DM Distribution Research Articles

Memory B cells are poised for robust antigen presentation by HLA-DO

Abstract The B cell is a uniquely efficient APC due to expression of BCR for antigen uptake and delivery to MHCII-enriched compartments (MIIC), and key regulatory molecules, invariant chain (Ii), HLA-DM and HLA-DO. All professional APCs express Ii and DM, whereas expression of DO is limited to B cells, certain DCs and thymic medullary epithelia. DO levels change dramatically in B cells entering or exiting the germinal center (GC). To determine effects of DO on other components of the MHCII pathway, we delineated the intracellular distribution of DO, DM, MHCII, and class II-associated CLIP in T2 cells with or without DO or DM expression using structured illumination microscopy. The distribution at steady state shows a very restricted lysosomal destination (LAMP1+) for DO and DM, and dual destinations (surface and LAMP1+) for CLIP and MHCII. DO expression increased overall CLIP compared to DM+DO-cells, but almost doubled the percent of CLIP co-localized with LAMP1, establishing peptide exchange potential (PEP) within MIICs, but not any other compartments or the cell surface. PEP enhancement associated with DO expression is likely due to its regulation of DM activity, as neither the overall CLIP level nor the percent of DR in MIICs increased. We then evaluated the extent of PEP in distinct primary B cell populations isolated from human tonsils, including memory (CD38−/IgD−), naïve (CD38−/IgD+), and GC (CD38+/IgD−) B cells. The measurement shows PEPMemory (significantly) > PEPNaïve > PEPGC−, although the percent of CLIP among all class II peptides is naïve > memory >> GC. These results argue that DO expression in memory B cells equips them for more efficient APC function upon re-encounter with antigen.

On wave dark matter in spiral and barred galaxies

We recover spiral and barred spiral patterns in disk galaxy simulations with a Wave Dark Matter (WDM) background (also known as Scalar Field Dark Matter (SFDM), Ultra-Light Axion (ULA) dark matter, and Bose-Einstein Condensate (BEC) dark matter). Here we show how the interaction between a baryonic disk and its Dark Matter Halo triggers the formation of spiral structures when the halo is allowed to have a triaxial shape and angular momentum. This is a more realistic picture within the WDM model since a non-spherical rotating halo seems to be more natural. By performing hydrodynamic simulations, along with earlier test particles simulations, we demonstrate another important way in which wave dark matter is consistent with observations. The common existence of bars in these simulations is particularly noteworthy. This may have consequences when trying to obtain information about the dark matter distribution in a galaxy, the mere presence of spiral arms or a bar usually indicates that baryonic matter dominates the central region and therefore observations, like rotation curves, may not tell us what the DM distribution is at the halo center. But here we show that spiral arms and bars can develop in DM dominated galaxies with a central density core without supposing its origin on mechanisms intrinsic to the baryonic matter.

The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations

We study the distribution of cold dark matter (CDM) in cosmological simulations from the FIRE (Feedback In Realistic Environments) project, for $M_{\ast}\sim10^{4-11}\,M_{\odot}$ galaxies in $M_{\rm h}\sim10^{9-12}\,M_{\odot}$ halos. FIRE incorporates explicit stellar feedback in the multi-phase ISM, with energetics from stellar population models. We find that stellar feedback, without "fine-tuned" parameters, greatly alleviates small-scale problems in CDM. Feedback causes bursts of star formation and outflows, altering the DM distribution. As a result, the inner slope of the DM halo profile ($\alpha$) shows a strong mass dependence: profiles are shallow at $M_{\rm h}\sim10^{10}-10^{11}\,M_{\odot}$ and steepen at higher/lower masses. The resulting core sizes and slopes are consistent with observations. This is broadly consistent with previous work using simpler feedback schemes, but we find steeper mass dependence of $\alpha$, and relatively late growth of cores. Because the star formation efficiency $M_{\ast}/M_{\rm h}$ is strongly halo mass dependent, a rapid change in $\alpha$ occurs around $M_{\rm h}\sim 10^{10}\,M_{\odot}$ ($M_{\ast}\sim10^{6}-10^{7}\,M_{\odot}$), as sufficient feedback energy becomes available to perturb the DM. Large cores are not established during the period of rapid growth of halos because of ongoing DM mass accumulation. Instead, cores require several bursts of star formation after the rapid buildup has completed. Stellar feedback dramatically reduces circular velocities in the inner kpc of massive dwarfs; this could be sufficient to explain the "Too Big To Fail" problem without invoking non-standard DM. Finally, feedback and baryonic contraction in Milky Way-mass halos produce DM profiles slightly shallower than the Navarro-Frenk-White profile, consistent with the normalization of the observed Tully-Fisher relation.

Socioeconomic inequalities in the prevalence of diabetes and hypertension in the Northern region of Portugal

Background Type 2 diabetes (DM\_2) and hypertension (HBP) are highly prevalent conditions in Portugal (41% and 13%, respectively), with severe consequences on morbidity and mortality. The unequal distribution of DM\_2 and HBP in the population, with a higher prevalence among underprivileged people, may be a major cause of the observed socioeconomic (SE) disparities in health and mortality. This study aims at measuring the association between SE factors and DM_2 and HBP prevalence in the …

Dynamic scaling and kinetic roughening of poly(ethylene) islands grown by vapor phase deposition

Vapor phase deposition of poly(ethylene) is shown to produce uncross-linked thin films consisting of linear (CH2)100 oligomers with narrow molar mass distribution of dispersity DM=1.10. Early stages of the film formation are characterized by the growth of two-dimensional compact islands of constant 7–8nm thickness. The transversal evolution of islands is studied in the context of the Dynamic Scaling Theory. The aggregation regime is found to be valid in a narrow range of coverage 0.1<θ<0.3. The critical island size is estimated to be i=1. Kinetic roughening of the growing front gives a set of the scaling exponents αloc=0.67, αs=0.85, β=0.33 (β=0.2 for the late stages of growth) and z=2.2 that does not fit into any of the known universality classes. Macromolecular relaxation at the island edges is suggested to explain the observed inconsistence.

The mutual interaction between Population III stars and self-annihilating dark matter

We use cosmological simulations of high-redshift minihalos to investigate the effect of dark matter annihilation (DMA) on the collapse of primordial gas. We numerically investigate the evolution of the gas as it assembles in a Population III stellar disk. We find that when DMA effects are neglected, the disk undergoes multiple fragmentation events beginning at ~ 500 yr after the appearance of the first protostar. On the other hand, DMA heating and ionization of the gas speeds the initial collapse of gas to protostellar densities and also affects the stability of the developing disk against fragmentation, depending on the DM distribution. We compare the evolution when we model the DM density with an analytical DM profile which remains centrally peaked, and when we simulate the DM profile using N-body particles (the 'live' DM halo). When utilizing the analytical DM profile, DMA suppresses disk fragmentation for ~ 3500 yr after the first protostar forms, in agreement with earlier work. However, when using a 'live' DM halo, the central DM density peak is gradually flattened due to the mutual interaction between the DM and the rotating gaseous disk, reducing the effects of DMA on the gas, and enabling secondary protostars of mass ~ 1 M_sol to be formed within ~ 900 yr. These simulations demonstrate that DMA is ineffective in suppressing gas collapse and subsequent fragmentation, rendering the formation of long-lived dark stars unlikely. However, DMA effects may still be significant in the early collapse and disk formation phase of primordial gas evolution.

SUPERMASSIVE BLACK HOLE FORMATION AT HIGH REDSHIFTS VIA DIRECT COLLAPSE: PHYSICAL PROCESSES IN THE EARLY STAGE

We use numerical simulations to explore whether direct collapse can lead to the formation of SMBH seeds at high-z. We follow the evolution of gas within DM halos of 2 x 10^8 Mo and 1 kpc. We adopt cosmological density profiles and j-distributions. Our goal is to understand how the collapsing flow overcomes the centrifugal barrier and whether it is subject to fragmentation. We find that the collapse leads either to a central runaway or to off-center fragmentation. A disk-like configuration is formed inside the centrifugal barrier. For more cuspy DM distribution, the gas collapses more and experiences a bar-like perturbation and a central runaway. We have followed this inflow down to ~10^{-4} pc. The flow remains isothermal and the specific angular momentum is efficiently transferred by gravitational torques in a cascade of nested bars. This cascade supports a self-similar, disk-like collapse. In the collapsing phase, virial supersonic turbulence develops and fragmentation is damped. For larger initial DM cores the timescales become longer. In models with more organized initial rotation, a torus forms and appears to be supported by turbulent motions. The evolution depends on the competition between two timescales, corresponding to the onset of the central runaway and off-center fragmentation. For less organized rotation, the torus is greatly weakened, the central accretion timescale is shortened, and off-center fragmentation is suppressed --- triggering the central runaway even in previously `stable' models. The resulting SMBH masses lie in the range 2 x 10^4 Mo - 2 x 10^6 Mo, much higher than for Population III remnants. We argue that the above upper limit appears to be more realistic mass. Corollaries of this model include a possible correlation between SMBH and DM halo masses, and similarity between the SMBH and halo mass functions, at time of formation.

Utility of Anti–Melanoma Differentiation–Associated Gene 5 Antibody Measurement in Identifying Patients With Dermatomyositis and a High Risk for Developing Rapidly Progressive Interstitial Lung Disease: A Review of the Literature and a Meta‐Analysis

To assess the utility of anti-melanoma differentiation-associated gene 5 (anti-MDA5) antibody measurement for predicting a risk for developing rapidly progressive interstitial lung disease (RP-ILD) in patients with polymyositis/dermatomyositis (PM/DM). A single-center cohort of 64 consecutive Chinese patients with PM/DM was examined. Serum anti-MDA5 antibody was measured by enzyme-linked immunosorbent assay. For meta-analysis, we searched PubMed and the Institute for Scientific Information Web of Knowledge for original studies that measured anti-MDA5 antibodies in patients with PM/DM. We calculated pooled sensitivity, specificity, diagnostic odds ratio (DOR), and the summary receiver operating characteristic (sROC) curve. In Chinese patients, anti-MDA5 antibodies were detected in 26 patients with classic DM or clinically amyopathic DM (CADM). Compared with anti-MDA5-negative patients, anti-MDA5-positive patients showed a higher prevalence of RP-ILD (P = 0.001). In a total of 233 patients with anti-MDA5 antibody, derived from 16 studies, a higher frequency of CADM was found in Japanese than in non-Japanese patients (74.7% versus 39.2%; P = 1.2 × 10(-7) ). Meta-analysis revealed that the pooled sensitivity and specificity of anti-MDA5 antibody for RP-ILD was 77% (95% confidence interval [95% CI] 64-87%) and 86% (95% CI 79-90%), respectively. The pooled DOR was 20.41 (95% CI 9.02-46.20) with a favorable area under the sROC curve of 0.89 (95% CI 0.63-0.98). Detection of anti-MDA5 antibody is a valuable tool for identifying DM patients with a high risk for developing RP-ILD, but the distribution of classic DM and CADM in patients with this antibody varies among ethnic groups.

Stellar mass map and dark matter distribution in M 31

Stellar mass distribution in M31 is estimated using optical and infrared imaging data. Combining the derived stellar mass model with various kinematical data, properties of the DM halo of the galaxy are constrained. SDSS observations through the ugriz filters and the Spitzer imaging at 3.6 microns are used to sample the SED of the galaxy at each imaging pixel. Intrinsic dust extinction effects are taken into account by using far-infrared observations. Synthetic SEDs created with different stellar population synthesis models are fitted to the observed SEDs, providing estimates for the stellar mass surface density. The stellar mass distribution of the galaxy is described with a 3D model consisting of a nucleus, a bulge, a disc, a young disc and a halo component, each following the Einasto density distribution (relations between different functional forms of the Einasto density distribution are given in App. B). By comparing the stellar mass distribution to the observed rotation curve and kinematics of outer globular clusters and satellite galaxies, the DM halo parameters are estimated. Stellar population synthesis models suggest that M31 is dominated by old stars throughout the galaxy. The total stellar mass is (10-15)10^10Msun, 30% of which is in the bulge and 56% in the disc. None of the tested DM distribution models can be falsified on the basis of the stellar matter distribution and the rotation curve of the galaxy. The virial mass of the DM halo is (0.8-1.1)10^12Msun and the virial radius is 189-213kpc, depending on the DM distribution. The central density of the DM halo is comparable to that of nearby dwarf galaxies, low-surface-brightness galaxies and distant massive disc galaxies, thus the evolution of central DM halo properties seems to be regulated by similar processes for a broad range of halo masses, environments, and cosmological epochs.

The use of non-standard CT conversion ramps for Monte Carlo verification of 6 MV prostate IMRT plans

Monte Carlo (MC) dose calculation algorithms have been widely used to verify the accuracy of intensity-modulated radiotherapy (IMRT) dose distributions computed by conventional algorithms due to the ability to precisely account for the effects of tissue inhomogeneities and multileaf collimator characteristics. Both algorithms present, however, a particular difference in terms of dose calculation and report. Whereas dose from conventional methods is traditionally computed and reported as the water-equivalent dose (Dw), MC dose algorithms calculate and report dose to medium (Dm). In order to compare consistently both methods, the conversion of MC Dm into Dw is therefore necessary.This study aims to assess the effect of applying the conversion of MC-based Dm distributions to Dw for prostate IMRT plans generated for 6 MV photon beams. MC phantoms were created from the patient CT images using three different ramps to convert CT numbers into material and mass density: a conventional four material ramp (CTCREATE) and two simplified CT conversion ramps: (1) air and water with variable densities and (2) air and water with unit density. MC simulations were performed using the BEAMnrc code for the treatment head simulation and the DOSXYZnrc code for the patient dose calculation. The conversion of Dm to Dw by scaling with the stopping power ratios of water to medium was also performed in a post-MC calculation process.The comparison of MC dose distributions calculated in conventional and simplified (water with variable densities) phantoms showed that the effect of material composition on dose-volume histograms (DVH) was less than 1% for soft tissue and about 2.5% near and inside bone structures. The effect of material density on DVH was less than 1% for all tissues through the comparison of MC distributions performed in the two simplified phantoms considering water. Additionally, MC dose distributions were compared with the predictions from an Eclipse treatment planning system (TPS), which employed a pencil beam convolution (PBC) algorithm with Modified Batho Power Law heterogeneity correction. Eclipse PBC and MC calculations (conventional and simplified phantoms) agreed well (<1%) for soft tissues. For femoral heads, differences up to 3% were observed between the DVH for Eclipse PBC and MC calculated in conventional phantoms. The use of the CT conversion ramp of water with variable densities for MC simulations showed no dose discrepancies (0.5%) with the PBC algorithm. Moreover, converting Dm to Dw using mass stopping power ratios resulted in a significant shift (up to 6%) in the DVH for the femoral heads compared to the Eclipse PBC one.Our results show that, for prostate IMRT plans delivered with 6 MV photon beams, no conversion of MC dose from medium to water using stopping power ratio is needed. In contrast, MC dose calculations using water with variable density may be a simple way to solve the problem found using the dose conversion method based on the stopping power ratio.

Morphological and physiological studies in three alfalfa varieties (Medicago sativa L.) under salt stress

Responses to salt stress were investigated in three alfalfa varieties (Gabes, Hunterfield, and Hyb.555). Seedlings were submitted to salinity induced by adding NaCl into water at 4 concentrations (0 2.5 5 and 10g.l). Growth parameters (DM, plant height, LA, LAR, SLA, leaves thickness, succulence), and hydraulic parameters (RWC, WC, WUE) were investigated in leaves, stems and roots after three months of salt stress. Results showed that NaCl decreased DMY of the three varieties. However, Gabes variety, compared to Hunterfield and Hyb.555 has a DMY significantly higher, in the absence and presence of NaCl. The severe decrease in the DMY of the introduced varieties was related to the premature senescence accelerated by the salt intensity and the duration. On the other hand, Gabes variety has a well-equilibrated distribution of DM between organs. The LAR and the SLA decreased significantly with the salt increasing. The salt increased the leaves thickness and succulence. WC increased in concomitance with the rise of leaf succulence. WUE under salt stress decreased in the three lucernes. However, Gabes variety has WUE significantly higher in all salt treatments. This study allowed highlighting the interest of the Gabes variety in any selection program for salt tolerance.

The density profiles of dark matter halos in spiral galaxies

In spiral galaxies, we explain their non-Keplerian rotation curves (RCs) by means of a non-luminous component embedding their stellar-gaseous disks. Understanding the detailed properties of this component (labelled Dark Matter, DM) is one of the most pressing issues of Cosmology. We investigate the recent relationship (claimed by Walker et al. 2010, hereafter W+10) between $r$, the galaxy radial coordinate, and $V_h(r)$, the dark halo contribution to the circular velocity at $r$, {\it a}) in the framework of the Universal Rotation Curve (URC) paradigm and directly {\it b}) by means of the kinematics of a large sample of DM dominated spirals. We find a general agreement between the W+10 claim, the distribution of DM emerging from the URC and that inferred in the (low luminosity) objects of our sample. We show that such a phenomenology, linking the spiral's luminosity, radii and circular velocities, implies an evident inconsistency with (naive) predictions in the $\Lambda$ Cold Dark Matter ($\Lambda$CDM) scenario.

Forward-Backward Asymmetry intt¯Production from Flavor Symmetries

We show that the forward-backward asymmetry in top quark pair production can be enhanced by fields that transform nontrivially under the flavor group and satisfy minimal flavor violation, while at the same time the constraints from associated effects on the dσ(tt)/dM(tt) distribution, dijet resonance searches, same-sign top-pair production, and other phenomenology are satisfied. We work out two examples in detail: one where a scalar color antisextet field that is also an antisextet of SU(3)(U) enhances the forward-backward asymmetry and one where the enhancement arises from a vector color octet field that is also an octet of SU(3)(U).

PPPC 4 DM ID: a poor particle physicist cookbookfor dark matter indirect detection

We provide ingredients and recipes for computing signals of TeV-scale Dark Matter annihilations and decays in the Galaxy and beyond. For each DM channel, we present the energy spectra of at production, computed by high-statistics simulations. We estimate the Monte Carlo uncertainty by comparing the results yielded by the Pythia and Herwig event generators. We then provide the propagation functions for charged particles in the Galaxy, for several DM distribution profiles and sets of propagation parameters. Propagation of e± is performed with an improved semi-analytic method that takes into account position-dependent energy losses in the Milky Way. Using such propagation functions, we compute the energy spectra of e±,p̄ and d̄ at the location of the Earth. We then present the gamma ray fluxes, both from prompt emission and from Inverse Compton scattering in the galactic halo. Finally, we provide the spectra of extragalactic gamma rays. All results are available in numerical form and ready to be consumed.

Sunflower biomass distribution and seed yield in saline soil of Mexico highlands

Soil salinity is a worldwide problem. The aim of this study was to evaluate biomass production and partition in the organs of sunflower under a gradient of salinity in the soil. The Victoria sunflower was sown on 15 June 2007 at a density of 100,000 plants ha-1 in Montecillo Mex. (19° N, 48° W and 2,400 m). The area has an arid climate (less dry), an annual rainfall of 558.5 mm, and an average temperature of 14.6°C. Based on soil analysis, three areas were used as the treatments, each having 4 replicates. These were: high salinity (EC 11 dS m-1, HS), medium salinity (EC 7 dS m-1, MS), and low salinity (EC 5 dS m-1, HS). Crop emergence occurred eight days after sowing (DAS), anthesis (R5) 80 DAS, and physiological maturity (R9) 130 DAS. Dry matter accumulation (%) in plant organs, total biomass, yield and survival all decreased with increasing salinity, whereas DM distribution did not. The highest biomass, yield and survival were found in the LS treatment (1055, 102 g m-2, and 100%), while the lowest values of these parameters were recorded in the area with HS (312, 29 g m-2, and 60%), respectively. The greatest dry matter accumulation was observed in the stem, followed by the receptacle, seeds and leaves. The harvest index and the filled capitulum index were not affected by salinity. In conclusion, biomass accumulation, yield and survival of sunflower decreased with increasing soil salinity. The phenology and biomass distribution in the plant organs were not affected by salinity.

Clumpiness enhancement of charged cosmic rays from dark matter annihilation with Sommerfeld effect

Boost factors of dark matter annihilation into antiprotons andelectrons/positrons due to the clumpiness of dark matter distributionare studied in detail in this work, taking the Sommerfeld effectinto account. It has been thought that the Sommerfeld effect, ifexists, will be more remarkable in substructures because they arecolder than the host halo, and may result in a larger boost factor.We give a full calculation of the boost factors based on the recentN-body simulations. Three typical cases of Sommerfeld effects, thenon-resonant, moderately resonant and strongly resonant cases areconsidered. We find that for the non-resonant and moderatelyresonant cases the enhancement effects of substructures due to theSommerfeld effect are very small ( ∼ \U0001d4aa(1)) becauseof the saturation behavior of the Sommerfeld effect. For the strongly resonant case the boost factor is typically smaller than ∼ \U0001d4aa(10). However, it is possible in some very extreme cases that DM distribution is adopted to give the maximal annihilation the boost factor can reach up to ∼ 1000.The variances of the boost factors due to different realizations ofsubstructures distribution are also discussed in the work.

2PIGG group masses via 2dF galaxyz-space distortion

Prompted by indications from QSO lensing that there may be more mass associated with galaxy groups than expected, we have made new dynamical infall estimates of the masses associated with 2PIGG groups and clusters. We have analysed the redshift distortions in the cluster-galaxy cross-correlation function as a function of cluster membership, cross-correlating z<0.12 2PIGG clusters and groups with the full 2dF galaxy catalogue. We have made estimates of the dynamical infall parameter beta and new estimates of the group velocity dispersions. We first find that the amplitude of the full 3-D redshift space cross-correlation function, xi_{cg}, rises monotonically with group membership. We use a simple linear-theory infall model to fit xi(sigma, pi) in the range 5<s<40h^{-1}Mpc. We find that the beta versus membership relation for the data shows a minimum at intermediate group membership n~20 or L~2x10^11h^-2Lsun, implying that the bias and hence M/L ratios rise by a significant factor (~5x) both for small groups and rich clusters. However, the mocks show a systematic shift between the location of the beta minimum and the M/L minimum at L~10^10h^-2Lsun given by direct calculation using the known DM distribution. Our overall conclusion is that bias estimates from dynamical infall appear to support the minimum in star-formation efficiency at intermediate halo masses. Nevertheless, there may still be significant systematic problems arising from measuring beta~1/b using large-scale infall rather than M/L using small-scale velocity dispersions.

Evaluation of an anti-p185HER2 (scFv-CH2-CH3)2 fragment following radioiodination using two different residualizing labels: SGMIB and IB-Mal-d-GEEEK

A 105-kDa double mutant single-chain Fv-Fc fragment (scFv-Fc DM) derived from the anti-p185(HER2) hu4D5v8 antibody (trastuzumab; Herceptin) has been described recently. The goal of this study was to investigate whether improved tumor targeting could be achieved with this fragment through the use of residualizing radioiodination methods. The scFv-Fc DM fragment was radioiodinated using N-succinimidyl 4-guanidinomethyl 3-[(131)I]iodobenzoate ([(131)I]SGMIB) and N(epsilon)-(3-[(131)I]iodobenzoyl)-Lys(5)-N(alpha)- maleimido-Gly(1)-GEEEK ([(131)I]IB-Mal-D-GEEEK), two residualizing radioiodination agents that have been used successfully with intact antibodies. Paired-label internalization assays of the labeled fragments were performed in vitro using MCF7 human breast cancer cells transfected to express HER2 (MCF7-HER2); comparisons were made to scFv-Fc DM directly radioiodinated using Iodogen. The tissue distribution of the scFv-Fc DM labeled with [(125)I]IB-Mal-d-GEEEK and [(131)I]SGMIB was compared in athymic mice bearing MCF7-HER2 xenografts. The scFv-Fc DM fragment was labeled with [(131)I]SGMIB and [(131)I]IB-Mal-d-GEEEK in conjugation yields of 53% and 25%, respectively, with preservation of immunoreactivity for HER2. Internalization assays indicated that labeling via SGMIB resulted in a 1.6- to 3.5-fold higher (P<.05) retention of radioactivity, compared to that from the directly labeled fragment, in HER2-expressing cells during a 24-h observation period. Likewise, the amount of radioactivity retained in cells from the IB-Mal-d-GEEEK-labeled fragment was 1.4- to 3.3-fold higher (P<.05). Tumor uptake of radioiodine activity in athymic mice bearing MCF7-HER2 xenografts in vivo was significantly higher for the [(125)I]IB-Mal-d-GEEEK-labeled scFv-Fc DM fragment compared with that of the [(131)I]SGMIB-labeled fragment, particularly at later time points. The uptake of (125)I was threefold (3.6+/-1.1 %ID/g vs. 1.2+/-0.4 %ID/g) and fourfold (3.1+/-1.7 %ID/g vs. 0.8+/-0.4 %ID/g) higher than that for (131)I at 24 and 48 h, respectively. However, the [(125)I]IB-Mal-d-GEEEK-labeled scFv-Fc DM fragment also exhibited considerably higher levels of radioiodine activity in liver, spleen and kidney. The overall results further demonstrate the potential utility of these two prosthetic groups for the radiohalogenation of internalizing monoclonal antibodies and their fragments. Specifically, the trastuzumab-derived double mutant fragment in combination with these residualizing agents warrants further evaluation for imaging and possibly treatment of HER2 expressing malignancies.

Spatial and seasonal variability of raindrop size distributions in southeast India

Long‐term measurements of raindrop size distribution (DSD) made with the Joss‐Waldvogel disdrometers at two sites (Gadanki, an inland station, and Cuddalore, a coastal station) in southeast India are utilized to study the seasonal and spatial variations of DSD. The stratified DSD data (based on rain rate R) show significant seasonal variation at both sites. Smaller‐drop concentration is higher in the northeast monsoon (NEM) than in the southwest monsoon (SWM) for the same R. Paucity of smaller drops in SWM increases the mass weighted mean diameter (Dm) considerably. The seasonal differences are pronounced at Gadanki. The seasonal differences are found to be a regular feature at these locations as they are observed in all the years. The DSD has also shown clear diurnal variation with large Dm values in evening hours. The possible causative mechanisms for the observed spatial and seasonal DSD differences are investigated in detail using satellite and radiosonde observations. In particular, the research attempted to address the following question: Are the observed seasonal differences in DSD arising at the cloud formation level or related to the microphysical processes occurring in the evolution of DSD. The low‐level wind pattern and cloud effective radius and Dm distributions in these seasons reveal that the cloud systems in SWM and NEM are continental and maritime, respectively, in nature. However, the microphysical and dynamical processes related to evaporation and convection also seem to play an important role in modifying the DSD. These processes are found predominantly in SWM and are, primarily, responsible for the changes in DSD during their evolution.

INDUCED MALE-STERILITY ALTERS DRY MATTER DISTRIBUTION IN SOLANUM VILLOSUM MILL.

INDUCED MALE-STERILITY ALTERS DRY MATTER DISTRIBUTION IN SOLANUM VILLOSUM MILL.