Local structure adaptability through multi cations for oxygen redox accommodation in Li-Rich layered oxides

Stable lattice oxygen redox (l-OR) is the key enabler for achieving attainable high energy density in Li-rich layered oxide cathode materials for Li-ion batteries. However, the unique local structure response to oxygen redox in these materials, resulting in energy inefficiency and hysteresis, still remains elusive, preventing their potential applications. By combining the state-of-the-art neutron pair distribution function with crystal orbital overlap analysis, we directly observe the distinct local structure adaption originated from the potential O–O chemical bonds. The structure adaptability is optimized based on the nature of multi transition metals in our model compound Li1.2Ni0.13Mn0.54Co0.13O2, which accommodates the oxygen redox and at the same time preserves the global layered structure. These findings not only advance the understanding of l-OR, but also provide new perspectives in the rational design of high-energy-density cathode materials with reversible and stable l-OR

ALMA-IMF IX: Catalog and Physical Properties of 315 SiO Outflow Candidates in 15 Massive Protoclusters

We present a catalog of 315 protostellar outflow candidates detected in SiO J=5-4 in the ALMA-IMF Large Program, observed with ~2000 au spatial resolution, 0.339 km/s velocity resolution, and 2-12 mJy/beam (0.18-0.8 K) sensitivity. We find median outflow masses, momenta, and kinetic energies of ~0.3 M$_{\odot}$, 4 M$_{\odot}$ km/s, and 10$^{45}$ erg, respectively. Median outflow lifetimes are 6,000 years, yielding median mass, momentum, and energy rates of $\dot{M}$ = 10$^{-4.4}$ M$_{\odot}$ yr$^{-1}$, $\dot{P}$ = 10$^{-3.2}$ M$_{\odot}$ km/s yr$^{-1}$, and $\dot{E}$ = 1 L$_{\odot}$. We analyze these outflow properties in the aggregate in each field. We find correlations between field-aggregated SiO outflow properties and total mass in cores (~3$-$5$\sigma$), and no correlations above 3$\sigma$ with clump mass, clump luminosity, or clump luminosity-to-mass ratio. We perform a linear regression analysis and find that the correlation between field-aggregated outflow mass and total clump mass - which has been previously described in the literature - may actually be mediated by the relationship between outflow mass and total mass in cores. We also find that the most massive SiO outflow in each field is typically responsible for only 15-30% of the total outflow mass (60% upper limit). Our data agree well with the established mechanical force-bolometric luminosity relationship in the literature, and our data extend this relationship up to L $\geq$ 10$^6$ L$_{\odot}$ and $\dot{P}$ $\geq$ 1 M$_{\odot}$ km/s yr$^{-1}$. Our lack of correlation with clump L/M is inconsistent with models of protocluster formation in which all protostars start forming at the same time.Comment: 46 pages, 14 figures, 10 tables. This publication has an associated Zenodo entry, which can be found here: https://zenodo.org/records/835059

ALMA-IMF. VII. First release of the full spectral line cubes: Core kinematics traced by DCN J=(3-2)

ALMA-IMF is an Atacama Large Millimeter/submillimeter Array (ALMA) Large Program designed to measure the core mass function (CMF) of 15 protoclusters chosen to span their early evolutionary stages. It further aims to understand their kinematics, chemistry, and the impact of gas inflow, accretion, and dynamics on the CMF. We present here the first release of the ALMA-IMF line data cubes (DR1), produced from the combination of two ALMA 12m-array configurations. The data include 12 spectral windows, with eight at 1.3mm and four at 3mm. The broad spectral coverage of ALMA-IMF (~6.7 GHz bandwidth coverage per field) hosts a wealth of simple atomic, molecular, ionised, and complex organic molecular lines. We describe the line cube calibration done by ALMA and the subsequent calibration and imaging we performed. We discuss our choice of calibration parameters and optimisation of the cleaning parameters, and we demonstrate the utility and necessity of additional processing compared to the ALMA archive pipeline. As a demonstration of the scientific potential of these data, we present a first analysis of the DCN (3-2) line. We find that DCN traces a diversity of morphologies and complex velocity structures, which tend to be more filamentary and widespread in evolved regions and are more compact in the young and intermediate-stage protoclusters. Furthermore, we used the DCN (3-2) emission as a tracer of the gas associated with 595 continuum cores across the 15 protoclusters, providing the first estimates of the core systemic velocities and linewidths within the sample. We find that DCN (3-2) is detected towards a higher percentage of cores in evolved regions than the young and intermediate-stage protoclusters and is likely a more complete tracer of the core population in more evolved protoclusters. The full ALMA 12m-array cubes for the ALMA-IMF Large Program are provided with this DR1 release.Comment: 75 pages (21 main body; 54 appendix), 37 figures. The ALMA-IMF DR1 line release is hosted at https://dataverse.harvard.edu/dataverse/alma-im

Erratum: "The ALMA Survey of 70micron dark High-mass Clumps in Early Stages (ASHES). IV. Star formation signatures in G023.477" (2021, ApJ, 923, 147)

This is a correction for 2021 ApJ 923 147DOI 10.3847/1538-4357/ac2365Interstellar matter and star formatio

Synthetic Biology Open Language (SBOL) Version 1.1.0

In this BioBricks Foundation Request for Comments (BBF RFC), we specify the Synthetic Biology Open Language (SBOL) Version 1.1.0 to enable the electronic exchange of information describing DNA components used in synthetic biology. We define: 1. the vocabulary, a set of preferred terms and 2. the core data model, a common computational representation

The ALMA survey of 70 μm dark high-mass clumps in early stages (ASHES): IV. Star formation signatures in G023.477

Interstellar matter and star formatio

The JCMT Plane Survey: First complete data release - emission maps and compact source catalogue

We present the first data release of the James Clerk Maxwell Telescope (JCMT) Plane Survey (JPS), the JPS Public Release 1 (JPSPR1). JPS is an 850-µm continuum survey of six fields in the northern inner Galactic Plane in a longitude range of ℓ = 7°–63°, made with the Sub-millimetre Common-User Bolometer Array 2 (SCUBA-2). This first data release consists of emission maps of the six JPS regions with an average pixel-to-pixel noise of 7.19 mJy beam−1, when smoothed over the beam, and a compact-source catalogue containing 7,813 sources. The 95 per cent completeness limits of the catalogue are estimated at 0.04 Jy beam−1 and 0.3 Jy for the peak and integrated flux densities, respectively. The emission contained in the compact-source catalogue is 42 ± 5 per cent of the total and, apart from the large-scale (greater than 8 arcmin) emission, there is excellent correspondence with features in the 500-µm Herschel maps. We find that, with two-dimensional matching, 98 ± 2 per cent of sources within the fields centred at ℓ = 20°, 30°, 40° and 50° are associated with molecular clouds, with 91 ± 3 per cent of the ℓ = 30° and 40° sources associated with dense molecular clumps. Matching the JPS catalogue to Herschel 70-µm sources, we find that 38 ± 1 per cent of sources show evidence of ongoing star formation. The images and catalogue will be a valuable resource for studies of star formation in the Galaxy and the role of environment and spiral arms in the star formation process

SINTESIS MAGNETIT (Fe3O4) NANOPARTIKEL DENGAN NATRIUM DODESIL SULFAT

Telah dilakukan sintesis magnetit (Fe3O4) nanopartikel dengan Natrium Dodesil Sulfat (NaDS). Penelitian ini bertujuan untuk mengetahui pengaruh NaDS terhadap karakter kimia dan fisik magnetit nanopartikel hasil sintesis dengan metode kopresipitasi. Sintesis magnetit nanopartikel dilakukan dengan mereaksikan FeSO4.7H2O dan FeCl3.6H2O dengan perbandingan mol 1:2 serta natrium hidroksida (NaOH) sebagai presipitan dengan proses pengadukan pada suhu 60 °C selama 2 jam. Kajian pengaruh surfaktan pada sintesis magnetit nanopartikel dilakukan dengan variasi konsentrasi NaDS dari 1%, 3% dan 6% (b/v). Material hasil sintesis dikarakterisasi dengan spektrofotometer X-ray diffraction (XRD), Fourier Transform Infrared Spectrometer (FTIR), Scanning Electron Microscope-Energy Dispersive X-ray (SEM-EDX) dan Surface Area Analyzer (SAA). Hasil penelitian menunjukkan bahwa magnetit nanopartikel berhasil disintesis. Magnetit ditunjukkan oleh puncak difraksi utama pada 2θ 30,43o; 35,53o; 43,46o; 57,32o dan 62,84o. Ikatan Fe–O ditunjukkan dengan puncak serapan 565 cm-1 yang dianalisa lebih lanjut menggunakan EDX menunjukkan adanya unsur Fe dan O. Adanya surfaktan NaDS menaikkan ukuran partikel dan ukuran kristal magnetit dengan meningkatnya konsentrasi NaDS yang ditambahkan. Morfologi magnetit-NaDS semakin homogen berbentuk butiran-butiran kecil (grain) dengan ukuran partikel sekitar 30-100 nm. Ukuran kristal magnetit sebesar 11,07 nm (magnetit tanpa surfaktan); 13,62 nm (magnetit-NaDS 1%); 16,12 nm (magnetit-NaDS 3%) dan 11,17 nm (magnetit-NaDS 6%). Luas permukaan magnetit nanopartikel berturut-turut sebesar 89,67 m2/g (magnetit tanpa surfaktan); 102,50 m2/g (magnetit-NaDS 1%); 98,45 m2/g (magnetit-NaDS 3%) dan 82,92 m2/g (magnetit-NaDS 6%)