Recurrent tidal disruption events (rTDEs) are sources that exhibit multiple TDE-like flares; many are likely powered by the recurring partial disruption of a bound star, in a repeating partial TDE (rpTDE). Two such sources, TDE 2022dbl (ASASSN-22ci) and TDE 2020vdq (ZTF20acaazkt), each exhibited two UV/optical flares and, under the assumption of periodicity, both were expected to exhibit a third flare in early 2026. Neither exhibited such a flare, to limits of L_UV/optical≲ 10^42 erg s^-1, ∼30× fainter than the previous flares. Here, we examine several possible explanations. Observing two independent TDEs from the same galaxy within ∼2 yr has a probability of ≲0.5

Early-time light curves of Type Ia Supernovae (SNe Ia) encode critical information about their progenitor systems. We characterize the rise of normal SNe Ia using a volume-complete sample of 972 events from the Zwicky Transient Facility Data Release 2, an order of magnitude larger than any previous dataset for similar analyses. Fitting light curves up to 30% of peak flux with a power-law model under a hierarchical Bayesian framework, we provide robust population-level constraints on the rise time (t_rise; μ=18.55±0.08 days, σ=1.42±0.07 days), rise index (α; μ=2.10±0.04, σ=0.48±0.03 in ZTF r), and g-r color evolution (α_g - α_r; μ=0.20±0.02, σ=0.17±0.02). These power-law fits are sensitive to the chosen truncation epoch if data beyond ∼40% of peak flux are included, but generally converge when restricted to earlier epochs. The relation between rise morphology and light-curve width ( x_1 stretch) bifurcates into two distinct regimes: high-stretch SNe Ia show clear trends where a higher x_1 correlates with shallower rises and more persistent blue colors, whereas low-stretch SNe Ia lack such trends. While rise times correlate positively with x_1 overall, this relation flattens significantly within the high-stretch population. Searching for anomalies, we identify several normal SNe Ia with unusually long rise times, which potentially exhibit short-duration (≲2 days) flux excesses over a smooth rise. Long-duration (∼5 days) flux excesses appear common within the high-stretch population and are tied to the shallow rises and early blue colors, pointing to widespread outward ^56Ni mixing. Multi-dimensional explosion models with more realistic progenitor setups are needed to fully reproduce the observed dichotomy in rise morphology and stretch.

We report the discovery and multi-wavelength analysis of a z∼0.7 transient PLATE-23a in the Abell 2744 field, as the first results of the Pandora Lensing, AGN, and Transient Exploration (PLATE) project. Using multi-epoch JWST NIRCam imaging spanning from 2022 to 2025, we detect PLATE-23a in 12 filters. Difference-imaging analysis reveals its rising and declining phases. The host galaxy of PLATE-23a is a barred spiral at z=0.688 with a stellar mass of ∼ 10^10.4M_⊙ and a star formation rate of ∼5.1M_⊙ yr^-1, placing it on the star-forming main sequence. Bayesian light-curve classification strongly favors a type IIP supernova (SN) origin. It lies ∼ 13 kpc (after lensing correction) from the galaxy center in a region of low local star formation, suggesting the progenitor may have migrated from a distant star-forming clump. Physical properties derived from blackbody modeling indicate a temperature decreasing from ∼8010 K to ∼6100 K at around 65 days after the explosion; the late-time SED is consistent with entering the radioactive decay phase at about one rest-frame year. This work demonstrates the power of deep, multi-epoch JWST observations for studying transients at cosmological distances.

Type Ia Supernovae (SNe Ia) are well known for their role as standardizable cosmological candles. Their uniformity is credited to their single origin as thermonuclear explosions of White dwarf (WD) stars. Nevertheless, some SNe Ia break this regularity. Prominently, the Iax subclass are less energetic and remarkably diverse, raising questions about their progenitor systems. While no progenitor system of a normal SN Ia has ever been detected, a luminous blue star was identified in pre-explosion images of the site of the bright SN Iax SN 2012Z, suggested to be a helium giant companion star acting as a mass donor to a WD SN progenitor. This is in line with models of weak mass accretion of a WD from a binary companion, producing an explosion that does not fully disrupt the star. However, these models fail to explain the properties of the faintest Type Iax explosions, suggesting either they originate from other WD binary systems, or even from massive progenitor stars. Here, we present the faint SN Iax SN 2024vjm - possibly the faintest supernova observed to date. Using a deep pre-explosion image taken by the recently launched Euclid space mission, we show that its progenitor system must be fainter than the helium giant SN Iax progenitor candidate of SN 2012Z, as well as that of the luminous red companion or remnant of the faint SN 2008ha, and may require a subdwarf helium star as a mass donor. The deep image also provides strong arguments against a massive star origin for this faint supernova. Our observations argue that SN 2024vjm is a WD explosion, but we find that remarkably faint SNe Iax fade more slowly than bright ones, i.e., they evolve in an opposite manner from the famous Phillips relation that makes regular SNe Ia cosmological candles.

We present optical and near-infrared (NIR) observations of the fast-declining Type Ia supernova (SN Ia) 2022an. The photometric and spectroscopic properties identify it as a standard 91bg-like event; however, our data reveal a relatively narrow absorption feature with a full width at half-maximum (FWHM) of 75 & Aring; near 1.037 mu m in the rest frame of the observed spectra that persists from around 30 days to nearly 90 days after maximum light. We attribute this feature to the He i 1.083 mu m line with a blueshifted velocity of 1.3 & times; 104 km s-1 and a FWHM of 2.1 & times; 103 km s-1, supported by the detection of multiple optical He i transitions at earlier epochs with a higher velocity of around 1.5 & times; 104 km s-1. The high velocity of the helium cannot be explained by helium external to the progenitor at the time of explosion, such as stripped surface helium from a companion star. The properties of the helium absorption in the spectra of SN 2022an instead point to unburned material in the outer ejecta, thus providing the most compelling evidence to date for helium-bearing ejecta in a 91bg-like SN Ia. Such helium has been predicted in sub-Chandrasekhar-mass double-detonation explosions involving a surface helium shell. No theoretical calculations of modern helium-shell double detonations have been performed at epochs similar to those observed for SN 2022an to study the effects of helium on their spectra, revealing a gap between observations and theoretical calculations in our understanding of how helium manifests in SNe Ia. Nevertheless, the discovery of persistent helium absorption in SN 2022an demonstrates the diagnostic power of NIR spectroscopy for understanding thermonuclear supernova explosions by probing the abundance and structure of their ejecta.

Bernhard-1 is a proposed KH 15D-like circumbinary disk occultation (CBO) system, but its binary nature and disk geometry have not previously been confirmed. We present new optical and near-infrared spectroscopy together with multi-band photometric monitoring of the system. The radial velocities confirm that Bernhard-1 hosts a highly eccentric binary with e = 0.80 ± 0.09, confirming that the periodic photometric variability arises from occultation by a misaligned circumbinary disk. Joint modeling of the spectra and phase-dependent spectral energy distributions yields pre-main-sequence components with masses of ∼ 1.1 M_⊙ and ∼ 0.8 M_⊙. Combining stellar isochrones with the measured lithium abundance yields a system age of ∼ 10 Myr. Together with the spatial, astrometric, and metallicity properties of Bernhard-1, this suggests that Bernhard-1 is probably a member of the open cluster Dolidze 42. By combining the RV orbit with a semi-transparent occultation-screen model, we infer a disk–binary mutual inclination of roughly 50^∘ or 130^∘, with the degeneracy arising from the unknown disk rotation direction. This geometric method can be applied to any CBO system once radial velocity monitoring yields an orbital solution. The new light curves deviate from earlier model predictions, consistent with ongoing disk precession, while the phase-dependent Hα profiles indicate pulsed accretion near periastron. Bernhard-1 therefore joins KH 15D and Bernhard-2 as a rare spectroscopically confirmed CBO system.

We present extensive ultraviolet to optical photometric and optical to near-infrared (NIR) spectroscopic follow-up observations of the nearby intermediate-luminosity (MV = -16.81 +/- 0.19 mag) Type Iax supernovae (SNe Iax) 2024pxl in NGC 6384. SN 2024pxl exhibits a faster light curve than the high-luminosity members of this class, and slower than low-luminosity events. The observationally well-constrained rise time of similar to 11 days and an estimated synthesized 56Ni mass of 0.03 M circle dot, based on analytical modeling of the integrated spectral energy distribution light curve, are consistent with models of the weak deflagration of a carbon-oxygen white dwarf. Our optical spectral sequence of SN 2024pxl shows weak Si ii lines and spectral evolution similar to other high-luminosity SNe Iax, but also a prominent early-time C ii line, like lower-luminosity SNe Iax. The late-time optical spectrum of SN 2024pxl closely matches that of SN 2014dt, and its NIR spectral evolution aligns with that of other well-studied, high-luminosity SNe Iax. The spectral-line expansion velocities of SN 2024pxl are at the lower end of the SNe Iax velocity distribution, and the velocity distribution of iron-group elements compared to intermediate-mass elements suggests that the ejecta are mixed on large scales, as expected in pure deflagration models. SN 2024pxl exhibits characteristics intermediate between those of high-luminosity and low-luminosity SNe Iax, further establishing a link across this diverse class.

A population of free-floating planets is known from gravitational microlensing surveys. None have a directly measured mass, owing to a degeneracy with the distance, but the population statistics indicate that many are less massive than Jupiter. We report a microlensing event-KMT-2024-BLG-0792/OGLE-2024-BLG-0516, which was observed from both ground- and space-based telescopes-that breaks the mass-distance degeneracy. The event was caused by an object with 0.219-0.046+0.075 Jupiter masses that is either gravitationally unbound or on a very wide orbit. Through comparison with the statistical properties of other observed microlensing events and predictions from simulations, we infer that this object likely formed in a protoplanetary disk (like a planet), not in isolation (like a brown dwarf). Dynamical processes then ejected it from its birthplace, producing a free-floating object.

We present panchromatic optical + near-infrared (NIR) + mid-infrared (MIR) observations of the intermediate-luminosity Type Iax supernova (SN Iax) 2024pxl and the extremely low-luminosity SN Iax 2024vjm. JWST observations provide unprecedented MIR spectroscopy of SN Iax, spanning from +11 to +42 day past maximum light. We detect forbidden emission lines in the MIR at these early times while the optical and NIR are dominated by permitted lines with an absorption component. Panchromatic spectra at early times can thus simultaneously show nebular and photospheric lines, probing both inner and outer layers of the ejecta. We identify spectral lines not seen before in SN Iax, including [Mg ii ] 4.76 μ m, [Mg ii ] 9.71 μ m, [Ne ii ] 12.81 μ m, and isolated O i 2.76 μ m that traces unburned material. Forbidden emission lines of all species are centrally peaked with similar kinematic distributions, indicating that the ejecta are well mixed in both SN 2024pxl and SN 2024vjm, a hallmark of pure deflagration explosion models. Radiative transfer modeling of SN 2024pxl shows good agreement with a weak deflagration of a near-Chandrasekhar-mass white dwarf, but additional IR flux is needed to match the observations, potentially attributable to a surviving remnant. Similarly, we find SN 2024vjm is also best explained by a weak deflagration model, despite the large difference in luminosity between the two supernovae. Future modeling should push to even weaker explosions and include the contribution of a bound remnant. Our observations demonstrate the diagnostic power of panchromatic spectroscopy for unveiling explosion physics in thermonuclear supernovae.

The AT 2018cow-like fast blue optical transient AT 2022tsd showed a large number of a few-minute-duration, high-luminosity (∼10 ^43 erg s ^−1 ) flares. We present an intensive search for such flares from another 18cow-like event, AT 2024wpp. We have used the Large Array Survey Telescope to observe this transient between 28 and 74 days after the approximate time of zero flux. The target was observed for about 23 hr to a sensitivity that allows one to detect 3 × 10 ^42 erg s ^−1 flares at a signal-to-noise ratio ≳ 5. No optical flares have been found, suggesting a one-sided 2 σ confidence upper limit of <0.02 on the flare’s duty cycle, and flare rate lower than about 0.11 hr ^−1 . These limits suggest that not all 18cow-like objects display a high rate of minute-timescale luminous flares. This can be explained either by diversity in the 18cow-like population or by viewing angle effects (e.g., beaming), or rather that the optical depth toward the central emitting region did not fall below unity during the particular search window.

BackgroundExisting epidemiological studies investigated the association between a single vitamin and hypertension. However, the potential relationship between the level of circulating multivitamins and blood pressure has not been explored. We aimed to investigate the association between multiple fat-soluble vitamin levels and blood pressure.MethodsA total of 2052 participants with essential hypertension were sampled nationwide. The plasma concentrations of fat-soluble vitamins (A, E, D, and K) were assessed using liquid chromatography coupled with the mass spectrometry method. Participants were categorized into different co-exposure patterns using the unsupervised K-means clustering method. The multiple linear regression model was used for subsequent analyses.ResultsParticipants were classified into two co-exposure patterns of fat-soluble vitamins. The levels of vitamins were relatively low in pattern 1, compared to pattern 2. Participants in pattern 2 had no significantly different blood pressure levels compared to pattern 1. However, the plasma 25-hydroxyvitamin D3 (VD3) levels were negatively associated with SBP (logarithmic 10 transformed) (β = −0.002, 95% CI: −0.004, 0); participants in the fourth α-tocopherol quartile had mean SBP levels that were 1.02% (95% CI: 0.43, 1.61%) greater than those in the lowest quartile (p for trend <0.01). In addition, no significant relationships were found between plasma VA/VK concentrations and blood pressure.DiscussionAlthough no significant association between fat-soluble vitamin co-exposure patterns and blood pressure was found, further analyses could imply that plasma α-tocopherol levels may offset the potential protective effect of plasma VD3 on blood pressure among hypertensive adults. This provided a novel perspective for exploring the joint effects of fat-soluble vitamins on blood pressure. Further studies are warranted to better understand the implications.

GRB 250702B was the longest gamma-ray burst ever detected, with a duration that challenges standard collapsar models and suggests an exotic progenitor. We collected a rich set of optical and infrared follow-up observations of its rapidly fading afterglow using a suite of telescopes including the W. M. Keck Observatory, the Gemini telescopes, the Magellan Baade Telescope, the Victor M. Blanco 4 m telescope, and the Fraunhofer Telescope at Wendelstein Observatory. Our analysis reveals that the afterglow emission is well described by forward shock emission from a highly obscured relativistic jet. Deep photometric observations of the host galaxy reveal a massive (10 ^10.66 M _⊙ ), dusty, and extremely asymmetric system that is consistent with two galaxies undergoing a major merger. The galactocentric offset, host galaxy properties, and jet characteristics disfavor a jetted tidal disruption event (TDE) around a supermassive black hole but do not definitively distinguish between competing progenitor scenarios. We find that the afterglow and host are consistent with a range of progenitors, including an atypical collapsar, a merger between a helium star and a stellar-mass black hole, the disruption of a star by a stellar-mass compact object (micro-TDE), and the tidal disruption of a star by an off-nuclear intermediate-mass black hole.

Stars are initially powered by the fusion of hydrogen to helium. These ashes serve as fuel in a series of stages1-3, transforming massive stars into a structure of shells. These are composed of natal hydrogen on the outside and consecutively heavier compositions inside, predicted to be dominated by He, C/O, O/Ne/Mg and O/Si/S (refs. 4,5). Silicon and sulfur are fused into iron, leading to the collapse of the core and either a supernova explosion or the formation of a black hole6-9. Stripped stars, in which the outer hydrogen layer has been removed and the internal He-rich or even the C/O layer below it is exposed10, provide evidence for this shell structure and the cosmic element production mechanism it reflects. The supernova types that arise from stripped stars embedded in shells of circumstellar material (CSM) confirm this scenario11-15. However, direct evidence for the most interior shells, which are responsible for producing elements heavier than oxygen, is lacking. Here we report the discovery of the supernova (SN) 2021yfj resulting from a star stripped to its O/Si/S-rich layer. We directly observe a thick, massive Si/S-rich shell, expelled by the progenitor shortly before the supernova explosion. Exposing such an inner stellar layer is theoretically challenging and probably requires a rarely observed mass-loss mechanism. This rare supernova event reveals advanced stages of stellar evolution, forming heavier elements, including silicon, sulfur and argon, than those detected on the surface of any known class of massive stars.

We present optical, radio, and X-ray observations of EP250108a/SN 2025kg, a broad-line Type Ic supernova (SN Ic-BL) accompanying an Einstein Probe (EP) fast X-ray transient (FXT) at $z=0.176$. EP250108a/SN 2025kg possesses a double-peaked optical light curve and its spectrum transitions from a blue underlying continuum to a typical SN Ic-BL spectrum over time. We fit a radioactive decay model to the second peak of the optical light curve and find SN parameters that are consistent with the SNe Ic-BL population, while its X-ray and radio properties are consistent with those of low-luminosity GRB (LLGRB) 060218/SN 2006aj. We explore three scenarios to understand the system's multi-wavelength emission -- (a) SN ejecta interacting with an extended circumstellar medium (CSM), (b) the shocked cocoon of a collapsar-driven jet choked in its stellar envelope, and (c) the shocked cocoon of a collapsar-driven jet choked in an extended CSM. All three models can explain the optical light curve and are also consistent with the radio and X-ray observations. We favor models (a) and (c) because they self-consistently explain both the X-ray prompt emission and first optical peak, but we do not rule out model (b). From the properties of the first peak in models (a) and (c), we find evidence that EP250108a/SN 2025kg interacts with an extended CSM, and infer an envelope mass $M_{\rm e} \sim 0.1\,\rm M_\odot$ and radius $R_{\rm e} \sim 4 \times 10^{13}$ cm. EP250108a/SN 2025kg's multi-wavelength properties make it a close analog to LLGRB 060218/SN 2006aj, and highlight the power of early follow-up observations in mapping the environments of massive stars prior to core collapse.

Background:The enzyme phosphatidylethanolamine N-methyltransferase (PEMT) is responsible for synthesizing phosphatidylcholine by methylating phosphatidylethanolamine. We hypothesized that a polymorphism of the PEMT gene, rs7946, is involved in carcinogenesis. Objectives:We aimed to investigate the relationship between PEMT rs7946 and digestive system cancer and examine possible effect modifiers and mediators. Methods:We conducted a nested, case-control study within the China H-type Hypertension Registry Study, including 751 cases and 1:1 matched controls. To assess the association of PEMT rs7946 and digestive system cancer, we estimated odds ratios with 95% confidence intervals (CIs) using conditional logistic regression. We used the bootstrap test to examine the potential mediating effects of related metabolites. Results:Our results revealed that wild-type homozygous CC genotype carriers of PEMT rs7946 had a significantly increased risk [odds ratio (OR): 1.31; 95% CI: 1.04, 1.66; P = 0.023] compared with the TT/CT combined genotypes. The effect was found to be more pronounced in individuals with a lower choline-to-betaine ratio (<0.412, P-interaction = 0.021). Furthermore, the mediation analysis indicated that the choline-to-betaine ratio played a significant role in mediating 13.55% of the association between PEMT rs7946 and digestive system cancer (P = 0.018). Conclusions:Our study suggested that PEMT rs7946 may affect risk of digestive system cancer through direct and indirect pathways, and the choline-to-betaine ratio may partially mediate the indirect effect.This trial was registered at Chinese Clinical Trial Registry as ChiCTR1800017274.

We study the mass spectra and radiative decays of D_s0^*(2317) and D_s1^'(2460) in an unquenched framework. In addition to coupled channel effects between the cs̅ cores and D^(*)K channels, D^(*)K-D^(*)K self interactions are also considered in this work and we succeed to reproduce their mass spectra. Furthermore, we study the radiative decays of the D_s0^*(2317) and D_s1^'(2460) by simultaneously including the compound structures of conventional cs̅ cores and D^(*)K components. We also calculate their bottom analogs with heavy quark symmetry. Our study offers useful insights into the important unquenched effects in the formation of D_s0^*(2317), D_s1^'(2460) and the bottom counterparts.

We present ultraviolet, optical, and near-infrared photometric and optical spectroscopic observations of the luminous fast blue optical transient (LFBOT) CSS 161010:045834-081803 (CSS 161010). The transient was found in a low-redshift (z = 0.033) dwarf galaxy. The light curves of CSS 161010 are characterized by an extremely fast evolution and blue colors. The V-band light curve shows that CSS 161010 reaches an absolute peak of MVmax=-20.66 +/- 0.06 mag in 3.8 days from the start of the outburst. After maximum, CSS 161010 follows a power-law decline proportional to t -2.8 +/- 0.1 in all optical bands. These photometric properties are comparable to those of well-observed LFBOTs such as AT 2018cow, AT 2020mrf, and AT 2020xnd. However, unlike these objects, the spectra of CSS 161010 show a remarkable transformation from a blue and featureless continuum to spectra dominated by very broad, entirely blueshifted hydrogen emission lines with velocities of up to 10% of the speed of light. The persistent blueshifted emission and the lack of any emission at the rest wavelength of CSS 161010 are unique features not seen in any transient before CSS 161010. The combined observational properties of CSS 161010 and its M * similar to 108 M circle dot dwarf galaxy host favor the tidal disruption of a star by an intermediate-mass black hole as its origin.

Supplementary Data from Intratumoral Expression of Mature Human Neutrophil Peptide-1 Mediates Antitumor Immunity in Mice

Abstract Background & aims: Few studies have explored the effect of serum dimethylglycine on cancer risk. This study aimed to investigate the relationship between serum dimethylglycine and the risk of new cancers. Methods We conducted a nested case-control study using data from the "H-type Hypertensive Stroke Prevention and Control Project" on adults with hypertension from the Rongcheng cohort, including 1510 cancer cases and 1510 matched controls. Univariate and multivariate logistic regression was used to study the relationship between serum dimethylglycine and cancer risk. Results Participants were 56% male with a mean age of 69.45 ± 7.73 years. A multivariate-adjusted restricted cubic spline plot showed that serum dimethylglycine concentrations were positively and non-linearly associated with cancer risk. Multivariate logistic regression results showed that with a cut-off value of 1.05ug/mL, serum dimethylglycine > 1.05ug/mL had a non-linear, positive correlation with the risk of cancer (P = 0.002). Stratified analysis showed that high levels of dimethylglycine and age < 65 years (vs. age ≥ 65 years), males (vs. females), BMI < 24 (vs. BMI ≥ 24kg/m2), no antihypertensive medication use (vs. antihypertensive medication use), no hypoglycemic medication use (vs. hypoglycemic medication use), former smokers (vs. non-smokers), former drinkers (vs. non-drinkers), fruit and vegetable intake (< 0.5 kg/week vs. >0.5 kg/week), or no family history of cancer (vs. family history of cancer) were associated with increased cancer risk. There was a significant interaction between dimethylglycine and hypoglycemic drug use, with high concentrations of dimethylglycine associated with higher cancer risk than low concentrations in patients not taking hypoglycemic drugs (P = 0.035 for interaction). Conclusions We found that elevated serum dimethylglycine levels were positively associated with cancer risk in patients with hypertension. Our findings may contribute to future cancer prevention and diagnosis.

Background: Vitamin B12 (VB12) is an essential biomarker for population health, and its deficiency status leads to severe health burdens. A comprehensive and updated investigation on the distribution of VB12 levels and status is critically needed to address public health and clinical concerns. Methods: We conducted a cross-sectional analysis using data obtained from the Precision Medical Program, which encompassed 14 provinces in China. Specific criteria based on previously published cutoffs and our study population’s characteristics are adopted to define B12 deficiency. Biochemical B12 deficiency was identified with circulating VB12 levels <148 pmol/L. Metabolic B12 deficiency was determined with circulating VB12 levels ≥148 and ≤258 pmol/L with concomitant elevated plasma total homocysteine (tHcy ≥14 µmol/L). Normal B12 status included VB12 levels >258 pmol/L or VB12 levels ranging from 148 to 258 pmol/L with tHcy levels below 14 µmol/L. VB12 levels and status were analyzed and stratified by age, sex, and geographical region. Results: This study enrolled a total of 2174 hypertensive adults, with a mean age of 63.0 years (±13.4) and 45.8% female. The overall mean VB12 levels were 322.3 (85.0) pmol/L. The prevalence rates of B12 biochemical deficiency, metabolic deficiency, metabolic deficiency with excluded renal dysfunction, and adequate status were 0.7%, 13.3%, 11.5%, and 85.9%, respectively. Females exhibited higher VB12 levels than males, with a β value of 19.72 (95% confidence interval [CI], 10.59–28.84) in the multivariate model. The southern population demonstrated higher VB12 levels than people from the north, with a β value of −18.14 (95% CI, −25.72 to −10.76). Males had a higher prevalence of metabolic VB12 deficiency in comparison to females (15.8% vs. 10.4%). Conclusions: Our study revealed that Chinese hypertensive adults exhibit relatively higher levels of VB12. Additionally, while biochemical B12 deficiency is uncommon, a noteworthy proportion of individuals were affected by metabolic VB12 deficiency. This study has important implications for nutritional counseling and vitamin B supplement strategies.