Pósters

1. (1B) Aguiar González, Marta (Instituto de Astrofísica de Canarias)
Arquitectura del Sistema de Control de QUIJOTE (MFI)
Autores: – Maria F. Gómez Reñasco – Marta Aguiar González – José Miguel Herreros Linares – Roger J. Hoyland – Vicente Sánchez de la Rosa – Afrodisio Vega Moreno – Teodora Viera Curbelo – Ricardo Génova Santos – Carlos López Caraballo – Rafael Rebolo López

Q-U-I JOint Tenerife-CMB es un sistema formado por dos telescopios y varios instrumentos destinados a caracterizar la polarización del fondo cósmico de microondas. Actualmente se encuentran en operación uno de los telescopios y el primer instrumento. El instrumento es multicanal y consiste en cinco polarizadores funcionando a diferentes frecuencias. El telescopio el del tipo altacimutal con varios modos de operación. En esta comunicación se presenta la arquitectura del sistema de control de ambos, telescopio e instrumento, que está basada en las tecnologías LXI-VXI y EtherCAT sobre las que se implementa el software de PLCs desarrollado en TwinCAT. La interfaz de usuario está desarrollada en LabView.
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2. (1C) Aivar Mateo, Jesús (LIDAX)
Cryogenic Space Mechanisms: Fourier Transform Scanning Mechanism For SAFARI/SPICA
Autores: J. Serrano-Tellez, M. Lamensans, F. Romera-Juarez, D. Gonzalez-de-Maria, H. Argelaguet-Vilaseca, LIDAX (Spain); J. Pérez-Díaz, E. Díez-Jiménez, J. Sánchez-Casarrubios, I. ValienteBlanco, Univ. Carlos III de Madrid (Spain)

LIDAX is a Space Technological SME dedicated to engineering, construction, integration and testing of Space Advanced Mechanical Equipments that forms part of complex Space Flight Systems and Instruments, such as: Opto-Mechanical Systems, High Accuracy Positioning Systems under Vacuum, Cryogenic and Radiation Environment, MGSE and OGSE. New instruments for space use have brought about the need to bypass cryogenic tribology issues and develop superconductive magnetic levitation positioning systems for optical components with high precision, stability and repeatability. While tribilogy concerns such as cold-welding, dry-lubrication wear and metal fatigue are removed, the testing of such systems on-ground requires a set of mechanisms (actuators, sensors) which are bound by standard design and must be re-thought and validated for cryogenic use. LIDAX and UC3M have designed a controllable non-contact linear slider for cryogenic temperature based on superconducting magnetic levitation, and have built and optically tested a prototype in order to measure and characterize its performances. The prototype consists of a magnet with a controllable levitation over type II superconductor disks. This control is carried out by applying continuous current to 4 electromagnets. The tests have been realized with the prototype inside a Cryostat cooled down to 12 Kelvin and the measurements have been taken by means of optical methods using interferometers and autocollimators.
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3. (2B) Alonso Floriano, Francisco Javier (Universidad Complutense de Madrid)
CARMENES. Low-resolution spectroscopy of M dwarfs with CAFOS at Calar Alto
Autores: F. J. Alonso-Floriano, J. A. Caballero, D. Montes, A. Klutsch, R. Mundt, et al.

We conduct long observational campaigns with CAFOS at the 2.2. m Calar Alto telescope to obtain low-resolution (R~1500) spectra of poorly-known M dwarfs and candidates that are bright enough to be considered potential CARMENES targets. We perform a spectral-type classification of the targets by comparing their acquired spectra with those of spectral-type standard stars observed during the same observing runs, and using spectral indices well calibrated for M dwarfs, such as TiO5, CaH2 and CaH3. We also measure chromospheric activity indicators. Up to now, over 400 M dwarfs have been observed and analysed, many of which had not been spectroscopically investigated yet.
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4. (3B) Arrillaga, Xabier (AVS)
MEGARA Multi-Object Spectroscopy robotic positioners
Autores: Xabier Arrillaga, Arkaitz Larman, Eider Ocerin, Miguel Angel Carrera

MEGARA (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía) es una IFU(optical Integral Unit) y un espectrógrafo multiobjeto(MOS) diseñado para el telescopio de 10.4m de GTC en La Palma.El modo IFU de MEGARA ofrecerá dos diferentes mazos de fibra óptica, una cubriendo 12.5” x 11.3” con un tamaño de spaxel de 0.62”((Large Compact Bundle; LCB) y otro cubriendo 8.5” x 6.7” con una tamaño de spaxel de 0.42” (Small Compact Bundle; SCB).El MOS de MEGARA permitirá observas hasta 100 obtejos en una región de 3.5’ x 3.5’ alrededor de las dos IFUs. 8 de los mazos del MOS se utilizarán para la determinación del cielo durante la observación con la LCB. Cada posicionador del MOS posiciona mazos de 7 fibras(0.62”/fibra) cubriendo 1.6″ en el cielo.la LCB IFU y el MOS de MEGARA proporcionarán una resolución espectral intermedia-alta(R~6000, 11000 and 18700).Con el SCB, MEGARA se eleva a R~21500 Dentro de la contribución de AVS en el instrumento de MEGARA, cabe destacar el desarrollo de los posicionadores que componen el MOS y el adaptador del MOS sobre rotador Folded Cassegrain.Los posicionadores de fibras obticas son subsistemas que requieren una elevada precisión de posicionado para el tamaño reducido de los mismos y que posicionan los mazos en un area de 23.21mm de diametro con una precisión de +/-25 micras.El adaptador del rotador cumple funciones estructurales, posicionado y de gestión de todos los mazos de fibra en la parte posterior del plano focal.
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5. (1A) Barrio, Juan Abel (Universidad Complutense de Madrid)
An Analog Trigger System for Atmospheric Cherenkov Telescope Arrays
Autores: M. Barcelo et al., for the CTA consortium

Arrays of Cherenkov telescopes typically use multi-level trigger schemes to keep the rate of random triggers from the night sky background low. At a first stage, individual telescopes produce a trigger signal from the pixel information in the telescope camera. The final event trigger is then formed by combining trigger signals from several telescopes. In this poster, we present a possible scheme for the Cherenkov Telescope Array (CTA) telescope trigger, which is based on the analog pulse information of the pixels in a telescope camera. Advanced versions of all components of the system have been produced and working prototypes have been tested, showing a performance that meets the original specifications. Finally, issues related to integrating the trigger system in a telescope camera and in the whole array will be dealt with
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6. (4B) Bouy, Herve (CAB CSIC)
Mining the astronomical archives
Autores: H. Bouy & E. Bertin

Most astronomical observatories now share their data through public archives. The quality and the quantity of wide field images in public archives now allows large scale studies taking advantage of not only the spatial and wavelength domains, but also of the time domain. Some of these archives indeed include data obtained 10 or sometimes 20 years ago, offering unique possibilities for the study of transient astronomy, long term evolution of astronomical objects (motions and/or variability), or pre-covery (solar system bodies, supernovae,…). In the context of the DANCe project, we have developed a set of tools to: 1) automatically process large amounts (Tb) of images; 2) perform semi-automatic control quality assessing the usability of the images; 3) derive precise photometric and astrometric solutions for tens of thousands of overlapping images 4) produce VO compliant multi-million-source catalogues including the multi-wavelength, multi-epoch photometry and astrometry. A number of astronomical facilities accessible to the Spanish community at the OR and CAHA were included in the current analysis.
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7. (2A) Bueno, Alberto (IAC)
Preóptica de HARMONI
Autores: Alberto Bueno, Jorge Sánchez-Capuchino.

Se muestra el diseño de todo el sistema de preóptica que alimentará a este instrumento de primera luz en el E-ELT.
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8. (5B) Caballero, Jose A. (CAB)
CARMENES. Preparation of the best target sample from Spain and Chile
Autores: Caballero, Montes, Ribas, Amado and the CARMENES Science Working Group

The CARMENES Science Working Group, which contains research staff members, post-docs and PhD students from Spain (UCM, IAA, ICE, IAC and CAB) and Germany (IAG, MPIA, LSW, HS and TLS), is preparing the best input catalogue for the CARMENES exoplanet survey. Hundreds of stars are being thoroughly investigated with CAFOS/2.2m Calar Alto (low-resolution spectroscopy), TCP/IAC80 (low-resolution imaging), CAFE/2.2m Calar Alto, FEROS/2.2m La Silla and HRS/Hobby Eberly Telescope (high-resolution spectroscopy), and FastCam/TCS (high-resolution imaging), among which we will choose the 300 brightest, latest, single M dwarfs with the lowest rotational velocities. Eventually, all these preparatory-science data will be public as a CARMENES legacy.
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9. (6B) Carrasco Licea, Esperanza (INAOE)
MEGARA Optics Manufacturing at INAOE and CIO
Autores: Carrasco Licea, Esperanza; Páez, Gonzalo; García-Vargas, María Luisa (FRACTAL); Sánchez-Blanco, Ernesto (FRACTAL); Gil de Paz, Armando (UCM); Gallego Maestro, Jesús (UCM); Vilchez Medina, José Manuel (IAA); Iglesias Páramo, Jorge (IAA), Sánchez F.M (UPM)

We describe the Optics Manufacturing plan and status for MEGARA, the next optical Integral Field Unit (IFU) and Multi-Object Spectrograph (MOS) for the 10.4-m Gran Telescopio CANARIAS (GTC). INAOE is part of MEGARA Consortium and it is in charge of the Optics Manufacturing work package. MEGARA passed the Optics Detailed Design Review in May 2013, and some of the blanks have been already ordered, being in the point of starting the Optics manufacturing phase. Except for the optical fibers and microlenses (manufactured in Europe), the complete MEGARA optical system will be manufactured in Mexico, between the workshops of CIO and INAOE. This implies a field lens, a 5-lenses collimator, a 7-lenses camera and a complete set of VPHs with 36 flat windows and 24 prisms, being all these elements very large and complex. Additionally, the optical tests and the complete assembly of the camera and collimator subsystems will be carried out in Mexico. The poster describes the progress and the plan to complete this work.
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10. (7B) Castillo-Morales, África (Universidad Complutense de Madrid)
MEGARA Control System
Autores: A. Castillo-Morales, B. Lefort, M. C. Eliche-Moral, S. Pascual, V. Villar, I. Morales, E. González, R. A. Marino, J. Gallego, N. Cardiel, F. Sánchez, J. Vílchez, J. Iglesias, A. Gil de Paz and MEGARA Team.

MEGARA (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía) is an optical Integral-Field Unit (IFU) and Multi-Object Spectrograph (MOS) designed for the GTC 10.4m telescope in La Palma. In this poster we will show the state of the MEGARA Control System which will provide the capabilities to move the different mechanisms of the instrument, to readout the data from the detector controller and the necessary routines for the Inspector Panels, the MEGARA Observing Preparation Software Suite (MOPSS) , the Data Factory and the Sequencer strategies.
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11. (2A) Colomé, Josep (ICE(IEEC/CSIC))
Artificial Intelligence for the CTA Observatory Scheduler
Autores: J.Colomé (IEEC/CSIC), P.Colomer (GTD), J.Campreciós (IEEC/CSIC), T.Coiffard (GTD)

The Cherenkov Telescope Array (CTA) project will be the next generation ground-based very high energy gamma-ray instrument. CTA will consist of two arrays of Cherenkov telescopes operated as a proposal-driven open observatory. It will handle several observation modes and will have to operate tens of telescopes with a highly efficient and reliable control. Thus, the CTA planning tool is a key element in the control layer for the optimization of the observatory time. The main purpose of the scheduler for CTA is the allocation of multiple tasks to one single array or to multiple sub-arrays of telescopes, while maximizing the scientific return of the facility and minimizing the operational costs. The scheduler considers long- and short-term varying conditions to optimize the prioritization of tasks. We describe the scheduler prototype that is based on Artificial Intelligence techniques. In particular, it uses Guarded Discrete Stochastic Neural Network and Constraint Propagation to obtain different long-term solutions from the search space. Afterwards, the most efficient solution is selected to be processed by the short-term scheduler, which is based on an Ant Colony Optimization algorithm that re-schedules the tasks depending on different notifications (i.e., change on weather conditions) received from the array control system.
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12. (8B) Colomé, Josep (ICE(IEEC/CSIC))
CARMENES Instrument Control System and Scheduler
Autores: Josep Guàrdia (IEEC/CSIC), Josep Colomé (IEEC/CSIC), Ignasi Ribas (IEEC/CSIC), and the CARMENES Consortium

The overall purpose of the CARMENES instrument is to perform high-precision measurements of radial velocities of late-type stars with long-term stability. CARMENES will be installed in 2015 at the 3.5 m telescope in the CAHA observatory (Spain) and will be equipped with two spectrographs in the near-infrared and visible windows. The technology involved in such instrument represents a challenge at all levels. The instrument coordination and management is handled by the Instrument Control System (ICS), which is responsible of carrying out the operations of the different subsystems and providing a tool to operate the instrument from low to high user interaction level. The main goal of the ICS is to maximize the instrument efficiency by operating it in an integrated and reliable manner. The CARMENES scheduler is another key element in the control layer. It is responsible for the observatory time optimization and, thus, it plays a critical role in achieving an efficient operation. Its main purpose is the allocation of tasks, while maximizing the scientific return of the facility and minimizing the operational costs. The scheduler is based on Artificial Intelligence techniques and considers long- and short-term varying conditions for the prioritization of tasks. The ICS and the scheduler application are described.
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13. (9B) Cortés Contreras, Miriam (Universidad Complutense de Madrid)
Study of M dwarf’s multiplicity with the IAC80
Autores: Cortés-Contreras et al.

Abstract. With the help of CARMENCITA, the CARMENES Cool dwarf Information and daTa Archive, we investigate the membership in double, triple or higher-order multiplicity systems of 54 M dwarfs in the solar neighbourhood. We measure angular separations and position angles from images taken with TCP and CAMELOT at the IAC80 telescope at the Observatorio del Teide, and compared them with those from the Washington Double Star catalogue and other bibliographic sources in order to analyze their evolution over time. Studying M dwarfs in multiple systems provides information on a wealth of topics, e.g. from dynamical masses, through distance and metallicity, to the formation and evolution of weakly bound systems. These 54 M dwarfs are part of a previous study of M-dwarf’s multiplicity from CARMENCITA database.
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14. (2C) Díaz García, José Javier (Instituto de Astrofísica de Canarias)
THERMAP (Thermal Map) para MARCO POLO-R
Autores: José Javier Díaz, Enrique Joven, Marcos Reyes, Javier Licandro

THERMAP es un instrumento capaz de proporcionar imagen y espectroscopía en el infrarrojo medio que formará parte de la instrumentación de la misión Marco Polo R de la ESA. El IAC participa en la definición y diseño de la ICU (Instrument Control Unit), de la puesta en funcionamiento y caracterización de los detectores así como del sistema de adquisición de datos y la electrónica de proximidad de éstos. El IAC también se responsabiliza del software de arranque y de aplicación.
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15. (3C) Díaz García, José Javier (Instituto de Astrofísica de Canarias)
NISP (Near Infrared spectrograph) at EUCLID
Autores: José Javier Díaz, Óscar Tubío

NISP es un instrumento capaz de ofrecer imagen y espectroscopía en el infrarrojo cercano, que forma parte de la instrumentación de EUCLID, misión de la ESA en el marco Cosmic Vision 2015-2025. El IAC participa en la definición y diseño de las unidades de la ICU (Instrument Control Unit) responsabilizándose de las placas de control electrónico para control de los mecanismos, una rueda de filtros y otra de grismas, las lámparas de calibración, y la monitorización y control de temperatura. Así mismo es responsable de proporcionar los EGSE (Electronic Ground Support Equipment) necesarios para la validación de éstos y de la propia ICU en su conjunto.
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16. (10B) Eliche-Moral, M. Carmen (Universidad Complutense de Madrid)
MEGARA Observing Preparation Software Suite (MOPSS)
Autores: M. C. Eliche-Moral, S. Pascual, I. Morales, V. Villar, R. Marino, A. Castillo-Morales, E. Carrasco, J. Gallego, M. García-Vargas, A. Gil de Paz, J. Iglesias, F. M. Sánchez Moreno, J. M. Vilchez, J. Zamorano, and the MEGARA Team

We describe the software components of the MEGARA Observing Preparation Software Suite (MOPSS). MEGARA (Multi-Espectrografo en GTC de Alta Resolucion para Astronomia) is an optical Integral-Field Unit (IFU) and Multi-Object Spectrograph (MOS) designed for the GTC 10.4m telescope in La Palma. The MEGARA IFU mode will offer two different fiber bundles, one covering 12.5×11.3 arcsec^2 (with a spaxel size of 0.62 arcsec) and another one covering 8.5×6.7 arcsec^2 (with a spaxel size of 0.42 arcsec). The MEGARA MOS will allow observing up to 100 objects in a region of 3.5’ x 3.5’ around the two IFU bundles. The MOPSS offers the tools needed by observers to plan their observations with GTC/MEGARA in an optimum way. It includes the MEGARA Exposure Time Calculator, the MEGARA Image Simulator, and the Fiber MOS Positioning Tool. An updated view of the current status of each tool is provided.
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17. (11B) Ferrusca, Daniel (Instituto Nacional de Astrofisica Optica y Electronica)
MEGARA Cryostat Detailed Design
Autores: D.Ferrusca, E.Castillo-Dominguez, M.Velazquez de la Rosa

We present the detailed design of the cryogenic system of MEGARA. The reported cryostat is a custome made design developed at the Instituto Nacional de Astrofisica Optica y Electronica in Mexico, and it will harbor the scientific CCD of the spectrograph. The cryostat is divided in two main parts: CCD head and dewar back. The CCD head contains an adjustable mechanism that will allow us to correct the CCD position in x,y,z, tip and tilt; the dewar back contains a liquid nitrogen tank that will provide > 40 hours hold time as a requirement. Mechanical designs and FEM results are presented as well as thermal model calculations. It is expected to start the fabrication of the cryostat in 2014.
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18. (4C) Gálvez Sánchez, José-Luis (Institut de Ciències de l’Espai (CSIC-IEEC)))
Development of CdTe pixel detectors for Hard X/gamma-ray imaging
Autores: J.L. Gálvez, M. Hernanz (CSIC-IEEC), on behalf of a larger collaboration

Our research and development activities aim to study a gamma-ray imaging spectrometer in the MeV range based on CdTe detectors, suited either for the focal plane of a focusing mission or as a calorimeter for a Compton camera. In addition, our undergoing detector design is proposed as the baseline for the payload of a balloon-borne experiment dedicated to hard X- and soft gamma-ray polarimetry, currently under study and called CµSP (CZT µ-Spectrometer Polarimeter). Other research institutes such as INAF-ISAF, DTU Space, LIP, INEM/CNR, CEA, are involved in this proposal. We will report on the main features of the prototype we are developing at ICE (CSIC-IEEC), a gamma-ray detector with imaging and polarimetry capabilities in order to fulfil the combined requirement of high detection efficiency with good spatial and energy resolution.
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19. (12B) Garcia Vargas, Maria Luisa (FRACTAL SLNE (MEGARA Team))
MEGARA Spectrograph Optical Detailed Design
Autores: García-Vargas, María Luisa (FRACTAL); Sánchez-Blanco, Ernesto (FRACTAL); Carrasco Licea, Esperanza (INAOE); Pérez-Calpena, Ana (FRACTAL); Gil de Paz, Armando (UCM); Gallego Maestro, Jesús (UCM); Vilchez Medina, José Manuel (IAA); Iglesias Páramo, Jorge (IAA)

We describe the optical design of MEGARA spectrograph. MEGARA is the future optical Integral Field Unit (IFU) and Multi-Object Spectrograph (MOS) for the 10.4-m Gran Telescopio CANARIAS (GTC). MEGARA is being built by a Consortium of public research institutions led by the Universidad Complutense de Madrid (UCM, Spain) that also includes INAOE (Mexico), IAA-CSIC (Spain) and UPM (Spain). MEGARA passed the Optics Detailed Design Review in May 2013 organized by GRANTECAN and it is currently starting the Optics Manufacturing phase.
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20. (5C) Garcia-Piquer, Álvaro (ICE (CSIC / IEEC))
EChO Long Term Mission Planning Tool
Autores: Álvaro Garcia-Piquer, Ignasi Ribas, Josep Colomé

The Exoplanet Characterisation Observatory (EChO) is one of the ESA M3 mission candidates currently assessed for an expected launch in 2022. EChO will be the first dedicated mission to investigate the physics and chemistry of Exoplanetary Atmospheres. IEEC task is focused on designing the Long Term Mission Planning Tool (LT-MPT) of the EChO mission. Mission planning for this mission is a complex scheduling problem because each exoplanet has to be observed a number of times to yield measurements of sufficient Signal-to-Noise Ratio for fulfilling the mission objectives. Moreover, several criteria have to be considered to carry out each observation: target visibility, time and duration of the events, number of events to be observed, target priority, and avoid task overlapping. A suitable mission plan increases the efficiency of operation, which represents an important benefit in terms of scientific return and operational cost. The LT-MPT is based on Artificial Intelligence techniques, which are mathematical methods for solving optimization problems considered NP-hard, such as the planning of several tasks. Specifically, the LT-MPT finds a solution that highly optimizes the mission objectives. The experiments show a good performance and emphasize the ability of the tool of obtaining competitive results independently of the exoplanet sample.
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21. (13B) Gil de Paz, Armando (Universidad Complutense de Madrid)
MEGARA Science and instrument performance
Autores: Gil de Paz, Armando; Carrasco, Esperanza; Gallego, Jesús; Sánchez-Moreno, Fco. M.; Vílchez, J.M.; García-Vargas, M.L. and the rest of the MEGARA Instrument and Science teams.

In order to show the strong involvement (and capabilities) of the Spanish research centers and companies in the different aspects of the design and construction of a state-of-the-art astronomical instrument we aim to present a series of posters that highlight the different work packages of MEGARA, the future optical spectrograph for GTC. This specific poster will provide a summary of the scientific objectives of the MEGARA instrument (and its proposing Science Team) along with its performance and how this compares with other instruments in other 8-10m telescope facilities. Other posters in the series will include a description of the MEGARA focal plane (robotic positioners and optical fiber bundles), the spectrograph optical and mechanical design and manufacturing, control system (including its data reduction pipeline) and preparatory AIV activities.
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22. (4A) Gonzalez, Laura (TTI)
Amplificadores criogénicos: evolución en radioastronomía
Autores: Francisco Diaz, Laura González

La necesidad de detectar señales muy débiles provenientes de objetos muy alejados de la Tierra ha llevado a los radioastrónomos a la necesidad de receptores extremadamente sensibles cuyo ruido sea menor que el nivel de las señales a recibir. Dado que los sistemas electrónicos generan menos ruido si son enfriados, se utilizan receptores refrigerados a temperaturas criogénicas. TTI lleva años desarrollando equipos que funcionan a temperaturas de hasta 4K. Los amplificadores de bajo ruido criogénicos están basados en tecnologías GaAs, InP HEMT o un hibrido de ambas, con alta estabilidad, ganancias de 33 a 39 dB, y Temperaturas de Ruido menores que 5K@15K. TTI ha desarrollado y fabricado amplificadores criogénicos (bandas S, C y X) tanto para estaciones de comunicaciones vía satélite como para observatorios de radioastronomía en todo el mundo: ESOC, IRAM, Asiaa Hawaii (US), etc. Los amplificadores criogénicos basados en InP ofrecen mejores prestaciones a cambio de un coste elevado. Actualmente se están analizando otras tecnologías para desarrollar amplificadores enfriados criogénicamente de muy bajo ruido. Es el caso de metamorphic GaAs o de la evolución natural consistente en la utilización de tecnologías de MMICs debido a que ofrecen repetitividad en las prestaciones y bajo coste para altas producciones.
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23. (5A) González de Rivera, Guillermo (Escuela Politécnica Superior. Univ. Autónoma de Madrid)
Desarrollos para el posicionador de BigBOSS: electrónica y comunicaciones
Autores: Guillermo Glez.-de-Rivera, Nasib Fahim, Justo Sánchez, Francisco Prada, Javier Garrido

En este trabajo se describen los desarrollos realizados para el control y gestión de los posicionadores de fibra óptica que se han diseñado para el proyecto BigBOSS. Se describe la electrónica de control diseñada para el manejo de los dos motores integrados en dicho posicionador, así como el desarrollo del firmware necesario, que incluye los algoritmos de posicionado, modulación de corriente, control de temperatura, técnicas de bajo consumo de potencia, etc. También se describe el protocolo de comunicación entre la unidad central que contiene la posición de cada fibra y cada uno de los 5.000 posicionadores de dichas fibras. Así mismo, se detallan las diferentes pruebas y test hachas para la validación del conjunto, realizadas tanto en las instalación del Instituto de Astrofísica de Andalucía (IAA-CSIC) como en las instalaciones del Lawrence Berkeley National Laboratory (LBNL).
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24. (14B) Gracia Temich, Félix (IAC)
HORS (High Optical Resolution Spectrograph)
Autores: Félix Gracia, Samuel Santana, Jose Peñate, Juan Calvo, Carlos Allende, Ramon García, Jose Luis Rasilla, Vicente Sánchez, Rafael Rebolo.

HORS es un espectrógrafo de dispersión cruzada de baja resolución (~ 25.000) diseñado para trabajar en GTC y optimizado para tolerar condiciones mediocres de seeing. Irá instalado en la plataforma Nasmyth B de GTC compartiendo foco con OSIRIS. Su finalidad científica se centra en el estudio de la composición química de estrellas, nebulosas y otros objetos, y la espectroscopia de planetas en tránsito. Esperamos que la instalación en GTC pueda tener lugar a finales de 2014 y que el instrumento esté operativo durante varios años.
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25. (15B) Gracia Temich, Félix (IAC)
Laboratorio de fibras del IAC
Autores: F. Gracia, J. L. Rasilla

En esta época en la que una gran mayoría de los instrumentos futuros dependerán de la alimentación por fibras óptica, queremos mostrar las facilidades que proporciona actualmente el laboratorio de fibras del IAC.
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26. (6A) Hernández, Elvio (Instituto de Astrofísica de Canarias)
Desarrollo de mecanismos criogénicos para HARMONI
Autores: E. Hernández, J. M. Herreros, L. F. Rodríguez

HARMONI es uno de los dos instrumentos seleccionados para primera luz del EELT. El IAC participó en el estudio de diseño conceptual de este espectrógrafo óptico/infrarrojo de campo integral, como miembro de un consorcio internacional. El desarrollo de HARMONI entra ahora en una fase de revisión del diseño conceptual. Uno de los aspectos que se identificó como probablemente necesario es la introducción de una máscara de pupila que limite la radiación de fondo que alcanza el detector y en teoría existiría la necesidad de hacer que esta máscara girase con arreglo a los movimientos de la pupila durante una observación. Estaríamos entonces en la necesidad de mover un objeto a velocidades extremadamente lentas pero con gran precisión (que encima incluye paso por cero y cambio de sentido), a temperaturas criogénicas, todo lo cual supone un reto tecnológico, por lo que se han realizado un conjunto de experimentos encaminados a adquirir conocimientos y experiencia en el control de mecanismos criogénicos capaces de realizar este tipo de movimiento.
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27. (16B) Hoyland, Roger (Instituto de Astrofisica de Canarias)
Design and Status of the QUIJOTE Thirty GigaHertz Instrument (TGI)
Autores: R. Hoyland, A. Pérez, V. Sánchez, A. Vega, M. Aguiar, M. F. Gómez, T. Viera .

The TGI is the 2nd QUIJOTE instrument which is planned to be mounted on the 2nd Quijote telescope. It is a 31 element array of polarimeters with state-of-the-art performance. Up until now we have been working on the components that make up each polarimeter. The novel design and present status of the TGI will be presented
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28. (17B) Hoyland, Roger (Instituto de Astrofisica de Canarias)
The status of the QUIJOTE Multi-Frequency-Instrument
Autores: R. Hoyland, A. Pérez, V. Sánchez, A. Vega, M. Aguiar, M. F. Gómez, T. Viera

We present the current status of the QUIJOTE first instrument (MFI), which is a multi-channel instrument with five separate polarimeters (providing 5 independent sky pixels): two which operate at 10-14 GHz, two which operate at 16-20 GHz, and a central polarimeter at 26-36 GHz. The science driver for this first instrument is the characterization of the galactic emission. The polarimeters use a novel cryogenic on-axis rotating polar modulator to derive linear polar parameters Q, U and I and switch out various systematics. Early results of commissioning will also be presented.
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29. (18B) Iglesias, Jorge (Instituto de Astrofísica de Andalucía)
Imaging Fourier Transform Spectrometer: an alternative for Wide-field 3D spectroscopy
Autores: J. Iglesias-Páramo, M. Mollá, M. García-Vargas

We present the concept of Imaging Fourier Transform Spectrometer (IFTS) as an alternative for Wide-field 3D spectroscopy. Different possibilities of IFTS for CAHA telescopes will be discussed.
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30. (6C) Jiménez Ortega, Jaime (IAA-CSIC)
Software developments oriented to space programmes
Autores: J. Jiménez, A.J. García, I. Martínez, J. Rodrigo

The Instituto de Astrofísica de Andalucía (CSIC) has planned a strategy allowing it to develop units and sub-units of instruments in different space missions within the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA). Amongst these missions, current developments are focused on power supplies (see talk by J. Rodrigo et al.) for the JANUS and GALA instruments on board the JUICE mission, on filter positioning mechanisms and its control electronics (see talk by I. Martínez-Navajas et al.). Those developments show the versatility of the working group skills which are currently being increased since the Electrical Ground Support Equipment (EGSE) and a Data Control Unit (DCU) simulator for the MarcoPolo-R (MaRIS instrument) and EChO missions are also under IAA’s responsibility. In addition, the workgroup is developing a General Data Processing Unit (GDPU) based on a FPGA for future space missions, (including Earth observations) which require high data rates. The GDPU will include many features that will be presented during the talk. . A LEON3 processor is included in this design. In this talk, we will show these developments, that is, EGSE, DCU and DPU and will discuss the approach we have taken to obtain the utmost of these designs.
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31. (19B) Joven, Enrique (Instituto de Astrofisica de Canarias (IAC))
Caracterización de detectores astronómicos en el IAC: Infraestructura LISA
Autores: E. Joven, J.J. García, M. Reyes

En los últimos años se ha llevado a cabo en el IAC la dotación y puesta a punto de una infraestructura específica para la caracterización de cámaras y detectores astronómicos, denominada LISA (Laboratorio de Imagen y Sensores para Astronomía). Se trata de una instalación estable, completamente automatizada para la caracterización de detectores en el rango visible (CCDs, EMCCDs, CMOS) y parcialmente en los rangos infrarrojo cercano (1-2.5 micras) y medio (8-14 micras).
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32. (7C) Lara, Luisa M. (IAA-CSIC)
The BepiColombo Laser Altimeter: Novel instrument elements
Autores: L.-M. Lara (1) N. Thomas (2), T. Spohn (3), U. Christensen (4), and the BeLA Team. (1) Instituto de Astrofisica de Andalucia (CSIC), Granada, SPAIN, (2) Physikalisches Institut, University of Bern, Bern, SWITZERLAND (3) DLR, Institute of Planetary Resear

We present a description of some of the novel elements of the BepiColombo Laser Altimeter (BELA). Emphasis is placed on the laser, the baffles used to protect the sensitive parts of the instrument from the Sun, the telescope solution and the digital reangefinder system. BeLA Team: J.-M. Castro (1), M. Herranz (1), J. Rodrigo (1), K. Seiferlin (2), , M. Affolter (2), T. Beck (2), U. Geissbühler (2), S. Graf (2), A. Peteut (2), D. Piazza (2), A. Servonet (2), H. Michaelis (3), T. Behnke (3), W. Bresch (3), H. Hussmann (3), A. Lichopoj (3), K. Lingenauber (3), F. Lüdicke (3), R. Schrödter (3), K. Wickhusen (3), R. Kallenbach (4), H. Perplies (4)
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33. (7A) Latorre, Teresa (IFT UAM/CSIC)
DESI focal plate and demonstrator
Autores: Teresa Latorre, Santiago Becerril, Francisco Prada, Paul Perry, Joe Silber, Andrew Lambert

Dark Energy Spectroscopic Instrument spanish participation: current focal plate design and demontrator
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34. (20B) Maldonado, Manuel (FRACTAL)
MEGARA Spectrograph Mechanical Detailed Design
Autores: Maldonado Medina, Manuel; García-Vargas, María Luisa (FRACTAL); Sánchez-Blanco, Ernesto (FRACTAL); Pérez-Calpena, Ana (FRACTAL); Gil de Paz, Armando (UCM); Gallego Maestro, Jesús (UCM); Vilchez Medina, José Manuel (IAA); Iglesias Páramo, Jorge (IAA), S

We describe the current mechanical design and the adopted solutions for the mechanisms and the opto-mechanical components of MEGARA spectrograph. MEGARA is the future optical Integral Field Unit (IFU) and Multi-Object Spectrograph (MOS) for the 10.4-m Gran Telescopio CANARIAS (GTC). MEGARA is in the final design phase.
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35. (21B) Manchado, Arturo (IAC)
LIRIS: El primer espectrógrafo infrarrojo con capacidad multi-objeto, Construido por el IAC, cumple 10 años en el telescopio “William Herschel”, del ORM
Autores: Arturo Manchado, Jose A. Acosta-Pulido, Mary Barreto (IAC)

LIRIS (Long-slit Intermediate Resolution Infrared Spectrograph), es un espectrógrafo para el rango del infrarrojo cercano (0.9 a 2.5 micras) construido por el IAC, que vio la primera luz en Abril de 2003 como instrumento de uso común en el telescopio de 4.2m WHT en el Observatorio del Roque de los Muchachos (La Palma). Desde entonces es el segundo instrumento mas utilizado en el WHT, y ha producido más de 100 papers en revistas incluidas en el ISI (incluido tres en la revista nature). Descripción de LIRIS: LIRIS es un espectrógrafo para el rango del infrarrojo cercano (0.9-2.5 micras) de resolución intermedia R = 700 (en las bandas ZJ y HK) y R=2500 (en las bandas J, H y Ks), con capacidad de imagen (con un campo de visión de 4′.2 x 4′.2). LIRIS tiene modos de observación únicos, como la polarimetría, coronografía y el modo multi-rendija. Es en especial este modo multi-rendija lo que hace que LIRIS sea un instrumento único en el mundo y más competitivo que otros espectrógrafos similares instalados en telescopios de la clase 10m. El proyecto ha tenido un presupuesto de 3.4 Meuros (incluyendo recursos humanos). Para más información visiten la página: ww.iac.es/proyect/LIRIS
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36. (8C) Marcos Arenal, Pablo (IvS, KU Leuven)
The PLATO Simulator software package: Realistic modelling of high-precision high-cadence space-based imaging.
Autores: P. Marcos-Arenal, W. Zima, J. De Ridder, R. Huygen, C. Aerts

The preparation of a space-mission that carries out any kind of imaging to detect high-precision low-amplitude variability of its targets requires a robust model for the expected performance of its instruments. This model cannot be derived from simple addition of noise properties due to the complex interaction between the various noise sources. While it is not feasible to build and test a prototype of the imaging device on-ground, realistic numerical simulations in the form of an end-to-end simulator can be used to model the noise propagation in the observations. These simulations not only allow studying the performance of the instrument, its noise source response and its data quality, but also the instrument design verification for different types of configurations, the observing strategy and the scientific feasibility of an observing proposal. In this way, a complete description and assessment of the objectives to expect from the mission can be derived. We present a high-precision simulation software package designed to simulate photometric time-series of CCD images by including realistic models of the CCD and its electronics, the telescope optics, the stellar field, the jitter movements of the spacecraft, and all important natural noise sources. This formalism has been implemented in a software tool, dubbed PLATO Simulator.
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37. (9C) Mas Hesse, J. Miguel (CAB (CSIC-INTA))
AstroMadrid: Astrofísica y desarrollos tecnológicos en la Comunidad de Madrid
Autores: J. Miguel Mas Hesse, en nombre del equipo AstroMadrid

El programa AstroMadrid fue aprobado en 2009 por la Comunidad de Madrid, y ha contribuido a financiar las actividades de desarrollo y explotación de de instrumentos astronómicos por parte de buena parte de los investigadores que trabajan en el área de Madrid. El póster presentará los objetivos y los logros principales del proyecto a lo largo de sus 4 años de vigencia, destacando el desarrollo de MEGARA para GTC, y la contribución a numerosos instrumentos espaciales.
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38. (22B) Montes, David (Universidad Complutense de Madrid, UCM)
CARMENES. High-resolution spectroscopy of M dwarfs with FEROS, CAFE and HRS
Autores: D. Montes, F. J. Alonso-Floriano, S. Jeffers, J. A. Caballero, et al.

A thorough preparation effort will be critical to ensure that most of the CARMENES observing time is spent on targets that stand the highest chance of success. Spectra with high resolution (R = 30,000-48,000) are being collected for the CARMENES survey preparation. Our aim is to have at least two spectra at different epochs of the 300 eventual CARMENES targets, from which deriving the projected rotational velocity vsini with an accuracy better than 0.5-0.2 km/s and radial-velocity stability better than 0.2-0.1 km/s. Our observations with FEROS at ESO/MPG 2.2 m La Silla, CAFE at 2.2 m Calar Alto and HRS at Hobby Eberly Telescope allow us to identify single- and double-line spectroscopic binaries and, especially, fast rotators, which should be discarded from the target list for exoplanet searches.
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39. (10C) Morales de los Rios Pappa, Jose Alberto (Universidad de Alcala)
An End to End Simulation code for the IR-Camera of the JEM-EUSO Observatory
Autores: J.A. MORALES DE LOS RIOS(1,2), L. DEL PERAL(2), G. SAEZ -CANO(2), H. PRIETO(2), J. H-CARRETERO(2), M.D. SABAU(3), T. BELENGUER(3), C. GONZALEZ ALVARADO(3), M. SANZ PALOMINO(3), J. LICANDRO(4,5), E. JOVEN(4), M. REYES(4) AND M.D. RODRIGUEZ FRIAS(2), FOR T

The Extreme Universe Space Observatory on the Japanese Experiment Module (JEM-EUSO) of the International Space Station (ISS) is the first space-based mission worldwide in the field of Ultra High-Energy Cosmic Rays (UHECR). JEM-EUSO will use our atmosphere as a huge calorimeter, to detect the electromagnetic components of the Extensive Air Shower (EAS). Therefore, the atmosphere must be calibrated and has to be considered as input for the analysis of the fluorescence signals. The JEM-EUSO space observatory is implementing an Atmospheric Monitoring System (AMS), to gather data of the atmosphere status during the UHECR observation period, it will include an IR-Camera and a LIDAR. The AMS IR-Camera is an infrared imaging system aimed to detect the presence of clouds. Our paper is focused on the End to End (E2E) simulation developed for the IR-Camera of the JEM-EUSO Space Mission. This work gives us the capabilities to study the impact of several scenarios of the atmosphere, in terms of retrieval temperature accuracy, detection capabilities, calibration procedures, and correction factors to be taken into account for the final data products of the AMS system of the JEM-EUSO Space Mission.
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40. (8A) MORENO VENTAS, JAVIER (CAB (INTA-CSIC))
Study on the performance of secondary guiding for HARMONI
Autores: Moreno-Ventas Mateos, Javier & Arribas Mocoroa, Santiago & HARMONI Collaboration

“HARMONI is a first light optical-infrared integral field spectrograph (IFS) for the European Extremely Large Telescope (E-ELT). Its optical range spans from 0,47 to 2,45 microns. Secondary guiding provides compensation for any differential image motion between the telescope (or AO) wavefront sensor and the instrument focal plane. Required accuracy changes substantially depending on the telescope PSF, so the secondary guiding implements both visible and near infrared sensing (NIR is more sensitive when the PSF is sharper). In order to constrain its design, we have started a study to understand the dependency of the main variables involved on its performance. Here we present some preliminary results which will help, for instance, to define the size of the field of view, pixelation, and working frequency (~1Hz) for this system.”
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41. (23B) Mujica Alvarez, Emma (FRACTAL SLNE)
MANATEE: Management Tool for Effective Engineering
Autores: Mujica Alvarez, Emma (FRACTAL); García-Vargas, María Luisa (FRACTAL) and Pérez-Calpena, Ana (FRACTAL)

This poster describes MANATEE, the project web tool developed by FRACTAL, specifically designed for managing large astronomical projects. MANATEE facilitates the management by providing an overall view of the project and the capabilities to control the three main projects parameters: scope, schedule and budget. MANATEE is one of the three tools of the FRACTAL System & Project Suite, which is composed also by GECO (System Engineering Tool) and DOCMA (Documentation Management Tool). These tools are especially suited for those Consortia and teams collaborating in a multi-discipline, complex project in a geographically distributed environment. Our Management view has been applied successfully in several projects and currently is being used for Managing MEGARA, the next instrument for the GTC 10m telescope; and CARMENES, the next double-arm echelle spectrograph for the 3.5m telescope of Calar Alto.
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42. (9A) Murga, Gaizka (IDOM)
IDOM Astronomy Projects
Autores: Gaizka Murga

IDOM is an international firm specializing in Engineering, Architecture and Consulting. IDOM operates globally in areas such as power generation, oil & gas, renewable and alternative energies, manufacturing industry, civil infrastructures, nuclear plants, large technological and scientific facilities, architecture and unique challenging engineering projects. IDOM ADA leads the company activity in technologically advanced and challenging projects involving applied mechanics, structural design, electronics and control. Our portfolio of clients and collaborators include ESO, AURA, IAC, GTC, EHU-UPV, TMT Observatory Corp., SNS/ORNL, GANIL, ESS-Bilbao, ESS, F4E/ITER, CENER, Clemson University, NaREC, Fraunhoffer Institute and others. IDOM collaboration with ESO started on 2007 with the Preliminary Design of the European Extremely Large Telescope (E-ELT) Dome and Foundations and has continued with the Detailed Design (FEED Study) of the E-ELT Dome and Foundations.
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43. (24B) Pascual, Sergio (Universidad Complutense de Madrid)
Development of Data Reduction Pipelines for GTC Instruments at the UCM
Autores: S. Pascual, M. C. Eliche-Moral, N. Cardiel, J. Gallego

The UCM Instrumentation Group (GUAIX) is developing currently Data Reduction Pipelines (DRP) for four instruments of the GTC: EMIR, FRIDA, MEGARA and MIRADAS. The purpose of the DRPs is to provide astronomers scientific quality data, removing instrumental biases, calibrating the images in physical units and providing a estimation of the associated uncertainties. We are developing all our processing tools using Python. The development is compatible with Python 2.7 All the developed packages are be released under GPLv3. They will be free for everyone to install, share and modify.
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44. (11C) Perez, Jose Santiago (UAH)
IR Camera contribution to the CNES EUSO-BALLOON pathfinder
Autores: S. Pérez 1*, H. Prieto 1, L. del Peral 1, J. A. Morales de los Ríos 1, G. Sáez-Cano 1, J. H. Carretero 1, L. Sabau 2, C. González 2, T. Belenguer 2, M. Sanz 2, J. Licandro 3, M. Reyes 3, E. Joven 3, M. D. Rodríguez Frías 1, for the JEM-EUSO Collaboration.

JEM-EUSO Balloon is a pathfinder missions for the Extreme Universe Space Observatory on-board the Japanese Experiment Module (JEM-EUSO) mission. Through a series of stratospheric balloon flights performed by the French Space Agency CNES, EUSO-BALLOON will serve as an evaluative test-bench for all the key technologies of JEM-EUSO, as well as other future missions dedicated to the observation of extensive air shower from space. The EUSO-Balloon IR Camera shall obtain IR images of clouds to study main parameters as their height and optical depth that affect the Extensive Air Shower (EAS) analysis. For instance, one of the most critical cloud parameters is the cloud temperature since the cloud altitude will be retrieved from it. This camera system is designed with the available commercial solutions of IR Cameras and a dedicated optical subsystem with filters selection, devoted to fulfill the performances necessary for this kind of mission. The IR camera is a stand-alone subsystem within the Spanish contribution to the EUSO-BALLOON mission. Its main goal is to provide cloud images in the middle infra-red range (8-12 µm). Currently, the EUSO-BALLOON IRcamera is in phase D after its Critical Design Review passed at CNES on December 2012.
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45. (25B) Pérez Calpena, Ana (FRACTAL SLNE)
MEGARA Fiber bundles
Autores: Pérez-Calpena, Ana (FRACTAL); Sánchez-Blanco, Ernesto (FRACTAL); García-Vargas, María Luisa (FRACTAL)); Gil de Paz, Armando (UCM); Arrillaga, Xabi (AVS); Aube Hervé (SEDI); Martínez-Delgado, Ismael, Gallego Maestro, Jesús (UCM); Vilchez Medina, José Manue

MEGARA is the future optical Integral Field Unit (IFU) and Multi-Object Spectrograph (MOS) for the 10.4-m Gran Telescopio CANARIAS (GTC). This poster summarizes the design of the MEGARA Fiber Bundles, from the GTC focal plane, to the entrance at the spectrograph pseudo-slits. MEGARA passed the Optics Detailed Design Review in May 2013 organized by GRANTECAN. The poster summarizes also the prototypes that are being tested at laboratory and the strategy of the installation at the GTC.
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46. (12C) Prieto, Hector (UAH/SPAS Group)
Multi-anode Photomultiplier Tube Reliability analysis and Radiation Hardness Assurance for the JEM-EUSO Space Mission
Autores: H.Prieto-Alfonso 1, K. Tsuno 1, L. del Peral 2 ,M. Casolino 2,3, J. A. Morales de los Ríos 1,2 , G. Sáez-Cano 1 ,T. Ebisuzaki 4 and M. D.Rodríguez Frías 2 for the JEM-EUSO collaboration. 1 SPace and AStroparticle (SPAS) Group. UAH, Madrid. Spain 2 EU

Reliability analysis is concerned with the analysis of devices and systems whose individual components are prone to failure. This reliability analysis pretends to evaluate the JEM-EUSO Photomultiplier tube component using the methods MIL-HDBK-217-F notice 2 and 217 Plus. The objective of this reliability analysis is to test the validity of concepts and technical choices made today for the JEM-EUSO Space mission scheduled for 2017 or any subsequent project aimed at achieving an observatory of giant air showers induced by energetic cosmic rays from space. The main aim of this work is to determine the failure rate, MTBF, Reliability Analysis of the JEM-EUSO Photomultiplier Tube (PMT’s) implemented on the focal surface of the space telescope as well as the radiation hardness assurance to evaluate its present and potential reliability. The PMT is a vital part of the instrumentation of the telescope, conducting a reliability analysis is crucial since PMT’s failure would be catastrophic for JEM-EUSO; due to PMT’s are the heart and critical elements of this experiment. The Reliability analysis and Radiation Hardness assurance of PMT’s for their qualification requires meeting stringent radiation tolerance levels. The majority of radiation hardness assurance have so far focused on laboratory test, therefore, as a first step towards understanding the long-term reliability of PMT’s in hostile radiation environments, is performing an analytical and theoretical, probabilistic estimation which predicts the reliability of the PMT’s in space environments and radiation conditions for JEM-EUSO. Keywords: Reliability, PMT’s, JEM-EUSO, Radiation
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47. (13C) Ramírez, Luis (Orbital Sistemas Aeroespaciales SL)
Multi CCD Electronics for ground and space applications.
Autores: Luis Ramírez, Carlos Echeandía

Orbital Aerospace has developed a front-end electronics that commands independently two space spectrometers which focal planes are base on a CCD from e2v manufacturer. The product developed is highly flexible and configurable and it has been design to support different families of e2v products including NIMO and AIMO devices, performing benchmarking of the product and exploring the devices characteristics beyond their limits together with e2v. The key features are low noise, reliable, high speed and space radiation compensation. Based on a flexible FPGA Core from Orbital this product is easily adapted to multiple needs and requirements and ready to be used in astronomical instruments.
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48. (10A) Rasilla, José L. (IAC)
ESPRESSO Fiber Llink
Autores: José L. Rasilla y Felix Gracia

ESPRESSO is a high resolution and ultrastable spectrograph which is located in the Combined Coudé Laboratory at the VLT. From this place the spectrograph could receive light from each VLT telescope. For this, the Combined Coudé Laboratory will carry the light from the telescope Nasmith focus to the CCL. There, Font-End subsystem will collect the light from each telescope, stabilizing both the image of the object as the pupil of the telescope, choosing the mode of observation required and feeding the Fiber Link. The Fiber Link subsystem allows carrying the light coming from the telescope through the Font End to the spectrograph.
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49. (26B) Redondo Caicoya, Pablo Gustavo (IAC)
Evolución en el desarrollo de Instrumentación Infrarroja en el Instituto de Astrofísica de Canarias
Autores: Redondo, Pablo; Barreto, Mary; Fernández, Patricia; Patrón, Jesús; Sánchez, Vicente; Tenegi, Fabio.

El póster resume la evolución del Instituto de Astrofísica de Canarias (IAC)en el desarrollo de instrumentación para el infrarrojo durante los últimos 20 años, a través de la comparativa de los tres proyectos que mejor representan dicha evolución: CAIN, LIRIS y EMIR. Cada uno de ellos ha representado una mejora tecnológica respecto a los anteriores: telescopios mayores han requerido instrumentos con mayores lentes, mecanismos más grandes y más complejos para posicionarlas, estructuras de soporte más rígidas y con mayor masa propia, y una nueva escala en el tamaño de los criostatos que mantienen en vacío y criogenia estos componentes. El incremento de la complejidad de los instrumentos ha impulsado también la mejora de la infraestructura de fabricación, integración y verificación del IAC. La comparativa incluye el ámbito de la gestión, que se han adaptado a presupuestos cada vez más importantes, equipos de proyecto más especializados y complejos, y a una creciente participación de colaboradores externos.
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50. (14C) Rodrigo Campos, Julio (IAA-CSIC)
Advanced Technologies on Distributed Power Supplies Applied to Space Instrumentation
Autores: J. Rodrigo, J. Jimenez, M. Herranz, J.M. Castro-Marin, L.M. Lara

Within the framework of the European Space Agency (ESA) Cosmic Vision 2015-2025 programme, members of the Solar System Department and of the ‘Unidad de Desarrollo Instrumental y Tecnológico’ (UDIT) at the ´Instituto de Astrofísica de Andalucía´ (IAA-CSIC) have acquired several responsibilities inside the international consortiums for missions in development. Some of these responsibilities are related to the development of different space power supplies for diverse instruments, each with specific requirements that make them unique. Concerning the ´Bepi-Colombo´ mission (ESA-JAXA), works related to the development of the Power Converter Module for the ´BepiColombo Laser Altimeter´ (BeLA) instrument were performed. Nowadays, many different power supplies solutions are being studied, simulated, fabricated and tested in-house in the early phases of their respective projects. Within the ESA mission ´Jupiter Icy moons Explorer´ (JUICE), the power supplies for the instruments ´Jovis Amorum ac Natorum Undique Scrutator´ (JANUS) and ´Ganymede Laser Altimeter´ (GALA). Within the candidate for M-class ESA mission ´Marco Polo-R´, the power supplies for the instruments ´MarcoPolo-R Imaging Scrutator´ (MaRIS) and ´Marco Polo-R Narrow Angle Camera´ (MaNAC). A brief summary of these space power supplies will be presented, as well as their technology state-of-the-art, advantages and disadvantages for their future use in space.
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51. (28B) Rodríguez Ramos, Luis Fernando (Instituto de Astrofísica de Canarias)
DIMMA: Differential Image Motion Monitor Automático
Autores: L. F. Rodríguez, J. M. Delgado, T. Varela, C. Muñoz-Tuñón

Con el objetivo general de lograr una evaluación permanente de las condiciones astro-meteorológicas del los observatorios de Canarias (ORM y OT), y basándose en el monitor de seeing desarrollado en el IAC que funciona regularmente desde 1995, se han instalado sendos sistemas DIMMA (Monitor de seeing automático) en dichos observatorios, incorporando una serie de prestaciones que suponen un salto cualitativo importante en su utilidad científica. Ambos sistemas están siendo operados habitualmente durante todo el año, al igual que había sucedido en el año anterior por técnicos en operaciones telescópicas, estando disponibles en tiempo real los datos obtenidos en el sitio web del IAC.
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52. (29B) Rosich, Josefina (IAC)
Sistema de Control de MIRADAS
Autores: Josefina Rosich, Carlos Martín, Paco Garzón

MIRADAS es un espectrógrafo para el Gran Telescopio Canarias (GTC) en el infrarrojo cercano y multi-objeto con una resolución espectral R = 20.000 y con un paso de banda de 1-2.5μm. En este póster se va a mostrar una visión general del software de control de MIRADAS, que sigue los estándares software y hardware definidos por el telescopio para permitir la integración de este software en el sistema de control de GTC (GCS). El Sistema de Control de MIRADAS se basa en una arquitectura distribuida de acuerdo con el modelo de componentes, donde cada subsistema es auto-contenido. GCS es un entorno distribuido orientado a objetos en C + +, que ejecuta los múltiples componentes y servicios de los que está compuesto en diferentes máquinas, y utiliza el middleware CORBA para comunicarse entre ellos. Todos los modos de observación de MIRADAS, incluyendo los modos de ingeniería, supervisión y calibración, tendrán su propia secuencia predefinida, que se ejecutarán en el secuenciador de GCS. Estas secuencias tendrán la capacidad de comunicarse con los otros subsistemas del telescopio para poder ordenar el apuntado de telescopio o del espejo secundario, etc.
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53. (15C) Ruiz, Vicente (ISDEFE/ESAC)
ON THE STUDY OF THE SPACE ENVIRONMENT: ESA´s Optical Surveillance System Test-Bed
Autores: Vicente Ruiz; Miguel Sánchez-Portal; Francisco Ocaña

In the context of the Space Situational Awareness (SSA) programme of ESA, it is foreseen to deploy several large robotic telescopes in remote locations to provide surveillance and tracking services for man-made as well as natural near-Earth objects (NEOs). The present project will implement a test-bed for the validation of an autonomous optical observing system in a realistic scenario, consisting of two telescopes located in Spain and Australia, to collect representative test data for precursor SSA services. It is foreseen that this test-bed environment will be used to validate future prototype software systems as well as to evaluate remote monitoring and control techniques. The test-bed system will be capable to deliver astrometric and photometric data of the observed objects in near real-time. This poster describes the current status of the project.
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54. (30B) Russu Berlanga, Andres (Space Research Group (SRG-UAH))
e-Callisto network of Solar Radio Telescopes at Spain
Autores: A. Russu1, R. Gómez-Herrero1, J. Rodriguez-Pacheco1, M. Prieto1, A. Moreno1 1 Space Research Group-University of Alcalá

The e-CALLISTO (Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory) is a worldwide network which aims to allow 24 hours a day solar radio burst monitoring. The e-CALLISTO network is lead by the Swiss Federal Institute of Technology Zurich (ETHZ Zurich), which work up collaborations with local host institutions. The CALLISTO spectrometer operates in a frequency range between 45 MHz and 870MHz with 400 maximum channels on 0.15 seconds time resolution. The CALLISTO spectrometer is built in the framework of IHY2007 and ISWI by the Institute for Astronomy, ETH Zurich, Switzerland (Principal Investigator Christian Monstein). More than 57 CALLISTO instruments have already been deployed through the IHY/UNBSSI and ISWI instrument deployment program. In 2013 the University of Alcalá has joined the e-CALLISTO network with the installation of two CALLISTO spectrometers: the Melibea-SRT that is located at Peralejos de las Truchas (Guadalajara) and the EA4RKU-SRT that is located on the University of Alcalá external campus. The Spanish e-Callisto Solar Radio Telescopes provide routine data to the network and the most intense Solar Radio Burst has been measured during this operation time. The University of Alcalá is working on several developments related with the network.
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55. (16C) Sáez-Cano, Guadalupe (Universidad de Alcalá)
OBSERVATION OF EXTENSIVE AIR SHOWERS PRODUCED BY ULTRA HIGH ENERGY COSMIC RAYS IN CLOUDY SKY DETECTED BY JEM-EUSO
Autores: Guadalupe Sáez-Cano¹, José Alberto Morales de los Ríos¹,², Kenji Shinozaki³, Luis del Peral¹, Héctor Prieto¹, Santiago Pérez Cano¹, & María Dolores Rodríguez Frías¹ for the JEM-EUSO collaboration 1: SPace and AStroparticle (SPAS) Group, UAH, Ctra. M

The JEM-EUSO space observatory will be launched in 2017. It will observe extensive air showers (EAS) produced by ultra high energy cosmic rays (UHECRs) when they enter in the atmosphere. Since JEM-EUSO will use the atmosphere as a detector, atmospheric conditions are important when these events are detected. Moreover, an advantage of a space based telescope is that also observation is possible under certain cloudy conditions, where most of the shower develops above the cloud. In this work, we analyze the photon propagation of EAS to the telescope under different atmospheric conditions. To do so, we have used ESAF (Euso Simulation and Analysis Framework), which is the JEM-EUSO official software, as a shower simulator, and SCSMEX (South China Sea Monsoon Experiment) to simulate how different atmospheric conditions would look like from the JEM-EUSO Infrared Camera point of view.
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56. (11A) SANCHEZ, Francisco (Universidad Politécnica de Madrid)
Presentación del proyecto GLORIA
Autores: Francisco SÁNCHEZ on behalf of GLORIA project

¿Qué es GLORIA? GLORIA significa “GLObal Robotic-telescopes Intelligent Array”. GLORIA será la primera red de telecopios robóticos del mundo de acceso libre. Será un entorno Web 2.0 donde los usuarios pueden hacer la investigación en la astronomía mediante la observación con telescopios robóticos, y/o análisis de los datos que otros usuarios han adquirido con GLORIA, o desde otras bases de datos de libre acceso, como el Observatorio Virtual Europeo (http:// www.euro-vo.org). ¿Quién puede acceder a GLORIA? La comunidad es la parte más importante del proyecto GLORIA. El acceso será libre para todo aquel que tenga una conexión a Internet y un navegador web. Por lo tanto, estará abierta no sólo a los astrónomos profesionales, sino también a cualquier persona con un interés por la astronomía. ¿Qué servicios ofrecerá GLORIA? Muchas comunidades de Internet ya se han formado para acelerar la investigación científica, a colaborar en la documentación de algo, o como proyectos sociales. La investigación en astronomía sólo puede beneficiarse de atraer muchas miradas hacia el cielo – para detectar objetos en el cielo requiere mirar en el lugar correcto en el momento oportuno. Nuestros telescopios robóticos puede buscar en el cielo, pero las grandes cantidades de datos que producen son mucho mayores que los astrónomos tienen tiempo para analizar. GLORIA proporcionará una forma de poner miles de ojos y mentes en el problema. GLORIA está destinada a ser una estructura Web 2.0, con la posibilidad de hacer experimentos reales. La comunidad no sólo va a generar contenido, como en la mayoría de la Web 2.0, sino que también podran controlar telescopios de todo el mundo, tanto directamente como a través de las observaciones programadas. La comunidad va a tomar decisiones para la red y que le dará a la “”inteligencia”” a Gloria, mientras que el trabajo esclavo (por ejemplo, la elaboración de los horarios del telescopio que satisfacen diversas limitaciones) se llevará a cabo por los algoritmos que se desarrollarán para este fin. ¿Cómo GLORIA afrontará a los desafíos? EL proyecto GLORIA definirá estándares, protocolos y metodología para: El control de telescopios robóticos: y todo relacionado con la instrumentación, es decir, cámaras, el filtro de ruedas, cúpulas, etc Dar acceso a la Web de la Red: el acceso a un número arbitrario de telescopios robóticos a través de un portal web. La realización de experimentos on-line: Será capaz de diseñar entornos web específicas para el control de telescopios para la investigación científica en algún tema específico. Llevar a cabo experimentos fuera de línea: Será capaz de diseñar entornos web específicas para el análisis de Astronomía de meta-datos producido por Gloria o otras bases de datos.”
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57. (31B) Sanchez, Juan Jose (Schott Advanced Optics)
Narrow bandpass steep edge optical filter for telescope instrumentation
Autores: S. Reichel, U. Brauneck, A Marin-Franch

The Observatorio Astrofisico de Javalambre in Spain observes with its telescope galaxies in the Local Universe in a systematic study. This is accomplished with a multi-band photometric all sky survey called Javalambre Photometric Local Universe Survey (JPLUS). A wide field camera receives the signals from universe via optical filters. In this presentation the development and design of a narrow bandpass steep edge filter with wide suppression will be shown. The filter has a full width half maximum in the range of 13-15 nm (with 15 bit obtained by a double gain scheme) to be used in MST and LST telescopes, with low power consumption (< 150 mW), bandwidth of 450 MHz and low noise (4700 electrons for 10 ns integration time). It is foreseen that a new version of the chip integrates part of the HV slow control and monitoring functionalities of the HVPA board in order to optimize cost, area, power consumption and reliability.
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58. (32B) Sánchez de la Rosa, Vicente (IAC)
Estatus de los telescopios del proyecto QUIJOTE
Autores: Vicente Sánchez de la Rosa, Afrodisio Vega Moreno, IDOM Ingeniería y Consultoría

El experimento QUIJOTE (Q-U-I JOint Tenerife) CMB, está instalado en el Observatorio del Teide con el objetivo de caracterizar la polarización del CMB y otros procesos de la emisión Galáctica y Extragaláctica en el rango de frecuencias de 10 a 40 GHz y a gran y mediana escalas angulares. El experimento QUIJOTE CMB se compondrá de dos telescopios y tres instrumentos instalados dentro de un único recinto, que ya está construido. La configuración de ambos telescopios se basa en una montura altazimutal que soporta a los reflectores primario y secundario dispuestos en una configuración Mizuguchi–Dragone cruzada. El primer telescopio y el primer instrumento multi-frecuencia (MFI 10-20 GHz) ya están operativos en el Observatorio. El segundo telescopio acaba de pasar la revisión crítica de diseño. En este poster se presenta el estatus (diseño, fabricación, integración y comisionado) de los dos telescopios del proyecto.
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59. (33B) Sánchez-Capuchino Revuelta, Jorge (Instituto de Astrofísica de Canarias)
Diseño óptico del Telescopio Solar Europeo (EST)
Autores: J. Sánchez-Capuchino y el equipo del EST.

Se presenta el diseño óptico propuesto para este telescopio solar avanzado.
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60. (12A) Santana Tschudi, Samuel (IAC-Instituto de Astrofisica de Canarias)
Diseño de las monturas opto-mecánicas del espectrógrafo ESPRESSO
Autores: Samuel Santana, Ana Fragoso

Se presenta el diseño optomecánico de este espectrógrafo ultra-estable de muy alta resolución espectral, tanto las monturas de la óptica como el banco óptico. Descripción detallada de la solución adoptada para diferentes monturas opto-mecánicas de 8 componentes ópticos del instrumento. La peculiaridad de este instrumento es que la mayor parte de los componentes ópticos son de sección rectangular en vez de circular y de pesos entre 50 y 3 kg, además las monturas tienen que estar diseñadas para que la óptica sobreviva seísmos de 3g.
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61. (13A) Santander Vela, Juan de Dios (Instituto de Astrofísica de Andalucía-CSIC)
VIA-SKA: Mapping the SKA-related capabilities of the Spanish industry
Autores: J.D. Santander-Vela, L. Verdes-Montenegro

Part of the activity of VIA-SKA has been to perform a detailed survey of the SKA-related technological capabilities of the Spanish academic centres and industrial companies involved in research infrastructures. In this poster, we will illustrate how this survey was performed, and its main results. Further information on the VIA-SKA project will be available in the talk from L. Verdes-Montenegro.
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62. (14A) Sanuy, Andreu (ICC-UB)
A preamplifier ASIC for CTA camera
Autores: A. Sanuy (ICC/UB), D. Gascon(ICC/UB), O. Blanch (IFAE), J. M. Paredes(ICC/UB), M. Ribo(ICC/UB), J. Sieiro (GRAF/UB)

The CTA project is an international initiative to build the next generation ground-based very high energy gamma-ray observatory. Having to equip a large number of channels (10^5), an integrated approach for signal processing elements has been pursued. We present a preamplifier ASIC (Application Specific Integrated Circuit) called PACTA, PreAmplifier for CTA cameras. A preamplifier is required since PMT gain of CTA on the operation will be adjusted as low as 4 times 10^4 so that PMT can be use longer than 10 years with being exposed to the night sky. With this gain, preamplifier has important role to keep sensitivity. It must be low noise to discriminate 1 p.e. signal and low power consumption and low cost. PACTA has wide dynamic range (> 15 bit obtained by a double gain scheme) to be used in MST and LST telescopes, with low power consumption (< 150 mW), bandwidth of 450 MHz and low noise (4700 electrons for 10 ns integration time). It is foreseen that a new version of the chip integrates part of the HV slow control and monitoring functionalities of the HVPA board in order to optimize cost, area, power consumption and reliability.
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63. (34B) Tenegi Sangines, Fabio (Instituto de Astrofísica de Canarias (IAC))
El Banco Óptico de EMIR: del papel a la realidad
Autores: F. Tenegi

Descripción de todo el proceso de diseño del Banco Óptico del instrumento EMIR, incluyendo guías de diseño, proceso de cálculo y comprobación de requerimientos, así como proceso de fabricación y resultado final.
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64. (35B) Zamorano, Jaime (UCM)
Instrument characterization facilities at LICA-UCM in preparation for MEGARA
Autores: J. Zamorano et al.
We describe the instrument characterization facilities at LICA-UCM that are being used in preparation for MEGARA.