{"id":2444,"date":"2020-02-22T17:02:54","date_gmt":"2020-02-22T20:02:54","guid":{"rendered":"http:\/\/scidev\/wordpress\/?page_id=2444"},"modified":"2020-07-16T12:56:48","modified_gmt":"2020-07-16T16:56:48","slug":"el-telescopio","status":"publish","type":"page","link":"https:\/\/www.apex-telescope.org\/ns\/es\/el-telescopio\/","title":{"rendered":"El Telescopio"},"content":{"rendered":"\n<figure class=\"wp-block-image size-large\"><img loading=\"lazy\" decoding=\"async\" width=\"1280\" height=\"857\" src=\"http:\/\/www.apex-telescope.org\/ns\/wp-content\/uploads\/2020\/07\/apex_non_stop-cc.jpg\" alt=\"\" class=\"wp-image-3413\"\/><\/figure>\n\n\n\n<h3 class=\"wp-block-heading\">Publicaci\u00f3n de referencia<\/h3>\n\n\n\n<blockquote class=\"wp-block-quote is-layout-flow wp-block-quote-is-layout-flow\"><p>The Atacama Pathfinder EXperiment (APEX) \u2013 a new submillimeter facility for southern skies o &#8220;El experimento pionero de Aacama(APEX) \u2013 Una nueva instalaci\u00f3n submilim\u00e9trica para los cielos australes&#8221;<\/p><p><em>R. G\u00fcsten,&nbsp;L.-\u00c5. Nyman,&nbsp;P. Schilke,&nbsp;K. Menten,&nbsp;C. Cesarsky y R. Booth, <\/em><a rel=\"noreferrer noopener\" aria-label=\"Astronomy and Astrophysics, (2006), Volume 454, Number 2, L13-L16 (opens in a new tab)\" href=\"https:\/\/www.aanda.org\/articles\/aa\/abs\/2006\/29\/aa5420-06\/aa5420-06.html\" target=\"_blank\">Astronomy y Astrophysics, (2006), Volume 454, N\u00famero 2, L13-L16<\/a>.<\/p><\/blockquote>\n\n\n\n<div class=\"wp-block-ugb-icon-list ugb-icon-list ugb-2948cd2 ugb-icon-list--v2 ugb-icon--icon-arrow ugb-main-block\" id=\"\"><style>.ugb-2948cd2 li{--icon-size:20px;margin-bottom:16px !important}.ugb-2948cd2 li::before{height:20px !important;width:20px !important;background-image:url('data:image\/svg+xml;base64,PHN2ZyB2aWV3Qm94PSIwIDAgMTk0IDE5NCIgeG1sbnM9Imh0dHA6Ly93d3cudzMub3JnLzIwMDAvc3ZnIiBzdHlsZT0iZmlsbDojMDBkMDg0Ij48cGF0aCBkPSJNOTYuOSAyYy01Mi40IDAtOTUgNDIuNi05NSA5NXM0Mi42IDk1IDk1IDk1IDk1LTQyLjYgOTUtOTUtNDIuNi05NS05NS05NXpNNzguMiAxNTAuNGwtMTAuNi0xMC42TDExMC4zIDk3IDY3LjYgNTQuMmwxMC42LTEwLjZMMTMxLjUgOTdsLTUzLjMgNTMuNHoiPjwvcGF0aD48L3N2Zz4=')}.ugb-2948cd2 li ul{margin-bottom:16px !important}.ugb-2948cd2.ugb-icon-list ul{columns:1}<\/style><div class=\"ugb-inner-block\"><div class=\"ugb-block-content\"><ul><li><a href=\"#factsheet\">Hoja t\u00e9cnica<\/a><\/li><li><a href=\"#wobbler\">Espejo secundario oscilante<\/a><\/li><\/ul><\/div><\/div><\/div>\n\n\n\n<a id=\"factsheet\"><\/a>\n\n\n\n<hr class=\"wp-block-separator\"\/>\n\n\n\n<div style=\"height:60px\" aria-hidden=\"true\" class=\"wp-block-spacer\"><\/div>\n\n\n\n<h3 class=\"wp-block-heading\">Hoja t\u00e9cnica<\/h3>\n\n\n\n<figure class=\"wp-block-table aligncenter is-style-stripes\"><table><tbody><tr><td class=\"has-text-align-left\" data-align=\"left\"><br>Ubicaci\u00f3n<br><\/td><td class=\"has-text-align-left\" data-align=\"left\">Llano de Chajnantor. 50 km al este de San Pedro de Atacama, Norte de Chile<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Coordenadas geod\u00e9sicas<sup>1<\/sup><\/td><td class=\"has-text-align-left\" data-align=\"left\">Latitud: 23\u00ba 00&#8242; 20&#8243;.8037 Sur<br>Longitud: 67\u00ba 45&#8242; 32&#8243;.9035 Oeste<br>Altitud: 5104.47 m<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Coordenadas geoc\u00e9ntricas (ITRF2005)<sup>1<\/sup><\/td><td class=\"has-text-align-left\" data-align=\"left\">X : 2225039.5297 m<br>Y: -5441197.6292 m<br>Z: -2479303.3597 m<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Reflector principal<\/td><td class=\"has-text-align-left\" data-align=\"left\">Di\u00e1metro: 12 m<br>264 paneles de aluminio con precisi\u00f3n superficial r.m.s. de 5 \u03bcm en promedio.<br>Precisi\u00f3n de la superficie del disco completo:  &lt; 15 \u03bcm r.m.s.<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Reflector secundario<\/td><td class=\"has-text-align-left\" data-align=\"left\">Di\u00e1metro: 0.75 m. <br>Hiperboloide de aluminio <br>Pulido con un r.m.s. promedio de  2 \u03bcm.<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Fabricante<\/td><td class=\"has-text-align-left\" data-align=\"left\">Vertex Antennentechnik<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Masa<\/td><td class=\"has-text-align-left\" data-align=\"left\">125.000 Kg<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Montura<\/td><td class=\"has-text-align-left\" data-align=\"left\">Altazimutal<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Distancia focal primaria<\/td><td class=\"has-text-align-left\" data-align=\"left\">4.8 m<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">f\/D Cassegrain <\/td><td class=\"has-text-align-left\" data-align=\"left\">8<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Anchura de haz<br>(resoluci\u00f3n)<\/td><td class=\"has-text-align-left\" data-align=\"left\">7.\u20338 \u00d7 (800 \/ f [GHz])<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Precisi\u00f3n de apuntado (r.m.s.)<\/td><td class=\"has-text-align-left\" data-align=\"left\">&lt; 2\u2033 sobre todo el cielo<br>Precisi\u00f3n de apuntado en seguimiento, 0.\u20336<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Cabinas de receptores<\/td><td class=\"has-text-align-left\" data-align=\"left\">2 Nasmyth (A,B) + 1 Cassegrain (C)<\/td><\/tr><\/tbody><\/table><\/figure>\n\n\n\n<p><sup>1<\/sup> Coordenadas medidas y descritas en <a rel=\"noreferrer noopener\" aria-label=\"Wagner at al. 2015, A&amp;A, 581, A32 (opens in a new tab)\" href=\"https:\/\/ui.adsabs.harvard.edu\/abs\/2015A%26A...581A..32W\/abstract\" target=\"_blank\">Wagner at al. 2015, A&amp;A, 581, A32<\/a>.<\/p>\n\n\n\n<a id=\"wobbler\"><\/a>\n\n\n\n<div style=\"height:60px\" aria-hidden=\"true\" class=\"wp-block-spacer\"><\/div>\n\n\n\n<h3 class=\"wp-block-heading\">Espejo secundario oscilante<\/h3>\n\n\n\n<p>En 2007 el subreflector est\u00e1tico fue reemplazado con \u00e9xito por un subreflector oscilante, el llamado &#8220;wobbler&#8221;. Este &#8220;wobbler&#8221;, en los casos donde puede ser usado, mejora significativamente la calidad de la observaci\u00f3n. Al alternar r\u00e1pidamente entre dos posiciones del cielo (el &#8220;throw&#8221;), las observaciones son menos sensibles a inestabilidades dependientes del tiempo, procedentes tanto del instrumento como de la atm\u00f3sfera. Por el momento, el wobbler se puede usar solamente con los receptores heterodinos.<\/p>\n\n\n\n<p>En el a\u00f1o 2018 se instal\u00f3 en APEX un nuevo mecanismo de oscilaci\u00f3n de dise\u00f1o m\u00e1s avanzado. Este nuevo wobbler tiene las siguientes caracter\u00edsticas:<\/p>\n\n\n\n<figure class=\"wp-block-table is-style-stripes\"><table><tbody><tr><td class=\"has-text-align-left\" data-align=\"left\">Direcci\u00f3n de movimiento<\/td><td class=\"has-text-align-left\" data-align=\"left\">Azimutal<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Frecuencia de oscilaci\u00f3n (R)<\/td><td class=\"has-text-align-left\" data-align=\"left\">Hasta 2.0 Hz<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">M\u00e1xima amplitud de oscilaci\u00f3n (T<sub>max<\/sub>)<\/td><td class=\"has-text-align-left\" data-align=\"left\">Si R \u2264 1.5 Hz,  T<sub>max<\/sub> = 300\u2033<br>Si R &gt; 1.5 Hz,  T<sub>max<\/sub> = (300 &#8211; 100 \u00d7 (R \u2212 1.5))\u2033<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Rendimiento<\/td><td class=\"has-text-align-left\" data-align=\"left\">90% para R = 0.5 Hz<br>70%-80% para R = 2.0 Hz, dependiendo de la amplitud<\/td><\/tr><tr><td class=\"has-text-align-left\" data-align=\"left\">Modos de operaci\u00f3n<\/td><td class=\"has-text-align-left\" data-align=\"left\">Negativo (izquierda)<br>Positivo (derecha)<br>Sim\u00e9trico (izq.-der.-der.-izq.)<\/td><\/tr><\/tbody><\/table><\/figure>\n\n\n\n<p>Cuando se hacen mediciones espectrosc\u00f3picas con los receptores heterodinos se recomienda no usar \u00a0<em>R<\/em> = 1.0 Hz como frecuencia de oscilaci\u00f3n ya que podr\u00eda entrar en resonancia con la frecuencia de funcionamiento de las bombas criog\u00e9nicas que tambi\u00e9n es de 1 Hz. Sin embargo, en el caso de observaciones en modo &#8220;total-power&#8221; con receptores heterodinos es una ventaja usar\u00a0<em>R<\/em> = 1.0 Hz. El espejo secundario oscilante mejora la calidad de las observaciones cuando se observan fuentes con extensiones menores a dos veces la m\u00e1xima amplitud de oscilaci\u00f3n (entre 8 y 10 minutos de arco). Las fuentes t\u00edpicas donde su uso puede ser beneficioso son: envolturas circumestelares, planetas, n\u00facleos moleculares calientes (hot-cores) y la mayor\u00eda de las galaxias.<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Publicaci\u00f3n de referencia The Atacama Pathfinder EXperiment (APEX) \u2013 a new submillimeter facility for southern skies o &#8220;El experimento pionero de Aacama(APEX) \u2013 Una nueva instalaci\u00f3n submilim\u00e9trica para los cielos australes&#8221; R. G\u00fcsten,&nbsp;L.-\u00c5. Nyman,&nbsp;P. Schilke,&nbsp;K. Menten,&nbsp;C. Cesarsky y R. Booth, <a href=\"https:\/\/www.apex-telescope.org\/ns\/es\/el-telescopio\/\" class=\"read-more\">Read More &#8230;<\/a><\/p>\n","protected":false},"author":1,"featured_media":0,"parent":0,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":{"ngg_post_thumbnail":0,"spay_email":"","footnotes":""},"class_list":["post-2444","page","type-page","status-publish","hentry"],"featured_image_urls":{"full":"","thumbnail":"","medium":"","medium_large":"","large":"","1536x1536":"","2048x2048":"","education-hub-thumb":""},"post_excerpt_stackable":"<p>Publicaci\u00f3n de referencia The Atacama Pathfinder EXperiment (APEX) \u2013 a new submillimeter facility for southern skies o &#8220;El experimento pionero de Aacama(APEX) \u2013 Una nueva instalaci\u00f3n submilim\u00e9trica para los cielos australes&#8221;R. G\u00fcsten,&nbsp;L.-\u00c5. Nyman,&nbsp;P. Schilke,&nbsp;K. Menten,&nbsp;C. Cesarsky y R. Booth, Astronomy y Astrophysics, (2006), Volume 454, N\u00famero 2, L13-L16. Hoja t\u00e9cnicaEspejo secundario oscilante Hoja t\u00e9cnica Ubicaci\u00f3nLlano de Chajnantor. 50 km al este de San Pedro de Atacama, Norte de ChileCoordenadas geod\u00e9sicas1Latitud: 23\u00ba 00&#8242; 20&#8243;.8037 SurLongitud: 67\u00ba 45&#8242; 32&#8243;.9035 OesteAltitud: 5104.47 mCoordenadas geoc\u00e9ntricas (ITRF2005)1X : 2225039.5297 mY: -5441197.6292 mZ: -2479303.3597 mReflector principalDi\u00e1metro: 12 m264 paneles de aluminio con precisi\u00f3n superficial r.m.s. de&hellip;<\/p>\n","category_list":"","author_info":{"name":"apex","url":"https:\/\/www.apex-telescope.org\/ns\/author\/apex\/"},"comments_num":"0 comments","featured_image_urls_v2":{"full":"","thumbnail":"","medium":"","medium_large":"","large":"","1536x1536":"","2048x2048":"","education-hub-thumb":""},"post_excerpt_stackable_v2":"<p>Publicaci\u00f3n de referencia The Atacama Pathfinder EXperiment (APEX) \u2013 a new submillimeter facility for southern skies o &#8220;El experimento pionero de Aacama(APEX) \u2013 Una nueva instalaci\u00f3n submilim\u00e9trica para los cielos australes&#8221;R. G\u00fcsten,&nbsp;L.-\u00c5. Nyman,&nbsp;P. Schilke,&nbsp;K. Menten,&nbsp;C. Cesarsky y R. Booth, Astronomy y Astrophysics, (2006), Volume 454, N\u00famero 2, L13-L16. Hoja t\u00e9cnicaEspejo secundario oscilante Hoja t\u00e9cnica Ubicaci\u00f3nLlano de Chajnantor. 50 km al este de San Pedro de Atacama, Norte de ChileCoordenadas geod\u00e9sicas1Latitud: 23\u00ba 00&#8242; 20&#8243;.8037 SurLongitud: 67\u00ba 45&#8242; 32&#8243;.9035 OesteAltitud: 5104.47 mCoordenadas geoc\u00e9ntricas (ITRF2005)1X : 2225039.5297 mY: -5441197.6292 mZ: -2479303.3597 mReflector principalDi\u00e1metro: 12 m264 paneles de aluminio con precisi\u00f3n superficial r.m.s. de&hellip;<\/p>\n","category_list_v2":"","author_info_v2":{"name":"apex","url":"https:\/\/www.apex-telescope.org\/ns\/author\/apex\/"},"comments_num_v2":"0 comments","_links":{"self":[{"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/pages\/2444","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/comments?post=2444"}],"version-history":[{"count":8,"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/pages\/2444\/revisions"}],"predecessor-version":[{"id":4795,"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/pages\/2444\/revisions\/4795"}],"wp:attachment":[{"href":"https:\/\/www.apex-telescope.org\/ns\/wp-json\/wp\/v2\/media?parent=2444"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}