{"id":16282,"date":"2017-09-06T10:01:51","date_gmt":"2017-09-06T13:01:51","guid":{"rendered":"http:\/\/www.astrofisicamas.cl\/?p=16282"},"modified":"2023-08-07T18:48:21","modified_gmt":"2023-08-07T18:48:21","slug":"nuestra-investigacion-cefeidas-de-tipo-ii-indicadores-de-distancia-usando-series-temporales-del-relevamiento-vvv","status":"publish","type":"post","link":"https:\/\/astrofisicamas.cl\/en\/nuestra-investigacion-cefeidas-de-tipo-ii-indicadores-de-distancia-usando-series-temporales-del-relevamiento-vvv\/","title":{"rendered":"Nuestra Investigaci\u00f3n: Cefeidas de tipo II: Indicadores de distancia usando series temporales  del relevamiento VVV"},"content":{"rendered":"<h4 data-fontsize=\"16\" data-lineheight=\"17\"><em><strong>Por Vittorio Braga, investigador postdoctoral MAS y\u00a0de la Universidad Andr\u00e9s Bello<\/strong><\/em><\/h4>\n<p><!--more--><\/p>\n<p><strong>Las estrellas variables de tipo Cefeidas son usadas, desde m\u00e1s de 100 a\u00f1os, como candelas est\u00e1ndares para la determinaci\u00f3n de distancias<\/strong>. El periodo de pulsaci\u00f3n de la mayor\u00eda de ellas es entre 1 y 100 d\u00edas, y \u00a0pueden ser distintas entre Cefeidas Cl\u00e1sicas (m\u00e1s j\u00f3venes de 300 mega-a\u00f1os) y Cefeidas de tipo II (CT2, m\u00e1s viejas de 10 giga-a\u00f1os). Las Cefeidas \u00a0Cl\u00e1sicas son las m\u00e1s usadas entre las dos, principalmente porqu\u00e9 son 3 magnitudes m\u00e1s brillantes que las CT2, y porqu\u00e9 permitieron la calibraci\u00f3n de la escala de distancia de las supernovas.<\/p>\n<p>Sin embargo, las Cefeidas Cl\u00e1sicas tienen la desventaja de encontrarse \u00a0solo donde hay formaci\u00f3n estelar en curso. Por otro lado, las CT2 se encuentran en casi todas partes, excepto en \u00a0los sistemas estelares con ramas horizontales demasiado rojas.<\/p>\n<p>El bulbo Gal\u00e1ctico es el lugar m\u00e1s denso de estrellas de la Galaxia y est\u00e1 \u00a0poblado por estrellas viejas, por lo tanto es el lugar m\u00e1s apropiado para encontrar un largo n\u00famero de CT2. Adem\u00e1s, mientras las regiones externas del bulbo fueron ya escaneadas por el sondeo OGLE en el visible&#8212;encontrando m\u00e1s de 300 CT2&#8212;hay todav\u00eda que investigar las \u00a0regiones centrales, entre un grado del plano Gal\u00e1ctico.<\/p>\n<p>De hecho, el polvo en estas regiones es tan abundante que solo \u00a0observando en las bandas del infrarrojo cercano se pueden detectar estas \u00a0variables.<\/p>\n<p>El sondeo VVV provee series temporales, en el infrarrojo cercano, de estrellas en una \u00e1rea de 520 grados cuadrados, incluido el bulbo \u00a0Gal\u00e1ctico.<\/p>\n<p>Como primer paso, encontramos las curvas de luz de CT2 conocidas y \u00a0obtuvimos sus distancias con la relaci\u00f3n entre periodo y luminosidad. Esta relaci\u00f3n provee el brillo intr\u00ednseco de una estrella, conociendo su \u00a0periodo. Hemos considerado varias calibraciones de esta relaci\u00f3n y obtuvimos distancias individuales hasta 65 kpc (es decir, en el Halo \u00a0gal\u00e1ctico al otro lado de la Galaxia) y una incertidumbre media de cerca el 3-4%.<\/p>\n<p>Como segundo paso, estamos trabajando en un software que seleccione las candidatas variables en las regiones m\u00e1s centrales, teniendo como input las series temporales. Los criterios de rechazo para distinguir \u00a0entre candidatas variables y estrellas no variables o estrellas con series temporales de calidad insuficiente, incluyen estad\u00edstica de los \u00a0m\u00e1ximos del periodograma, la amplitud de la serie de Fourier de ajuste de la curva de luz y el rechazo de datos basado en la desviaci\u00f3n est\u00e1ndar de la media.<\/p>\n<p><strong>Las CT2 ofrecen la oportunidad de delinear la estructura del bulbo Gal\u00e1ctico con estrellas viejas. Son mucho menos que las RR Lyrae, que \u00a0tambi\u00e9n se usan para determinaci\u00f3n de distancias, pero son m\u00e1s brillantes y por \u00a0eso pueden proveer distancias de sistemas estelares m\u00e1s lejanos en el Grupo Local de galaxias<\/strong>. Por otro lado, las CT2 gal\u00e1cticas conocidas, hasta \u00a0ahora, son menos de 1000. Por eso es importante investigar el interior del bulbo Gal\u00e1ctico para aumentar la estad\u00edstica de estos objetos.<\/p>\n<p><a href=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/09\/2017_09_06_VBraga2.jpg\"><img loading=\"lazy\" decoding=\"async\" class=\"aligncenter wp-image-16283 size-large\" src=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/09\/2017_09_06_VBraga2-1024x906.jpg\" alt=\"\" width=\"1024\" height=\"906\" \/><\/a><\/p>","protected":false},"excerpt":{"rendered":"<p>Por Vittorio Braga, investigador postdoctoral MAS y\u00a0de la Universidad Andr\u00e9s Bello<\/p>","protected":false},"author":3,"featured_media":29246,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_coblocks_attr":"","_coblocks_dimensions":"","_coblocks_responsive_height":"","_coblocks_accordion_ie_support":"","_eb_attr":"","footnotes":""},"categories":[59,1],"tags":[],"class_list":["post-16282","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-columnas","category-uncategorized"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v27.2 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>Nuestra Investigaci\u00f3n: Cefeidas de tipo II: Indicadores de distancia usando series temporales del relevamiento VVV - Instituto Milenio de Astrof\u00edsica MAS<\/title>\n<meta name=\"robots\" content=\"index, follow, max-snippet:-1, max-image-preview:large, max-video-preview:-1\" \/>\n<link rel=\"canonical\" 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