Element Abundances Research Articles

Tuning conduction properties and clarifying thermoelectric performance of P-type half-Heusler alloys TiNi1−xCoxSn (0 ≤ x ≤ 0.15)

TiNiSn is an N-type thermoelectric material with a high-power factor composed of low toxicity and abundant elements. TiNiSn also shows P-type electrical conduction by hole doping. In this study, we tune the conduction properties of TiNi1−xCoxSn (0 ≤ x ≤ 0.15) with Co substitution at the Ni site. The samples were prepared by the arc melting method, and thermoelectric properties were investigated up to 800 K. The results of the Hall effect and the Seebeck coefficient measurements indicate that the majority of charge carriers changes from electrons to holes at x ≥ 0.03, suggesting that Co acts as an acceptor. We report for the first time that Ti0.994Ni1.00Co0.051Sn1.01 exhibits ZT = 0.12 at 675 K. This work reveals that Ti0.994Ni1.00Co0.051Sn1.01 could be a potential P-type thermoelectric material operating at high temperatures.

Chemical Composition, In vitro and In silico Evaluation of Essential Oil Extracted from Mentha Piperita L. for Lung Cancer

Background: Mentha piperita, a naturally occurring herb, is utilized in medicinal formulations. It possesses abundant bioactive elements, including flavonoids and phenolic acid compounds,that exhibit various properties such as antioxidants, anti-inflammatory and anti-cancer. Objective: In the present study, chemical constituents of essential oil extracted from Mentha piperita were analyzed and identified through GC-MS. In vitro antiproliferative activity was performed on A549 lung cancer cell line lines. In silico study was conducted by Schrodinger’s Maestro’s software to identify chemical constituents in the plant as potential EGFR (Epidermal Growth Factor Receptors) inhibitors Methods: Hydro-distilled essential oil was analyzed by GC-MS to identify chemical components based on the retention index and mass fragmentation pattern, which was then tested for its antiproliferative activity by MTT assay against human lung cancer cell lines. All the identified constituents were investigated in silico for their affinity towards EGFR (Epidermal Growth Factor Receptors). Results: A total of thirty constituents were identified where D-carvone (56.69%), L-limonene (12.36%), squalene (3.36%), cis-carveol (2.93%), and α-amorphene (2.36%) were observed as major constituents of the essential oil. The essential mentha oil also exhibited antiproliferative activity against lung cancer cell lines with an IC50 value of 86.05 µg/ml. Furthermore, from the in silico study, five constituents were identified to have a better affinity for EGFR (Epidermal Growth Factor Receptors) than that of the standard drug Osimertinib. Conclusion: In the present study, the aerial part of the plant Mentha piperita was hydrodistilled.Thirty phytoconstituents were identified through GC-MS data. An in-silico study was performed using Schrodinger software, and a further in vitro study was performed in which essential oil showedgood antiproliferative activity against the A549 cancer cell line.

Gaia-Sausage-Enceladus star formation history as revealed by detailed elemental abundances. An archival study using SAGA data

The Gaia-Sausage-Enceladus merger was a major event in the history of the Milky Way. Debris from this merger has been extensively studied with full kinematic data from the Gaia mission. Understanding the star formation history of the progenitor galaxy aids in our understanding of the evolution of the Milky Way and galaxy formation in general. We aimed to constrain the star formation history of the Gaia-Sausage-Enceladus progenitor galaxy using elemental abundances of member stars. Previous studies on Milky Way satellite dwarf galaxies show that key elemental abundance patterns, which probe different nucleosynthetic channels, reflect the host galaxy's star formation history. We gathered Mg, Fe, Ba, and Eu abundance measurements for Gaia-Sausage-Enceladus stars from the SAGA database. Gaia-Sausage-Enceladus members were selected kinematically. Inspired by previous studies, we used Fe/Mg Ba/Mg Eu/Mg and Eu/Ba as a function of Fe/H to constrain the star formation history of Gaia-Sausage-Enceladus. We used the known star formation histories and elemental abundance patterns of the Sculptor and Fornax dwarf spheroidal galaxies as a comparison. The elemental abundance ratios of Fe/Mg Ba/Mg Eu/Mg and Eu/Ba all increase with Fe/H in Gaia-Sausage-Enceladus. The Eu/Mg begins to increase at Fe/H -2.0$ and continues steadily, contrasting with the trend observed in the Sculptor dSph galaxy. The Eu/Ba increases and remains high across the Fe/H range, unlike the pattern seen in the Sculptor dSph galaxy, and deviates from the Fornax dSph galaxy at high Fe/H . The Ba/Mg is higher than those of the Sculptor dSph galaxy at the lowest Fe/H and gradually increases, similar to the Fornax dSph galaxy. We constrained three main properties of the Gaia-Sausage-Enceladus star formation history: 1) star formation started gradually, 2) it extended for over 2 Gyr, and 3) it was quenched around Fe/H of $-0.5$, likely when it fell into the Milky Way. We show that the elemental abundance ratios Fe/Mg Ba/Mg Eu/Mg and Eu/Ba can be used to trace the star formation history of a disrupted galaxy when these measurements are available over an Fe/H range that is representative of the progenitor galaxy's stellar population.

A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances

Stars in an open cluster are assumed to have formed from a broadly homogeneous distribution of gas, implying that they should be chemically homogeneous. Quantifying the level to which open clusters are chemically homogeneous can therefore tell us about interstellar medium pollution and gas mixing in progenitor molecular clouds. Using Sloan Digital Sky Survey (SDSS)-V Milky Way Mapper and SDSS-IV Apache Point Observatory Galaxy Evolution Experiment DR17 abundances, we test this assumption by quantifying intrinsic chemical scatter in up to 20 different chemical abundances across 26 Milky Way open clusters. We find that we can place 3σ upper limits on open cluster homogeneity within 0.02 dex or less in the majority of elements, while for neutron capture elements, as well as those elements having weak lines, we place limits on their homogeneity within 0.2 dex. Finally, we find that giant stars in open clusters are ∼0.01 dex more homogeneous than a matched sample of field stars.

The Radcliffe wave as traced by young open clusters. Stellar parameters, activity indicators, and abundances of solar-type members of eight young clusters

The Radcliffe wave has only recently been recognised as a approx 3\,kpc long coherent gas structure encompassing most of the star-forming regions in the solar vicinity. Since its discovery, it has been mainly studied from the perspective of dynamics, but a detailed chemical study is necessary to understand its nature and the composition of the natal clouds that gave rise to it. For this paper we used some of the connected young open clusters (age lesssim 100 Myr) as tracers of the molecular clouds. We performed high-resolution spectroscopy with GIARPS at the TNG of 53 stars that are bona fide members of seven clusters located at different positions along the Radcliffe wave. We provide radial velocities and atmospheric parameters for all of them. For a subsample consisting of 41 FGK stars, we also studied the chromospheric activity and the content of Li, from which we inferred the age of the parent clusters. These values agree with the evolutionary ages reported in the literature. For these FGK stars, we determined the chemical abundances for 25 species. Pleiades, ASCC\,16, and NGC\,7058 exhibit a solar metallicity while Melotte\,20, ASCC\,19, NGC\,2232, and Roslund\,6 show a slightly subsolar value (approx \,$-$0.1\,dex). On average, the clusters show a chemical composition compatible with that of the Sun, especially for alpha - and Fe-peak elements. Neutron-capture elements, on the other hand, present a slight overabundance of about 0.2\,dex, especially barium. Finally, considering also ASCC\,123, which was studied by our group in a previous research project, we inferred a correlation between the chemical composition and the age or position of the clusters along the wave, demonstrating their physical connection within an inhomogeneous mixing scenario.

Occurrence, non-carcinogenic and carcinogenic risk assessment of trace elements in rainwater in the vicinity of a cement factory in northeastern Nigeria

Rapid industrialization and urbanization result in atmospheric pollution with trace elements precipitated and deposited by rain, affecting human health. This study determined the concentrations and non-carcinogenic and carcinogenic risks associated with trace elements in rainwater in the vicinity of the Ashaka cement factory. Samples were collected using a bulk sampler fitted with a high-density polythene funnel. A total of 140 samples were collected in 2020 and analyzed for 15 trace elements using ICP-OES. Multivariate analysis was used to identify the sources of the rainwater trace elements. The results show that the abundance of trace elements in the collected samples was in the following order: Fe > Sb > Cu > Ba > V > Sc > Sr > Mn > Zn > Ti > Hg > Al > Mo > Co. Crustal enrichment factors (EFc) indicated that the samples were extremely enriched with Hg, Sb, Cu, and Mo, moderately enriched with Zn, Ba, V, Co, Sr, Cr, and Sc, and unenriched with Fe, Mn, Ti, and Al. Chronic daily intake (CDI) for both the ingestion and dermal pathways was in the order Fe > Cu > Ba > Cr > V > Mn > Zn > Hg > Mo. The hazard index (HI) was > 1 through the ingestion pathway, indicating a likely non-carcinogenic advertising effect. Similarly, the carcinogenic risk (CR) exceeded the (1.0 × 10–4—1.0 × 10–4) acceptable limit for children and adults, indicating the likely development of cancer among consumers. This revealed that the elements present in rainwater are anthropogenic and are brought about by cement production.

The ninth art, tells the story of cultural China and the world: Cultural interaction in cross-cultural video game communication-based on 'Genshin Impact' YouTube comments.

China has attached increasing importance to the overseas dissemination of traditional culture as it continues to strengthen its comprehensive national strength and develop globalization initiatives. The electronic game, as the 'ninth art', with its booming development and inherent cross-cultural communication platform attributes, has taken on the important task of taking culture abroad. This study selects 'Genshin Impact', a game highly praised and well-received globally, which contains an abundance of Chinese cultural elements and cultural elements from various regions of the world, to study cultural interaction in cross-cultural communication of electronic games. This study conducts text sentiment analysis and semantic network analysis on the comments of 'Genshin Impact' videos on the overseas video platform YouTube and studies the cultural interaction in the cross-cultural communication of the 'ninth art', telling the cultural stories of China and the world from a multicultural perspective. The study found that games and derivative videos triggered positive emotional responses from audiences both at home and abroad. While experiencing pleasure and surprise, audiences also arouse deeper emotions such as admiration, identification, and expectation. Meanwhile, in the complex art form of the 'ninth art', audiences can absorb the cultural elements of different cultures, resonate with the elements of their cultural circle, and even trigger further profound thinking. Finally, this study provides constructive suggestions on using the 'ninth art' to better 'tell China's stories and disseminate China's voice'.

Two-Dimensional MXene (Ti3C2Tx)-based Nano-Photosensitizers for Enhanced Photothermal Ablation of Tumor Cells

Cancer remains one of the leading causes of death globally, accounting for approximately one in every six deaths. Traditional cancer therapies, including surgery, chemotherapy, chemoimmunotherapy, and radiation, face numerous challenges and limitations. In this context, we explore the advantages of photothermal therapy (PTT) using two-dimensional (2D) MXene-based nanocomposites for cancer treatment. MXenes, composed of abundant and non-toxic elements, such as titanium (Ti), carbon (C), fluorine (F), and oxygen (O), demonstrate low toxicity and are promising candidates in photothermal cancer therapies. Their ultrathin planar nanostructure, high photothermal conversion efficiency, strong near-infrared (NIR) responsiveness, and chemically modifiable surfaces enhance their therapeutic potential. Recent innovations include the development of folic acid-functionalized Au@c-Ti3C2 nanostructures, a skin-mountable electrostimulation patch (eT-patch), ionic gels containing MXene (Ti3C2Tx), and composite scaffolds made of MXene, collagen, silk fibroin, and quercetin. These MXene-based photosensitive compounds offer efficient targeting and selective treatment of cancer cells, highlighting their significant role in advancing cancer therapies.

Full Abundance Study of Two Newly Discovered Barium Giants

Barium (Ba) stars are chemically peculiar stars that show enhanced surface abundances of heavy elements produced by the slow-neutron-capture process, the so-called s-process. These stars are not sufficiently evolved to undergo the s-process in their interiors, so they are considered products of binary interactions. Ba stars form when a former Asymptotic Giant Branch (AGB) companion, which is now a white dwarf, pollutes them with s-process-rich material through mass transfer. This paper presents a detailed chemical characterization of two newly discovered Ba giants. Our main goal is to confirm their status as extrinsic s-process stars and explore potential binarity and white dwarf companions. We obtained high-resolution spectra with UVES on the Very Large Telescope to determine the chemical properties of the targets. We perform line-by-line analyses and measure 22 elements with an internal precision up to 0.04 dex. The binary nature of the targets is investigated through radial velocity variability and spectral energy distribution fitting. We found that both targets are enhanced in all the measured s-process elements, classifying our targets as Ba giants. This is the first time they are classified as such in the literature. Additionally, both stars present a mild enhancement in Eu, but less than in pure s-process elements, suggesting that the sources that polluted them were pure s-process sources. Finally, we confirmed that the two targets are RV variable and likely binary systems. The abundances in these two newly discovered polluted binaries align with classical Ba giants, providing observational constraints to better understand the s-process in AGB stars.

Elemental mapping in single-particle reconstructions by reconstructed electron energy-loss analysis.

For macromolecular structures determined by cryogenic electron microscopy, no technique currently exists for mapping elements to defined locations, leading to errors in the assignment of metals and other ions, cofactors, substrates, inhibitors and lipids that play essential roles in activity and regulation. Elemental mapping in the electron microscope is well established for dose-tolerant samples but is challenging for biological samples, especially in a cryo-preserved state. Here we combine electron energy-loss spectroscopy with single-particle image processing to allow elemental mapping in cryo-preserved macromolecular complexes. Proof-of-principle data show that our method, reconstructed electron energy-loss (REEL) analysis, allows a three-dimensional reconstruction of electron energy-loss spectroscopy data, such that a high total electron dose is accumulated across many copies of a complex. Working with two test samples, we demonstrate that we can reliably localize abundant elements. We discuss the current limitations of the method and potential future developments.

Differences in elemental abundances between CI chondrites and the solar photosphere

AbstractCI chondrites have been a proxy for the solar system since the mid‐20th century. The photospheric and CI chondrite abundances (P and CI, respectively) show a strong correlation. CI as a proxy is also justified by the (i) smoothness of their abundances plotted as a function of odd mass number and (ii) agreement within the error of P as determined spectroscopically. But our statistical assessment of spectroscopic studies and solar wind from the Genesis mission indicates that the small, ~10%–30%, differences (residuals) between CI and P depend on the 50% condensation temperature (Tc50). So, if CI is to be used as a proxy for P, Cosmochemists may want to add a correction to individual elements. Our work is consistent with two published hypotheses: that (i) residuals are linear with Tc50 and (ii) that elements having Tc50 > 1343 K are depleted relative to those with 495 K < Tc50 < 1343 K in CI. We discuss other interpretations which are also feasible. Understanding these small differences of the CI and P for different elements and their variation with Tc50 can help constrain future models of solar system formation and the history of CI chondrites.

Geochemical Characteristic of the Carbonaceous Sediments of the Upper Paleozoic Kuantan Group, Malaysia

The geochemical parameters discussed in this paper are based on an average values of twelve outcrop carbonaceous samples, mainly black shales, were determined using X-Ray Fluorescence (XRF) and Inductively Coupled Plasma-Mass Spectrometer (ICP-MS) techniques, representative of Charu, Sagor, and Permian formations.The aim of this study is to define and discuss their characteristics, the distribution abundance of major and minor elements, investigation the dominant mineralogical composition and reconstruct the depositional environment for these sediments.The bulk chemical result showed that, the average values of the major elements are 65.83%, 64.82 %, 71.4 % SiO2, 18.27 %, 22.2 %, 15.66 % Al2O3, 1.53 %, 0.99 %, 2.49 % Fe2O3. 4.06 %, 6.25 %, 3.66 % K2O , whereas in the case of the miner elements, the results read values of 524.4 ppm, 758.8 ppm, 446.3 ppm Ba , 366 ppm, 399.3 ppm, 257.3 ppm Rb, 88 ppm, 67.3 ppm, 47.3 ppm Sr , 308 ppm, 288.8 ppm, 327ppm Zr for the Charu, Sagor, and Permian formations respectively. The major oxides reflect the dominant mineralogical composition of quartz and other silicate minerals (e.g. illite, kaolinte, smectite) and deficiency in carbonates.The high Rb/K ratio suggests brackish marine environment or rapid depositions that prevent equilibrium between Rb and K in these study shales and marine environment. The high Rb/Sr ratios of 4.16, 5.89 and 5.44 for the Charu, Sagor, and Permian formations respectively possibly attributed to the lowest contents of Sr content due to reducing environment prevailing during deposition of these sediments.

Rare earth element assessment in Jezero crater using the Planetary Instrument for X-ray Lithochemistry on the Mars 2020 rover Perseverance: A case study of cerium

The “Planetary Instrument for X-ray Lithochemistry” (PIXL) X-ray spectrometer conducts in situ geochemical analyses of martian rocks and regolith interrogated by the Mars 2020 rover, Perseverance. In addition to quantifying primary rock-forming elements, PIXL can quantify trace elements that in turn can provide additional constraints on the geologic history of Mars. Accurate quantifications of trace elements can require additional analytical techniques to mitigate experimental, background, and crystalline effects within PIXL spectra. In this study, we focus on reducing the impact of these effects and investigate the potential presence of rare earth elements (REEs). The study specifically investigates cerium given its typical relative abundance in many geologic materials compared to other REEs and its potential to mimic fluorescence features produced by organics under deep UV excitation. A detailed analysis of PIXL targets analyzed through the first 887 martian days of the Perseverance mission did not produce any conclusive Ce detections. Phosphorus-enriched materials analyzed by PIXL are estimated to contain sub-675 ppm Ce and sulfate-enriched materials sub-450 ppm Ce. The method presented can help constrain limits on the abundance of additional trace elements of interest that also face a similar analytical burden. PIXL's potential to assess REE abundances, outside of yttrium, is limited for expected concentrations in surface materials. Determining most REE concentrations in materials interrogated by Perseverance will therefore likely require terrestrial analyses.

Ba and Sr isotopic patterns from step‐leaching experiments on the pristine Aguas Zarcas CM2 meteorite

AbstractStepwise acid leaching experiments were performed on the pre‐rain CM2 fall Aguas Zarcas to interrogate release patterns and isolate fractions with isotopic anomalies. Acid leachates and a bulk sample were analyzed for elemental abundances via solution ICP‐MS, and Sr and Ba isotopic compositions were measured using TIMS. Isotopic systematics reveal diverse values for the bulk sample and leachates, interpreted to reflect the Aguas Zarcas parent body history. Compared with the NBS987 standard, μ84Sr values for the bulk sample average + 90, while the leach fractions yield +326 to −2089, with the largest μ84Sr depletions in the strongest acid leachates. For Ba isotopes, the bulk sample shows resolvable depletions (μ values) in 130Ba (−210), 135Ba (−64), 137Ba (−73) and 138Ba (−89). Early leachates show positive anomalies in 130Ba (up to +2295), 132Ba, 135Ba, 137Ba, and 138Ba. In contrast, final leachates show strong depletions for the same nuclides (up to −60,000 ppm μ130Ba). The Sr and Ba isotopic anomalies found in the earlier leachates suggest that nucleosynthetic signatures were redistributed to more soluble phases during parent body alteration. Moreover, contrasting p‐nuclide Sr and Ba nucleosynthetic anomalies suggest that presolar contributions came from a variety of nucleosynthetic sources, including possibly a rotating massive star undergoing a core‐collapse supernova or an electron capture supernova.

On the Nature of the C IV-bearing Circumgalactic Medium at z~1

This paper presents a detailed study of the physical properties of seven C IV absorbers identified at z_abs = 0.68-1.28 along the line of sight toward QSO PG 1522+101 (z_QSO = 1.330). The study leverages high-quality QSO spectra from HST COS and STIS, and Keck HIRES to resolve component structures and to constrain the gas density and elemental abundances of individual components. Under the assumption of photoionization equilibrium (PIE), five of the 12 C IV components require a mixture of high- and low-density phases to fully explain the observed relative abundances between low-, intermediate-, and high-ionization species. In addition, galaxy surveys carried out using VLT MUSE and Magellan LDSS3C are utilized to characterize the galaxy environments. The results of this analysis are summarized as follows: (1) no luminous galaxies (> 0.1 L*) are found within 100 kpc in projected distance from the C IV absorbers; (2) the C IV selection preferentially targets high-metallicity (near solar) and chemically-evolved gas (~ solar [C/O] elemental abundances) in galaxy halos; (3) the observed narrow line widths of individual C IV components, places a stringent limit on the gas temperature (< 5e4 K) and supports a photoionization origin; (4) additional local ionizing sources beyond the UV ionizing background may be necessary for at least one absorber based on the observed deficit of He I relative to H I; and (5) a PIE assumption may not apply when the gas metallicity exceeds the solar value and the component line width implies a warmer temperature than expected from PIE models.

Separating the Spectral Counterparts in NGC 1275/Perseus Cluster in X-Rays

We present a model-independent method for separating the spectral counterparts of the active galactic nucleus (AGN) NGC 1275 from the surrounding emission of the Perseus cluster, as observed by Suzaku/XIS cameras. The Perseus cluster emission extends to higher energies than typically observed in AGN environments, reaching up to 9–10 keV. This necessitates precise separation of AGN and cluster spectra. To circumvent the degeneracy arising from numerous spectral fitting parameters, including elemental abundances, thermal and Compton emissions from the nucleus, and spectral parameters of the jet synchrotron self-Compton/inverse Compton emissions, we avoid traditional spectral fitting methods. Instead, we leverage spatial resolution and employ a double background subtraction approach. We apply this procedure to the complete set of Suzaku/XIS observational data for NGC 1275, resulting in cleaned spectra and a light curve of the AGN emission in this system. To demonstrate the applicability of our method, we also utilize the available XMM-Newton/EPIC data.

Multielectron Reduction of Nitrosoarene via Aluminylene-Silylene Cooperation.

The cooperative effects of main-group elements pave the way for novel chemical transformations. However, the potential of bimetallic complexes featuring the most abundant aluminum and silicon elements remains largely unexplored. In this study, we present the synthesis and characterization of bis(silylene)-stabilized aluminylene 2. The cooperation between aluminylene and silylene allows for the facile cleavage of the N-O bond in nitrosoarenes, producing an aluminum imide complex 4 and tetracyclic oxazasilaalanes 5 and 6, and also promotes the dearomatization of 2-methylquinoline, yielding a silylalane 7. In addition, 2 is an effective precatalyst for the reductive coupling of nitrosoarenes to azoxyarenes. These results outline an approach for orchestrating aluminum and silicon cooperation to facilitate chemical bond activation.

A comparative high-resolution spectroscopic analysis of in situ and accreted globular clusters

Globular clusters (GCs) are extremely intriguing systems that help in reconstructing the assembly of the Milky Way via the characterisation of their chemo-chrono-dynamical properties. In this study, we use high-resolution spectroscopic archival data from UVES and UVES-FLAMES at the VLT to compare the chemistry of GCs dynamically tagged as either Galactic (NGC 6218, NGC 6522, and NGC 6626) or accreted from distinct merger events (NGC 362 and NGC 1261 from Gaia -Sausage-Enceladus, and Ruprecht 106 from the Helmi Streams) in the metallicity regime where abundance patterns of field stars with different origin effectively separate $( -1.3 We find remarkable similarities in the abundances of the two Gaia -Sausage-Enceladus GCs across all chemical elements. They both display depletion in the alpha -elements (Mg, Si and Ca) and statistically significant differences in Zn and Eu compared to in situ GCs. Additionally, we confirm that Ruprecht 106 exhibits a completely different chemical makeup from the other target clusters, being underabundant in all chemical elements. This demonstrates that when high precision is achieved, the abundances of certain chemical elements can not only efficiently separate in situ from accreted GCs, but can also distinguish among GCs born in different progenitor galaxies. In the end, we investigate the possible origin of the chemical peculiarity of Ruprecht 106. Given that its abundances do not match the chemical patterns of the field stars associated with its most likely parent galaxy (i.e. the Helmi Streams), being depleted in the abundances of alpha -elements in particular, we believe Ruprecht 106 to originate from a less massive galaxy compared to the progenitor of the Helmi Streams.

Mineral Composition of Fifteen Species of Asteraceae Family Growing in the Republic of Moldova Using Neutron Activation Analysis

Members of Asteraceae family have properties enabling their application for medical purposes. The major- and microelement content in 15 medicinal species of the Asteraceae family growing in the National Botanical Garden, Republic of Moldova was determined by instrumental neutron activation analysis. A total of 31 chemical elements, Na, Mg, Al, Cl, K, Ca, Sc, V, Cr, Mn, Fe, Co, Ni, Zn, As, Se, Br, Rb, Sr, Mo, Sb, Cs, Ba, La, Ce, Sm, Tb, Hf, Ta, Th and U, were identified in herbal samples. Potassium was found to be the most abundant major element; its content in plants ranged from 20,700 mg/kg in Artemisia lerchiana to 58,000 mg/kg in Matricaria recutita. The content of other major elements existed in the following ranges: Ca from 4700 to 14,200 mg/kg and Mg from 1710 to 3870 mg/kg. The maximum content of Mg, K and Ca in analyzed plants was higher compared to data presented in the literature. Among essential microelements the most abundant were Fe (83–910 mg/kg), Mn (23–150 mg/kg) and Zn (27–76 mg/kg). The daily intake of metal and the health risk index for selected elements (As, Ni, Sb, V, Mn, Cr, Co, U, Sr, Al, Fe, and Zn) were calculated. Health risk indexes were obtained for V and Co in Calendula officinalis, Tanacetum balsamita, Achillea clypeolata, Artemisia balchanorum, Artemisia lerchiana, Helichrysum arenarium, and Matricaria recutita. The principal component analysis showed three associations of elements, which can be defined as physiological, geological and anthropogenic sources of elements.

GA-NIFS: An extremely nitrogen-loud and chemically stratified galaxy at z ∼ 5.55

Abstract We report the chemical abundance pattern of GS_3073, a galaxy hosting an overmassive active black hole at z = 5.55, by leveraging observations from JWST/NIRSpec and VLT/VIMOS. Based on the rest-frame UV emission lines, which trace high-density (∼105 cm−3) and highly ionized gas, we derive $\rm \log (N/O) = 0.42^{+0.13}_{-0.10}$. At an estimated metallicity of 0.2 Z⊙, this is the most extreme nitrogen-rich object found by JWST thus far. In comparison, the relative carbon abundance derived is $\rm \log (C/O) = -0.38^{+0.13}_{-0.11}$, which is not significantly higher than those in local galaxies and stars with similar metallicities. We also found potential detection of [Fe vii]λ6087 and [Fe xiv]λ5303, both blended with [Ca v]. We inferred a range of Fe abundances compatible with those in local stars and galaxies. Overall, the chemical abundance pattern of GS_3073 is compatible with enrichment by supermassive stars with M* ≳ 1000 M⊙, asymptotic giant branch (AGB) stars, or Wolf-Rayet (WR) stars. Interestingly, when using optical emission lines which trace lower density (∼103 cm−3) and lower ionization gas, we found a sub-solar N/O ratio, consistent with local galaxies at the same metallicity. We interpret the difference in N/O derived from UV lines and optical lines as evidence for a stratified system, where the inner and denser region is both more chemically enriched and more ionized. Our results suggest that nitrogen loudness in high-z galaxies might be confined to the central, dense, and highly ionized regions of the galaxies, while the bulk of the galaxies evolves more normally.