Line Width Research Articles

Pearls on a String: Dark and Bright Galaxies on a Strikingly Straight and Narrow Filament

Abstract We identify a chain of galaxies along an almost straight line in the nearby Universe with a projected length of ~5 Mpc. The galaxies are distributed within projected distances of only 7–105 kpc from the axis of the identified filament. They have redshifts in a very small range of z = 0.0361−0.0370 so that their radial velocities are consistent with galaxy proper motions. The filament galaxies are mainly star forming and have stellar masses in a range of 109.1−1010.7 M ⊙. We search for systems with similar geometrical properties in the full-sky mock galaxy catalog of the MillenniumTNG simulations and find that, although such straight filaments are unusual and rare, they are predicted by ΛCDM simulations (4% incidence). We study the cold H i gas in a 1.3 Mpc section of the filament through H i 21 cm emission line observations and detect 11 H i sources, many more than expected from the H i mass function in a similar volume. They have H i masses 108.5−109.5 M ⊙ and are mostly within ~120 kpc projected distance from the filament axis. None of these H i sources has a confirmed optical counterpart. Their darkness together with their large H i 21 cm line widths indicates that they contain gas that might not yet be virialized. These clouds must be marking the peaks of the dark matter and H i distributions over large scales within the filament. The presence of such gas clouds around the filament spines is predicted by simulations, but this is the first time that the existence of such clouds in a filament is observationally confirmed.

Ultranarrowband Chiral Absorbers in the Visible Region Based on Brillouin Zone Folding Metasurfaces.

Chiral perfect absorbers that enable the handedness-dependent near-unity absorption of circularly polarized light are highly desirable for enhancing various chiral interactions. However, the experimental realization of ultranarrowband absorbers with extreme chiral responses remains challenging. Here, we realize such chiral absorbers by incorporating Brillouin zone folding and mirror symmetry breaking in the design of planar dielectric metasurface. When the metasurface is backed by a reflection mirror, strong chiral absorption with ultranarrow line width can be achieved in the normal direction. We experimentally achieve a substantial differential absorptance of 0.75 with an ultranarrow line width of 1.4 nm in the visible region. Furthermore, by leveraging handedness-dependent strong field enhancement, high levels of chiral emission with a luminescence line width of 1.75 nm are demonstrated from quantum dots coated on the absorber surface. Our findings may unlock interesting opportunities in chiral photodetectors, optical filters, nonlinear optics, light sources, and quantum photonic devices.

Surface brightness-colour relations of dwarf stars from detached eclipsing binaries

Aims. Surface brightness-colour relations (SBCRs) are useful tools for predicting the angular diameters of stars. They offer the possibility to calculate precise spectrophotometric distances based on the eclipsing binary method or the Baade–Wesselink method. Double-lined detached eclipsing binary stars (SB2 DEBs), with precisely known trigonometric parallaxes, allow us to calibrate SBCRs with a high level of precision. To improve such calibrations, it is important to supplement the sample of suitable eclipsing binaries with precisely determined physical parameters. Methods. We selected ten SB2 DEBs within 0.8 kpc of the Sun, which feature components of spectral types ranging from B9 to K3. We analysed their TESS and Kepler K2 space-based photometry simultaneously with the radial velocities derived from HARPS spectra using the Wilson–Devinney code. The disentangled spectra of DEBs were used to derive atmospheric parameters of their components by applying the GSSP code. The direct effective temperatures were also calculated using spectral energy distribution analysis. The O–C diagrams of the minima times were investigated to detect long-term period changes or apsidal motions. Results. Most of the systems are composed of significantly unequal components, with mass ratios as low as ~0.5. We derived precise masses, radii, and surface temperatures for them, along with their metallicities. The average precision of mass and radii determinations is 0.3% and 1.4%, respectively, for the surface temperature. The spectroscopic and photometric temperatures of the components are usually consistent to within 100 K, but in some systems, the difference is much larger. The components of HD 149946 show the highest difference (up to 400 K), while the atmospheric models favour different surface metallicities. We also provide an updated calibration of the equivalent width of the interstellar sodium D1 line and the reddening E(B–V).

Influence of annealing on the thermal quenching of photoluminescence in GaAsBi/GaAs quantum dots with bimodal inhomogeneous broadening

GaAsBi/GaAs quantum dots (QDs) samples with a bimodal size distribution grown by atmospheric pressure metalorganic vapor phase epitaxy (AP-MOVPE) on p-GaAs substrates and annealed at different temperatures were investigated by photoluminescence (PL) measurements. The analyses of the Arrhenius fit of the integrated PL intensity show two types of non-radiative recombination processes, describing the strong thermal quenching of PL. The thermal quenching of the as-grown sample is clearly quicker compared to the annealed QD samples. It is attributed to a higher density of non-radiative Bi complexes and native defects related to GaAs host lattice. The activation energy value for the large QD increases in the annealed samples suggests a modification in the depth of the confining potential. The temperature dependence of the PL peak energy of small QD presents an S-shape variation, while the PL line width follows a non-monotonic form. These behaviors have been progressively reduced in the annealed samples. These experimental results have been interpreted in the context of the thermally activated carrier transfer process between different QDs. Thus, annealing reduces the localized state density and therefore improves the optical quality of GaAsBi/GaAs QDs.

Impact of infill pattern and line width on tensile strength of PLA FDM 3d printing

Mechanical properties of Fused Deposition Modelling (FDM) 3D-printed products are a top priority in prosthesis manufacturing. Damage to 3D-printed products is often caused by the low mechanical strength when subjected to loading. Many parameters can influence the strength of the printed product during the process, including the infill pattern and line width. The infill pattern and line width serve as benchmarks for product quality, making it important to understand the impact of printing parameters to achieve optimal product strength. This study aims to analyze the mechanical properties of 3D-printed products through tensile testing with variations in infill pattern and line width. The method used to determine the mechanical properties is tensile testing. The tensile test samples were made using a Creality Ender 3 Pro 3D printer. The printing parameters were varied with three patterns: cubic, line, and triangle, as well as two infill line widths: 0.4 mm and 0.5 mm. The tensile test results showed significant differences in the variations of infill pattern and line width. The highest tensile strength was obtained with the line pattern and 0.5 mm line width, with an average tensile strength of 28.85 MPa, while the lowest value was observed with the cubic pattern and 0.4 mm line width, with an average of 27.63 MPa. These findings can serve as a valuable reference in the printing of prosthetic products using FDM 3D printing

Green Synthesis of Luminous Indium Phosphide Nanocrystals.

Indium phosphide (InP) nanocrystals (NCs) have garnered significant attention for displays and bioimaging due to their superior optical properties and low toxicity. However, the high cost and operational risks associated with the colloidal synthesis of InP NCs hinder their widespread development and application. In this study, we presented a green synthesis method for InP NCs using solid ammonium hypophosphite ((NH4)H2PO2) as an economical and safe phosphorus precursor. (NH4)H2PO2 was decomposed controllably to produce highly reactive gaseous phosphine (PH3) through precise temperature management. The released PH3 then reacted with indium carboxylate to form InP clusters, which serve as intermediate precursors. This cluster-assisted method endowed a continuous supply of monomers for the nucleation and growth of high-quality InP NCs with uniform size distribution. Following a surface treatment that balances etching and passivating capabilities, the InP NCs exhibited a narrow emission line width of 46 nm and a near-unity photoluminescence quantum yield (PLQY), representing one of the best emission performances for shell-less InP NCs. The economical and stable nature of the raw materials used in this approach opens a pathway for the green synthesis of InP NCs.

Searching for signatures of Fe II atomic processes in spectra of active galactic nuclei

We use a large sample of Type 1 active galactic nuclei (AGNs) spectra in order to investigate which atomic processes are responsible for some observed properties of the Fe II emission lines and how they are connected with macroscopic physical characteristics of AGN emission regions. We especially focus on the violated relative intensities between different optical Fe II lines, whose relative strengths do not follow the expected values according to atomic parameters. We investigated the connection between this effect and the ratio of optical to UV Fe II lines (Fe II_opt/Fe II_UV). We divided the optical Fe II lines into two large line groups: consistent (Fe II_cons), whose relative intensities are in accordance with their atomic properties, and inconsistent (Fe II_incons), whose relative intensities are significantly stronger than theoretically expected. We fitted the spectra with a flexible and complex optical Fe II model, where both consistent and inconsistent Fe II lines were divided into several line groups according to their atomic characteristics and fitted independently in order to obtain more empirical clues about their properties. We focused particularly on understanding the processes that produce strong inconsistent Fe II lines, and therefore, we investigated their correlations with Fe II_cons as well as with UV Fe II lines and some measured spectral parameters. The ratios of Fe II_incons/Fe II_cons and Fe II_opt/Fe II_UV increase as the Eddington ratio increases and as the line widths decrease. It is possible that both ratios are affected by the process of self-absorption of stronger lines, which is responsible for the transmission of energy from the UV to the optical Fe II emission lines and, analogously, from the Fe II_cons to the Fe II_incons lines. In this scenario, the high Eddington ratio causes an increase in the optical depth in Fe II lines, which results in the triggering of the process of self-absorption. Measured average widths for different Fe II line groups indicate the stratification of the optical Fe II emission region. This implies that the observed Fe II spectrum is probably a complex mixture of radiation from emission regions with different physical conditions and distances from the black hole.

A candidate quadruple AGN system at z∼3

Multiple galaxies hosting active galactic nuclei (AGNs) at kiloparsec separations from each other are exceedingly rare, and in fact, only one quadruple AGN is known so far. These extreme densities of AGNs are expected to pinpoint protocluster environments and therefore should be surrounded by large galaxy overdensities. In this letter, we present another quadruple AGN candidate at z ∼ 3 including two SDSS quasars at a separation of roughly 480 kpc. The brighter quasar is accompanied by two AGN candidates (a type 1 AGN and a likely type 2 quasar) at a close (∼ 20 kpc) separation identified through emission line ratios, line widths, and high ionization lines, such as The extended Lyα emission associated with the close triple system is more modest in extent and brightness compared to similar multiple AGN systems and could be caused by ram-pressure stripping of the type 2 quasar host during infall into the central dark matter halo. The predicted evolution of the system into a z=0 galaxy cluster with the AGN host galaxies forming the brightest cluster galaxy needs to be further tested by galaxy overdensity studies on large scales around the quadruple AGN candidate. If confirmed as a quadruple AGN with X-ray observations or rest-frame optical line ratios, this system would represent a second AGN quartet and be the highest-redshift multiplet and the closest high-redshift triplet known.

Observations of UX Ori in deep minima with the Nordic Optical Telescope. I. Analysis of spectral lines

UX Orionis stars are the most active young stars; they undergo sporadic fadings of 2 to 4 magnitudes in the V-band, due to variable circumstellar extinction caused by a nearly edge-on star--disc system. The long-lasting monitoring of a number of stars of this type with the Nordic Optical Telescope from 2019 to 2024 has given a rich collection of material of high-resolution (R ∼ 25000) spectra obtained during different brightness states of the stars. In this paper we present the results of observations for UX Ori itself. Until now only one spectrum of high resolution had been obtained for this star during brightness minimum, making it difficult to do a comprehensive analysis. Our aim is to analyse how different spectral lines change during such irregular fading events, when the star is going in and out of eclipses, obscured by dust along the line of sight. For this purpose we provide a comparative analysis of the profiles and equivalent widths of the spectral lines belonging to the different atoms and ions. In addition we compare the results for UX Ori with those made for another target in our sample: RR Tau. Common features of variability are revealed: (1) a strengthening of the Hα line relatively to the continuum during eclipses; (2) the appearance of additional emission on the frequencies of photospheric lines (e.g. FeII, CaII, SiII). The different behaviour of the spectral lines during fading found for UX Ori and RR Tau may be caused by two effects: a different contribution of the scattered light to the stellar flux during eclipses or a less intense disc wind of UX Ori.

Evaluation of Mesoporous Silica Nanoparticles as Carriers of Triarylmethyl Radical Spin Probes for EPR Oximetry.

In vivo measurement and mapping of oxygen levels within the tissues are crucial in understanding the physiopathological processes of numerous diseases, such as cancer, diabetes, or peripheral vascular diseases. Electron paramagnetic resonance (EPR) associated with biocompatible exogenous spin probes, such as Ox071 triarylmethyl (TAM) radical, is becoming the new gold standard for oxygen mapping in preclinical settings. However, these probes do not show tissue selectivity when injected systemically, and they are not cell permeable, reporting oxygen from the extracellular compartment only. Recently, Ox071-loaded mesoporous silica nanoparticles (MSNs) were proposed for intracellular tumor oxygen mapping in both in vitro and in vivo models. However, the EPR spectrum of the Ox071 spin probe is poorly sensitive to mobility due to the small anisotropy of its g-factor and the absence of hyperfine splitting, making it more difficult to study the mobility of the radical inside the MSNs or its location. Using 13C1 isotopologues of Ox071 and the deuterated Finland trityl (dFT) spin probes, which are highly sensitive to molecular tumbling, we showed that the loading of the probes inside homemade and commercial cationic MSNs drastically decreases their mobility while the high local concentration of the probe inside the MSNs leads to dipolar line width broadening (self-relaxation). This decrease in molecular tumbling and line broadening hampers the oxygen-sensing properties of Ox071 or dFT probes used for EPR oximetry when loaded into MSNs.

Global and Local Infall in the ASHES Sample (GLASHES). I. Pilot Study in G337.541

Abstract Recent high-angular-resolution observations indicate the need for core growth to form high-mass stars. To understand the gas dynamics at the core scale in the very early evolutionary stages before being severely affected by feedback, we have conducted Atacama Large Millimeter/submillimeter Array (ALMA) observations toward a 70 μm dark massive clump, G337.541-00.082 as part of the Global and Local infall in the ASHES sample (GLASHES) program. Using dense gas tracers such as N2H+ (J = 1–0) and HNC (J = 3–2), we find signs of infall from the position–velocity diagram and more directly from the blue asymmetry profile in addition to the clump-scale velocity gradient. We estimate infall velocities from intermediate and low-mass cores to be 0.28–1.45 km s−1, and infall rates to be on the order of 10−4–10−3 M ⊙ yr−1, both are higher than those measured in low-mass star-forming regions by more than a factor of 5 and an order of magnitude, respectively. We find a strong correlation between the infall velocity with the nonthermal velocity dispersion, suggesting that infall may contribute significantly to the observed line width. Consistent with clump-fed scenarios, we show that the mass infall rate is larger for larger core masses and shorter distances to the clump center. Such high infall rates in cores embedded in IRDCs can be considered as strong signs of core growth, allowing high-mass star formation from intermediate-mass cores that would not initially form high-mass stars at their current mass.

Data on Stark Broadening of Sn II Spectral Lines

Data on spectral line widths and shifts broadened by interactions with charged particles, for 44 lines in the spectrum of ionized tin, for collisions with electrons and H II and HeII ions, are presented as online available tables. We obtained them by employing the semiclassical perturbation theory for temperatures, T, within the 5000–100,000 K range, and for a grid of perturber densities from 1014 cm−3 to 1020 cm−3. The presented Stark broadening data are of interest for the analysis and synthesis of ionized tin lines in the spectra of hot and dense stars, such as, for example, for white dwarfs and hot subwarfs, and for the modelling of their atmospheres. They are also useful for the diagnostics of laser-induced plasmas for high-order harmonics generation in ablated materials.

Single Rare-Earth Ion Doped Tin-Oxo Nanocluster Photoresists for High-Resolution Extreme Ultraviolet Lithography.

Rare-earth (RE) metals are known as industrial vitamins and show significant regulatory effects in many fields. In this work, we first demonstrated that the vitamin effect of RE metals can also be applied to extreme ultraviolet (EUV) lithography. Using a Sn8RE oxo cluster as the universal platform, different individual RE metal ions were successfully doped to obtain a series of isomorphic heterometallic clusters (RE = Y, Sm, Eu, Ho, Er). Lithography experiments have shown that the doped RE ions displayed a significant influence on technical parameters. As a result, an electron-beam lithography (EBL) line width of 11.95 nm was achieved by Sn8Er, and an EUV lithography critical dimension (CD) of 15.90 nm was obtained by Sn8Ho under an exposure dose of 52.64 mJ/cm2. These findings expand the applications of rare earths in high-precision semiconductor manufacturing and provide a new strategy for the development of high-resolution EUV photoresists.

A Set of Three GdIII Spin Labels with Methanethiosulfonyl Groups for Bioconjugation Covering a Wide Range of EPR Line Widths.

Spin labels based on GdIII complexes are important tools for the elucidation of the structure, dynamics and interaction of biomolecules by electron paramagnetic resonance (EPR) spectroscopy. Their EPR spectroscopic properties line width and relaxation times influence their performance in a particular application. To be able to apply a complex well-suited for a specific application, a set of GdIII complexes with different EPR spectroscopic properties ready-made for spin labeling will be highly useful. We prepared three GdIII complexes with DO3APic, NO3Pic, and PyMTA as the basic ligand units. They cover a wide range of EPR line widths but have in common a cysteine-targeting methanethiosulfonyl (MTS) group connected to a pyridine ring, which is an intrinsic part of the ligand. The reaction with a cysteine-containing pentapeptide (0.45 mM in the peptide, pH ∼ 7) was complete within 90 s and chemoselective. The MTS group hydrolyzed with half-lives of >24, 8, 2, and 1 h at pH 5, 6, 7, and 8, respectively. The structurally related nicotinic acid-substituted disulfide (NDS) group was found to be hydrolytically much more stable. However, the MTS spin label clearly won the competition for the pentapeptide over the NDS spin label. If high reactivity is essential, MTS is clearly the better choice.

NMR Spectral Editing, Water Suppression, and Dipolar Decoupling in Low-Field NMR Spectroscopy Using Optimal Control Pulses and Multiple-Pulse Sequence.

Spectral dispersion in low-field nuclear magnetic resonance (NMR) can significantly affect NMR spectral analysis, particularly when studying complex mixtures like metabolic profiling of biological samples. To address signal superposition in these spectra, we employed spectral editing with selective excitation pulses, proving it to be a suitable approach. Optimal control pulses were implemented in low-field NMR and demonstrated their capability to selectively excite and eliminate specific amino acids, such as phenylalanine and taurine, either individually or simultaneously. The broadening of NMR signals in viscous samples, like bio samples, due to homonuclear dipolar coupling often leads to loss of spectral details, impacting spectral assignments. Therefore, in this work, the multiple-pulse WAHUHA sequence at both high and low field NMR was employed resulting in approximately 63 and 25% reduction in line widths respectively, evident from line width changes in the NMR spectra. The effectiveness of this process was validated by comparing its performance with that of magic angle spinning NMR. Additionally, water suppression was achieved through selective excitation by adding a term representing the water signal to the overall Hamiltonian, expressing the water signal peak frequency, and covering adjacent frequencies on both sides of the water peak within the water signal.

RF Heating Effects in CEST NMR with Hyperpolarized 129Xe Considering Different Spin Exchange Kinetics and Saturation Schemes.

Chemical exchange saturation transfer (CEST) improves the sensitivity of NMRbut depending on the spin exchange kinetics, it can require substantial RF energy deposition to label magnetization. Potential side effects like RF-induced heating may occur and must be monitored. Here, we explore the parameter space considering not only undesired heating but efficient CEST build-up (depolarization rate), spectral resolution (line width), and subsequent effects like changes in chemical shifts of CEST responses must be considered, too. We present a systematic study to compare conventional block pulse with shaped-pulse saturation and quantify how the effective average saturation power impacts these parameters. Pulse shape and nominal excitation bandwidth, however, turned out to have little impact on acquired z-spectra and temperature changes. This study illustrates how different exchange kinetics define different regimes of suitable RF power within the dynamic range of fully saturable magnetization from hyperpolarized 129Xe. Temperature-related changes in the resonance frequency of bound spins were also quantified for the two Xe hosts CB6 and CrA-ma and put into context for typically used CEST acquisition parameters, including the stability of the magnetic field.

Radial-dependent Responsivity of Broad-line Regions in Active Galactic Nuclei: Observational Consequences for Reverberation Mapping and Black Hole Mass Measurements

Abstract The reverberation mapping (RM) technique has seen wide applications in probing geometry and kinematics of broad-line regions (BLRs) and measuring masses of supermassive black holes (SMBHs) in active galactic nuclei. However, key quantities in RM analysis such as emissivity, responsivity, transfer functions, and mean and rms spectra are fragmentally defined in the literature and largely lack a unified formulation. Here we establish a rigorous framework for BLR RM and include a locally dependent responsivity according to photoionization calculations. The mean and rms spectra are analytically expressed with emissivity- and responsivity-weighted transfer functions, respectively. We demonstrate that the rms spectrum is proportional to the responsivity-weighted transfer function only when the continuum variation timescale is much longer than the typical extension in time delay of the BLR; otherwise, biases arise in the obtained rms line widths. The long-standing phenomenon pertaining to the different shapes between the mean and rms spectra can be explained by a radial-increasing responsivity of BLRs. The debate on the choice of emission-line widths for SMBH mass measurements is explored, and the virial factors are suggested to also depend on the luminosity states, in addition to the geometry and kinematics of BLRs.

Multi-scale analysis of the Monoceros OB 1 star-forming region. III. Tracing the dense gas in the massive clump G202.3+2.5

Young massive clumps are relatively rare objects and are typically found at large distances. The G202.02+2.85 (hereafter, G202) massive clump was identified in the Monoceros OB 1 molecular complex at a distance of about 700 pc. It was found to be undergoing active star formation and located at the junction point between two colliding filaments. We aim to further clarify the evolutionary stage of the clump and the nature of the collision and of six dense cores in the area; specifically, we investigate whether the clump is collapsing as a whole and/or whether it shows signs of shocks. To this end, we examined the dense gas properties, notably through NH_3 and mathrm N_ H^ and their deuterated counterparts. We examined the evolutionary stages of the cores through deuterium fractionation values. We performed a mapping of the clump and deeper pointed molecular line observations towards the dense cores with the IRAM 30-m and Effelsberg 100-m telescopes in the 3-mm and centimetre ranges, respectively. The clump internal dynamics was examined using tracers of various gas densities (CO isotopologues, CS, ammonia, and diazenylium), along with a classical infall diagnosis with HCO^+ and diazenylium. Furthermore, SiO and methanol were used to characterise the shock properties. The evolutionary stages of the dense cores were evaluated from the deuterium fractionation of ammonia and diazenylium. The clump seen in dust continuum emission was detected in all dense-gas molecular tracers, including deuterated ammonia and diazenylium, contrasting with the distributions in shock tracers SiO and CH_3OH. These latter include both features compatible with protostellar outflows and a more diffuse emission in the clump, all with SiO line width corresponding to relatively low velocity shocks (lesssim 10 ). This could arise from multiple, blended outflows or be a signature of the filament collision. All the dense cores, except for the source 1446, were found to be in early evolutionary stages, the most massive one, the source 1450, being at most a Class 0 object. This is consistent with the idea that they originate in the same clump-compression event. They all present virial parameters indicating gravitational instability, while source 1450 and its surroundings show blue-shift asymmetry in HCO^+ compatible with gravitational infall, suggesting that this star formation activity came out of the collision. We find that, in contrast to NH_3 deuterium fractionation, the N_2H^+ deuterium fractionation values are likely to be correlated with the source evolutionary stage. Our results provide additional evidence that the star-forming cores in the G202 clump originate in the clump compression due to filament collision or convergence. Based on its physical parameters, we find that the source 1454 in the northern clump of G202 may represent the physical state of the region before the collision of the two filaments that make up the junction region. Determining the origin of the collision will require the examination of the large-scale motion of the gas.

OPTO: Automated Optimization for Solid-State NMR Spectroscopy.

NMR spectroscopy presents boundless opportunities for understanding the structure, dynamics, and function for a broad range of scientific applications. Solid-state NMR (SSNMR), in particular, provides novel insights into biological and material systems that are not amenable to other approaches. However, a major bottleneck is the extent of user training and the difficulty of obtaining reproducible, high-quality experimental results, especially for the sophisticated multidimensional pulse sequences that are essential to provide site-resolved measurements in large biomolecules. Here, we present OPTO, a software operating environment that addresses these challenges and enhances the performance of many types of commonly utilized SSNMR experiments. OPTO is compatible with Varian OpenVnmrJ and Bruker Topspin, with a front-end graphical user interface that presents the instrument operator with access to powerful underlying optimization algorithms, including simplex and grid searches of the dozens of parameter settings required for optimal performance. Therefore, OPTO efficiently leverages instrument time and enables instrument operators to find optimal experimental conditions reliably. We demonstrate examples including improvements in (1) resolution, with an automated, global search of 21 shimming parameters to achieve a 12 parts per billion line width; (2) sensitivity, with searches and refinements of several cross-polarization conditions dependent on 16 parameters in triple resonance experiments; and (3) robustness, with results from protein samples on several spectrometers operating at different magnetic field strengths and magic-angle spinning rates.

Separation of Line Widths of HOD Peaks of Healthy and Diseased Blood and Urine Groups Using 400 MHz NMR

Separation of Line Widths of HOD Peaks of Healthy and Diseased Blood and Urine Groups Using 400 MHz NMR