White dwarf-main-sequence binaries from Gaia EDR3: The unresolved 100 pc volume-limited sample

We use the data provided by the Gaia Early Data Release 3 to search for a highly-complete volume-limited sample of unresolved binaries consisting of a white dwarf and a main sequence companion (i.e. WDMS binaries) within 100 pc. We select 112 objects based on their location within the Hertzsprung-Russell diagram, of which 97 are new identifications. We fit their spectral energy distributions (SED) with a two-body fitting algorithm implemented in VOSA (Virtual Observatory SED Analyser) to derive the effective temperatures, luminosities and radii (hence surface gravities and masses) of both componentsARM acknowledges financial support from the MINECO under the Ramón y Cajal program (RYC-2016-20254). ST and ARM acknowledge support from the MINECO under the AYA2017-86274-P grant, and the AGAUR grant SGR-661/2017. ESM and FJE acknowledge financial support from the MINECO under the AYA2017-86274-P grant. FJE acknowledges support from the H2020 ESCAPE project (Grant Agreement no. 824064). LMC, LGA and AHC acknowledge support from AGENCIA through the Programa de Modernización Tecnológica BID 1728/OC-AR, and from CONICET through the PIP 2017-2019 GI grant. This publication makes use of VOSA and SVO DiscTool, developed under the Spanish Virtual Observatory project supported from the Spanish MINECO through grant AyA2017-84089. This research has made use of Aladin sky atlas developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000; Boch & Fernique 2014). TOPCAT (Taylor 2005) and STILTS (Taylor 2006) have also been widely used in this paper. We thank the anonymous referee for the helpful suggestions. The authors are greatly indebted to Detlev Koester for sharing his grid of model atmosphere white dwarf spectra. The authors also thank Roberto Raddi for sharing the grid of white dwarf absolute magnitudes calculated for the Gaia EDR3 bandpasses. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/ gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/ consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral AgreementPostprint (updated version

Estudi de síntesi poblacional de la població de nanes blanques de Gaia

We conduct a population synthesis study of the white dwarf population within 100pc from the Sun. Such simulations are based on a detailed Monte Carlo code, which provides synthetic samples of both single and binary stars for different input parameters. Synthetic outcomes are compared with observed data obtained from the recent Gaia mission in its early data release 3. In a first step we compute the outcome of the synthetic sample in the Gaia magnitude system, introduce the photometric and astrometric errors according to Gaia prescriptions and apply the corresponding selection cuts. Then we analyze the general statistical properties, such as the number-counts and percentages of the complete range of sub-populations which contain at least one white dwarf component, i.e. single and merger white dwarfs, white dwarf plus main sequence binaries, and double white dwarfs; in its two modalities, resolved and unresolved systems. The comparison between the observed and the several outcomes of the simulations are mainly based of the fractions of the different sub-samples and their distribution within the Hertzsrpung-Russell diagram. To assist the statistical analysis of observed and synthetic distributions we introduce a generalization of the Kolmogorov-Smirnov test applied to two-dimensional density distributions. Our analysis reveals that any of the models analyzed in this project perfectly agrees with the observed percentages of all the different sub-populations. However, a flat or even a decreasing initial mass ratio distribution seems to be a reasonable first guess, while an increasing relation can be discarded. Further work is needed expanding the number of models and input parameters.Realizamos un estudio de síntesis de población de la población de enanas blancas a menos de 100pcs del sol. Estas simulaciones se basan en un detallado código de Monte Carlo, que proporciona muestras sintéticas de estrellas simples y binarias para diferentes parámetros de entrada. Los resultados sintéticos se comparan con los datos observados obtenidos de la reciente misión de Gaia en su early data release 3. En un primer paso, calculamos el resultado de la muestra sintética al sistema de magnitud de Gaia, introducimos los errores fotométricos y astrométricos según las prescripciones de Gaia y aplicamos los cortes de selección correspondientes. A continuación, analizamos las propiedades estadísticas generales, como los números y porcentajes del rango completo de subpoblaciones que contienen al menos una componente de enana blanca, es decir, enanas blancas simples y de mergers, binarias de enana blanca más secuencia principal y dobles enanas blancas; en sus dos modalidades, sistemas resueltos y no resueltos. La comparación entre los resultados observados y los de las diversas simulaciones se basa principalmente en las fracciones de las diferentes submuestras y su distribución dentro del diagrama de Hertzsrpung-Russell. Para ayudar al análisis estadístico de las distribuciones observadas y sintéticas, introducimos una generalización de la prueba de Kolmogorov-Smirnov aplicada a distribuciones de densidad bidimensionales. Nuestro análisis revela que ninguno de los modelos analizados en este proyecto coincide perfectamente con los porcentajes observados de todas las diferentes subpoblaciones. Sin embargo, una relación de distribución inicial de la masa plana, o incluso una decreciente, parece ser una primera suposición razonable, mientras que se puede descartar una relación creciente. Es necesario continuar trabajando ampliando el número de modelos y parámetros de entrada.Realitzem un estudi de síntesi de població de la població de nanes blanques a menys de 100pc del Sol. Aquestes simulacions es basen en un detallat codi de Monte Carlo, que proporciona mostres sintètiques d'estrelles simples i binàries per a diferents paràmetres d'entrada. Els resultats sintètics es comparen amb les dades observades obtingudes de la recent missió de Gaia en la seu early data release 3. En un primer pas, calculem el resultat de la mostra sintètica al sistema de magnitud de Gaia, introduïm la errors fotomètrics i astromètrics segons les prescripcions de Gaia i apliquem els talls de selecció corresponents. A continuació, analitzem les propietats estadístiques generals, com ara els nombres i percentatges del rang complet de subpoblacions que contenen almenys un component de nana blanca, és a dir, nanes blanques simples i de mergers, binàries de nana blanca més seqüència principal i doble nanes blanques; en les seves dues modalitats, sistemes resolts i no resolts. La comparació entre els resultats observats i els de les diverses simulacions es basa principalment en les fraccions de les diferents submostres i la seva distribució dins del diagrama de Hertzsrpung-Russell. Per ajudar a l'anàlisi estadística de les distribucions observades i sintètiques, introduïm una generalització de la prova de Kolmogorov-Smirnov aplicada a distribucions de densitat bidimensionals. La nostra anàlisi revela que cap dels models analitzats en aquest projecte coincideix perfectament amb els percentatges observats de totes les diferents subpoblacions. No obstant això, una relació de distribució inicial de la massa plana, o fins i tot una decreixent, sembla ser una primera suposició raonable, mentre que es pot descartar una relació creixent. Es necessari continuar treballant ampliant el nombre de models i paràmetres d'entrada

Modeling and Design of a Paul Ion Trap

The aim of this project is to carry out a series of simulations of a Paul ion trap, also referred to as quadrupole ion trap, which takes advantage of the sinusoidal potential created by hyperbolic electrodes to confine charged particles. The current report includes the description of the discretization technique used to work with the main integral equations, known as Method of Moments (MoM); and the head steps made to get the final results, starting from the calculation of capacitances, the design of the hyperbolic electrodes and the calculation of the potential and electric field, and ending up with the representation of the trajectory of an ion inside the 3D trap, in addition to showing the relation between charge/mass of the particle with the characteristics of the potential2019/202

Modeling and Design of a Paul Ion Trap

The aim of this project is to carry out a series of simulations of a Paul ion trap, also referred to as quadrupole ion trap, which takes advantage of the sinusoidal potential created by hyperbolic electrodes to confine charged particles. The current report includes the description of the discretization technique used to work with the main integral equations, known as Method of Moments (MoM); and the head steps made to get the final results, starting from the calculation of capacitances, the design of the hyperbolic electrodes and the calculation of the potential and electric field, and ending up with the representation of the trajectory of an ion inside the 3D trap, in addition to showing the relation between charge/mass of the particle with the characteristics of the potential2019/202