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Primeras "franjas interferométricas" de ALMA en Chajnantor
16 de Noviembre de 2009
Un equipo de astrónomos e ingenieros del Atacama Large Millimeter/submillimeter Array (ALMA) han realizado las primeras mediciones interferométricas en señales de radio –llamadas “franjas”- de una fuente astronómica, desde el alto sitio del observatorio ubicado a 5.000 metros en Chajnantor. Ello constituye un importante paso técnico para ALMA, que implicó el uso de un equipo de producción completo, incluyendo dos de las antenas de 12 metros de diámetro y sofisticados sistemas electrónicos para recibir y combinar las señales. Esta es la primera vez que todas estas piezas complejas, casi todas las cuales se encuentran a la vanguardia tecnológica, se han utilizado juntas como un solo sistema.
Las antenas fueron trasladadas hacia el Llano de Chajnantor el 16 y 17 de octubre pasado. En las semanas siguientes, el sistema fue conectado y testeado. Finalmente, se midieron las “franjas”, efecto visto cuando las señales recibidas por un par de antenas se combinan sincronizadamente. Para lograrlo, usaron una variedad de conocidos objetos astronómicos, que incluyeron la nube molecular Orión y el quásar 3C84. El equipo desarrolló experimentos para determinar exactamente la distancia entre las antenas (la “línea base”), que fue calculada en 159.8331 metros con una precisión de medio milímetro, y la diferencia de tiempo (el “retraso”) que le tomó a las señales viajar desde el edificio central, calculado en 1959.642 nanosegundos con una precisión de dos centésimas de nanosegundo. Al mismo tiempo fueron sometidos a prueba los equipos y conexiones necesarias para la operación a longitudes de onda menores. Las mediciones de las franjas del quasar 3C454.3 marcaron la primera vez en que los equipos de ALMA han detectado franjas a longitudes de onda de menos de 1mm, por lo que ALMA es ahora verdaderamente un telescopio “submilimétrico”, así como milimétrico.
Para generar las franjas, que constituyen el primer paso hacia la obtención de imágenes detalladas de los objetos astronómicos que están siendo observados, las señales son recibidas y procesadas por los sistemas de detección y electrónica de la antena, y luego transmitidas por fibra óptica al Edificio de Operaciones Técnicas de ALMA, donde son combinadas y almacenadas en los archivos.
El equipo está ahora esperando realizar los próximos pasos en el proceso –la suma de una tercera antena que les permitirá verificar mejor el software y hardware, obteniendo un “cierre de fase”, una importante capacidad que requiere de al menos tres antenas, para eliminar los errores de fase en la señal producidos por los instrumentos y la atmósfera.
El Atacama Large Millimeter/submillimeter Array (ALMA), instalación astronómica internacional, es una alianza entre Europa, Norteamérica y Asia Oriental en cooperación con la República de Chile.
Enlaces
Contactos
Douglas Pierce-Price
ESO, Garching, Alemania
Tel: +49-89-3200-6759
E-mail: dpiercep@eso.org
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