Resultados de investigación

The current architecture of a given multi-planetary system is a key fingerprint of its past formation and dynamical evolution history. Long-term follow-up observations are key to complete their picture. In this paper we focus on the confirmation and characterization of the components of the TOI-969 planetary system, where TESS detected a Neptune-size planet candidate in a very close-in orbit around a late K-dwarf star. We use a set of precise radial velocity observations from HARPS, PFS and CORALIE instruments covering more than two years in combination with the TESS photometric light curve and other ground-based follow-up observations to confirm and characterize the components of this planetary system. We find that TOI-969 b is a transiting close-in (Pb~1.82days) mini-Neptune planet (m_b_=9.1^+1.1^_1.0_M_{Earth}_, R_b_=2.765^+0.088^_0.097_R_{Earth}_), thus placing it on the {lower boundary} of the hot-Neptune desert (T_eq,b_=941+/-31K). The analysis of its internal structure shows that TOI-969 b is a volatile-rich planet, suggesting it underwent an inward migration. The radial velocity model also favors the presence of a second massive body in the system, TOI-969 c, with a long period of P_c_=1700^+290^_280_days and a minimum mass of m_c_sini_c_=11.3^+1.1^_0.9_M_Jup_, and with a highly-eccentric orbit of e_c_=0.628^+0.043^_0.036_. The TOI-969 planetary system is one of the few around K-dwarfs known to have this extended configuration going from a very close-in planet to a wide-separation gaseous giant. TOI-969 b has a transmission spectroscopy metric of 93, and it orbits a moderately bright (G=11.3mag) star, thus becoming an excellent target for atmospheric studies. The architecture of this planetary system can also provide valuable information about migration and formation of planetary systems., Detection and characterization of the planet TOI-969b and its external long-period planetary-mass companion with radial velocity, high-spatial resolution imaging and high-precision photometry., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No

The 4D Eigenvector 1 empirical formalism (4DE1) and its main sequence (MS) for quasars has emerged as a powerful tool for organising the diversity among quasar populations, as several key observational measures and physical parameters are systematically changing along it. Trends revealed by 4DE1 are very well established to explain all the diverse characteristics seen in low-redshift quasar samples. Nevertheless, the situation is far less clear when dealing with high-luminosity and high-redshift sources. Here, we aim to evaluate the behaviour of our sample of 22 quasars at high redshift (2.2<=z<=3.7) and high luminosity (47.39<=L_bol_<=48.36) in the context of the 4DE1. Our approach involves studying quasar physics through a spectroscopic exploration of UV and optical emission line diagnostics. We used new observations from the ISAAC instrument at ESO-VLT and primarily from the SDSS to cover the optical and the UV rest-frames, respectively. The emission lines were characterised both via a quantitative parametrisation of the line profiles and a decomposition of the emission line profiles using multicomponent fitting routines. We provide spectrophotometric properties and line profile measurements for H{beta}+[OIII]4959,5007, as well as SiIV1397+OIV]1402, CIV1549+HeII1640, and the 1900{AA} blend (including AlIII1860, SiIII]1892, and CIII]1909). For six out of the 22 objects, a significantly blueshifted component on the H{beta} profile is present. In 14 out of 22 cases, an H{beta} outflowing component associated with [OIII] is detected. The majority of [OIII]4959,5007 emission line profiles show blueshifted velocities higher than 250km/s. We find extremely broad [OIII]4959,5007 emission that is comparable to the width of H{beta} broad profile in some highly accreting quasars. The [OIII]4959,5007 and CIV1549 blueshifts show very high amplitudes and a high degree of correlation. The line widths and shifts are correlated for both [OIII]4959,5007 and CIV1549, suggesting that emission from outflowing gas is providing a substantial broadening effect to both lines. Otherwise, the links between CIV1549 centroid velocity at half intensity (c(1/2)), Eddington ratio (L/L_Edd_), and bolometric luminosity are found to be in agreement with previous studies of high-luminosity quasars. Our analysis suggests that the behaviour of quasars of very high luminosity all along the main sequence is strongly affected by powerful outflows involving a broad range of spatial scales. The main sequence correlations remain valid at high redshift and high luminosity even if a systematic increase in line width is observed. Scaling laws based on UV AlIII1860 and H{beta} emission lines are equally reliable estimators of M_BH_., Our sample consists of 22 quasars with high redshift, going from z=2.2 to z=3.7, and with high luminosity (47.39<=logLbol<=48.36[erg/s]), including both radio-loud and radio-quiet sources that were observed under the ESO programmes 083.B-0273(A) and 085.B-0162(A). Our sample covers a redshift that allows for the detection and observation of the H{alpha}+[OIII]4959,5007 region through the transparent window in the near-infrared with the ISAAC spectrograph at VLT (Sulentic et al., 2006A&A...456..929S, 2017A&A...608A.122S, Cat. J/A+A/608/A122). Table 1 presents the main properties of our sample. Spectra were taken in service mode in 2009 and 2010, with the infrared spectrometer ISAAC, mounted at the Nasmyth B focus of VLT-U1 (Antu) until August 2009, and later at the Nasmyth A focus of VLT-U3 (Melipal) at the ESO Paranal Observatory., Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No

We present results from wide-field imaging of the resolved stellar populations of the dwarf spheroidal galaxies CassiopeiaIII (AndXXXII) and PerseusI (AndXXXIII), two satellites in the outer stellar halo of the Andromeda galaxy (M31). Our WIYN pODI photometry traces the red giant star population in each galaxy to ~2.5-3 half-light radii from the galaxy center. We use the tip of the red giant branch (TRGB) method to derive distances of (m-M)0=24.62{+/-}0.12mag (839_-45_^+48^kpc, or 156_-13_^+16^kpc from M31) for CasIII and 24.47{+/-}0.13mag (738_-45_^+48^kpc, or 351_-16_^+17^kpc from M31) for Per I. These values are consistent within the errors with TRGB distances derived from a deeper Hubble Space Telescope study of the galaxies inner regions. For each galaxy, we derive structural parameters, total magnitude, and central surface brightness. We also place upper limits on the ratio of neutral hydrogen gas mass to optical luminosity, confirming the gas-poor nature of both galaxies. We combine our data set with corresponding data for the M31 satellite galaxy LacertaI (AndXXXI) from earlier work and search for substructure within the RGB star populations of CasIII, PerI, and Lac I. We find an overdense region on the west side of Lac I at a significance level of 2.5{sigma}-3{sigma} and a low-significance filament extending in the direction of M31. In CasIII, we identify two modestly significant overdensities near the center of the galaxy and another at two half-light radii. PerI shows no evidence for substructure in its RGB star population, which may reflect this galaxy's isolated nature., "Observations of Cas III and Per I were obtained on 2013 October 2-3 and 2013 October 29-31, respectively, with the WIYN 3.5m telescope and the One Degree Imager camera with a partially filled focal plane. The field of view of the central imaging area in pODI was ~24x24', with a pixel scale of 0.11""/pixel. The galaxies were observed in the SDSS g and i filters. Several 600-700s exposures were taken of each galaxy in each filter over the course of the observing run.", Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033, No

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