Catálogo Messier Para Observaciones De Cielo Profundo

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Catálogo Messier Para Observaciones De Cielo Profundo Catálogo Messier para observaciones de Cielo Profundo ÍNDICE M1 ………………………………………….…3 M28 ……………………………………….38 M2 ……………………………………….…....5 M29 ……………………………………….39 M3 …………………………………………….7 M30 ……………………………………….40 M4 …..………………………………………...9 M31 ……………………………………….41 M5 …..………………………………………..11 M32 ……………………………………….44 M6 …..…………………….………………….13 M33 ……………………………………….46 M7 …..……………………….……………….14 M34 ……………………………………….47 M8 …..………………………….…………….15 M35 ……………………………………….48 M9 …..…………………………….………….16 M36 ……………………………………….50 M10 ….……………………………………….18 M37 ……………………………………….51 M11 ….……………………………………….19 M38 ……………………………………….52 M12 ….……………………………………….20 M39 ……………………………………….53 M13 ….……………………………………….21 M40 ……………………………………….54 M14 ….……………………………………..…22 M41 ……………………………………….55 M15 ….………………………………………..24 M42 ……………………………………….56 M16 ….…………………………………….….26 M43 ……………………………………….58 M17 ….………………………………….….…27 M44 ……………………………………….59 M18 ….………………………………….….…28 M45 ……………………………………….60 M19 ….……………………………………..…29 M46 ……………………………………….63 M20 ….…………………………………….….30 M47 ……………………………………….64 M21 ….…………………………………….….31 M48 ……………………………………….65 M22 ….………………………………….….…32 M49 ……………………………………….66 M23 ….………………………………….….…33 M50 ……………………………………….67 M24 ….………………………………….….…34 M51 ……………………………………….68 M25 ….………………………………….….…35 M52 ……………………………………….69 M26 ….………………………………….….…36 M53 ……………………………………….70 M27 ….……………………………………..…37 M54 ……………………………………….71 1 Catálogo Messier para observaciones de Cielo Profundo M55 …………………………………………....72 M85 ………………………………….………109 M56 ……………………………………………73 M86 ………………………………….………110 M57 ……………………………………………74 M87 ………………………………….………111 M58 ……………………………………………76 M88 ………………………………………….113 M59 ……………………………………………77 M89 ……………………………………….…114 M60 ……………………………………………78 M90 ……………………………………….…115 M61 ……………………………………………79 M91 ……………………………………….…116 M62 ……………………………………………80 M92 ……………………………………….…117 M63 ……………………………………………81 M93 ………………………………………….118 M64 ……………………………………………82 M94 …………………………………….....…119 M65 ……………………………………………84 M95 ……………………………………...…..120 M66 ……………………………………………85 M96 ……………………………………...…..121 M67 ……………………………………………86 M97 ……………………………………...…..122 M68 ……………………………………………87 M98 ……………………………………...…..123 M69 ……………………………………………88 M99 ……………………………………….…124 M70 ……………………………………………89 M100 …………………………………….…..125 M71 ……………………………………………90 M101 ……………………………………...…126 M72 ……………………………………………91 M102 ……………………………………...…127 M73 ……………………………………………92 M103 ………………………………………...128 M74 ……………………………………………94 M104 ………………………………………...129 M75 ……………………………………………95 M105 …………………………………………130 M76 ……………………………………………96 M106 …………………………………………131 M77 ……………………………………………98 M107 …………………………………………132 M78 …………………………………………...100 M108 …………………………………………133 M79 ……………………………………..….…101 M109 …………………………………………134 M80 ………………………………….……..…102 M110 …………………………………………135 M81 ………………………………….….….…104 M82 ………………………………….…..……105 M83 ………………………………….………..106 M84 ………………………………….………..108 2 Catálogo Messier para observaciones de Cielo Profundo La Nebulosa del Cangrejo 05:34.5 M 1 Ascensión Recta (horas:minutos) +22:01 Declinación Restos de Supernova M 1 (grados:minutos) (NGC 1952) en Taurus Distancia 6 300 (años luz) Magnitud 8,4 (magnitud) Aparente Tamaño 6x4 (arc.min) Aparente Historia La Nebulosa del Cangrejo es una nube de gas creado por la explosión de una estrella supernova. Fue registrada el 4 de Julio de 1054 D.C por astrónomos chinos, siendo su brillo cuatro veces más brillante que Venus (aproximadamente magnitud -6). De acuerdo con los registros, fue visible a la luz del día durante 23 días y 653 días en el cielo nocturno. También fue probablemente registrado por los artistas indios Anasazi, como indican los descubrimientos en el Cañón Navaho y en White Mesa (ambos en Arizona) así como en el Parque Nacional del Cañón Chaco (Nuevo México). La supernova de 1054 también tuvo asignada la designación de estrella variable CM Tauri. Esta es una de las pocas supernovas observadas a lo largo de la historia en nuestra Galaxia de la Vía Láctea. Los restos de la nebulosa fueron descubiertos por John Bevis en 1731, quien lo añadió a su atlas del cielo, Uranographia Britannica . Charles Messier la encontró de forma independiente el 28 de Agosto de 1758, cuando estaba buscando el cometa Halley en su primer retorno pronosticado, y en principio pensó que era el cometa. Por supuesto, pronto reconoció que no tenía el movimiento propio aparente, y lo catalogó el 12 de Septiembre de 1758. El descubrimiento de este objeto fue lo que llevó a Charles Messier a comenzar la compilación de este catálogo. También fue el descubrimiento de este objeto, el cual tenía un gran parecido con un cometa (1758 De la Nux, C/1758 K1) el que le atrajo a la búsqueda de cometas. Aunque el catálogo de Messier fue ante todo una compilación para prevenir confusiones de estos objetos con cometas, M 1 fue nuevamente confundido con el cometa Halley en el segundo retorno pronosticado de 1835. Esta nebulosa fue bautizada como “Nebulosa del Cangrejo” con motivo de un dibujo realizado por Lord Rosse en 1844. De los primeros observadores Messier, Bode y William Herschel comentaron que esta nebulosa no era posible resolverle las estrellas. A pesar de ello, William Herschel pensó que era un sistema estelar que podría resolverse con telescopios mayores. Éste y otros, incluyendo a Lassell en los 1850, confundieron estructuras filamentosas como indicación de resolubilidad. Las primeras observaciones espectroscópicas, por ejemplo por Winlock, revelaron la naturaleza gaseosa de este objeto a finales del siglo XIX. La primera fotografía se obtuvo en 1892 con un telescopio de 50 centímetros. Las primeras investigaciones serias de su espectro se llevaron a cabo en 1913 por Vesto Slipher. Éste encontró que las líneas de emisión espectral tenían divisiones; más tarde se reconoció que la verdadera razón de esto era el desplazamiento Doppler, debido a que unas partes de la nebulosa se acercaban a nosotros (las líneas estaban desplazadas al azul) y otras alejándose (líneas desplazadas al rojo). Heber D. Curtis, en su descripción de este objeto basada en las fotografías del Observatorio Lick, la clasificó de forma dudosa como una nebulosa planetaria (Curtis 1918), una visión que solo fue refutada en 1933. 3 Catálogo Messier para observaciones de Cielo Profundo Localización La Nebulosa del Cangrejo puede encontrarse con bastante facilidad a partir de Zeta Tauri (o 123 Tauri), el 'Cuerno Sur' del Toro, una estrella de tercera magnitud que puede encontrarse fácilmente al Este-Noreste de Aldebarán (Alfa Tauri). M 1 se encuentra más o menos a 1 grado Norte y 1 grado Oeste de Zeta, ligeramente al sur y aproximadamente medio grado al Oeste de la estrella de magnitud 6, Struve 742. Descripción La nebulosa puede verse bien bajo un cielo oscuro y despejado, pero puede ser igualmente fácil perderla con el fondo de contaminación lumínica en condiciones menos favorables. M 1 es visible como una mancha tenue con unos binoculares 7x50 o 10x50. Con un poco más de aumento, puede verse como una mancha nebulosa ovalada, rodeada por un halo. En telescopios de a partir de 10 centímetros de apertura, comienzan a aparecer algunos detalles de su forma, con algunos indicios de estructuras de puntos o rayas en la zona central de la nebulosa; John Mallas informa que bajo condiciones excelentes, un observador experto puede ver a través de la porción interior de la nebulosa. Los aficionados pueden comprobar la impresión de Messier de que M 1 efectivamente parece un débil comenta sin cola en pequeños instrumentos. Solo bajo excelentes condiciones y con mayores telescopios, a partir de 40 centímetros de apertura, empiezan a hacerse visibles los filamentos estructuras finas. Como la Nebulosa del Cangrejo se sitúa solo a 1 grado y medio de la eclíptica, existen frecuentes conjunciones y ocasionales tránsitos de planetas, así como ocultaciones por parte de la Luna. M1 es rico en estrellas, aunque una mirada más atenta descubrirá que la densidad disminuye alrededor de la nebulosa, probablemente, por efecto de materia oscura. La más brillante de las estrellas es la bellísima doble S422, de magnitudes 7,1 y 7,7, a 3"6, en posición E-W, amarilla y anaranjada. 4 Catálogo Messier para observaciones de Cielo Profundo Catálogo Charles Messier: Objeto M 2 21:33.5 M 2 Ascensión Recta (horas:minutos) Cúmulo Globular M 2 (NGC -00:49 Declinación 7089), clase II en Aquarius (grados:minutos) Distancia 37 500 (años luz) Magnitud 6,5 (magnitud) Aparente Dimensión 16,0 (min.arco) Aparente Historia Descubierta por Jean-Dominique Maraldi en 1746, Charles Messier la descubrió independientemente y la catalogó exactamente 14 años después, el 11 de Septiembre de 1760 como una 'nebulosa sin estrellas'. William Herschel fue el primero que definió sus estrellas. Localización M 2 se encuentra fácilmente desde Alfa y Beta Aquarii, así como Epsilon Pegasi. Está 5 grados al norte de Beta Aquarii, en la misma declinación que Alfa Aquarii. Descripción M 2 tiene un diámetro de unos 175 años luz. Contiene unas 150 000 estrellas y es uno de los cúmulos más ricos y compactos, como indica su clasificación en la clase de densidad II. Este cúmulo es de notable elipticidad (elipticidad 9, o forma E1). El cúmulo se encuentra a unos 37 500 años luz (de acuerdo con la base de datos de W.E. Harris), se sitúa bastante más allá del Centro Galáctico. Visualmente es de una magnitud aparente de 6,5 y abarca unos 6 - 8 minutos de arco de diámetro, presentando una brillante región central comprimida de unos 5'. En las fotografías típicas puede extenderse hasta los 12,9 minutos de arco, y las fotografías detalladas revelan que se extiende hasta un diámetro
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