Titulo Resumen Adjunto
OAFA: The place under the sky of the Andes that houses the MASTER

Resumen en el archivo adjunto


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SLR Latin American Network and its contribution to the ITRF 2014

Resumen en el archivo adjunto


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ESTABLISHMENT OF VLBI FOR THE MEXICAN ASTRONOMICAL GEODESICAL

The RAGN serves as a unique analytical reference framework that coordinates all the scientific and technical measuremens of the mexican country. It determines its dimensions and combined with other countries networks provides the basis to define the reference ellipsoid parameters as well as to study the Earth as a planet. The RAGN helps in the control of artificial satellites (SAT);furthermore, it provides the basis to study the deformation of the Earth´s crust in the country. The RAGN in México was developed in roughly three periods. In the first, from1915 to 1965, it was dependent on optomechanical methods of triangulation and polygonation. In the second, at the end of the 1970´s, the RAGN was adjusted to the “Transit Satellite System”. In the third epoch which started at the beginning of the 1990´s, with the help of the “Navigation Global Positional System” (NAVSTAR), the current “National Satellital Geodesic Network” (RGNS) was implemented.


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RESULTS OF PARTICIPATION OF THE ASTRONOMICAL CENTER OF THE AUTONOMOUS UNIVERSITY OF SINALOA IN THE EXPLORATION OF SPACE DEBRIS IN THE FRAME OF THE INTERNATIONAL NETWORK OF OPTICAL OBSERVATIONS (SCIENTIFIC NETWORK OF OPTICAL INSTRUMENTS FOR ASTROMETRIC AND PHOTOMETRIC OBSERVATIONS)

The astronomical center of the Autonomous University of Sinaloa (AUS) continues working. Near Cosala at altitude of 600 m the astronomical observatory takes active part in observations of international network ISON. In the astronomical pavilion with the movable roof 25-cm telescope ORI-25 started working in May, 2012. During 5 years the observations were made for 760 nights, 925 348 measurements. The astronomical center studied of space debris and satellites in high orbit. The Astronomical Center carried out detecting 17 not-cataloged objects. In work progress 23 lost objects were detected. Obtained measurements are supplied to the database of Keldysh Institute of Applied Mathematics Russian Academy of Sciences for prediction of dangerous proximities with satellites.


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Membership determination in globular clusters with GaiaDR2 astrometry

En este trabajo se presenta un método, aún en desarrollo, para identificar posibles miembros de cúmulos globulares con datos del Catálogo de GaiaDR2. El método se basa en un algoritmo de clustering aplicado en un espacio 4D determinado básicamente por las posiciones en el cielo y los movimientos propios. Para confirmar si los agrupamientos encontrados automáticamente por el método corresponden a cúmulos globulares se analizan los diagramas color-magnitud. Se muestran los resultados obtenidos en algunos cúmulos y se compara con otros autores. In this work we present a method -still under development- to identify possible members of globular clusters using data from GaiaDR2. The method is based on a clustering algorithm applied on a 4D space that is determined basically by the positions on the sky and the proper motions. In order to confirm that the clusters automatically detected by the method correspond to actual globular clusters, the colour-magnitude diagrams are analysed. We show the results for some clusters and we compare them with other authors.


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The variable stars of Clement Catalogue in some southern Globular Clusters using Gaia DR2

En este trabajo se estudia la identificación y pertenencia a cúmulos de las estrellas variables del Catalogue of Variable Stars in Galactic Globular Clusters de Christine Clement usando GaiaDR2. Se aborda el problema de la identificación cruzada. Se presentan resultados preliminares correspondientes a los cúmulos australes NGC 6397, NGC 6352 y NGC 3201. In this work we study the identification and membership to clusters of the stars in the Catalogue of Variable Stars in Galactic Globular Clusters by Christine Clement, using GaiaDR2. We discuss the issue of cross identification. We show preliminary results corresponding to the southern clusters NGC 6397, NGC 6352 and NGC 3201.


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Planetary-Nebulae / Open-Clusters associations

To date, distances to individual Planetary Nebuale (PNe) have shown to be difficult to establish. Determining real associations between open clusters (OCs) and PNe can provide an accuracy distance as well as important constraints for their fundamental properties. Unfortunately, the number of Galactic PNe that are members of star clusters is quite small. Nowadays, just four association PN/OC have been confirmed in open clusters. In this work, we will present the first of a series of works aimed to assess membership among some PNe lying in the line of sight of OPs. More specifically, we have assessed the discussed membership of the PN NGC 2452 in OP NGC 2453 via radial velocity on intermediate-resolution spectra. This pair PN/OC has shown to be hard becasue the line of sight in which they lie are highly contaminated for field stars belonging to Puppis OB associations and Perseus arm. Additional deep UBVRI photometry and data of the Gaia\'s second Data Release (DR2) were acquired to establish more accurately the fundamental parameters of the cluster as distance, proper motion, reddening and age. We conclude finally that NGC 2452 is not a member of NGC 2453, but a most likely member of the Galaxy Arm.


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CHARACTERIZATION OF SYSTEMATIC ERRORS ON SPACE DEBRIS ASTRONOMICAL COORDINATES OBTAINED FROM THE 1-M REFLECTOR AT OAN-VENEZUELA

Optical systems as well as atmospheric refraction are known to introduce non-negligible random and sys- tematic errors on astronomical coordinates. We aim to characterize such systematic errors or distorsions, including the contribution of atmospheric refraction at different zenith distances, using overlapping ob- servations taken along the Celestial Equator and the local meridian. We hope to improve the obtained astronomical coordinates, in particular for space de- bris objects on which this error reduction translate into a significantly more precise geocentric position, given their proximity to Earth. By correcting for the aforementioned distortions, we also hope to reach the precision limit of the optical system being used, in this case the 1-m Reflector telescope at Llano del Hato Observatory (MPC 303) in Venezuela. We ap- ply this procedure in the observation of space debris located at the Laplace plane.


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Orbit determination based on sun sensor and magnetometer for nanosatellite applications

Increasing capabilities of nanosatellite (1Kg to 10Kg) applications in Low Earth Orbit (LEO) demand robust and reliable methods for orbit determination, typical implementations such as SGP4 propagators may result in significant errors over long periods of time, while using a GNSS receiver on board can result in more precise positioning of the satellite, the small volume, mass restriction and low power budget of a nanosatellite platform often make the implementation of a GNSS receiver unfeasible. Another alternative is the method described in this work, it uses the data collected from two sensors for attitude determination in an algorithm based on an Extended Kalman Filter (EKF), the measurements are from the magnetometer and sun sensors which are found in every nanosatellite platform. The algorithm is tested with simulations using the CelestLab library for space mechanics in the Scilab environment; the results show that this method may serve as a complementary orbit determination system to the standard use of TLE sets and SGP4 propagation to increase reliability in nanosatellite missions.


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Actividades de divulgación en Astronomía y Ciencias Espaciales - Bolivia.

Actividades de divulgación en Astronomía y Ciencias Espaciales - Bolivia


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