Model of the polarized foreground diffuse Galactic emissions from 33 to 353 GHz

We present 3D models of the Galactic magnetic field including regular and turbulent components, and of the distribution of matter in the Galaxy including relativistic electrons and dust grains. By integrating along the line of sight, we construct maps of the polarized Galactic synchrotron and thermal dust emissions for each of these models. We perform a likelihood analysis to compare the maps of the Ka, Q, V and W bands of the Wilkinson Microwave Anisotropy Probe (Wmap) and the 353 GHz Archeops data to the models obtained by varying the pitch angle of the regular magnetic field, the relative amplitude of the turbulent magnetic field and the extrapolation spectral indices of the synchrotron and thermal dust emissions. The best-fit parameters obtained for the different frequency bands are very similar and globally the data seem to favor a negligible isotropic turbulent magnetic field component at large angular scales (an anisotropic line-of-sight ordered component can not be studied using these data). From this study, we conclude that we are able to propose a consistent model of the polarized diffuse Galac- tic synchrotron and thermal dust emissions in the frequency range from 33 to 353 GHz, where most of the CMB studies are performed and where we expect a mixture of these two main foreground emissions. This model can be very helpful to estimate the contamination by foregrounds of the polarized CMB anisotropies, for experiments like the Planck satellite.Comment: 22 pages, 4 figure

Diseño del sistema de distribución del afluente en unidades de tratamiento de aguas residuales domésticas

The efficient treatment of domestic wastewater is associated with good operational practices in wastewater treatment plants (WWTP) and the proper design of each treatment unit, which ensures the correct hydraulic performance of each WWTP. For this reason, the objective of this article was to study the design of the multiple influent distribution systems of a high-rate primary sedimentary, a UASB (Upflow Anaerobic Sludge Blanket) reactor, and an up-flow anaerobic filter (FAFA) in the WWTPs of the municipalities of San Carlos and San Roque, and in the township of Santiago, respectively, located in Antioquia-Colombia. For this purpose, the methodology proposed by Hudson in 1981 was used to evaluate the performance of the current design and, subsequently, a pre-dimensioning was carried out to distribute the flow uniformly, to have velocities within the ranges recommended by the literature, and to obtain the total head loss generated by the distribution manifold in each treatment unit evaluated. It was found that the existing design is not efficient and that the new pre-dimensioning ensures homogeneous flow distribution and provides velocities that contribute positively to the treatment process. The study concludes that the smaller the number of orifices and the larger the pipe diameter, the more uniform the flow distribution, and that the total head loss depends on both the velocity head and the head loss coefficient. The diameter of the orifice was the predominant parameter to control the inlet velocity of the treatment units.El tratamiento eficiente de las aguas residuales domésticas está asociado a las buenas prácticas operacionales en las plantas de tratamiento de agua residual (PTAR) y al diseño adecuado de cada unidad de tratamiento, con lo cual se asegura el correcto funcionamiento hidráulico de cada PTAR. Por tal motivo, el objetivo de este artículo fue estudiar el diseño de los múltiples sistemas de distribución del afluente de un sedimentador primario de alta tasa, un reactor UASB (Upflow Anaerobic Sludge Blanket) y un filtro anaerobio de flujo ascendente (FAFA) en las PTAR de los municipios de San Carlos y San Roque, y en el corregimiento de Santiago, respectivamente, ubicados en Antioquia-Colombia. Para ello, se utilizó la metodología propuesta por Hudson en 1981 para evaluar el funcionamiento del diseño actual y, posteriormente, se realizó un predimensionamiento que permitiera distribuir el caudal uniformemente, tener velocidades dentro de los rangos recomendados por la literatura y obtener la pérdida de carga total generada por el múltiple de distribución en cada unidad de tratamiento evaluada. Se evidenció que el diseño existente no es eficiente y que el nuevo predimensionamiento asegura la distribución homogénea del caudal y proporciona velocidades que contribuyen positivamente al proceso de tratamiento. El estudio concluye que a menor número de orificios y mayor diámetro de tubería se presenta una distribución uniforme del caudal, además que la pérdida de carga total depende, tanto de la cabeza de velocidad, como del coeficiente de pérdida de carga. El diámetro del orificio fue el parámetro predominante para controlar la velocidad de entrada a las unidades de tratamiento

Corona-Australis DANCe I. Revisiting the census of stars with Gaia-DR2 data

Context. Corona-Australis is one of the nearest regions to the Sun with recent and ongoing star formation, but the current picture of its stellar (and substellar) content is not complete yet. Aims. We take advantage of the second data release of the Gaia space mission to revisit the stellar census and search for additional members of the young stellar association in Corona-Australis. Methods. We applied a probabilistic method to infer membership probabilities based on a multidimensional astrometric and photometric data set over a field of 128 deg(2) around the dark clouds of the region. Results. We identify 313 high-probability candidate members to the Corona-Australis association, 262 of which had never been reported as members before. Our sample of members covers the magnitude range between G greater than or similar to 5 mag and G less than or similar to 20 mag, and it reveals the existence of two kinematically and spatially distinct subgroups. There is a distributed "off-cloud" population of stars located in the north of the dark clouds that is twice as numerous as the historically known "on-cloud" population that is concentrated around the densest cores. By comparing the location of the stars in the HR-diagram with evolutionary models, we show that these two populations are younger than 10 Myr. Based on their infrared excess emission, we identify 28 Class II and 215 Class III stars among the sources with available infrared photometry, and we conclude that the frequency of Class II stars (i.e. "disc-bearing" stars) in the on-cloud region is twice as large as compared to the off-cloud population. The distance derived for the Corona-Australis region based on this updated census is d = 149.4(-0.4)(+0.4) pc, which exceeds previous estimates by about 20 pc. Conclusions. In this paper we provide the most complete census of stars in Corona-Australis available to date that can be confirmed with Gaia data. Furthermore, we report on the discovery of an extended and more evolved population of young stars beyond the region of the dark clouds, which was extensively surveyed in the past

Alteración de las rocas gneisicas con riebeckita del área de Vigo

[Resumen] Se estudian los factores del medio físico, procesos de alteración y cambios químicos y mineralógicos producidos en la meteorización de un grupo de rocas gneisicas de composiciónquímica heterogénea en el área de Vigo. El proceso de alteración origina una saprolita masivade textura arenosa a areno-francosa, constituida por minerales heredados (cuarzo, feldespatos, plagioclasas, micas y anfíboles), micas degradadas y minerales neoformados (caolinita, gibbsita , goethita). El proceso de meteorización es una hidrólisis ácida con pérdida de bases y silicio y enriquecimiento relativo en aluminio. Los minerales de neoformación indican un predominio de la "monosialitización" cuando el sistema presenta drenaje ralentizado y de la "alitización")en fases incipientes de la alteración}cuando el sistema no tiene materia orgánica y el drenaje es excesivo[Abstract] It has been studied the physical environmental factors, alteration processes, and chemical and mineralogical changes produced during the gneisic rocks group from Vigo area ~eathering. ln these rocks great heterogenity in the chemical composition has been found. The weathering prevailing process in the area give rise to the formation of a saprolite with sandy to sandy-loamy textures,increasing permeability and it is composed of inherited minerals :quarz, feldspars and/or plagioclases,micas, amphiboles; neoformed materials, gibbsite,caolinite,goethite and degraded micas)the last two occasionally. The weathering process is an acid hydrolysis with desbasification and Al relative enrichment tendencies. With slow drainage systems the neoformed minerals indicate a monosiallitization predominance (formation of silicates 1:1); while 1ack i ng organ i c matter and in good dra i ned zones, the neoformed minerals indicate an incipient allititatio

NIKEL_AMC: Readout electronics for the NIKA2 experiment

The New Iram Kid Arrays-2 (NIKA2) instrument has recently been installed at the IRAM 30 m telescope. NIKA2 is a state-of-art instrument dedicated to mm-wave astronomy using microwave kinetic inductance detectors (KID) as sensors. The three arrays installed in the camera, two at 1.25 mm and one at 2.05 mm, feature a total of 3300 KIDs. To instrument these large array of detectors, a specifically designed electronics, composed of 20 readout boards and hosted in three microTCA crates, has been developed. The implemented solution and the achieved performances are presented in this paper. We find that multiplexing factors of up to 400 detectors per board can be achieved with homogeneous performance across boards in real observing conditions, and a factor of more than 3 decrease in volume with respect to previous generations.Comment: 21 pages; 16 figure

Measurement of the Crab nebula polarization at 90 GHz as a calibrator for CMB experiments

CMB experiments aiming at a precise measurement of the CMB polarization, such as the Planck satellite, need a strong polarized absolute calibrator on the sky to accurately set the detectors polarization angle and the cross-polarization leakage. As the most intense polarized source in the microwave sky at angular scales of few arcminutes, the Crab nebula will be used for this purpose. Our goal was to measure the Crab nebula polarization characteristics at 90 GHz with unprecedented precision. The observations were carried out with the IRAM 30m telescope employing the correlation polarimeter XPOL and using two orthogonally polarized receivers. We processed the Stokes I, Q, and U maps from our observations in order to compute the polarization angle and linear polarization fraction. The first is almost constant in the region of maximum emission in polarization with a mean value of alpha_Sky=152.1+/-0.3 deg in equatorial coordinates, and the second is found to reach a maximum of Pi=30% for the most polarized pixels. We find that a CMB experiment having a 5 arcmin circular beam will see a mean polarization angle of alpha_Sky=149.9+/-0.2 deg and a mean polarization fraction of Pi=8.8+/-0.2%.Comment: Accepted for publication in A&A, 9 pages, 4 figure

A Characterization of the Diffuse Galactic Emissions in the Anticenter of the Galaxy

Using the Archeops and WMAP data, we perform a study of the anticenter Galactic diffuse emissions—thermal dust, synchrotron, free-free, and anomalous emissions—at degree scales. The high-frequency data are used to infer the thermal dust electromagnetic spectrum and spatial distribution allowing us to precisely subtract this component at lower frequencies. After subtraction of the thermal dust component, a mixture of standard synchrotron and free-free emissions does not account for the residuals at these low frequencies. Including the all-sky 408 MHz Haslam data we find evidence for anomalous emission with a spectral index of −2.5 in units. However, we are not able to provide coclusion regarding the nature of this anomalous emission in this region. For this purpose, data between 408 MHz and 20 GHz covering the same sky region are needed

Phytoplankton pigment distribution in the northwestern Alboran Sea and meteorological forcing: A remote sensing study

A set of weekly-composite SeaWiFS (Sea-viewing Wide Field of view Sensor) imagery (from 1998 to 2004) has been used to asses the temporal and spatial variability of the surface chlorophyll distribution in the Northwestern Alboran Sea. Empirical Orthogonal Function (EOF) analysis of the images series shows the existence of three different regions in which surface chlorophyll presents a homogeneous temporal behavior in the neighborhood of the Strait of Gibraltar.The temporal patterns of surface chlorophyll concentrations in each region have been characterized by studying the role of several forcing factors, mainly the zonal component of the wind field.The first identified region occupies the coastal area in front of Estepona and Málaga and shows the highest chlorophyll concentration in the entire region of study in absence of easterly winds. A second region is located far offshore, in the zone usually occupied by the Atlantic jet entering the Alboran Sea, showing high concentrations of chlorophyll when the easterlies blow. Finally, a third region has been situated in the normal location of the Western Alboran Gyre (WAG).The zonal wind field arises as a main forcing function in the modulation of the intensity and location of the upwelling processes in the area, while the entrance of the Atlantic jet seems to be the main agent feeding of all these processes

CCD Photometry of the Globular Cluster NGC 5897

We report CCD photometric observations of the globular cluster NGC 5897, in the Johnson system filters B, V , R, and I. With the values for these magnitudes we obtain various colour indices and produce several colour-magnitude diagrams. We present eight colour-magnitude diagrams: V vs B-V , B vs B-V , V vs V-I, I vs V-I, R vs R-I, I vs R-I, V vs V-R, and R vs V-R. In all of these diagrams we can clearly see the Giant Branch, the Horizontal Branch and the beginning of the Main Sequence. To the left of the Main Sequence turn-off point we detect a somewhat large number of Blue Straggler stars. We determine the mean value of the visual magnitude of the HB as $16.60 \pm 0.46$. This value is fainter than the value found by other authors.Comment: 28 pages, 7 figures, accepted for publication RevMexAA, vol. 60-1, April 2024. arXiv admin note: text overlap with arXiv:1606.0452

Supersymmetric FRW model and the ground state of supergravity

In this work we construct the vacuum configuration of supergravity interacting with homogeneous complex scalar matter fields. The corresponding configuration is of the FRW model invariant under the $n=2$ local conformal time supersymmetry, which is a subgroup of the four dimensional space-time supersymmetry. We show, that the potential of the scalar matter fields is a function of the K\"ahler potential and of the arbitrary parameter $\alpha$. This parameter enumerates the vacuum states. The scalar matter potential induces the spontaneous breaking of supersymmetry in supergravity. On the quantum level our model is a specific supersymmetric quantum mechanics, which admits quantum states in supergravity, and the states with zero energy are described by the wave function of the FRW universe.Comment: 18 pages, Revtex, submitted to PR