Proteomics in Pancreatic Cancer Research

Pancreatic cancer is a highly aggressive malignancy with a poor prognosis and deeply affects the life of people. Therefore, the earlier diagnosis and better treatments are urgently needed. In recent years, the proteomic technologies are well established and growing rapidly and have been widely applied in clinical applications, especially in pancreatic cancer research. In this paper, we attempt to discuss the development of current proteomic technologies and the application of proteomics to the field of pancreatic cancer research. This will explore the potential perspective in revealing pathogenesis, making the diagnosis earlier and treatment

MaNGA DynPop -- I. Quality-assessed stellar dynamical modelling from integral-field spectroscopy of 10K nearby galaxies: a catalogue of masses, mass-to-light ratios, density profiles and dark matter

This is the first paper in our series on the combined analysis of the Dynamics and stellar Population (DynPop) for the MaNGA survey in the final SDSS Data Release 17 (DR17). Here we present a catalogue of dynamically-determined quantities for over 10000 nearby galaxies based on integral-field stellar kinematics from the MaNGA survey. The dynamical properties are extracted using the axisymmetric Jeans Anisotropic Modelling (JAM) method, which was previously shown to be the most accurate for this kind of study. We assess systematic uncertainties using eight dynamical models with different assumptions. We use two orientations of the velocity ellipsoid: either cylindrically-aligned JAM$_{\rm cyl}$ or spherically-aligned JAM$_{\rm sph}$. We also make four assumptions for the models' dark vs. luminous matter distributions: (1) mass-follows-light, (2) free NFW dark halo, (3) cosmologically-constrained NFW halo, (4) generalized NFW dark halo, i.e. with free inner slope. In this catalogue, we provide the quantities related to the mass distributions (e.g. the density slopes and enclosed mass within a sphere of a given radius for total mass, stellar mass, and dark matter mass components). We also provide the complete models which can be used to compute the full luminous and mass distribution of each galaxy. Additionally, we visually assess the qualities of the models to help with model selections. We estimate the observed scatter in the measured quantities which decreases as expected with improvements in quality. For the best data quality, we find a remarkable consistency of measured quantities between different models, highlighting the robustness of the results.Comment: 30 pages, 15 figures, 4 tables, accepted by MNRAS, the catalogue is available here https://manga-dynpop.github.io

MaNGA DynPop – III. Stellar dynamics versus stellar population relations in 6000 early-type and spiral galaxies: Fundamental Plane, mass-to-light ratios, total density slopes, and dark matter fractions

We present dynamical scaling relations, combined with the stellar population properties, for a subsample of about 6000 nearbygalaxies with the most reliable dynamical models extracted from the full Mapping Nearby Galaxies at Apache Point Observatory(MaNGA) sample of 10 000 galaxies. We show that the inclination-corrected mass plane for both early-type galaxies (ETGs) andlate-type galaxies (LTGs), which links dynamical mass, projected half-light radius Re, and the second stellar velocity momentσe within Re, satisfies the virial theorem and is even tighter than the uncorrected one. We find a clear parabolic relation betweenlg(M/L)e, the total mass-to-light ratio (M/L) within a sphere of radius Re, and lg σe, with the M/L increasing with σe andfor older stellar populations. However, the relation for ETGs is linear and the one for the youngest galaxies is constant. Weconfirm and improve the relation between mass-weighted total density slopes γT and σe: γT become steeper with increasingσe until lg(σe/km s−1) ≈ 2.2 and then remain constant around γT ≈ 2.2. The γT –σe variation is larger for LTGs than ETGs. Atfixed σe the total density profiles steepen with galaxy age and for ETGs. We find generally low dark matter fractions, medianfDM(<Re) = 8 per cent, within a sphere of radius Re. However, we find that fDM(<Re) depends on σe better than stellar mass:dark matter increases to a median fDM(<Re) = 33 per cent for galaxies with σe 100 km s−1. The increased fDM(<Re) at lowσe explains the parabolic lg(M/L)e– lg σe relation

The microstructure and mechanical properties of friction stir welded Ti6Al4V titanium alloy under β transus temperature

Ti6Al4V titanium alloy is friction stir welded using a W-Re rotational tool. The effects of welding speed on the microstructure, tensile strength and fracture properties of weld are investigated. At the rotational velocity of 250 r/min, the peak temperature is lower than β transus temperature, and the weld nugget is made up of fine α phase and transformed β phase. The grain size of shoulder affected zone is bigger than that of weld nugget because of low thermal conductivity of Ti6Al4V titanium alloy. By increasing the welding speed, the grain size of weld nugget, the tensile strength and the ductility of weld all are decreased

MaNGA DynPop – IV. Stacked total density profile of galaxy groups and clusters from combining dynamical models of integral-field stellar kinematics and galaxy–galaxy lensing

We present the measurement of total and stellar/dark matter decomposed mass density profile around a sample of galaxy groupsand clusters with dynamical masses derived from integral-field stellar kinematics from the MaNGA survey in Paper I and weaklensing derived from the DECaLS imaging survey. Combining the two data sets enables accurate measurement of the radialdensity distribution from several kpc to Mpc scales. Intriguingly, we find that the excess surface density derived from stellarkinematics in the inner region cannot be explained by simply adding an NFW dark matter halo extrapolated from lensingmeasurement at a larger scale to a stellar mass component derived from the NASA-Sloan Atlas (NSA) catalogue. We find that agood fit to both data sets requires a stellar mass normalization about three times higher than that derived from the NSA catalogue,which would require an unrealistically too-heavy initial mass function for stellar mass estimation. If we keep the stellar massnormalization to that of the NSA catalogue but allow a varying inner dark matter density profile, we obtain an asymptotic slopeof γ gnfw = 1.82+0.15−0.25 and γ gnfw = 1.48+0.20 −0.41 for the group bin and the cluster bin, respectively, significantly steeper than the NFWcase. We also compare the total mass inner density slopes with those from TNG300 and find that the values from the simulationare lower than the observation by about 2σ level