Stellar population synthesis models between 2.5 and 5 {\mu}m based on the empirical IRTF stellar library

We present the first single-burst stellar population models in the infrared wavelength range between 2.5 and 5 {\mu}m which are exclusively based on empirical stellar spectra. Our models take as input 180 spectra from the stellar IRTF (Infrared Telescope Facility) library. Our final single-burst stellar population models are calculated based on two different sets of isochrones and various types of initial mass functions of different slopes, ages larger than 1 Gyr and metallicities between [Fe/H] = -0.70 and 0.26. They are made available online to the scientific community on the MILES web page. We analyse the behaviour of the Spitzer [3.6]-[4.5] colour calculated from our single stellar population models and find only slight dependences on both metallicity and age. When comparing to the colours of observed early-type galaxies, we find a good agreement for older, more massive galaxies that resemble a single-burst population. Younger, less massive and more metal-poor galaxies show redder colours with respect to our models. This mismatch can be explained by a more extended star formation history of these galaxies which includes a metal-poor or/and young population. Moreover, the colours derived from our models agree very well with most other models available in this wavelength range. We confirm that the mass-to-light ratio determined in the Spitzer [3.6] {\mu}m band changes much less as a function of both age and metallicity than in the optical bands.Comment: 25 pages, 19 figures, published in MNRAS, models can be downloaded from http://miles.iac.e

MILES extended: Stellar population synthesis models from the optical to the infrared

We present the first single-burst stellar population models which covers the optical and the infrared wavelength range between 3500 and 50000 Angstrom and which are exclusively based on empirical stellar spectra. To obtain these joint models, we combined the extended MILES models in the optical with our new infrared models that are based on the IRTF (Infrared Telescope Facility) library. The latter are available only for a limited range in terms of both age and metallicity. Our combined single-burst stellar population models were calculated for ages larger than 1 Gyr, for metallicities between [Fe/H] = -0.40 and 0.26, for initial mass functions of various types and slopes, and on the basis of two different sets of isochrones. They are available to the scientific community on the MILES web page. We checked the internal consistency of our models and compared their colour predictions to those of other models that are available in the literature. Optical and near infrared colours that are measured from our models are found to reproduce the colours well that were observed for various samples of early-type galaxies. Our models will enable a detailed analysis of the stellar populations of observed galaxies.Comment: 9 pages, 10 figures, published in A&

Single Stellar Populations in the Near-Infrared - I. Preparation of the IRTF spectral stellar library

We present a detailed study of the stars of the IRTF spectral library to understand its full extent and reliability for use with Stellar Population (SP) modeling. The library consist of 210 stars, with a total of 292 spectra, covering the wavelength range of 0.94 to 2.41 micron at a resolution R = 2000. For every star we infer the effective temperature (Teff), gravity (logg) and metallicity ([Z/Zsun]) using a full-spectrum fitting approach in a section of the K band (2.19 to 2.34 micron) and temperature-NIR colour relations. We test the flux calibration of these stars by calculating their integrated colours and comparing them with the Pickles library colour-temperature relations. We also investigate the NIR colours as a function of the calculated effective temperature and compared them in colour-colour diagrams with the Pickles library. This latter test shows a good broad-band flux calibration, important for the SP models. Finally, we measure the resolution R as a function of wavelength. We find that the resolution increases as a function of lambda from about 6 angstrom in J to 10 angstrom in the red part of the K-band. With these tests we establish that the IRTF library, the largest currently available general library of stars at intermediate resolution in the NIR, is an excellent candidate to be used in stellar population models. We present these models in the next paper of this series.Comment: 17 pages, 19 figures. Accepted for publication in Astronomy and Astrophysic

Static quantities of a neutral bilepton in the 331 model with right-handed neutrinos

A neutral vector boson can possess static electromagnetic properties provided that the associated field is no self-conjugate. This possibility is explored in the $SU_C(3) X SU_L(3) X U_N(1)$ model with right-handed neutrinos, which predicts a complex neutral gauge boson $Y^0$ in a nontrivial representation of the electroweak group. In this model the only nonvanishing form factors are the CP-even ones, which arise from both the quark and gauge sectors, and contribute to the magnetic dipole and the electric quadrupole moments of this neutral particle.Comment: 10 pages, 6 figures, submitted to Phys. Rev.

IN VIVO MEASUREMENT OF STIFFNESS AND VISCOSITY OF SURAL TRICEPS

The purpose of this study is the evaluation of the stiffness and viscosity of a particular muscle-tendon complex (MTC), the Surae Triceps (ST). The knowledge of these properties is essential for assessing and monitoring the physical condition of an athlete or sportman. A measurement procedure based on the free vibration technique, assuming that a part of the body behaves as a one degree of freedom system, has been developed to obtain the aforementioned properties. The apparent properties of MTC are obtained adjusting the experimental record of a force to a theoretical record assuming a one degree of freedom system. Assuming a Hill model for the behaviour of the muscle, the knowledge of these apparent properties leads, by a fitting procedure, to obtain the separate values of these properties for the soleus and the Achilles tendon

Characterizing stellar populations in spiral disks

It is now possible to measure detailed spectral indices for stellar populations in spiral disks. We propose to interpret these data using evolutionary synthesis models computed from the Star Formation Histories obtained from chemical evolutionary models. We find that this technique is a powerful tool to discriminate between old and young stellar populations. We show an example of the power of Integral Field spectroscopy in unveiling the spatial distribution of populations in a barred galaxy.Comment: 5 pages, to be published in "Science Perspectives for 3D Spectroscopy", Eds. M. Kissler-Patig, M.M. Roth and J.R. Walsh (Springer-Verlag, ESO astrophysics symposia series

Design and manufacture of a high-temperature PEMFC and its cooling system to power a lightweight UAV for a high altitude mission

In the present study, the optimal design of a high-temperature proton exchange membrane fuel cell (HT-PEMFC) that will be used to power an unmanned aerial vehicle (UAV) in a high altitude mission is performed. The use of PEMFCs for service ceiling above 10 km implies overcoming a number of problems caused by the harsh environmental conditions. Among them, new strategies to manage the heat generated by electrochemical reactions are needed. The maximum power required by the UAV was determined solving the aerodynamic problem, and the design of the lightweight HT-PEMFC, including its cooling system, was optimized. To perform the numerical solution of the heat transfer problem, a computational code was implemented using the EES software. The decisions adopted resulted in a 40-cells stack with an electric power above 1 kW and a weight around 3.65 kg. Besides, it is demonstrated that, for the configuration considered in the study, a passive cooling system without any additional fan system can be used to maintain the stack temperature in 160 °C

Caracterización del crecimiento y desarrollo del maíz en condiciones de no laboreo en la Mancha oriental

La biomasa es se define como la materia orgánica, viva o muerta, que se produce por un cultivo. Por medio de la metodología de los grados-día acumulados (GDA), se puede cuantificar la energía acumulada por el cultivo durante su ciclo. El objetivo de este trabajo es estudiar los principales parámetros que caracterizan el cultivo del maíz, en una parcela comercial y en condiciones de no laboreo, en una zona semiárida localizada en La Mancha Oriental. Se realizó un seguimiento fenológico durante todo el ciclo en una parcela comercial de maíz grano durante la campaña de riego del año 2015. Se recogieron muestras de plantas durante todo el ciclo del maíz. Se registraron los cambios fenológicos del cultivo siguiendo para ello la escala BBCH. Con los datos obtenidos en campo y en el laboratorio, los resultados obtenidos de Índice de Área Foliar (IAF) frente a días después de emergencia (DDE), Materia Seca (MS) frente a GDA, entre otros, fueron sometidos a un análisis estadístico descriptivo. Los resultados estadísticos indican que la MS frente a DDE presentó mejor ajuste en el modelo logístico, con un coeficiente de determinación (R2) de 0,96 y raíz del error cuadrático medio (RMSE)= 248,55 g m-2. En relación al IAF, las dos metodologías (DDE y GDA) presentaron mejor ajuste en el modelo polinomial cuadrático, con R2= 0,85 y 0,88, y RMSE= 0,88 m2 planta m-2 suelo y 0,78 m2 planta m-2 suelo, respectivamente. Se concluye que la MS y el IAF presentan comportamientos distintos en el cultivo del maíz. Con los valores de los GDA calculados, fue posible definir la duración de cada etapa del desarrollo fisiológico del maíz

Census of HII regions in NGC 6754 derived with MUSE: Constraints on the metal mixing scale

We present a study of the HII regions in the galaxy NGC 6754 from a two pointing mosaic comprising 197,637 individual spectra, using Integral Field Spectrocopy (IFS) recently acquired with the MUSE instrument during its Science Verification program. The data cover the entire galaxy out to ~2 effective radii (re ), sampling its morphological structures with unprecedented spatial resolution for a wide-field IFU. A complete census of the H ii regions limited by the atmospheric seeing conditions was derived, comprising 396 individual ionized sources. This is one of the largest and most complete catalogue of H ii regions with spectroscopic information in a single galaxy. We use this catalogue to derive the radial abundance gradient in this SBb galaxy, finding a negative gradient with a slope consistent with the characteristic value for disk galaxies recently reported. The large number of H ii regions allow us to estimate the typical mixing scale-length (rmix ~0.4 re ), which sets strong constraints on the proposed mechanisms for metal mixing in disk galaxies, like radial movements associated with bars and spiral arms, when comparing with simulations. We found evidence for an azimuthal variation of the oxygen abundance, that may be related with the radial migration. These results illustrate the unique capabilities of MUSE for the study of the enrichment mechanisms in Local Universe galaxies.Comment: 13 pages, 7 Figurs, accepted for publishing in A&