Estudio por espectroscopia Raman-IR del estado de orden en materia carbonosa

La espectroscopia Raman es una técnica analítica no destructiva y no intrusiva recientemente introducida en el estudio de la paleobiología. En esta línea se pretende emplear está técnica en el estudio de la posible vida en Marte y en el estudio de la vida en la Tierra. El empleo de la espectroscopia micro Raman nos permite analizar en detalle las muestras a la escala típica del grano mineral. La espectroscopia Raman muestra la información vibracional de los grupos moleculares y su ordenamiento cristalin odentro de los sólidos,por tanto, de los espectros podremos deducir composición, grado de cristalinidad, fases presentes de un mismo elemento etc. En este caso se ha aplicado la técnica al estudio del estado de orden de la materia carbonosa. Se han podido mostrar parámetros que permitan identificar los procesos de maduración de las estructuras del carbono, así como métodos de diferenciación de tipos de carbones. Para ello, se ha obtenido la información de los espectros mediante selección y ajuste de bandas. Se ha realizado un análisis detallado de las características de las bandas presentes en el espectro. Esto nos permite inferir patrones de diferenciación entre los diversos alótropos del carbono con fases amorfas, denotados genéricamente como carbones. El objetivo es realizar ciencia de soporte para el instrumento RLS desarrollado en la Unidad Asociada UVa-CSIC que pertenece a la misión ExoMars. Dentro del mismo programa, se desarrolló un automuestreador que simula las condiciones de operación del instrumento que debe viajar a Marte. Con el objetivo de sacar el máximo partido del instrumento una vez en Marte, se ha realizado un análisis de la materia carbonosa de forma automática empleando dicho simulador.Grado en Físic

Primeras luces de un espectroscopio impreso en 3D

La espectroscopía aplicada a la astronomía es una de las técnicas más potentes que tenemos para poder estudiar la naturaleza física de los astros. Esta técnica nos ha permitido, entre otras cosas, poder determinar la composición química de las fotosferas estelares, la detección de exoplanetas y es la técnica que nos ha permitido poder medir la expansión del universo. Al tratarse de una técnica tan potente los miembros del Grupo Universitario de Astronomía decidimos iniciarnos en esta técnica

The wide-field, multiplexed, spectroscopic facility WEAVE : survey design, overview, and simulated implementation

Funding for the WEAVE facility has been provided by UKRI STFC, the University of Oxford, NOVA, NWO, Instituto de Astrofísica de Canarias (IAC), the Isaac Newton Group partners (STFC, NWO, and Spain, led by the IAC), INAF, CNRS-INSU, the Observatoire de Paris, Région Île-de-France, CONCYT through INAOE, Konkoly Observatory (CSFK), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Lund University, the Leibniz Institute for Astrophysics Potsdam (AIP), the Swedish Research Council, the European Commission, and the University of Pennsylvania.WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366-959 nm at R ∼ 5000, or two shorter ranges at R ∼ 20,000. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for ∼ 3 million stars and detailed abundances for ∼ 1.5 million brighter field and open-cluster stars; (ii) survey ∼ 0.4 million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey  ∼ 400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in z 1 million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.PostprintPeer reviewe

The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366$-$959\,nm at $R\sim5000$, or two shorter ranges at $R\sim20\,000$. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for $\sim$3 million stars and detailed abundances for $\sim1.5$ million brighter field and open-cluster stars; (ii) survey $\sim0.4$ million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey $\sim400$ neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in $z<0.5$ cluster galaxies; (vi) survey stellar populations and kinematics in $\sim25\,000$ field galaxies at $0.3\lesssim z \lesssim 0.7$; (vii) study the cosmic evolution of accretion and star formation using $>1$ million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at $z>2$. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.Comment: 41 pages, 27 figures, accepted for publication by MNRA

The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366−959\,nm at R∼5000, or two shorter ranges at R∼20000. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for ∼3 million stars and detailed abundances for ∼1.5 million brighter field and open-cluster stars; (ii) survey ∼0.4 million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey ∼400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in z1 million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at z>2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator

Synergies between Gaia Data Release 2 and OCCASO survey in the study of Open Clusters

Galactic Open Clusters (OCs) are crucial to investigate the formation and evolution of the Galactic disc. The Open Clusters Chemical Abundance from Spanish Observatory survey (OCCASO) aims to provide high precision radial velocity (typical uncertainties between 100 to 200 m/s) and to determine abundances for more than 20 chemical species in around 30 Northern OCs (Casamiquela et al, 2016). We use high resolution (R > 65,000) high signal-to-noise (˜70) spectra of at least 6 Red Clump stars for each cluster. In this work we combined Gaia DR2 mean parallaxes and proper motions, and OCCASO radial velocities to obtain 3D spatial velocities and determine the orbits of the clusters. We also study Galactic trends with Galactocentric radius and age of Fe peak and alpha elements for the 18 OCs currently observed in the OCCASO survey, and we compare them with chemo-dynamical models of the Milky Way