{"id":18788,"date":"2018-12-21T08:18:55","date_gmt":"2018-12-21T11:18:55","guid":{"rendered":"http:\/\/www.astrofisicamas.cl\/?p=18788"},"modified":"2023-08-04T21:42:27","modified_gmt":"2023-08-04T21:42:27","slug":"fast-2-2","status":"publish","type":"post","link":"https:\/\/astrofisicamas.cl\/en\/fast-2-2\/","title":{"rendered":"Nuestra investigaci\u00f3n: C\u00famulos estelares ocultos en nuestra galaxia"},"content":{"rendered":"<h4><em><strong>Por\u00a0Jura Borissova, investigadora asociada del MAS y docente de la Universidad de Valpara\u00edso<\/strong><\/em><\/h4>\n<p><!--more--><\/p>\n<p><strong>Las Nubes Moleculares Gigantes (GMC, por sus siglas en ingl\u00e9s) son complejas gigantes de gas y polvo interestelar que, por lo general, se sit\u00faan en el plano de las galaxias, en la regi\u00f3n que llamamos \u201cdiscos gal\u00e1cticos\u201d.<\/strong> Estas son bastante fr\u00edas, con un promedio de temperatura de 10\u00ba Kelvin (260\u00baC aproximadamente), y muy grandes y su masa sobrepasa f\u00e1cilmente por millones a la de nuestro Sol. <strong>En nuestra V\u00eda L\u00e1ctea, existe la principal reserva de materia de f\u00e1cil acceso para la formaci\u00f3n de estrellas\u2026 y ah\u00ed se forman.<\/strong> A veces, las estrellas nacen de forma individual, pero, por lo general, se forman en grandes grupos a los que llamamos c\u00famulos estelares. Al encontrarse incrustados en el GMC, la abundante materia interestelar que las rodea bloquea la luz que emiten las estrellas j\u00f3venes de este nuevo c\u00famulo durante su primera evoluci\u00f3n. Por tanto, solo pueden verse a trav\u00e9s de ondas infrarrojas, las que traspasan la barrera de polvo mucho m\u00e1s f\u00e1cil que la luz visible. <strong>The \u201cVISTA Variables in the Via L\u00e1ctea eXtended (VVVX)\u00bb del Observatorio Austral Europeo (ESO, <\/strong><strong>por sus siglas en ingl\u00e9s)<\/strong> <strong>es un sondeo de rastreo cercano al infrarrojo que cubre aproximadamente 1700 grados cuadrados del disco gal\u00e1ctico y el bulbo, y que ofrece una oportunidad excelente para buscar nuevos y desconocidos c\u00famulos estelares en nuestra galaxia.<\/strong><\/p>\n<p><strong>Hemos hecho un cat\u00e1logo de 120 c\u00famulos infrarrojos nuevos y de grupos estelares presentes a lo largo del \u00e1rea del disco.<\/strong> Esta b\u00fasqueda la realiz\u00f3 la inspecci\u00f3n visual del <em>pipeline<\/em>, el que proces\u00f3 y calibr\u00f3 las im\u00e1genes obtenidas en filtro KS. Despu\u00e9s de esto, la lista inicial de candidatos se eval\u00faa usando im\u00e1genes JHK<a href=\"#_ftn1\" name=\"_ftnref1\">[1]<\/a> a color y diagramas color-magnitud K<sub>s<\/sub> v\/s (J-Ks). Cuando es posible, los par\u00e1metros Gaia DR2 se usan para calcular los movimientos propios medios, las velocidades radiales, el enrojecimiento y las distancias.<\/p>\n<p>Aproximadamente, la mitad de ellos (47%) son d\u00e9biles, compactos, muy rojos y pareciese que estuvieran asociados a otros indicadores de reciente formaci\u00f3n estelar, como los YSO, los M\u00e1seres, las regiones HII o las burbujas m\u00e1s cercanas. Se detect\u00f3 una proporci\u00f3n m\u00e1s peque\u00f1a de candidatos que est\u00e1n incrustados en comparaci\u00f3n con las b\u00fasquedas previas del VVV, como habr\u00eda de esperarse ya que la mayor parte del \u00e1rea rastreada est\u00e1 un poco m\u00e1s all\u00e1 del Ecuador gal\u00e1ctico. La menor densidad num\u00e9rica de los candidatos se debe a que el \u00e1rea que cubre esta nueva b\u00fasqueda (la parte externa del disco gal\u00e1ctico) es considerablemente menos poblada y menos rojiza que el de las b\u00fasquedas previas. Las determinaciones de distancia preliminares nos permiten rastrear c\u00famulos hasta 4,5 kpc, sin embargo, la mayor\u00eda de los candidatos a c\u00famulos est\u00e1n cercanos a 2,2 kpc. Los movimientos propios medios de los c\u00famulos muestran que, en general, siguen el movimiento del disco, tal y como era de esperarse.<\/p>\n<p><a href=\"http:\/\/adsabs.harvard.edu\/abs\/2018MNRAS.481.3902B\">http:\/\/adsabs.harvard.edu\/abs\/2018MNRAS.481.3902B<\/a><\/p>\n<p><a href=\"#_ftnref1\" name=\"_ftn1\">[1]<\/a> J, H y Ks son los nombres de los filtros pasa banda que permiten que la luz de 1.25, 1.65 y 2,15 micras pueda pasar.<\/p>","protected":false},"excerpt":{"rendered":"<p>Por\u00a0Jura Borissova, investigadora asociada del MAS y docente de la Universidad de Valpara\u00edso<\/p>","protected":false},"author":5,"featured_media":29168,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"_coblocks_attr":"","_coblocks_dimensions":"","_coblocks_responsive_height":"","_coblocks_accordion_ie_support":"","_eb_attr":"","footnotes":""},"categories":[59],"tags":[],"class_list":["post-18788","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-columnas"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v27.2 - 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