Enregistrament i masterització d'una cançó i el seu videoclip

Aquest projecte tracta, per una banda, en el mètode d’enregistrament d’una de les cançons creades per un grup de música, d’estil pop rock; i per l’altra, en el procés de pre-producció, producció i postproducció del videoclip d’aquesta cançó. La primera part inclou informació bàsica de la peça musical, el mètode d’enregistrament i els aparells i software que s’han utilitzat per fer-ho. En la segona part hi ha la documentació necessària per a poder iniciar la producció d’un videoclip: guió tècnic, guió literari,(permisos de gravació si són necessaris) i pla de rodatge. També es fa menció al codi del videoclip i la relació de ritme i motiu de llurs imatges amb la música. Finalment, hi ha els costos que comporta la creació i el manteniment d’una empresa dedicada a la producció de projectes d’aquest estil, tenint en compte la metodologia emprada en aquest projecte: de bona qualitat i, a la llarga, econòmica

Diagnosi i prevenció de complicacions trombòtiques en poltres nounats

Els poltres nounats són susceptibles de patir septicèmia, una infecció greu potencialment mortal, que pot produir hipercoagulació i microtrombes que poden generar una fallada multiorgànica. Aquesta tesi doctoral ha estudiat el paper que juga el dímer-D plasmàtic per a la realització de diagnòstics i pronòstics, així com l'ús d'heparines de baix pes molecular per prevenir els trombes.Los potros neonatos son susceptibles de sufrir septicemia, una infección grave potencialmente mortal, que puede producir hipercoagulación y microtrombos que pueden generar un fallo multiorgánico. Esta tesis doctoral ha estudiado el papel que juega el dímero-D plasmático para la realización de diagnósticos y pronósticos, así como el uso de heparinas de bajo peso molecular para prevenir los trombos.Neonate foals are susceptible to sepsis, a severe life-threatening infection which can cause hypercoagulation and microthrombi, which can generate multiple organ failure. This thesis studies the role of plasma D- dimer to perform diagnostics and prognostics, as well as the use of low molecular weight heparins to prevent thrombus

The CALIFA survey across the Hubble sequence Spatially resolved stellar population properties in galaxies

Various different physical processes contribute to the star formation and stellar mass assembly histories of galaxies. One important approach to understanding the significance of these different processes on galaxy evolution is the study of the stellar population content of today’s galaxies in a spatially resolved manner. The aim of this paper is to characterize in detail the radial structure of stellar population properties of galaxies in the nearby universe, based on a uniquely large galaxy sample, considering the quality and coverage of the data. The sample under study was drawn from the CALIFA survey and contains 300 galaxies observed with integral field spectroscopy. These cover a wide range of Hubble types, from spheroids to spiral galaxies, while stellar masses range from M? ∼ 109 to 7 × 1011 M . We apply the fossil record method based on spectral synthesis techniques to recover the following physical properties for each spatial resolution element in our target galaxies: the stellar mass surface density (µ?), stellar extinction (AV ), light-weighted and mass-weighted ages (hlog ageiL, hlog ageiM), and mass-weighted metallicity (hlog Z?iM). To study mean trends with overall galaxy properties, the individual radial profiles are stacked in seven bins of galaxy morphology (E, S0, Sa, Sb, Sbc, Sc, and Sd). We confirm that more massive galaxies are more compact, older, more metal rich, and less reddened by dust. Additionally, we find that these trends are preserved spatially with the radial distance to the nucleus. Deviations from these relations appear correlated with Hubble type: earlier types are more compact, older, and more metal rich for a given M?, which is evidence that quenching is related to morphology, but not driven by mass. Negative gradients of hlog ageiL are consistent with an inside-out growth of galaxies, with the largest hlog ageiL gradients in Sb–Sbc galaxies. Further, the mean stellar ages of disks and bulges are correlated and with disks covering a wider range of ages, and late-type spirals hosting younger disks. However, age gradients are only mildly negative or flat beyond R ∼ 2 HLR (half light radius), indicating that star formation is more uniformly distributed or that stellar migration is important at these distances. The gradients in stellar mass surface density depend mostly on stellar mass, in the sense that more massive galaxies are more centrally concentrated. Whatever sets the concentration indices of galaxies obviously depends less on quenching/morphology than on the depth of the potential well. There is a secondary correlation in the sense that at the same M? early-type galaxies have steeper gradients. The µ? gradients outside 1 HLR show no dependence on Hubble type. We find mildly negative hlog Z?iM gradients, which are shallower than predicted from models of galaxy evolution in isolation. In general, metallicity gradients depend on stellar mass, and less on morphology, hinting that metallicity is affected by both – the depth of the potential well and morphology/quenching. Thus, the largest hlog Z?iM gradients occur in Milky Way-like Sb–Sbc galaxies, and are similar to those measured above the Galactic disk. Sc spirals show flatter hlog Z?iM gradients, possibly indicating a larger contribution from secular evolution in disks. The galaxies from the sample have decreasing-outward stellar extinction; all spirals show similar radial profiles, independent from the stellar mass, but redder than E and S0. Overall, we conclude that quenching processes act in manners that are independent of mass, while metallicity and galaxy structure are influenced by mass-dependent processes.CALIFA is the first legacy survey carried out at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. We also thank the CAHA staff for the dedication to this project. Support from the Spanish Ministerio de Economía y Competitividad, through projects AYA2010-15081 (PI R.G.D.), and Junta de Andalucía FQ1580 (PI R.G.D.), AYA2010-22111-C03-03, and AYA2010-10904E (S.F.S.). We also thank the Viabilidad, Diseño, Acceso y Mejora funding program, ICTS-2009-10, for funding the data acquisition of this project. R.C.F. thanks the hospitality of the IAA and the support of CAPES and CNPq. R.G.D. acknowledges the support of CNPq (Brazil) through Programa Ciencia sem Fronteiras (401452/2012-3). A.G. acknowledges support from EU FP7/2007-2013 under grant agreement n.267251 (AstroFIt) and from the EU Marie Curie Integration Grant “SteMaGE” Nr. PCIG12-GA-2012-326466. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. E.P. acknowledges support from the Guillermo Haro program at INAOE. Support for L.G. is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. J.I.P. acknowledges financial support from the Spanish MINECO under grant AYA2010-21887- C04-01 and from Junta de Andalucía Excellence Project PEX2011-FQM7058. I.M., J.M. and A.d.O. acknowledge support from the project AYA2013-42227-P. RAM is funded by the Spanish program of International Campus of Excellence Moncloa (CEI). J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild

Unveiling the past evolution of the progenitor of the Helmi streams

Aims. We aim to determine unique features that characterise the past evolution of the progenitor of the Helmi streams through the analysis of star formation histories (SFHs). Methods. From the 5D Gaia EDR3 dataset, we extracted local samples of stars dominated by the Helmi streams, the Galactic (thick and thin) disc, and the local retrograde halo. We did this by identifying regions in a pseudo-Cartesian velocity space (obtained by setting line-of-sight velocities to zero), where stars belonging to these components, as identified in samples with 6D phase-space information, are predominantly found. We made use of an updated absolute colour-magnitude diagram (CMD) fitting methodology to contrast the SFHs of these samples to unveil distinct signatures of the past evolution of a disrupted accreted system: the Helmi streams. To this end, special attention was given to the correct characterisation of Gaia completeness effects and observational errors on the CMD. We further investigated alternative sample selections to improve the purity of our 5D Helmi stream catalogues. Results. We find that the progenitor of the Helmi streams experienced an early star formation that was sustained for longer (until 7-9 Gyr ago) than for the MilkyWay halo (10-11 Gyr ago). As a consequence, half of its stellar mass was in place similar to 0.7 Gyr later. The quenching of star formation in the Helmi stream progenitor similar to 8 Gyr ago suggests it was accreted by the Milky Way around this time, in concert with previous estimates based on the dynamics of the streams.Spinoza prize MCIN/AEI PID2020-114414GB-100 IJC2020-043742-IFundacion Jesus SerraInstituto de Astrofisica de Canaria

La Huella de Jørn Utzon

Uno de los pocos edificios modernos que ha trasladado las ideas de las compartimentaciones espaciales de la arquitectura islámica es Can Lis. Analizaremos las fuertes relaciones que existen entre Can lis y esa arquitectura, y la reinterpretación que nos devuelve Utzon de su sentido espacial

ED-2: A cold but not so narrow stellar stream crossing the solar neighbourhood

Context. ED-2 is a stellar stream identified as a compact group in integrals-of-motion space in a local sample of halo stars from the third Gaia data release. Aims. We investigate its nature and possible association with known halo substructures. Methods. We explored the current properties of ED-2 members in phase-space and also analysed the expected distribution via orbit integration. In addition, we studied the metallicity of ED-2 using APOGEE DR17 and LAMOST DR8 (and re-calibrated DR3). Results. ED-2 forms a compact group in the x − z (or R − z) plane, showing a pancake-like structure as it crosses the solar neighbourhood. Dynamically, it is most similar to the globular clusters NGC 3201 and NGC 6101 and to the stellar streams Ylgr and Phlegethon. However, its orbit is sufficiently different for none of these objects to likely be the ED-2 progenitor. We also find ED-2 to be quite metal poor: all of its stars have [Fe/H]≤ − 2.42, with a median [Fe/H] = −2.60−0.21+0.20. At this low metallicity, it is unlikely that ED-2 stems from any known globular cluster. Instead, ED-2 seems to be in a similar category as the recently discovered Phoenix and C-19 stellar streams. We find that ED-2 members are scattered across the whole sky, which is due to its current orbital phase. We predict that as this object moves to its next apocentre, it will acquire an on-sky morphology that is similar to that of cold stellar streams. Finally, because ED-2 is nearing pericentre, we predict that additional members found below the plane will have high radial velocities of close to ∼500 km s−1 in the present-day direction of the globular cluster NGC 6101.Juan de la Cierva fellowship (IJC2020-043742-I),MCIN/AEI/10.13039/501100011033European Space Agency (ESA

Systematization, accumulation and process in the work of three andalusian photographers: Clara González Ortega, Gabriel Campuzano and Juan Carlos Bracho

Este artículo pretende contribuir a los estudios sobre fotografía contemporánea. Nuestra investigación analiza métodos de fragmentación, empleados para la conformación de imágenes: sistematización, acumulación y proceso. Centramos nuestro estudio en la obra de tres artistas del ámbito andaluz: Clara González Ortega, aborda conceptos de espacio y tiempo mediante una repetición sistemática de tomas fotográficas; Gabriel Campuzano, con la idea de archivo reordena la acumulación de las imágenes fotográficas para generar un nuevo discurso; y Juan Carlos Bracho, juega con el proceso que es la conjunción de un método sistemático y de acumulación. Haciendo uso de una metodología analítico-comparativa, nuestra principal conclusión subraya que la fragmentación permite establecer nuevas estrategias de representación para la imagen.This article aims to contribute to studies on contemporary photography. We focus our attention on fragmentation methods and it is used for shaping images: systematization, accumulation and process. We focus our studio on the work of three Andalusian artists: Clara González Ortega, who deals the concepts of space and time through a systematic repetition of photographic shots; Gabriel Campuzano that works with the archive idea for reordering the accumulation of photographic images and generating a new discourse; and Juan Carlos Bracho that works with the process as the conjunction of the systematic method and accumulation. We make use of an analytical-comparative methodology, our main conclusion emphasizes that the fragmentation through the different processes allows us to approach new strategies of representation

Preferences for efficiency, rather than preferences for morality, drive cooperation in the one-shot Stag-Hunt game

Recent work highlights that cooperation in the one-shot Prisoner's dilemma (PD) is primarily driven by moral preferences for doing the right thing, rather than social preferences for equity or efficiency. To our knowledge, nothing is known on whether moral preferences affect cooperation in the Stag-Hunt Game (SHG). Cooperation in the SHG fundamentally differs from cooperation in the PD in that it is not costly, but risky: players have no temptation to deviate from the cooperative outcome, but cooperation only pays off if the other player cooperates. Here we provide data from two experiments (total N = 523) to investigate SHG cooperation. Contrary to what has been observed for the PD, we find that SHG cooperation is primarily driven by preferences for efficiency, rather than moral preferences for doing the right thing

The role of stellar radial motions in shaping galaxy surface brightness profiles

Aims. The physics driving features such as breaks observed in galaxy surface brightness (SB) profiles remains contentious. Here, we assess the importance of stellar radial motions in shaping their characteristics. Methods. We use the simulated Milky Way-mass cosmological discs from the Ramses Disc Environment Study (RaDES) to characterise the radial redistribution of stars in galaxies displaying type-I (pure exponentials), II (downbending), and III (upbending) SB profiles. We compare radial profiles of the mass fractions and the velocity dispersions of different sub-populations of stars according to their birth and current location. Results. Radial redistribution of stars is important in all galaxies regardless of their light profiles. Type-II breaks seem to be a consequence of the combined effects of outward-moving and accreted stars. The former produce shallower inner profiles (lack of stars in the inner disc) and accumulate material around the break radius and beyond, strengthening the break; the latter can weaken or even convert the break into a pure exponential. Further accretion from satellites can concentrate material in the outermost parts, leading to type-III breaks that can coexist with type-II breaks, but situated further out. Type-III galaxies would be the result of an important radial redistribution of material throughout the entire disc, as well as a concentration of accreted material in the outskirts. In addition, type-III galaxies display the most efficient radial redistribution and the largest number of accreted stars, followed by type-I and II systems, suggesting that type-I galaxies may be an intermediate case between types-II and III. In general, the velocity dispersion profiles of all galaxies tend to flatten or even increase around the locations where the breaks are found. The age and metallicity profiles are also affected, exhibiting different inner gradients depending on their SB profile, being steeper in the case of type-II systems (as found observationally). The steep type-II profiles might be inherent to their formation rather than acquired via radial redistribution