using galaxies, quasars, and Lyα forests from the completed Sloan Digital Sky Survey (SDSS) lineage of experiments in large-scale structure. These experiments, composed of data from SDSS, SDSS-II, BOSS, and eBOSS, offer independent measurements of baryon acoustic oscillation (BAO) measurements of angular-diameter distances and Hubble distances relative to the sound horizon, r d , from eight different samples and six measurements of the growth rate parameter, fσ 8 , from redshift-space distortions (RSD). This composite sample is the most constraining of its kind and allows us to perform a comprehensive assessment of the cosmological model after two decades of dedicated spectroscopic observation. We show that the BAO data alone are able to rule out dark-energy-free models at more than eight standard deviations in an extension to the flat, ΛCDM model that allows for curvature. When combined with Planck Cosmic Microwave Background (CMB) measurements of temperature and polarization, under the same model, the BAO data provide nearly an order of magnitude improvement on curvature constraints relative to primary CMB constraints alone. Independent of distance measurements, the SDSS RSD data complement weak lensing measurements from the Dark Energy Survey (DES) in demonstrating a preference for a flat ΛCDM cosmological model when combined with Planck measurements. The combined BAO and RSD measurements indicate σ 8 =0.85±0.03, implying a growth rate that is consistent with predictions from Planck temperature and polarization data and with General Relativity. When combining the results of SDSS BAO and RSD, Planck, Pantheon Type Ia supernovae (SNe Ia), and DES weak lensing and clustering measurements, all multiple-parameter extensions remain consistent with a ΛCDM model. Regardless of cosmological model, the precision on each of the three parameters, Ω Λ , H 0 , and σ 8 , remains at roughly 1%, showing changes of less than 0.6% in the central values between models. In a model that allows for free curvature and a time-evolving equation of state for dark energy, the combined samples produce a constraint Ω K =-0.0022±0.0022. The dark energy constraints lead to w 0 =-0.909±0.081 and w a =$-0.49_{-0.30}^{+0.35}$, corresponding to an equation of state of w p =-1.018±0.032 at a pivot redshift z p =0.29 and a Dark Energy Task Force Figure of Merit of 94. The inverse distance ladder measurement under this model yields H 0 =68.18±0.79 km s -1 Mpc -1 , remaining in tension with several direct determination methods; the BAO data allow Hubble constant estimates that are robust against the assumption of the cosmological model. In addition, the BAO data allow estimates of H 0 that are independent of the CMB data, with similar central values and precision under a ΛCDM model. Our most constraining combination of data gives the upper limit on the sum of neutrino masses at Σm ν <0.115 eV (95% confidence). Finally, we consider the improvements in cosmology constraints over the last decade by comparing our results to a sample representative of the period 2000-2010. We compute the relative gain across the five dimensions spanned by w, Ω k , Σm ν , H 0 , and σ 8 and find that the SDSS BAO and RSD data reduce the total posterior volume by a factor of 40 relative to the previous generation. Finally, adding again the Planck, DES, and Pantheon SN Ia samples leads to an overall contraction in the five-dimensional posterior volume of 3 orders of magnitude.

79 ASTRONOMY AND ASTROPHYSICS↗

Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample

The cosmological information extracted from photometric surveys is most robust when multiple probes of the large scale structure of the Universe are used. Two of the most sensitive probes are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the way galaxies trace matter (the galaxy bias factor). The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000 deg 2 of the Dark Energy Survey’s first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies, especially selected to optimize such combination, and 100 million background shapes. We consider two flat cosmological models, the Standard Model with dark energy and cold dark matter ( Λ CDM ) a variation with a free parameter for the dark energy equation of state ( w CDM ). Both models are marginalized over 25 astrophysical and systematic nuisance parameters. In Λ CDM we obtain for the matter density Ω m = 0.320 - 0.034 + 0.041 and for the clustering amplitude S 8 ≡ σ 8 ( Ω m / 0.3 ) 0.5 = 0.778 - 0.031 + 0.037 , at 68% C.L. The latter is only 1 σ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In w CDM we find Ω m = 0.32 - 0.046 + 0.044 , S 8 = 0.777 - 0.051 + 0.049 and dark energy equation of state w = - 1.031 - 0.379 + 0.218 . We find that including smaller scales, while marginalizing over nonlinear galaxy bias, improves the constraining power in the Ω m - S 8 plane by 31% and in the Ω m - w plane by 41% while yielding consistent cosmological parameters from those in the linear bias case. These results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions ( 3 × 2 pt ).

79 ASTRONOMY AND ASTROPHYSICS↗

Dark Energy Survey Year 3 results: Measurement of the baryon acoustic oscillations with three-dimensional clustering

The three-dimensional correlation function offers an effective way to summarize the correlation of the large-scale structure even for imaging galaxy surveys. We have applied the projected three-dimensional correlation function, ξ p to measure the baryonic acoustic oscillations (BAO) scale on the first-three years Dark Energy Survey data. The sample consists of about 7 million galaxies in the redshift range 0.6< z p < 1.1 over a footprint of 4108 deg 2 . Our theory modeling includes the impact of realistic true redshift distributions beyond Gaussian photo-z approximation. ξ p is obtained by projecting the three-dimensional correlation to the transverse direction. To increase the signal-to-noise of the measurements, we have considered a Gaussian stacking window function in place of the commonly used top-hat. ξ p is sensitive to D M (z eff )/r s , the ratio between the comoving angular diameter distance and the sound horizon. Using the full sample, D M (z eff )/r s is constrained to be19.00 ± 0.67 (top-hat) and 19.15 ± 0.58 (Gaussian) at z eff = 0.835. The constraint is weaker than the angular correlation w constraint 18.84 ± 0.50), and we trace this to the fact that the BAO signals are heterogeneous across redshift. While ξ p responds to the heterogeneous signals by enlarging the error bar, w can still give a tight bound on D M s in this case. When a homogeneous BAO-signal subsample in the range 0.7 < z p <1.0 (z eff = 0.845) is considered, ξp yields 19.80 ± 0.67 (top-hat) and 19.84 ± 0.53 (Gaussian). The latter is mildly stronger than the w constraint (19.86 ± 0.55). We find that the ξ p results are more sensitive to photo-z because ξ p keeps the three-dimensional clustering information causing it to be more prone to photo-z noise. The Gaussian window gives more robust results than the top-hat as the former is designed to suppress the low signal modes. ξ p and the angular statistics such as w have their own pros and cons, and they serve an important crosscheck with each other.

79 ASTRONOMY AND ASTROPHYSICS↗

Dark Energy Survey Year 3 results: Constraints on extensions to Λ CDM with weak lensing and galaxy clustering

We constrain six possible extensions to the Λ cold dark matter (CDM) model using measurements from the Dark Energy Survey’s first three years of observations, alone and in combination with external cosmological probes. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data vectors and blind analyses of real data to validate the robustness of our results to astrophysical and modeling systematic errors. In many cases, constraining power is limited by the absence of theoretical predictions beyond the linear regime that are reliable at our required precision. The Λ CDM extensions are dark energy with a time-dependent equation of state, nonzero spatial curvature, additional relativistic degrees of freedom, sterile neutrinos with eV-scale mass, modifications of gravitational physics, and a binned σ 8 ( z ) model which serves as a phenomenological probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find ( w p , w a ) = ( - 0.9 9 - 0.17 + 0.28 , - 0.9 ± 1.2 ) at 68% confidence with z p = 0.24 from the DES measurements alone, and ( w p , w a ) = ( - 1.0 3 - 0.03 + 0.04 , - 0. 4 - 0.3 + 0.4 ) with z p = 0.21 for the combination of all data considered. Curvature constraints of Ω k = 0.0009 ± 0.0017 and effective relativistic species N eff = 3.1 0 - 0.16 + 0.15 are dominated by external data, though adding DES information to external low-redshift probes tightens the Ω k constraints that can be made without cosmic microwave background observables by 20%. For massive sterile neutrinos, DES combined with external data improves the upper bound on the mass m eff by a factor of 3 compared to previous analyses, giving 95% limits of ( Δ N eff , m eff ) ≤ ( 0.28 , 0.20 eV ) when using priors matching a comparable Planck analysis. For modified gravity, we constrain changes to the lensing and Poisson equations controlled by functions Σ ( k , z ) = Σ 0 Ω Λ ( z ) / Ω Λ , 0 and μ ( k , z ) = μ 0 Ω Λ ( z ) / Ω Λ , 0 , respectively, to Σ 0 = 0. 6 - 0.5 + 0.4 from DES alone and ( Σ 0 , μ 0 ) = ( 0.04 ± 0.05 , 0.0 8 - 0.19 + 0.21 ) for the combination of all data, both at 68% confidence. Overall, we find no significant evidence for physics beyond Λ CDM .

79 ASTRONOMY AND ASTROPHYSICS↗

Search for high-mass resonances in final states with a τ-lepton and missing transverse momentum with the ATLAS detector

A search for high-mass resonances decaying into a τ-lepton and a neutrino using proton-proton collisions at a center-of-mass energy of $\sqrt{s}$ =13 TeV is presented. The full run 2 data sample corresponding to an integrated luminosity of 139 fb -1 recorded by the ATLAS experiment in the years 2015–2018 is analyzed. The τ-lepton is reconstructed in its hadronic decay modes and the total transverse momentum carried out by neutrinos is inferred from the reconstructed missing transverse momentum. The search for new physics is performed on the transverse mass between the τ-lepton and the missing transverse momentum. No excess of events above the Standard Model expectation is observed and upper exclusion limits are set on the W' →τ⁢v production cross section. Heavy W' vector bosons with masses up to 5.0 TeV are excluded at 95% confidence level, assuming that they have the same couplings as the Standard Model W boson. For nonuniversal couplings, W' bosons are excluded for masses less than 3.5–5.0 TeV, depending on the model parameters. In addition, model-independent limits on the visible cross section times branching ratio are determined as a function of the lower threshold on the transverse mass of the τ-lepton and missing transverse momentum.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗

Data from Reactive Species and Reaction Pathways for the Oxidative Cleavage of 4-Octene and Oleic Acid with H2O2 over Tungsten Oxide Catalysts

Oxidative cleavage of carbon–carbon double bonds (C═C) in alkenes and fatty acids produces aldehydes and acids valued as chemical intermediates. Solid tungsten oxide catalysts are low cost, nontoxic, and selective for the oxidative cleavage of C═C bonds with hydrogen peroxide (H2O2) and are, therefore, a promising option for continuous processes. Despite the relevance of these materials, the elementary steps involved and their sensitivity to the form of W sites present on surfaces have not been described. Here, we combine in situ spectroscopy and rate measurements to identify significant steps in the reaction and the reactive species present on the catalysts and examine differences between the kinetics of this reaction on isolated W atoms grafted to alumina and on those exposed on crystalline WO3 nanoparticles. Raman spectroscopy shows that W–peroxo complexes (W–(η2-O2)) formed from H2O2 react with alkenes in a kinetically relevant step to produce epoxides, which undergo hydrolysis at protic surface sites. Subsequently, the CH3CN solvent deprotonates diols to form alpha-hydroxy ketones that react to form aldehydes and water following nucleophilic attack of H2O2. Turnover rates for oxidative cleavage, determined by in situ site titrations, on WOx–Al2O3 are 75% greater than those on WO3 at standard conditions. These differences reflect the activation enthalpies (ΔH‡) for the oxidative cleavage of 4-octene that are much lower than those for the isolated WOx sites (36 ± 3 and 60 ± 6 kJ·mol–1 for WOx–Al2O3 and WO3, respectively) and correlate strongly with the difference between the enthalpies of adsorption for epoxyoctane (ΔHads,epox), which resembles the transition state for epoxidation. The WOx–Al2O3 catalysts mediate oxidative cleavage of oleic acid with H2O2 following a mechanism comparable to that for the oxidative cleavage of 4-octene. The WO3 materials, however, form only the epoxide and do not cleave the C–C bond or produce aldehydes and acids. These differences reflect the distinct site requirements for these reaction pathways and indicate that acid sites required for diol formation are strongly inhibited by oleic acids and epoxides on WO3 whereas the Al2O3 support provides sites competent for this reaction and increase the yield of the oxidative cleavage products.

Catalysis↗

Materials Data on Co3W by Materials Project

Co3W is beta Cu3Ti-like structured and crystallizes in the hexagonal P6_3/mmc space group. The structure is three-dimensional. W is bonded to twelve Co atoms to form WCo12 cuboctahedra that share corners with six equivalent WCo12 cuboctahedra, corners with twelve CoCo8W4 cuboctahedra, edges with eighteen CoCo8W4 cuboctahedra, faces with eight equivalent WCo12 cuboctahedra, and faces with twelve CoCo8W4 cuboctahedra. There are six shorter (2.55 Å) and six longer (2.56 Å) W–Co bond lengths. There are two inequivalent Co sites. In the first Co site, Co is bonded to four equivalent W and eight Co atoms to form distorted CoCo8W4 cuboctahedra that share corners with four equivalent WCo12 cuboctahedra, corners with fourteen CoCo8W4 cuboctahedra, edges with six equivalent WCo12 cuboctahedra, edges with twelve CoCo8W4 cuboctahedra, faces with four equivalent WCo12 cuboctahedra, and faces with sixteen CoCo8W4 cuboctahedra. There are a spread of Co–Co bond distances ranging from 2.48–2.63 Å. In the second Co site, Co is bonded to four equivalent W and eight equivalent Co atoms to form distorted CoCo8W4 cuboctahedra that share corners with four equivalent WCo12 cuboctahedra, corners with fourteen CoCo8W4 cuboctahedra, edges with six equivalent WCo12 cuboctahedra, edges with twelve equivalent CoCo8W4 cuboctahedra, faces with four equivalent WCo12 cuboctahedra, and faces with sixteen CoCo8W4 cuboctahedra.

36 MATERIALS SCIENCE↗

Materials Data on WCl5 by Materials Project

WCl5 crystallizes in the monoclinic C2/m space group. The structure is zero-dimensional and consists of six WCl5 clusters. In two of the WCl5 clusters, W5+ is bonded to six Cl1- atoms to form edge-sharing WCl6 octahedra. There are four shorter (2.28 Å) and two longer (2.54 Å) W–Cl bond lengths. There are three inequivalent Cl1- sites. In the first Cl1- site, Cl1- is bonded in a single-bond geometry to one W5+ atom. The Cl–W bond length is 2.28 Å. In the second Cl1- site, Cl1- is bonded in a water-like geometry to two equivalent W5+ atoms. Both Cl–W bond lengths are 2.54 Å. In the third Cl1- site, Cl1- is bonded in a single-bond geometry to one W5+ atom. The Cl–W bond length is 2.28 Å. In four of the WCl5 clusters, W5+ is bonded to six Cl1- atoms to form edge-sharing WCl6 octahedra. There are six inequivalent Cl1- sites. In the first Cl1- site, Cl1- is bonded in a single-bond geometry to one W5+ atom. In the second Cl1- site, Cl1- is bonded in a water-like geometry to two equivalent W5+ atoms. In the third Cl1- site, Cl1- is bonded in a single-bond geometry to one W5+ atom. In the fourth Cl1- site, Cl1- is bonded in a single-bond geometry to one W5+ atom. In the fifth Cl1- site, Cl1- is bonded in a water-like geometry to two equivalent W5+ atoms. In the sixth Cl1- site, Cl1- is bonded in a single-bond geometry to one W5+ atom.

36 MATERIALS SCIENCE↗

Materials Data on Cu2WO4 by Materials Project

Cu2WO4 crystallizes in the triclinic P1 space group. The structure is three-dimensional. there are four inequivalent W6+ sites. In the first W6+ site, W6+ is bonded to six O2- atoms to form distorted edge-sharing WO6 octahedra. There are a spread of W–O bond distances ranging from 1.81–2.21 Å. In the second W6+ site, W6+ is bonded in a 6-coordinate geometry to six O2- atoms. There are a spread of W–O bond distances ranging from 1.77–2.30 Å. In the third W6+ site, W6+ is bonded to six O2- atoms to form distorted edge-sharing WO6 octahedra. There are a spread of W–O bond distances ranging from 1.81–2.21 Å. In the fourth W6+ site, W6+ is bonded in a 6-coordinate geometry to six O2- atoms. There are a spread of W–O bond distances ranging from 1.78–2.29 Å. There are eight inequivalent Cu1+ sites. In the first Cu1+ site, Cu1+ is bonded in a distorted T-shaped geometry to three O2- atoms. There are a spread of Cu–O bond distances ranging from 1.86–2.20 Å. In the second Cu1+ site, Cu1+ is bonded in a distorted T-shaped geometry to three O2- atoms. There are a spread of Cu–O bond distances ranging from 1.86–2.17 Å. In the third Cu1+ site, Cu1+ is bonded in a T-shaped geometry to three O2- atoms. There are a spread of Cu–O bond distances ranging from 1.85–2.46 Å. In the fourth Cu1+ site, Cu1+ is bonded in a linear geometry to two O2- atoms. Both Cu–O bond lengths are 1.85 Å. In the fifth Cu1+ site, Cu1+ is bonded in a linear geometry to two O2- atoms. There is one shorter (1.87 Å) and one longer (1.88 Å) Cu–O bond length. In the sixth Cu1+ site, Cu1+ is bonded in a T-shaped geometry to three O2- atoms. There are a spread of Cu–O bond distances ranging from 1.85–2.44 Å. In the seventh Cu1+ site, Cu1+ is bonded in a linear geometry to two O2- atoms. There is one shorter (1.87 Å) and one longer (1.88 Å) Cu–O bond length. In the eighth Cu1+ site, Cu1+ is bonded in a linear geometry to two O2- atoms. Both Cu–O bond lengths are 1.91 Å. There are sixteen inequivalent O2- sites. In the first O2- site, O2- is bonded in a bent 150 degrees geometry to one W6+ and one Cu1+ atom. In the second O2- site, O2- is bonded in a bent 150 degrees geometry to one W6+ and one Cu1+ atom. In the third O2- site, O2- is bonded in a bent 150 degrees geometry to one W6+ and one Cu1+ atom. In the fourth O2- site, O2- is bonded in a distorted trigonal planar geometry to two W6+ and one Cu1+ atom. In the fifth O2- site, O2- is bonded in a distorted trigonal planar geometry to two W6+ and one Cu1+ atom. In the sixth O2- site, O2- is bonded in a bent 150 degrees geometry to one W6+ and one Cu1+ atom. In the seventh O2- site, O2- is bonded in a 3-coordinate geometry to one W6+ and two Cu1+ atoms. In the eighth O2- site, O2- is bonded in a distorted trigonal planar geometry to two W6+ and one Cu1+ atom. In the ninth O2- site, O2- is bonded in a linear geometry to one W6+ and one Cu1+ atom. In the tenth O2- site, O2- is bonded in a linear geometry to one W6+ and one Cu1+ atom. In the eleventh O2- site, O2- is bonded in a trigonal planar geometry to one W6+ and two Cu1+ atoms. In the twelfth O2- site, O2- is bonded in a 3-coordinate geometry to one W6+ and two Cu1+ atoms. In the thirteenth O2- site, O2- is bonded in a 4-coordinate geometry to three W6+ and one Cu1+ atom. In the fourteenth O2- site, O2- is bonded in a trigonal planar geometry to one W6+ and two Cu1+ atoms. In the fifteenth O2- site, O2- is bonded in a distorted trigonal planar geometry to two W6+ and one Cu1+ atom. In the sixteenth O2- site, O2- is bonded in a 4-coordinate geometry to three W6+ and one Cu1+ atom.

36 MATERIALS SCIENCE↗

Materials Data on WOF4 by Materials Project

WOF4 crystallizes in the monoclinic C2/m space group. The structure is zero-dimensional and consists of two WOF4 clusters. there are two inequivalent W6+ sites. In the first W6+ site, W6+ is bonded to two equivalent O2- and four F1- atoms to form corner-sharing WO2F4 octahedra. The corner-sharing octahedral tilt angles are 1°. Both W–O bond lengths are 1.92 Å. There is three shorter (1.88 Å) and one longer (1.89 Å) W–F bond length. In the second W6+ site, W6+ is bonded to two equivalent O2- and four F1- atoms to form corner-sharing WO2F4 octahedra. The corner-sharing octahedral tilt angles are 1°. Both W–O bond lengths are 1.92 Å. All W–F bond lengths are 1.89 Å. O2- is bonded in a linear geometry to two W6+ atoms. There are five inequivalent F1- sites. In the first F1- site, F1- is bonded in a single-bond geometry to one W6+ atom. In the second F1- site, F1- is bonded in a single-bond geometry to one W6+ atom. In the third F1- site, F1- is bonded in a single-bond geometry to one W6+ atom. In the fourth F1- site, F1- is bonded in a single-bond geometry to one W6+ atom. In the fifth F1- site, F1- is bonded in a single-bond geometry to one W6+ atom.

36 MATERIALS SCIENCE↗

Materials Data on Rb(WO3)3 by Materials Project

Rb(WO3)3 crystallizes in the hexagonal P6_3/mcm space group. The structure is three-dimensional. Rb1+ is bonded to twelve equivalent O2- atoms to form RbO12 cuboctahedra that share edges with twelve equivalent WO6 octahedra and faces with two equivalent RbO12 cuboctahedra. All Rb–O bond lengths are 3.36 Å. W+5.67+ is bonded to six O2- atoms to form WO6 octahedra that share corners with six equivalent WO6 octahedra and edges with four equivalent RbO12 cuboctahedra. The corner-sharing octahedra tilt angles range from 0–31°. There are a spread of W–O bond distances ranging from 1.94–1.96 Å. There are two inequivalent O2- sites. In the first O2- site, O2- is bonded in a bent 150 degrees geometry to two equivalent Rb1+ and two equivalent W+5.67+ atoms. In the second O2- site, O2- is bonded in a linear geometry to two equivalent W+5.67+ atoms.

36 MATERIALS SCIENCE↗

Materials Data on RbNa5(WN3)2 by Materials Project

RbNa5(WN3)2 crystallizes in the monoclinic P2_1/c space group. The structure is three-dimensional. there are two inequivalent Rb1+ sites. In the first Rb1+ site, Rb1+ is bonded in a 3-coordinate geometry to three N3- atoms. There are two shorter (2.93 Å) and one longer (3.17 Å) Rb–N bond lengths. In the second Rb1+ site, Rb1+ is bonded in a 4-coordinate geometry to four N3- atoms. There are a spread of Rb–N bond distances ranging from 3.00–3.23 Å. There are ten inequivalent Na1+ sites. In the first Na1+ site, Na1+ is bonded in a 4-coordinate geometry to four N3- atoms. There are a spread of Na–N bond distances ranging from 2.43–2.80 Å. In the second Na1+ site, Na1+ is bonded to four N3- atoms to form distorted NaN4 tetrahedra that share corners with four WN4 tetrahedra and an edgeedge with one NaN4 tetrahedra. There are a spread of Na–N bond distances ranging from 2.40–2.52 Å. In the third Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.51–2.92 Å. In the fourth Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.42–2.85 Å. In the fifth Na1+ site, Na1+ is bonded to four N3- atoms to form distorted NaN4 tetrahedra that share corners with four WN4 tetrahedra and an edgeedge with one NaN4 tetrahedra. There are a spread of Na–N bond distances ranging from 2.44–2.49 Å. In the sixth Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.44–2.69 Å. In the seventh Na1+ site, Na1+ is bonded in a 3-coordinate geometry to four N3- atoms. There are a spread of Na–N bond distances ranging from 2.39–2.83 Å. In the eighth Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.51–2.77 Å. In the ninth Na1+ site, Na1+ is bonded in a 6-coordinate geometry to six N3- atoms. There are a spread of Na–N bond distances ranging from 2.51–3.08 Å. In the tenth Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.52–2.82 Å. There are four inequivalent W6+ sites. In the first W6+ site, W6+ is bonded to four N3- atoms to form WN4 tetrahedra that share corners with two WN4 tetrahedra and corners with four NaN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.84–1.94 Å. In the second W6+ site, W6+ is bonded to four N3- atoms to form WN4 tetrahedra that share corners with two NaN4 tetrahedra and corners with two WN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.83–1.94 Å. In the third W6+ site, W6+ is bonded to four N3- atoms to form WN4 tetrahedra that share corners with two NaN4 tetrahedra and corners with two WN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.83–1.96 Å. In the fourth W6+ site, W6+ is bonded to four N3- atoms to form corner-sharing WN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.84–1.94 Å. There are twelve inequivalent N3- sites. In the first N3- site, N3- is bonded in a 6-coordinate geometry to one Rb1+, four Na1+, and one W6+ atom. In the second N3- site, N3- is bonded in a 6-coordinate geometry to five Na1+ and one W6+ atom. In the third N3- site, N3- is bonded to four Na1+ and two W6+ atoms to form NNa4W2 octahedra that share corners with two equivalent NNa4W2 octahedra and an edgeedge with one NRbNa3W2 octahedra. The corner-sharing octahedral tilt angles are 45°. In the fourth N3- site, N3- is bonded in a 6-coordinate geometry to one Rb1+, four Na1+, and one W6+ atom. In the fifth N3- site, N3- is bonded in a 5-coordinate geometry to one Rb1+, three Na1+, and one W6+ atom. In the sixth N3- site, N3- is bonded to one Rb1+, three Na1+, and two W6+ atoms to form distorted edge-sharing NRbNa3W2 octahedra. In the seventh N3- site, N3- is bonded in a 6-coordinate geometry to one Rb1+, four Na1+, and one W6+ atom. In the eighth N3- site, N3- is bonded in a 6-coordinate geometry to five Na1+ and one W6+ atom. In the ninth N3- site, N3- is bonded in a 5-coordinate geometry to four Na1+ and one W6+ atom. In the tenth N3- site, N3- is bonded to four Na1+ and two W6+ atoms to form distorted NNa4W2 octahedra that share corners with two equivalent NNa4W2 octahedra and an edgeedge with one NRbNa3W2 octahedra. The corner-sharing octahedral tilt angles are 45°. In the eleventh N3- site, N3- is bonded in a 6-coordinate geometry to one Rb1+, four Na1+, and one W6+ atom. In the twelfth N3- site, N3- is bonded in a 6-coordinate geometry to one Rb1+, three Na1+, and two W6+ atoms.

36 MATERIALS SCIENCE↗

Materials Data on CsNa5(WN3)2 by Materials Project

CsNa5(WN3)2 crystallizes in the monoclinic P2_1/c space group. The structure is three-dimensional. there are two inequivalent Cs1+ sites. In the first Cs1+ site, Cs1+ is bonded in a 6-coordinate geometry to four N3- atoms. There are a spread of Cs–N bond distances ranging from 3.13–3.33 Å. In the second Cs1+ site, Cs1+ is bonded in a 3-coordinate geometry to three N3- atoms. There are two shorter (3.06 Å) and one longer (3.27 Å) Cs–N bond lengths. There are ten inequivalent Na1+ sites. In the first Na1+ site, Na1+ is bonded in a 3-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.43–3.02 Å. In the second Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.49–2.69 Å. In the third Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.55–2.78 Å. In the fourth Na1+ site, Na1+ is bonded in a 6-coordinate geometry to six N3- atoms. There are a spread of Na–N bond distances ranging from 2.52–3.12 Å. In the fifth Na1+ site, Na1+ is bonded in a 4-coordinate geometry to four N3- atoms. There are a spread of Na–N bond distances ranging from 2.45–2.74 Å. In the sixth Na1+ site, Na1+ is bonded to four N3- atoms to form distorted NaN4 tetrahedra that share corners with four WN4 tetrahedra and an edgeedge with one NaN4 tetrahedra. There are a spread of Na–N bond distances ranging from 2.42–2.55 Å. In the seventh Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.42–2.88 Å. In the eighth Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.52–2.82 Å. In the ninth Na1+ site, Na1+ is bonded in a 5-coordinate geometry to five N3- atoms. There are a spread of Na–N bond distances ranging from 2.53–2.94 Å. In the tenth Na1+ site, Na1+ is bonded to four N3- atoms to form distorted NaN4 tetrahedra that share corners with four WN4 tetrahedra and an edgeedge with one NaN4 tetrahedra. There are a spread of Na–N bond distances ranging from 2.47–2.51 Å. There are four inequivalent W6+ sites. In the first W6+ site, W6+ is bonded to four N3- atoms to form WN4 tetrahedra that share corners with two NaN4 tetrahedra and corners with two WN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.83–1.93 Å. In the second W6+ site, W6+ is bonded to four N3- atoms to form WN4 tetrahedra that share corners with two WN4 tetrahedra and corners with four NaN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.84–1.94 Å. In the third W6+ site, W6+ is bonded to four N3- atoms to form WN4 tetrahedra that share corners with two NaN4 tetrahedra and corners with two WN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.84–1.96 Å. In the fourth W6+ site, W6+ is bonded to four N3- atoms to form corner-sharing WN4 tetrahedra. There are a spread of W–N bond distances ranging from 1.84–1.94 Å. There are twelve inequivalent N3- sites. In the first N3- site, N3- is bonded in a 6-coordinate geometry to one Cs1+, four Na1+, and one W6+ atom. In the second N3- site, N3- is bonded to four Na1+ and two W6+ atoms to form distorted corner-sharing NNa4W2 octahedra. The corner-sharing octahedral tilt angles are 45°. In the third N3- site, N3- is bonded in a 5-coordinate geometry to one Cs1+, three Na1+, and one W6+ atom. In the fourth N3- site, N3- is bonded in a 7-coordinate geometry to one Cs1+, five Na1+, and one W6+ atom. In the fifth N3- site, N3- is bonded in a 6-coordinate geometry to five Na1+ and one W6+ atom. In the sixth N3- site, N3- is bonded in a 7-coordinate geometry to one Cs1+, five Na1+, and one W6+ atom. In the seventh N3- site, N3- is bonded in a 6-coordinate geometry to one Cs1+, three Na1+, and two W6+ atoms. In the eighth N3- site, N3- is bonded in a 6-coordinate geometry to one Cs1+, three Na1+, and two W6+ atoms. In the ninth N3- site, N3- is bonded in a 3-coordinate geometry to one Cs1+, three Na1+, and one W6+ atom. In the tenth N3- site, N3- is bonded in a 6-coordinate geometry to five Na1+ and one W6+ atom. In the eleventh N3- site, N3- is bonded to four Na1+ and two W6+ atoms to form corner-sharing NNa4W2 octahedra. The corner-sharing octahedral tilt angles are 45°. In the twelfth N3- site, N3- is bonded in a 5-coordinate geometry to four Na1+ and one W6+ atom.

36 MATERIALS SCIENCE↗