Lead is one of the most toxic heavy metals that frequently occur in the environment. Advancing applications that involve lead and its speciation across various samples require a detailed atomic-level investigation of lead compounds using X-ray absorption spectroscopy (XAS). In the present work, the XAS measurements across the L-3 absorption edge of Pb for different compounds (PbO, PbO2, PbSO4, Pb(NO3)(2), and PbCl2) have been done at the scanning EXAFS beamline (BL-9) of Indus-2, RRCAT, Indore (INDIA). The shift in the L-3 absorption edge in reference to Pb foil showed a linear relation with the partial charge present on the lead atom in lead compounds. The structural features of lead compounds have been explored using the wavelet transform of EXAFS spectra.

Hafnium compounds are fascinating due to their applications across diverse fields such as electronics, catalysis, nuclear energy, and biomedical materials. The study of chemical effects in hafnium compounds is necessary to check their purity and tailor their properties to meet the specific application requirements. The x-ray intensity ratios, I Lk /I L alpha (k = l, beta, gamma 1,5, gamma 2,3, gamma 4), for 72Hf foil and its different compounds have been measured by tuning the synchrotron radiation energies across its L i (i = 1-3) absorption-edge energies in order to investigate the influence of chemical effects on these intensity ratios in the presence of the many-body effects. The present measured intensity ratios (I Lk /I L alpha ) have been compared with two sets of values calculated using the nonrelativistic Hartree-Fock-Slater model-based L i (i = 1-3) subshell photoionization cross sections, the Dirac-Fock model-based x-ray emission rates, and two sets of the fluorescence and Coster-Kronig yields. The shift in L 3 absorption-edge of hafnium in its compounds has been deduced from the XANES spectra recorded in this study.

The study of space exploration has been studied for a very long time, and as technology has developed, so too have the methods and techniques employed, along with the quantity and type of data acquired. We now receive so much astronomical data, and so much brand new data is being generated every day, that it is physically impracticable to examine it all only by human work. In our study, we look at a number of astronomers face while working with this massive amount of data, and they use deep learning techniques to discover the best data for each objective. [1]previously SVM, KNN, the random forest approach, decision trees, and other multi-class classification algorithms are all used in the methodology. Galaxies' propensity to belong to specific classes is forecasted using regression. even if the findings from the random forest method were the best it was unable to effectively divide galaxies into the five groups. This approach does not explain real-time categorization and does not take outliers into consideration. The model's adaptability is constrained. This categorization scheme is unable to account for the modelling of galaxies as well as their evolution. Here, we suggest using Inception v3 for categorization and VGG-19 for image analysis. Segmentation is a method for discovering and classifying galaxies. These techniques greatly advance certain fields of study where there are enormous volumes of duplicate data that must be deleted in accordance with the demands of the study, thanks to Python's high performance in the investigation of image processing and computer vision.. As a result, there is less of a need for researchers to carefully sort through all of the data that has been collected from satellite telescopes, sky surveys, etc. [2]

The intensity ratios, (exp)(k=ξ, γ, m1; n=total, αβ), for some heavy elements, 70Yb, 79Au, 81Tl, 82Pb and 83Bi induced by 1000 keV –1750 keV Nq+ (q=4, 5) ions have been measured in order to investigate their dependence on the projectile energy and atomic number of the respective target elements. The measured intensity ratios have been compared with two sets of values calculated using the Mj (j=1–5) sub-shell ionization cross sections based on the ECPSSR-UA model, the X-ray emission rates based on the Dirac-Hartree Slater (DHS) model, two sets of the fluorescence and Coster-Kronig yields based on the DHS model and those evaluated by McGuire employing non-relativistic Hartree-Slater model. Significant differences have been observed between the present measured (exp) (k = ξ, γ, m1) intensity ratios and those calculated using independent particle approximation (IPA) models based single atomic vacancy state physical parameters.

In the present work, the Hf target was irradiated by tuning the energy (Ep) of synchrotron radiation across the Li (i=1-3) edge-energies ranging from 9.6keV to 14.0keV in order to measure the cross sections for production of the fluorescent Lk X-rays (k = l, α, η, β1,6, β3, β4, β2,15, β5,7, β9,10, γ1,5, γ2,3,6,8, γ4). These measurements were performed with the aim to check the validity of independent particle approximation (IPA) models at incident photon energies in proximity to the Li absorption edges of a heavy transition element. The measured cross sections were compared with three sets of values calculated using the X-ray emission rates based on the Dirac-Fock model, the Li (i = 1-3) sub-shell photoionization cross-sections based on the non-relativistic Hartree-Fock-Slater model and three sets of the fluorescence (ωi) and Coster-Kronig (fji) yields.

We have measured the X‐ray production cross sections (XRPCS) for the Lp (p = l, α, η, β1,3,4,6, β2,15, γ1,5, γ2,3,4) emission lines of Sn and Sb using synchrotron induced mono‐chromatic radiation tuned across their respective Li (i = 1–3) sub‐shell absorption edges covering the range 4.0 keV–5.0 keV. These measured XRPCS have been compared with the corresponding values calculated using the non‐relativistic Hartree‐Fock‐Slater model based Li (i = 1–3) photoionization cross‐sections, the Dirac‐Fock model based X‐ray emission rates and three sets of fluorescence and Coster‐Kronig (CK) yields based on the Dirac‐Hartree‐Slater model, the semi‐empirical values tabulated by Krause and recently reported experimental values. The present measured Lp XRPCS for both Sn and Sb at different investigated photon energies are found to be in good agreement with those calculated using the experimental photoionization cross sections, fluorescence and CK yields. Further, a good agreement observed between the present measured and calculated branching ratios for both Sn and Sb indicates the reliability of the Dirac‐Fock model based X‐ray emission rates. The Lp XRPCS and intensity ratios for Sn and Sb calculated using the experimental photoionization cross sections, the DF model based X‐ray emission rates and the experimental fluorescence and CK yields are recommended for use in different applications.

The synchrotron radiation induced Lk (k = l, *, alpha, beta 1,3,4,6, beta 2,15,9,10, gamma 1,5, gamma 2,3,4) X-ray production cross-sections (XRPCS) have been measured for Sn and Sb at energies ranging 6-14 keV. These present measured Lk XRPCS have been compared with different sets of theoretical cross sections calculated using the Dirac-Fock (DF) model based X-ray emission rates, the non-relativistic Hartree-Fock-Slater (HFS) model based photoionization crosssections and three sets of fluorescence and Coster-Kronig (CK) yields based on the Dirac-Hartree-Slater (DHS) model, the semi-empirical values tabulated by Krause, and the recently reported experimental values. The present measured Lk XRP cross sections for Sn and Sb are found to differ by up to 25% from different sets of presently calculated values. Further, the average L-shell fluorescence yields (omega L) have been deduced from the present measured total L XRPCS using the theoretical photoionization cross sections and are compared with the values available in literature.

The Ll/Lα, Lβ/Lα and Lγ/Lα intensity ratios have been measured for 51Sb at different incident photon energies across its Li(i=1-3) sub-shell absorption edge energies using synchrotron radiation as photon source. These experimental values have been compared with the two different sets of intensity ratios calculated using the photoionization cross sections based on the relativistic Hartree-Fock-Slater model, the X-ray emission rates based on the Dirac-Fock model and two sets of the fluorescence and Coster Kronig yields based on the DHS model and the semi-empirical values tabulated by Krause.

In the present work, we have deduced the fluorescence ( ω 1 , ω 2 , ω 3 ) and Coster–Kronig (CK)( f 12 , f 13 , f 23 ) yields for Sn ( Z = 50) and Sb ( Z = 51) from the L i ( i = 1–3) sub-shell x-ray intensities measured using the energy tunable synchrotron radiation employing the selective photoionization method. For both the elements, yields have been obtained using two sets of theoretical photoionization cross sections based on the non-relativistic Hartree–Fock–Slater (HFS) model and the self-consistent Dirac–Hartree–Fock (DHF) model. In case of Sb, we have obtained a third set of measured yields also by using the experimental photoionization cross sections evaluated from independent measurements of the mass-attenuation coefficients. The experimental yields for Sb are reported for the first time by us. We have compared the present deduced fluorescence and CK yields with the Dirac–Hartree–Slater model based values, the semi-empirical values tabulated by Krause and the earlier reported values. In case of Sn, using the DHF and the HFS model based photoionization cross sections, two sets of present measured L 1 sub-shell fluorescence yields ( ω 1 ) are found to be 0.039 ± 0.007 and 0.036 ± 0.003, and the CK yields ( f 13 ) are found to be 0.428 ± 0.107 and 0.405 ± 0.028, respectively. In case of Sb, using three sets of the photoionization cross sections (DHF, HFS and recent experimental values), the ω 1 values are measured to be 0.042 ± 0.007, 0.040 ± 0.004 and 0.047 ± 0.005, and the CK yields are measured to be 0.343 ± 0.085, 0.297 ± 0.021 and 0.247 ± 0.022, respectively. The comparison of these present measured yields with the theoretical values provided a reliable experimental evidence indicating cut-off of the intense L 1 –L 3 M 4,5 CK transitions at Z = 50.

In the present work, the L-k (k = l, alpha, eta, beta(1), beta(3), beta(6), beta(4), beta(2,15), beta(5,7), beta(9,10), gamma(1,5), gamma(2,3,6,8), gamma(4)) x ray production (XRP) cross sections have been measured for Re at energies across its L-i (i = 1-3) sub-shell ionization threshold energies covering the region 10.5 keV-14.0 keV using synchrotron radiation. The measured values have been compared with the three sets of XRP cross sections calculated using the Dirac-Fock model based x ray emission rates, the non-relativistic Hartree-Fock-Slater model based L-i (i = 1-3) sub-shell photoionization cross-sections and three sets of the fluorescence (omega(i)) and Coster-Kronig (f(ij)) yields based on the Dirac-Hartree-Slater model based values, the semi-empirical values and the experimental values reported earlier by us. The present measured XRP cross sections are found to be in a good agreement with those calculated using the experimental omega(i)/f(ij) values; whereas these are found to be significantly lower (similar to 30%) than those calculated using the theoretical and the semiempirical omega(i)/f(ij) values. In view of the observed good agreement of the present measured Lk XRP cross sections with those calculated using the experimental fluorescence and Coster-Kronig yields and that of the measured branching ratios (I-Ll/I-L alpha,; I-L beta 2,I-15/I-L alpha,; I-L eta/I-L beta 1; I-L gamma 1,I-5/I-L beta 1 and I-L gamma 2,I-3/I-L beta 3) with the theoretical values calculated using the Dirac-Fock model based x ray emission rates, the use of these parameters is recommended for different analytical applications.

L shell fluorescence and Coster–Kronig yields for W and Re were deduced from synchrotron radiation induced X-ray line intensities measured at different incident energies across the Li absorption edge energies of both elements based on HFS and DHF models.

The L x-ray intensity ratios, ILk/ILα (k = l, β, γ), for 75Re have been measured at some incident photon energies across its Li (i = 1-3) sub-shell absorption edge energies using synchrotron radiation. The present measured intensity ratios have been compared with two sets of values calculated using the Hartree-Fock-Slater model based photoionization cross-sections, the Dirac-Fock model based X-ray emission rates and two sets of fluorescence and Coster-Kronig yields based on the semi-empirical and the DHSmodels.

The cross sections for production of the Mk (k = ξ, δ, α, β, ζ, γ, m1, m2) X-rays induced by 0.06 - 2 MeV protons have been calculated for 71Lu and 80Hg using the Mi (i=1-5) sub-shell X-ray emission rates based on the Dirac-Hartree- Slater (DHS) model, the fluorescence and Coster-Kronig yields based on the DHS model and two sets of proton ionization cross sections based on the DHS model and the ECPSSR model. The two sets of calculated cross sections have been compared with each other in order to assess the influence of the wave function on the XRP cross sections. The calculated cross sections have been compared with the measured cross sections reported in the recent compilation to check the reliability of the calculated values.

In the present work, the X-ray mass attenuation coefficients have been measured for Sb-51 (a medium-Z element) at forty energies across its L-i (i = 1-3) sub-shell absorption edges covering an extended energy region within 4.0 keV-14.0 keV. The aim of this study is to experimentally determine the key X-ray fundamental parameters for Sb-51 with improved accuracy by using tunable energy synchrotron radiation. From the present measured mass attenuation coefficients, the L-i (i = 1-3) sub-shell photoionization cross sections (sigma(P)(Li)) have been deduced at twenty four energies across the L-i (i = 1-3) edge-energies of Sb-51 covering the region 4.150 keV-5.0 keV by using experimentally deduced L-i (i = 1-3) edge jump ratios. Two theoretical datasets of X-ray mass attenuation coefficients and total photoionization cross sections were served to evaluate their consistency with the present experimental values and reveal possible discrepancies, in particular, across the L-i (i = 1-3) edge-energies of Sb-51.

In the present work, the X‐ray intensity ratios, ILk/ILα (k = l, β, γ1,5, γ2,3, γ4), have been measured for different compounds of 66Dy, namely, Dy2O3, Dy2(CO3)3, Dy2(SO4)3.8H2O, DyI2, and the 66Dy metallic foil by tuning the incident photon energies across its Li (i = 1–3) absorption‐edge energies covering the region 7.8–10 keV in order to investigate the influence of chemical effects on these intensity ratios in the presence of the many‐body effects, which become significant at photon energies in proximity to the Li absorption‐edge energies. The present measured intensity ratios ILk/ILα have been compared with two sets of values calculated using the nonrelativistic Hartree–Fock–Slater model‐based Li (i = 1–3) subshell photoionization cross sections, the Dirac–Fock model‐based X‐ray emission rates, and two sets of the fluorescence and Coster–Kronig yields. The L3 absorption‐edge energy of 66Dy in its different compounds and metallic foil has been deduced from the XANES spectra recorded in the present work. The L3 absorption‐edge energy shifts obtained from these absorption‐edge energies are found to increase linearly with the partial charge on the metal atom (66Dy).

In the present work, the intensity ratios, I-Mk/I-Mn (exp) (k = xi, beta, gamma, m(1); n = alpha beta, alpha), for Yb-70, Pb-82 and( 83)Bi induced by the Cq+ (q = 4, 5) ions having energies in the range 800-1500 keV have been measured. These intensity ratios have been compared with those calculated using the ECPSSR model based carbon ion induced M-j (j = 1-5) sub-shell ionization cross sections, the X-ray emission rates based on the Dirac-Fock (DF) model, two sets of the fluorescence and Coster-Kronig yields based on the non-relativistic Hermann-Skillman potential calculations and those based on the relativistic Dirac-Hartree-Slater model. Significant differences observed between the present measured and calculated ratios could be due to multiple-ionization induced in the investigated elements by the incident carbon ions.

The X‐ray production (XRP) cross sections for the 66Dy Lk (k = l, α, η, β2,6,7,15, β1,6, β1,3,4,6, β2,7,15, γ1,5, γ2,3) emission lines have been measured by tuning the incident synchrotron radiation at energies over the range 7.8–9.2 keV and ~10–370 eV above the respective Li (i = 1–3) absorption edges. These measurements aim to check the reliability of the independent particle approximation models used to generate the theoretical data sets of different physical parameters required to calculate the XRP cross sections and also investigate the influence of many body effects on the photoionization process. The measured values have been compared with 4 sets of XRP cross sections calculated using the Dirac–Fock model‐based X‐ray emission rates, 2 sets of the Li (i = 1–3) subshell photoionization cross sections deduced from the self‐consistent Dirac–Hartree–Fock model‐based values and the nonrelativistic Hartree–Fock–Slater model‐based values, and 2 sets of the fluorescence (ωi) and Coster–Kronig (fij) yields. The present measured Lγ2,3 (originating from decay of the L1 subshell vacancies) XRP cross sections are found to be significantly higher than different sets of theoretical values, whereas a good agreement is generally observed for the various other XRP cross sections and relative intensities.

The total M shell and the Mk (k = ξ, αβ, γ, m) X‐ray production cross sections for 66Dy have been measured at incident photon energies across its Lj (j = 1–3) subshell absorption edge energies, ranging 7.8–9.2 keV. This study aims to investigate the evolution of the probability for cascade decay of Lj subshell vacancies as the tunable incident energy ionizes progressively different 66Dy Lj subshells. The experimental X‐ray production cross sections have been compared with theoretical ones calculated using the nonrelativistic Hartree–Fock–Slater (HFS) model‐based photoionization cross sections; three sets of the X‐ray emission rates, fluorescence and Coster–Kronig yield based on the nonrelativistic Hartree–Slater (NRHS) model, Dirac–Hartree–Slater (DHS) model and Dirac–Fock (DF) model; the Lj (j = 1–3) subshell to the Mi (i = 1–5) subshell vacancy transfer probabilities evaluated in the present work. Presently measured total M shell and the Mαβ X‐ray production cross sections are found to be significantly lower than the theoretical ones evaluated using physical parameters based on the relativistic Dirac–Fock/Dirac–Hartree–Slater model calculations, whereas a much better agreement is observed with respect to the NRHS model‐based calculations; however, the measured X‐ray production cross sections are still systematically lower than the NRHS values.