Original article can be found at: http://www.iop.org/EJ/journal/1538-3881 Copyright American Astronomical Society. DOI: 10.1088/0004-6256/137/6/4670 [Full text of this article is not available in the UHRA]

HERACLES: The HERA CO-Line Extragalactic Survey

We have compiled high-resolution position-velocity diagrams observed along the major axes of nearby spiral galaxies in the CO-line emission, and derived rotation curves for the inner regions of the galaxies. We have combined the inner rotation curves with the outer HI and optical rotation curves to obtain the total rotation curves. The inner rotation curves are characterized by a steep increase within a few hundred pc radius, indicating a compact massive concentration near the nucleus. We fit the obtained rotation curves for individual galaxies by a modified Miyamoto-Nagai's potential by assuming existence of four mass components; a nuclear mass component with a scale radius of 100-150 pc and a mass of $\sim 3-5\times 10^{9}Msun$; a central bulge of 0.5 to 1 kpc radius of a mass $\sim 10^{10}Msun$; a disk with scale radius 5 to 7 kpc and thickness 0.5 kpc of a mass $\sim 1-2 Mgal$; and a massive halo of scale radius 15 to 20 kpc with a mass $\sim 2-3 Mgal$. We discuss the implication of the nuclear compact mass component for the formation mechanism of multiple structures within the galactic bulge during its formation.

The Most Completely Sampled Rotation Curves for Galaxies

In this paper we present the detailed formalism at the core of the Spectral Line Identification and Modelling (SLIM) within the MAdrid Data CUBe Analysis (MADCUBA) package and their main data handling functionalities. These tools have been developed to visualize, analyze and model large spectroscopic data cubes. We present the highly interactive on-the-fly visualization and modelling tools of MADCUBA and SLIM, which includes an stand-alone spectroscopic database. The parameters stored therein are used to solve the full radiative transfer equation under Local Thermodynamic Equilibrium (LTE). SLIM provides tools to generate synthetic LTE model spectra based on input physical parameters of column density, excitation temperature, velocity, line width and source size. SLIM also provides an automatic fitting algorithm to obtain the physical parameters (with their associated errors) better fitting the observations. Synthetic spectra can be overlayed in the data cubes/spectra to easy the task of multi-molecular line identification and modelling.We present the Java-based MADCUBA and its internal module SLIM packages which provide all the necessary tools for manipulation and analysis of spectroscopic data cubes. We describe in detail the spectroscopic fitting equations and make use of this tool to explore the breaking conditions and implicit errors of commonly used approximations in the literature. Easy-to-use tools like MADCUBA allow the users to derive the physical information from spectroscopic data without the need of resourcing to simple approximations. SLIM allows to use the full radiative transfer equation, and to interactively explore the space of physical parameters and associated uncertainties from observational data.

/pdf/spectral-line-identification-and-modelling-slim-in-the-25e4mdjby6.pdf

Spectral Line Identification and Modelling (SLIM) in the MAdrid Data CUBe Analysis (MADCUBA) package: An interactive software for data cube analysis

Context. The increase in bandwidth and sensitivity of state-of-the-art radio observatories is providing a wealth of molecular data from nearby star-forming regions up to high-z galaxies. Analysing large data sets of spectral cubes requires efficient and user-friendly tools optimised for astronomers with a wide range of backgrounds.Aims. In this paper we present the detailed formalism at the core of Spectral Line Identification and Modelling (SLIM) within the MAdrid Data CUBe Analysis (MADCUBA) package and their main data-handling functionalities. These tools have been developed to visualise, analyse, and model large spectroscopic data cubes.Methods. We present the highly interactive on-the-fly visualisation and modelling tools of MADCUBA and SLIM, which includes a stand-alone spectroscopic database. The parameters stored therein are used to solve the full radiative transfer equation under local thermodynamic equilibrium (LTE). The SLIM package provides tools to generate synthetic LTE model spectra based on input physical parameters of column density, excitation temperature, velocity, line width, and source size. It also provides an automatic fitting algorithm to obtain the physical parameters (with their associated errors) better fitting the observations. Synthetic spectra can be overlayed in the data cubes/spectra to ease the task of multi-molecular line identification and modelling.Results. We present the Java-based MADCUBA and its internal module SLIM packages which provide all the necessary tools for manipulation and analysis of spectroscopic data cubes. We describe in detail the spectroscopic fitting equations and make use of this tool to explore the breaking conditions and implicit errors of commonly used approximations in the literature.Conclusions. Easy-to-use tools like MADCUBA allow users to derive physical information from spectroscopic data without the need for simple approximations. The SLIM tool allows the full radiative transfer equation to be used, and to interactively explore the space of physical parameters and associated uncertainties from observational data.

/pdf/spectral-line-identification-and-modelling-slim-in-the-19zxk0xbm1.pdf

Spectral Line Identification and Modelling (SLIM) in the MAdrid Data CUBe Analysis (MADCUBA) package: Interactive software for data cube analysis

The quest for a B-mode imprint from primordial gravity waves on the polarization of the cosmic microwave background (CMB) requires the characterization of foreground polarization from Galactic dust. We present a statistical study of the filamentary structure of the 353 GHz Planck Stokes maps at high Galactic latitude, relevant to the study of dust emission as a polarized foreground to the CMB. We filter the intensity and polarization maps to isolate filaments in the range of angular scales where the power asymmetry between E-modes and B-modes is observed. Using the Smoothed Hessian Major Axis Filament Finder (SMAFF), we identify 259 filaments at high Galactic latitude, with lengths larger or equal to 2° (corresponding to 3.5 pc in length for a typical distance of 100 pc). Thesefilaments show a preferred orientation parallel to the magnetic field projected onto the plane of the sky, derived from their polarization angles. We present mean maps of the filaments in Stokes I, Q, U, E, and B, computed by stacking individual images rotated to align the orientations of the filaments. Combining the stacked images and the histogram of relative orientations, we estimate the mean polarization fraction of the filaments to be 11%. Furthermore, we show that the correlation between the filaments and the magnetic field orientations may account for the E and B asymmetry and the ClTE/ClEE ratio, reported in the power spectra analysis of the Planck353 GHz polarization maps. Future models of the dust foreground for CMB polarization studies will need to take into account the observed correlation between the dust polarization and the structure of interstellar matter.

/pdf/planck-intermediate-results-xxxviii-e-and-b-modes-of-dust-56krfucm3x.pdf

Planck intermediate results: XXXVIII. E- and B-modes of dust polarization from the magnetized filamentary structure of the interstellar medium

Fil: Acena, Andres Esteban. Escuela Politecnica Nacional; Ecuador. Universidad Nacional de Cuyo. Facultad de Ciencias Exactas y Naturales; Argentina. Consejo Nacional de Investigaciones Cientificas y Tecnicas; Argentina

Isoperimetric surfaces and area-angular momentum inequality in a rotating black hole in new massive gravity

We use observations of the neutral atomic hydrogen (HI) 21-cm emission line to study the spatial distribution of the HI gas in a 80$\degree\times~$90$\degree$ region of the Galaxy halo. The HI column densities in the range of \mbox{3--11$\times$10$^{20}$ cm$^{-2}$} have been estimated for some of the studied regions. In our map---obtained with a spectral sensitivity of $\sim$2 K---we do not detect any HI 21-cm emission line {above 2$\sigma$} at Galactic latitudes higher than $\sim${46}$\degree$. {This report summarizes our contribution presented at the conference on the origin and evolution of barionic Galaxy halos}.

The HI Distribution Observed toward a Halo Region of the Milky Way

Resume Des etudes recentes ont montre que les variants genetiques, impliques dans l'inegalite face au risque infectieux, concernaient les genes de proteines impliquees soit dans la reconnaissance de l'agent infectieux, soit dans la cascade inflammatoire, soit dans le domaine de la coagulation. Par exemple, des etudes ont clairement demontre qu'en cas d'atteinte du premier jumeau par une pathologie infectieuse, le risque d'atteinte par le meme pathogene du second jumeau etait significativement superieur chez les jumeaux homozygotes que chez les jumeaux heterozygotes. Il a ete mis en evidence chez les caucasiens une mutation ponctuelle du domaine cytosolique de TLR2 bloquant la reponse aux lipoproteines bacteriennes et a certaines bacteries Gram positif et qui pourrait etre responsable d'une plus grande susceptibilite au choc septique. Plusieurs polymorphismes du gene tlr4 ont ete associes a la survenue de chocs septiques, d'infections postoperatoires a bacilles Gram negatif. De facon paradoxale ces variants semblent proteger contre la legionellose. En pediatrie, des polymorphismes de tlr4 ont egalement ete clairement identifies comme facteurs de risque de survenue de meningococcemies de bronchiolites severes a virus respiratoire syncytial (VRS) chez les enfants de moins de deux ans. Un polymorphisme du gene du recepteur TLR5, qui cree un codon stop et qui est responsable d'une non-fonctionnalite du recepteur a ete associe a la survenue de legionellose grave. L'analyse du role de ces polymorphismes genetiques dans la genese du sepsis ouvre un grand nombre de voies de recherches therapeutiques specifiques, ciblees sur l'anomalie genetique.

Polymorphismes génétiques et infections

Observable radiation contains information on its'source as well as on the medium through which it has propagated. Measuring the angular broadening suffered by crossing radiation through any magnetoactive plasma, it is possible to obtain important conclusions about the physical plasma parameters, such as the electron density distribution, magnetic field and macroscopic plasma velocity. In this work we describe the physical picture for propagation of the electromagnetic waves in the magnetoactive plasma, taking into account the macroscopic velocity of the system. In moving magnetoactive plasma, the relations for the dielectric permittivity tensor, the dispersion equations and the refractive indexes are established. These results can be evaluated, for example, by the determination of the angular displacement of the radiation coming to us from far radio sources, after passing through solar corona and solar wind plasmas.

Dispersion of electromagnetic waves in active moving plasma

The Magnetic Data Acquisition System (MAGDAS) was installed in the protected Jerusalem Park in Malchingui- Ecuador in October of 2012, under the joint collaboration between Kyushu University of Japan and the Quito Astronomical Observatory of the National Polytechnic School of Ecuador. In this paper, we describe the installation process and present the preliminary data obtained with the MAGDAS equipment. The behavior of the four components, D, H, Z and F allow us to see the importance of having the Ecuador station where the magnetic field has not been systematically measured before, in valuable contribution to study the equatorial electrodynamics.

/pdf/first-magdas-equipment-in-ecuador-35a6nhxy1q.pdf

First magdas equipment in ecuador

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