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Repositorio Universidad Nacional UNIVERSIDAD NACIONAL DE COLOMBIA FACULTAD DE CIENCIAS DEPARTAMENTO DE F´ISICA LA REGION´ DE L´INEAS CORONALES EN GALAXIAS SEYFERT 1 Y SEYFERT 2 Jos´eGregorio Portilla B. Tesis realizada bajo la orientaci´on y direcci´on de los investigadores Dr. Juan Manuel Tejeiro S. (Universidad Nacional de Colombia) y el Dr. Alberto Rodr´ıguez Ardila (Director Asociado) del Laborat´orio Nacional de Astrofisica, M. G., Brasil, y presentada como requisito parcial para la obtenci´on del t´ıtulo de Doctor en f´ısica te´orica. Bogot´a, 2011 . A mis padres Mar´ıa Teresa y Jos´e Gregorio y mi hermano Luis Rodrigo Agradecimientos Reservo este espacio para agradecer a todas aquellas personas que de una u otra forma, con su amistad, apoyo, aliento y conocimientos permitieron que esta tesis llegara a su feliz t´ermino. Mi agradecimiento puntual va para: Alberto Rodr´ıguez-Ardila, a quien le debo mi conocimiento en galaxias activas, por su muy valiosa amistad, su paciencia sin l´ımites, aliento y consejos en los momentos dif´ıciles y por su comprensi´on. Si esta tesis sali´ofinalmente adelante se debe a ´el. Juan Manuel Tejeiro, quien me alent´oa proseguir mis estudios en f´ısica y obtener el doctorado, por su amistad, apoyo incondicional y confianza. Los colegas del Observatorio Astron´omico, por su invaluable amistad, apoyo, comprensi´on y sobre todo aliento. Debo agradecer, muy espec´ıficamente, a Armando Higuera, quien me anim´oa realizar el doctorado conjuntamente con ´el. Su apoyo irrestricto en todo momento permiti´oadentrarme conjuntamente con ´el en el estudio de las galaxias activas. A la Dra. Almudena Prieto, del Instituto Astrof´ısico de Canarias (IAC), por sus muy valiosas su- gerencias y por su muy gentil invitaci´on y colaboraci´on en mi pasant´ıa realizada en el IAC. Al Dr. Luc Binnet, del Instituto de Astronom´ıa de la UNAM, a quien debo agradecer no solo por su hospitalaria recepci´on en el mencionado instituto sino tambi´en por sus valiosas sugerencias en lo relacionado con los modelos de fotoionizaci´on. Al personal t´ecnico y cient´ıfico del Laborat´orio Nacional de Astrofisica, en Itajub´a, Brasil, por su disponibilidad, accesibilidad y don de gentes, pues con ello hicieron m´as f´acil las medidas espec- trosc´opicas realizadas all´ı. A mis padres y mi hermano, por su comprensi´on, aliento y amor incondicional. A los profesores de la Universidad Nacional Oscar´ Osorno, Emiliano Barreto y Luis Carlos Jim´enez, por su amistad y apoyo. A Ingrid Mar´ıa, por existir. 4 Resumen Varias muestras de espectros galaxias activas, casi en su totalidad conformadas por galaxias Seyfert, fueron analizadas con el prop´osito de estudiar la emisi´on de l´ıneas coronales, LCs, (l´ıneas prohibidas de alta ionizaci´on). La primera muestra est´aconformada por 54 n´ucleos activos con espectros en el infrarrojo cercano (0.8-2.3 µm); la segunda es una selecci´on de 265 galaxias en las que se detect´oal menos una l´ınea coronal en el rango ´optico del espectro, obtenidos por la prospecci´on del cielo Sloan (SDSS, por sus siglas en ingl´es). Una tercera muestra est´aconstituida por 34 galaxias emisoras de l´ıneas coronales (20 de las cuales fueron obtenidas del SDSS) y las restantes tomadas en el observatorio de Pico dos Dias en Brasil. Se observa emisi´on coronal en el infrarrojo cercano en el 63 % de las galaxias que conforman la primera mues- tra, siendo las l´ıneas de [Si vi] 1.9630 µmy[S viii] 0.9913 µm las que aparecen con mayor frecuencia en las galaxias Seyfert 2 que en las Seyfert 1. L´ıneas con m´as alto potencial de ionizaci´on (PI), como [Si x] 1.4301 µm y [S ix] 1.2520 µm, aunque menos conspicuas que las anteriores, son igualmente observadas en ambos tipos de galaxias en proporciones similares. La proporci´on de LCs es semejante en objetos Sy1 y Sy2. Correlaci´on entre el ancho completo a mitad de la altura (FWHM) con respecto al PI es solo observada en pocos objetos. Parece existir evidencia de desexcitaci´on colisional para las l´ıneas de m´as alto PI a trav´es de un gradiente de densidad. Tambi´en presentamos la influencia que tiene sobre la emisi´on coronal la luminosidad en rayos X tanto suaves (0.1-2.4 keV) como duros (2-10 keV). Con respecto a los datos del SDSS, se encontr´oque de 659 espectros de galaxias Seyfert con magnitudes aparen- tes hasta 17.5, la tercera parte muestran emisi´on de Fe vii. Discriminadas por tipo se hall´oque las probabilidades de emisi´on de ese i´on son de 43 %, 15 % y 56 % para las galaxias Sy1 normales Sy2 y NLS1, respectivamente. Se confirma la anisotrop´ıa de emisi´on de [Fe vii] λ6087 entre objetos Sy1 y Sy2 (mayor cantidad de emisi´on en los primeros que en los segundos). Dicha anisotrop´ıa es observada tambi´en en las l´ıneas de [Ne v] λ3426 y de [Fe x] λ6374. Se observa, con base a ´ındices de color, que en aquellas galaxias emisoras de LCs, las Sy1 tienden a ser m´as azuladas que las Sy2. Todo lo anterior sugiere que la principal regi´on de emisi´on de Fe vii reside en la cara interna del toroide oscurecedor. Por otro lado, se observan fuertes correlaciones entre las luminosidades de las LCs (como tambi´en en sus flujos). Tambi´en existen correlaciones entre los flujos de las LCs y los flujos de l´ıneas prohibidas de menor PI. Tambi´en existen correlaciones fuertes entre las LCs y los rayos X suaves (0.1-2.4 keV) y entre el Fe vii y Ne v y los rayos X duros (2-10 keV) aunque este ´ultimo resultado es marginal. En suma, esto apoya un proceso de fotoionizaci´on proveniente de una fuente central como mecanismo principal de ionizaci´on de las LCs. Se reporta tambi´en una relaci´on entre la luminosidad de algunas LCs y la luminosidad en radio en 1.4 GHz hasta un valor − − de luminosidad en radio (log L ∼31.5 erg. s 1 Hz 1) a partir del cual la luminosidad de la LC es irregular y con tendencia a disminuir. Algo semejante se observa con l´ıneas de m´as baja ionizaci´on. Se determinaron condiciones f´ısicas para la zona de emisi´on de Fe vii: se hallaron valores de temperatura comprendidos entre 10000 y 50000 K − y densidades electr´onicas que pueden alcanzar a los sumo 106 a 107 cm 3. Finalmente, con la tercera muestra conformada por espectros con emisi´on coronal particularmente intensa, se realiz´oun estudio cinem´atico de la zona de emisi´on coronal. El comportamiento de las LCs es diferente del que presentan l´ıneas de baja ionizaci´on tales como O iii y O i. Las LCs tienden por lo general a presentar un FWHM un poco mayor, ´ındice de asimetr´ıa (IA) negativo, valor de kurtosis m´as peque˜no y desplazamiento de pico de l´ınea pronunciado hacia el azul. Dicho desplazamiento del pico de l´ınea sugiere la existencia de dos poblaciones de galaxias con relaci´on a la emisi´on de [Fe vii] λ6087. Se estableci´oque para este i´on el desplazamiento del pico de l´ınea hacia al azul viene acompa˜nado por un marcado IA con alas extendidas tambi´en hacia el azul que pueden indicar que el gas coronal hace parte de outflows producidos por el chorro de radio. Se encontraron anticorrelaciones moderadas entre luminosidades en radio a 1.4 GHz y el desplazamiento del pico de l´ınea de las LCs que sugiere una participaci´on del chorro de radio en el desplazamiento del gas coronal en direcci´on hacia el observador. ´Indice general 1. N´ucleos activos de galaxias 13 1.1. Definici´on ..................................... ........ 13 1.2. LasgalaxiasSeyfert ............................. .......... 14 1.3. OtrasgalaxiasconAGNs . ......... 16 1.4. ParadigmadelAGN ................................ ....... 17 1.5. Laregi´ondel´ıneascoronales . .............. 19 1.5.1. L´ıneascoronalesenAGNs . ......... 20 1.6. Estatesis ...................................... ....... 26 2. Observaciones en el IR cercano 29 2.1. Introducci´on.................................. .......... 29 2.2. L´ıneas coronales en el infrarrojo cercano . .................. 29 2.3. Selecci´ondelamuestra . ........... 31 2.4. Resultados..................................... ........ 33 2.4.1. Cinem´aticadelasLCs . ........ 49 2.4.2. Relaci´on entre las luminosidades de las LCs . ............... 53 2.4.3. Relaci´onentreLCsyrayosX . ......... 56 2.4.4. RayosXsuaves(0.1-2.4keV) . ......... 57 2.4.5. RayosXduros(2-10keV) . ....... 59 2.5. Conclusiones ................................... ........ 62 3. L´ıneas coronales en una muestra del SDSS (I) 63 3.1. Introducci´on.................................. .......... 63 3.2. Laprospecci´onSloan. ........... 65 3.3. Selecci´ondelamuestra . ........... 66 3.4. Lamuestra ...................................... ...... 69 4. L´ıneas coronales en una muestra del SDSS (II) 79 4.1. Laemisi´oncoronalenlamuestraMT . ............ 79 4.2. Anisotrop´ıa de emisi´on de Fe vii engalaxiasSeyfert .. .. .. .. .. .. .. .. .. 83 4.3. Velocidad de la regi´on de emisi´on coronal . ................. 90 5 6 ´INDICE GENERAL 4.4. ¿Fotoionizaci´onocolisi´on?. ................ 94 4.4.1. Relaciones entre las luminosidades . ............. 95 4.5. Relaci´onconemisi´onderayosX . ............. 99 4.5.1. RayosXsuaves:Rosat(0.1-2.4keV) . ........... 99 4.5.2. RayosXduros:2-10keV . ...... 101 4.6. Relaci´onconemisi´onderadio . .............. 103 4.7. Temperatura y densidad con base a emisi´on de Fe vii ..................... 109 4.8. Unadiscusi´onadicional . ............ 116 5. Cinem´atica de l´ıneas coronales en el ´optico 125 5.1. Introducci´on.................................. .......... 125 5.2. Cinem´aticadelaCLRenAGNs . ......... 125 5.3. Selecci´ondelamuestra . ........... 127 5.4. Observaci´on y reducci´on de datos de la submuestra P .
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