Lengua e internacionalización: el papel de la lengua en la internacionalización de las operadoras de telecomunicaciones

The analysis made to a large group of international telecom operators, reveals that, even when the disposition of an international linguistic community is not a condition for internationalization, operators have an international language of reference. This language could be considered as a conditioning factor for the area of its international expansion. At the same time, we analyze the importance of language as explanatory variable of these firms effectiveness. The results obtained suggest that the higher the number of customers speaking the operator’s language, the higher the level of effectiveness of the firm. Therefore, even when the domestic market still has a relevant role in explaining this variable, the internationalization of telecom operators within their linguistic community of reference would allow them to improve their levels of effectiveness.El análisis realizado para un amplio conjunto de operadoras mundiales de telecomunicaciones revela que, aun cuando la disposición de una comunidad lingüística internacional no es una condición previa para la internacionalización, cuando las operadoras sí disponen de una lengua internacional de referencia, está puede considerarse como un factor que condiciona la geografía de su expansión internacional. Al mismo tiempo, se analiza la importancia de la lengua como variable explicativa de la eficiencia de estas empresas. Los resultados obtenidos sugieren que cuanto mayor sea el porcentaje de clientes que hablan el idioma de una operadora, mayor tiende a ser el nivel de eficiencia mostrado por ésta. Por tanto, aun cuando el mercado nacional sigue mostrando un papel relevante en la explicación de esta variable, la internacionalización de las operadoras de telecomunicaciones dentro de su comunidad lingüística de referencia les permitiría mejorar sus niveles de eficiencia.Comunidad lingüística internacional, Internacionalización, Operadoras de telecomunicaciones

Sociedad de la Información y presencia del español en Internet

In this work an analysis has been made of the Information Society from a linguistic viewpoint, presenting the information available for three reference communities: the Spanish, the English and the French. The analysis carried out for the Spanish-speaking community clearly links the presence of Spanish on the Internet with the state in which the Information Society is to be found in countries making up this area. Nevertheless, the pre-eminence of English in this medium shows up the existence of other factors which have favoured it being considered as the lingua franca of communication. En este trabajo se ha realizado un análisis de la Sociedad de la Información desde una perspectiva lingüística, presentando la información disponible para tres comunidades de referencia: la del español, la del inglés y la del francés. El análisis llevado a cabo para la comunidad hispanohablante vincula claramente la presencia del castellano en Internet con el estadio en que se encuentra la Sociedad de la Información en los países que componen esta área. No obstante, la preeminencia del inglés en este medio pone de manifiesto la existencia de muchos otros factores que han favorecido su consideración de lengua franca de comunicación.competitiveness, FDI, high-tech, middle income countries, competitividad, IDE, alta tecnología, países de renta media

Basedat 2. Gestión de Bases de datos para la docencia

Se presentan un conjunto de 11 guías de usuario y aplicaciones didácticas. Bases de datos SABI, AMADEUS, PITEC, Encuesta Industrial, COMTRADE, OMC, TRADECAN, FDIstat, Contabilidad Nacional de España del INE, Contabilidad Nacional de Eurostat e Indicadores de Desarrollo Mundial

Constraints on the cosmic expansion history from GWTC-3

We use 47 gravitational-wave sources from the Third LIGO-Virgo-KAGRA Gravitational-Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter $H(z)$, including its current value, the Hubble constant $H_0$. Each gravitational-wave (GW) signal provides the luminosity distance to the source and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and $H(z)$. The source mass distribution displays a peak around $34\, {\rm M_\odot}$, followed by a drop-off. Assuming this mass scale does not evolve with redshift results in a $H(z)$ measurement, yielding $H_0=68^{+12}_{-7} {\rm km\,s^{-1}\,Mpc^{-1}}$ ($68\%$ credible interval) when combined with the $H_0$ measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the $H_0$ estimate from GWTC-1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of $H_0=68^{+8}_{-6} {\rm km\,s^{-1}\,Mpc^{-1}}$ with the galaxy catalog method, an improvement of 42% with respect to our GWTC-1 result and 20% with respect to recent $H_0$ studies using GWTC-2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about $H_0$) is the well-localized event GW190814

GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses

We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO’s and Virgo’s third observing run. The signal was recorded on April 12, 2019 at 05∶30∶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ∼30 M_⊙ black hole merged with a ∼8 M_⊙ black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein’s general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs

The population of merging compact binaries inferred using gravitational waves through GWTC-3

We report on the population properties of 76 compact binary mergers detected with gravitational waves below a false alarm rate of 1 per year through GWTC-3. The catalog contains three classes of binary mergers: BBH, BNS, and NSBH mergers. We infer the BNS merger rate to be between 10 $\rm{Gpc^{-3} yr^{-1}}$ and 1700 $\rm{Gpc^{-3} yr^{-1}}$ and the NSBH merger rate to be between 7.8 $\rm{Gpc^{-3}\, yr^{-1}}$ and 140 $\rm{Gpc^{-3} yr^{-1}}$ , assuming a constant rate density versus comoving volume and taking the union of 90% credible intervals for methods used in this work. Accounting for the BBH merger rate to evolve with redshift, we find the BBH merger rate to be between 17.9 $\rm{Gpc^{-3}\, yr^{-1}}$ and 44 $\rm{Gpc^{-3}\, yr^{-1}}$ at a fiducial redshift (z=0.2). We obtain a broad neutron star mass distribution extending from $1.2^{+0.1}_{-0.2} M_\odot$ to $2.0^{+0.3}_{-0.3} M_\odot$. We can confidently identify a rapid decrease in merger rate versus component mass between neutron star-like masses and black-hole-like masses, but there is no evidence that the merger rate increases again before 10 $M_\odot$. We also find the BBH mass distribution has localized over- and under-densities relative to a power law distribution. While we continue to find the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above $\sim 60 M_\odot$. The rate of BBH mergers is observed to increase with redshift at a rate proportional to $(1+z)^{\kappa}$ with $\kappa = 2.9^{+1.7}_{-1.8}$ for $z\lesssim 1$. Observed black hole spins are small, with half of spin magnitudes below $\chi_i \simeq 0.25$. We observe evidence of negative aligned spins in the population, and an increase in spin magnitude for systems with more unequal mass ratio