Resultados de investigación

As evidenced by recent survey results, the majority of asteroids are slow rotators (spin periods longer than 12h), but lack spin and shape models because of selection bias. This bias is skewing our overall understanding of the spins, shapes, and sizes of asteroids, as well as of their other properties. Also, diameter determinations for large (>60km) and medium-sized asteroids (between 30 and 60km) often vary by over 30% for multiple reasons. Our long-term project is focused on a few tens of slow rotators with periods of up to 60 h. We aim to obtain their full light curves and reconstruct their spins and shapes. We also precisely scale the models, typically with an accuracy of a few percent. We used wide sets of dense light curves for spin and shape reconstructions via light-curve inversion. Precisely scaling them with thermal data was not possible here because of poor infrared datasets: large bodies tend to saturate in WISE mission detectors. Therefore, we recently also launched a special campaign among stellar occultation observers, both in order to scale these models and to verify the shape solutions, often allowing us to break the mirror pole ambiguity. The presented scheme resulted in shape models for 16 slow rotators, most of them for the first time. Fitting them to chords from stellar occultation timings resolved previous inconsistencies in size determinations. For around half of the targets, this fitting also allowed us to identify a clearly preferred pole solution from the pair of two mirror pole solutions, thus removing the ambiguity inherent to light-curve inversion. We also address the influence of the uncertainty of the shape models on the derived diameters. Overall, our project has already provided reliable models for around 50 slow rotators. Such well-determined and scaled asteroid shapes will, for example, constitute a solid basis for precise density determinations when coupled with mass information. Spin and shape models in general continue to fill the gaps caused by various biases., "The files contain asteroid brightness and geometry for corresponding epochs. The ""*lcs.dat"" files were used for obtaining shape models and spin states of the asteroids using multi-apparition data. Individual lightcurves within a file are separated by an empty line, all lightcurves are relative.", Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No

Hot Jupiters have been perceived as loners devoid of planetary companions in close orbital proximity. However, recent discoveries based on space-borne precise photometry have revealed that at least some fraction of giant planets coexists with low-mass planets in compact orbital architectures. We report detecting a 1.446-d transit-like signal in the photometric time series acquired with the Transiting Exoplanet Survey Satellite (TESS) for the WASP-84 system, which is known to contain a hot Jupiter on a circular 8.5-d orbit. The planet was validated based on TESS photometry, and its signal was distilled in radial velocity measurements. The joint analysis of photometric and Doppler data resulted in a multiplanetary model of the system. With a mass of 15M_{sun}_, radius of 2R_{sun}_, and orbital distance of 0.024au, the new planet WASP-84 c was classified as a hot super-Earth with the equilibrium temperature of 1300K. A growing number of companions to hot Jupiters indicates that a non-negligible part of them must have formed under a quiescent scenario such as disc migration or in situ formation., We provide the photometric time series for transits of WASP-84 b acquired with the ground-based telescopes: the 1.2m Trebur one-meter telescope (TRE120) at the Michael Adrian Observatory in Trebur (Germany) and the 0.9m Ritchey-Chretien telescope (OSN090) at the Sierra Nevada Observatory (Spain). The data were collected from 2016-2018. The details on observations and data processing are given in the paper., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No

We describe the target selection and characteristics of the DESI Peculiar Velocity Survey, the largest survey of peculiar velocities (PVs) using both the fundamental plane (FP) and the Tully-Fisher (TF) relationship planned to date. We detail how we identify suitable early-type galaxies (ETGs) for the FP and suitable late-type galaxies (LTGs) for the TF relation using the photometric data provided by the DESI Legacy Imaging Survey DR9. Subsequently, we provide targets for 373533 ETGs and 118637 LTGs within the DESI 5-year footprint. We validate these photometric selections using existing morphological classifications. Furthermore, we demonstrate using survey validation data that DESI is able to measure the spectroscopic properties to sufficient precision to obtain PVs for our targets. Based on realistic DESI fiber assignment simulations and spectroscopic success rates, we predict the final DESI PV Survey will obtain ~133000 FP-based and ~53000 TF-based PV measurements over an area of 14000deg^2^. We forecast the ability of using these data to measure the clustering of galaxy positions and PVs from the combined DESI PV and Bright Galaxy Surveys (BGS), which allows for cancellation of cosmic variance at low redshifts. With these forecasts, we anticipate a 4% statistical measurement on the growth rate of structure at z<0.15. This is over two times better than achievable with redshifts from the BGS alone. The combined DESI PV and BGS will enable the most precise tests to date of the time and scale dependence of large-scale structure growth at z<0.15., These tables provide the target catalogs for the DESI peculiar velocity survey as well as all supplementary information to reproduce them and the methods presented in our paper., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No

Computed LDOS of the Co islands, free-electron-like state of the Co layers, energy onset and effective mass of the free-electron-like surface states, Nc-tip preparation and calibration, inelastic spectra above the Co bilayer, computed spin-state energies vs exchange field, excitation and exchange energies of the Co monolayer, spin-excitation lifetimes in the Nc tip, Cu at the corners of a trilayer island, and computed excitation energies and tilt angle of Nc., Peer reviewed

Recuperación de un libro del antiguo Instituto Alonso Barba, encontrado en el Centro de Edafología y Biología Aplicada del Segura (CEBAS) en Murcia, Peer reviewed

(Te, Tl)-AIMDEF simulations from which the training data set is obtained, comparison of energies and forces between NNPES and DFT, details on the (Te, Tl)-MDEF simulations, parameters used in the 2TM, calculation of the friction coefficients, time-convergence tests, and observed trapping dynamics., Peer reviewed

Supplementary information index: -Supplementary Figures 1-10 -Supplementary Figure 11-Graphical Abstract -Unprocessed Scans of westerns from Supplementary Figures, The E3 SUMO ligase PIAS2 is expressed at high levels in differentiated papillary thyroid carcinomas but at low levels in anaplastic thyroid carcinomas (ATC), an undifferentiated cancer with high mortality. We show here that depletion of the PIAS2 beta isoform with a transcribed double-stranded RNA-directed RNA interference (PIAS2b-dsRNAi) specifically inhibits growth of ATC cell lines and patient primary cultures in vitro and of orthotopic patient-derived xenografts (oPDX) in vivo. Critically, PIAS2b-dsRNAi does not affect growth of normal or non-anaplastic thyroid tumor cultures (differentiated carcinoma, benign lesions) or cell lines. PIAS2b-dsRNAi also has an anti-cancer effect on other anaplastic human cancers (pancreas, lung, and gastric). Mechanistically, PIAS2b is required for proper mitotic spindle and centrosome assembly, and it is a dosage-sensitive protein in ATC. PIAS2b depletion promotes mitotic catastrophe at prophase. High-throughput proteomics reveals the proteasome (PSMC5) and spindle cytoskeleton (TUBB3) to be direct targets of PIAS2b SUMOylation at mitotic initiation. These results identify PIAS2b-dsRNAi as a promising therapy for ATC and other aggressive anaplastic carcinomas., Supplementary information Reporting Summary Description of Additional Supplementary Files Peer Review File Supplementary Movie 1 Supplementary Movie 2 Supplementary Movie 3 Supplementary Dataset 1 Supplementary Dataset 2 Supplementary Dataset 3 Supplementary Dataset 4 Source data, Peer reviewed

Analysis of the NSE results in dilute solution in terms of the ZIF., Peer reviewed

Georeferenced database on the spatial properties of all individual shallow-water tropical coral reefs worldwide. The dataset was obtained by processing and analyzing the global-scale coral reef benthic data provided by the Allen Coral Atlas (ACA), a publicly available dataset of high-resolution satellite imagery and machine learning-based coral reef classifications. The original data, already divided into different coral provinces, was segmented to identify the individual reefs of each province using a label assignment algorithm. This allows to analyze several spatial properties of coral reefs such as the size distribution, area-perimeter relationship, fractal dimensions and shape measures. The dataset contains measures of area, perimeter, fractal dimension, compactness and elongation index (diameter ratio) for each individual reef in each coral province., Peer reviewed

PA chemical structures, mass spectra, HPLC chromatograms, and H NMR spectrum; TEM images of PA 1–3 at pH 7.4; AFM images of PA 1–3 at pH 1, 6, and 9; cryo-EM images of PA 1–3 at pH 6; SAXS modeling of PAs prepared at different pHs; TEM and AFM images of 4–9 at pH 1, 6, and 9; TEM images of PA 10–13 at pH 1, 6, and 9; FT-IR spectrum of PA 10–13 at pH 1, 4, 6, and 7; VT-AFM images of PA 4–6; VT-SAXS plots of PA 4–9; FRET assay of PA 1–3; dynamic simulation methods; TEM images of PA 4–6 prepared with NaCl and urea solution; TEM images and width measurement of PA 1–9 incubated with cell media for 2 h; cytotoxicity assay of PA 4–9 toward HEp2 and HaCaT cell lines; AFM and height profile of PA 1–3-treated bacteria; zeta potential and calculated logP value of PA 1–9; live/dead images of PA 1–3 at 32 μg/mL; and SEM images of MRSA JE2 treated with PA 1 overnight., Peer reviewed