AS NUVENS DE MAGALHÃES

Meu Projeto

Os desenhos formados pelas estrelas - AS CONSTELAÇÕES - são como janelas que se abrem para a infinitude do universo

e que possibilitam nossa mente a ir percebendo que existe mais, bem mais, entre o céu e a terra...;

bem como percebendo que o caos, vagarosamente, vai se tornando Cosmos e este por nossa mente sendo conscientizado.

Quer dizer, nossa mente é tão infinita quanto infinito é o Cosmos.

Com um abraço estrelado,

Janine Milward

AS NUVENS DE MAGALHÃES

As Nuvens de Magalhães nos trazem imensa felicidade

por morarmos no hemisfério sul e podermos, então,

usufruir da maravilhosa observação a olho nu

dessas Nuvens que não são nuvens e sim galáxias

e que escondem um verdadeiro mundo de tesouros....

Tesouros que vão sendo, vagarosamente,

descobertos e trazidos ao nosso conhecimento!

http://apod.nasa.gov/apod/image/1105/vltsky_beletsky_3114.jpg

Wonder and Mystery above the Very Large Telescopes

Credit: Yuri Beletsky (ESO)

Uma das grandes alegrias em morar na roça

e buscando céus mais escuros e transparentes,

é poder observar a olho nu

as Nuvens Pequena e Grande de Magalhães.

Eu sempre me divirto (e até quase fico tonta)

quando me deparo ao norte

com a maravilhante visão da Galáxia de Andromeda

(que pode ser observada a olho nu e usando a vista enviesada)

e, num giro corporal, volto-me para os céus do sul

e me deparo com a belíssima visão das Nuvens Pequena e Grande de Magalhães!

(Talvez a tontura também fique por conta

do fato de que posso olhar à visão desarmada

para três Galáxias que,

adjuntando com a Galáxia onde me encontro, a Via Lactea,

formam os principais conjuntos estelares

do nossa família galáctica tão intimamente nomeada de Grupo Local!).

Aqui na roça, um antigo caseiro meu

dizia que estas duas "Nuvens"

são as mulas do presépio do Menino Jesus...

Não importa o que se pense sobre estas Nuvens

- que quase sempre nos enganam, parecendo nuvens mesmo! -,

porque o importante é que elas a nós se apresentam enfeitando os céus do sul...,

e fazem isso de maneira tão simples, quase humilde!

Quer dizer,

as nuvens que nomeamos de Nuvens e que sabemos serem Galáxias

parecem esconder (assim como as nuvens escondem)

um mundo de maravilhas.... ,

porém apenas se apresentando

enquanto nuvens, simples nuvens, simples quase-enganos.

Com um abraço estrelado,

Janine Milward

http://apod.nasa.gov/apod/image/1105/vltsky_beletsky_3114.jpg

Wonder and Mystery above the Very Large Telescopes

Credit: Yuri Beletsky (ESO)

http://en.wikipedia.org/wiki/Zone_of_Avoidance#mediaviewer/File:Milky_Way_infrared.jpg

Milky Way infraredPublic Domain

The Milky Way creates a Zone of Avoidance for local observers

http://en.wikipedia.org/wiki/Milky_Way#mediaviewer/File:5_Local_Galactic_Group_(ELitU).png

5 Local Galactic Group (ELitU)CC BY-SA 3.0

Andrew Z. Colvin - Own work

http://en.wikipedia.org/wiki/Magellanic_Clouds#mediaviewer/File:Magellanic_Clouds_%E2%80%95_Irregular_Dwarf_Galaxies.jpg

Magellanic Clouds ― Irregular Dwarf Galaxies

ESO/S. Brunier - ESO

As Nuvens de Magalhães

Existem duas pequenas nuvens esfumaçadas que pareciam ser fragmentos da Via Láctea e que formam um quase triangulo com o pólo sul celestial. Estas nuvens foram primeiramente descritas pelo navegante português Fernando de Magalhães, no começo do século dezesseis. Porém, somente nos anos de 1920, os astrônomos determinaram que as Nuvens de Magalhães são galáxias, irregulares, pequena e próximas.

As Nuvens de Magalhães são ligadas entre si e à nossa Galáxia não somente pela força de gravidade mas também pela ponte gigantesca de hidrogênio neutro e frio. O brilho azulado das Nuvens de Magalhães revelam a presença de um imenso número de estrelas jovens, quentes e gigantes muito luminosas.

Se pudéssemos olhar para nossa Galáxia de um ponto externo à mesma, veríamos três pequenos e próximos satélites (galáxias-satélites), as Nuvens de Magalhães. Um sistema similar acontece com a Galáxia de ndrômeda, onde podemos observar várias pequenas galáxias satélites.

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

The Magellanic Clouds have been known since the first millennium in Western Asia. The first preserved mention of the Large Magellanic Cloud is by the Persian astronomer Al Sufi.^[4]^[5] In 964, in his Book of Fixed Stars, he called it al-Bakr ("the Sheep") "of the southern Arabs"; he noted that the Cloud is not visible from northern Arabia and Baghdad, but can be seen at the strait of Bab el Mandeb (12°15' N), which is the southernmost point of Arabia.^[2]

In Europe, the Clouds were first observed by Italian explorers Peter Martyr d'Anghiera and Andrea Corsali at the end of the 15th century. Subsequently, they were reported byAntonio Pigafetta, who accompanied the expedition of Ferdinand Magellan on its circumnavigation of the world in 1519-1522.^[2] However, naming the clouds after Magellan did not become widespread until much later. In Bayer's Uranometria they are designated as nubecula major and nubecula minor.^[6] In the 1756 star map of the French astronomer Lacaille, they are designated as le Grand Nuage and le Petit Nuage ("the Large Cloud" and "the Small Cloud").^[7]

In Sri Lanka, from ancient times, these clouds have been referred to as the 'Maha Mera Paruwathaya' meaning "the great mountain", as they look like the peaks of a distant mountain range.

http://en.wikipedia.org/wiki/Magellanic_Clouds

In the southern hemisphere, the Magellanic clouds have long been included in the lore of native inhabitants, including south sea islanders and indigenous Australians. Persian astronomer Al Sufi labelled the larger of the two clouds as Al Bakr, the White Ox. European sailors may have first noticed the clouds during the Middle Ages when they were used for navigation.Portuguese and Dutch sailors called them the Cape Clouds, a name that was retained for several centuries. During the circumnavigation of the Earth by Ferdinand Magellan in 1519–22, they were described by Antonio Pigafetta as dim clusters of stars.^[8] In Johann Bayer's celestial atlas Uranometria, published in 1603, he named the smaller cloud, Nubecula Minor.^[9]In Latin, Nubecula means a little cloud.^[10]

Between 1834 and 1838, John Frederick William Herschel made observations of the southern skies with his 14-inch (36 cm) reflector from the Royal Observatory at the Cape of Good Hope. While observing the Nubecula Minor, he described it as a cloudy mass of light with an oval shape and a bright center. Within the area of this cloud he catalogued a concentration of 37 nebulae and clusters.^[11]

In 1891, Harvard College Observatory opened an observing station at Arequipa in Peru. Between 1893 and 1906, under the direction of Solon Bailey, the 24-inch (610 mm) telescope at this site was used to survey photographically both the Large and Small Magellanic Clouds.^[12] Henrietta Swan Leavitt, an astronomer at the Harvard College Observatory, used the plates from Arequipa to study the variations in relative luminosity of stars in the SMC. In 1908, the results of her study were published, which showed that a type of variable star called a "cluster variable", later called a Cepheid variable after the prototype star Delta Cephei, showed a definite relationship between the variability period and the star's luminosity.^[13] This important period-luminosity relation allowed the distance to any other cepheid variable to be estimated in terms of the distance to the SMC. Hence, once the distance to the SMC was known with greater accuracy, Cepheid variables could be used as a standard candle for measuring the distances to other galaxies.^[14]

Using this period-luminosity relation, in 1913 the distance to the SMC was first estimated by Ejnar Hertzsprung. First he measured thirteen nearby cepheid variables to find the absolute magnitude of a variable with a period of one day. By comparing this to the periodicity of the variables as measured by Leavitt, he was able to estimate a distance of 10,000 parsecs (30,000 light years) between the Sun and the SMC.^[15] This later proved to be a gross underestimate of the true distance, but it did demonstrate the potential usefulness of this technique.^[16]

Announced in 2006, measurements with the Hubble Space Telescope suggest the Large and Small Magellanic Clouds may be moving too fast to be orbiting the Milky Way.^[17]

http://en.wikipedia.org/wiki/Small_Magellanic_Cloud

Veja o Vídeo:

https://www.youtube.com/watch?v=53yokIKAnDs&feature=youtube_gdata

Astronomers at NASA's Goddard Space Flight Center in Greenbelt, Md., and the Pennsylvania State University in University Park, Pa., have used NASA's Swift satellite to create the most detailed surveys of the Large and Small Magellanic Clouds, the two closest major galaxies, in ultraviolet light.
Thousands of images were assembled into seamless portraits of the main body of each galaxy to produce the highest-resolution surveys of the Magellanic Clouds at ultraviolet wavelengths. The project was proposed by Stefan Immler, an astronomer at Goddard.

The Large and Small Magellanic Clouds, or LMC and SMC for short, lie about 163,000 and 200,000 light-years away, respectively, and orbit each other as well as our own Milky Way galaxy.

Compared to the Milky Way, the LMC has about one-tenth its physical size and only 1 percent of its mass. The SMC is only half the size of the LMC and contains about two-thirds of its mass.
The new images reveal about a million ultraviolet sources within the LMC and about 250,000 in the SMC.

Viewing in the ultraviolet allows astronomers to suppress the light of normal stars like the sun, which are not very bright at these higher energies, and provide a clearer picture of the hottest stars and star-formation regions.

Only Swift's Ultraviolet/Optical Telescope, or UVOT, is capable of producing such high-resolution wide-field multi-color surveys in the ultraviolet. The LMC and SMC images range from 1,600 to 3,300 angstroms, UV wavelengths largely blocked by Earth's atmosphere.

The Large and Small Magellanic Clouds are readily visible from the Southern Hemisphere as faint, glowing patches in the night sky. The galaxies are named after Ferdinand Magellan, the Portuguese explorer who in 1519 led an expedition to sail around the world. He and his crew were among the first Europeans to sight the objects. All visible light imagery provided by Axel Mellinger, Central Michigan University.

This video is public domain and can be downloaded at:http://svs.gsfc.nasa.gov/goto?11293

http://en.wikipedia.org/wiki/Small_Magellanic_Cloud

Panoramic Large and Small Magellanic Clouds

ESO/Y. Beletsky - http://www.eso.org/public/images/potw1114a/

NASA's Hubble Space Telescope Finds Source of Magellanic Stream

Astronomers using NASA's Hubble Space Telescope have solved a 40-year mystery on the origin of the Magellanic Stream, a long ribbon of gas stretching nearly halfway around our Milky Way galaxy.

The Large and Small Magellanic Clouds, two dwarf galaxies orbiting the Milky Way, are at the head of the gaseous stream. Since the stream's discovery by radio telescopes in the early 1970s, astronomers have wondered whether the gas comes from one or both of the satellite galaxies. New Hubble observations reveal most of the gas was stripped from the Small Magellanic Cloud about 2 billion years ago, and a second region of the stream originated more recently from the Large Magellanic Cloud.

Globular cluster 47 Tucanae and the Small Magellanic Cloud (ground-based image)

http://www.spacetelescope.org/images/heic0616e/

This photo was taken by the Japanese astrophotographer Akira Fujii and shows a wide-angle view of the globular cluster 47 Tucanae and the Small Magellanic Cloud.

Credit: Akira Fujii

NGC 104 = 47 Tucanae - Aglomerado Globular

AR 00h23m Declinação - 72^o.11 Magnitude média das 25 estrelas mais brilhantes 13,54 Magnitude fotográfica global 4,4 Diâmetro aparente em minuto de arco 44’,0

Número conhecido de Variáveis 11 Distância kpc 5,0

Velocidade Radial (km/s) -24

Imenso Aglomerado Globular na constelação de Tucano. É o segundo aglomerado em tamanho, depois de Omega Centauri. Visível a olho nú em noites escuras e transparentes, a cerca de 2^o. a sudoeste de Theta Tucanae. Com um bom par de binóculos, observamos uma forte condensação central (onde as estrelas parecem estar amontoadas umas sobre as outras) e com um telescópio podemos vislumbrar um dos objetos mais belos do céu.

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

http://www.spacetelescope.org/images/heic0616c/

A photo of the globular star cluster 47 Tucanae taken with the Very Large Telescope, in Chile. It is one of the densest globular clusters in the Southern hemisphere. The cluster contains one million stars.

Credit:

Very Large Telescope/European Southern Observatory, R. Kotak and H. Boffin (ESO)

47 Tucanae (NGC 104) ou apenas 47 Tuc é um aglomerado globular situado na constelação de Tucana. Está a de cerca de 16 700 anos-luz de distância da Terra, e tem 120 anos-luz de diâmetro. Pode ser visto a olho nu, e é brilhante o suficiente para ganhar uma designação de Flamsteed com uma magnitude visual de 4,0. É apenas uma de um pequeno número de características com essa designação do céu do sul.

47 Tucanae foi descoberto por Nicolas Louis de Lacaille em 1751; a sua localização muito ao sul tem escondido de observadores europeus até então. O aglomerado aparece aproximadamente com o tamanho da lua cheia no céu em condições ideais.

É o segundo aglomerado globular mais brilhante no céu (depois de Omega Centauri), e é conhecido por ter um núcleo muito brilhante e denso. Ele tem de 22 pulsares milisegundos conhecidos, e pelo menos 21 estrelas retardatárias azuis (blue stragglers) perto do centro.4

47 Tucanae está incluído no Catálogo Caldwell de Sir Patrick Moore como C106.

NGC 104 concorre com NGC 5139 (Omega Centauri) para o título: O mais esplêndido Aglomerado Globular no céu. NGC 104 tem duas características em seu favor. Ele é arredondado e tem um centro mais compacto. No entanto, devido à localização, mais observadores vão para NGC 5139.

http://pt.wikipedia.org/wiki/47_Tucanae

http://www.spacetelescope.org/news/heic0616/
Image credit: NASA, ESA, and G. Meylan (?cole Polytechnique Federale de Lausanne)

A seven year study with the NASA/ESA Hubble Space Telescope has provided astronomers with the best observational evidence yet that globular clusters sort out stars according to their mass, governed by a gravitational billiard ball game between stars. Heavier stars slow down and sink to the cluster's core, while lighter stars pick up speed and move across the cluster to its periphery. This process, called "mass segregation", has long been suspected for globular star clusters, but has never before been directly seen in action.

A Hubble Space Telescope (HST) image of NGC 602. Credit: HST/NASA/ESA.
Observation data (J2000 epoch)
Constellation	Hydrus
Right ascension	01^h 29^m 32.133^s^[1]
Declination	−73° 33′ 38.13″^[1]
Distance	196 kly^[2] (61 kpc^[2])
Apparent magnitude (V)	- />
Apparent dimensions (V)	1′.5 × 0′.7^[3]
Physical characteristics
Mass	- M_☉
Radius	90 ly
Estimated age	5 My^[4]
Notable features	-
Other designations	N90^[2]

Image: Hubble Observes Infant Stars in Nearby Galaxy

http://hubblesite.org/newscenter/archive/releases/2007/04/image/a/format/web_print/

Zooming on NGC 602

http://www.spacetelescope.org/videos/heic0702a/

Credit:

Akira Fujii, Digitized Sky Survey 2 and ESA/Hubble

http://heritage.stsci.edu/2007/04/images/NGC602_AAS209_lg.jpg

NGC 602: Ongoing Star Formation in a Young SMC Cluster

Lynn Redding Carlson (JHU), Antonella Nota (STScI/ESA), Elena Sabbi (STScI), Marco Sirianni (STScI/ESA), Joseph L. Hora (Harvard/CfA), Margaret Meixner (STScI), M. Clampin (NASA/Goddard), J. Gallagher (U. Wisconsin), M. S. Oey (U. Michigan), A. Pasquali (Inst. Of Astron., ETH), L. J. Smith (UCL), M. Tosi (Bologna Obs.), R. Walterbos (U. New Mexico)

(The following is a poster presentation made at the American
Astronomical Society conference in January 2007 in Seattle, Washington.)

The young stellar cluster NGC 602 is located in the wing of the SMC, Z~0.004, a low density region far from the main body of the galaxy with low gas and stellar content. From deep optical imaging with the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope (HST), we have discovered the existence of an extensive pre-Main Sequence (PMS) population, with stellar masses in the range 0.6–3 Mo. This pre-Main Sequence population formed coevally with the central cluster about 5 Myr ago. Spitzer Space Telescope (SST) images of the region in all four Infrared Array Camera (IRAC) bands reveal a second population of Young Stellar Objects (YSOs), which formed after the stars seen with HST/ACS imaging. Some of these very young objects are still embedded in nebular material. We infer that star formation started in this region ~5 Myr ago with the formation of the central cluster and gradually propagated towards the outskirts where we find evidence of on going star formation (~1 Myr).

http://heritage.stsci.edu/2007/04/supplemental.html

NGC 1511 é uma galáxia espiral (Sa) localizada na direcção da constelação de Hydrus. Possui uma declinação de -67° 38' 05" e uma ascensão recta de 3 horas, 59minutos e 36,8 segundos.

A galáxia NGC 1511 foi descoberta em 2 de Novembro de 1834 por John Herschel.

http://pt.wikipedia.org/wiki/NGC_1511

http://en.wikipedia.org/wiki/Large_Magellanic_Cloud#mediaviewer/File:Large_and_small_magellanic_cloud_from_new_zealand.jpg

Large and small magellanic cloud from new zealand

Markrosenrosen - Own work

A Pequena Nuvem de Magalhães

http://en.wikipedia.org/wiki/Magellanic_Clouds#mediaviewer/File:Magellanic_Clouds_%E2%80%95_Irregular_Dwarf_Galaxies.jpg

Magellanic Clouds ― Irregular Dwarf Galaxies

ESO/S. Brunier - ESO

http://www.spacetelescope.org/images/heic0603d/

The two-colour image shows an overview of the full Small Magellanic Cloud (SMC) and was composed from two images from the Digitized Sky Survey 2. The field of view is slightly larger than 3.5›.

Credit:

ESA/Hubble and Digitized Sky Survey 2. Acknowledgements: Davide De Martin

Galáxia Tucano - Pequena Nuvem de Magalhães

Ascensão Reta 00h52m Declinação -72^o.56

Magnitude fotográfica aparente 2,86

Dimensões Angulares 216 X 216 Distância (milhões de anos-luz) 0,2

A Pequena Nuvem de Magalhães

Esta é uma galáxia irregular e próxima e que, juntamente com a Grande Nuvem de Magalhães, órbita nossa Galáxia como se ambas fossem nossos satélites.

A maior parte da massa da Pequena Nuvem de Magalhães consiste de nuvens interestelares de hidrogênio, o material básico de formação das estrelas - que nesta galáxia acontecem em larga escala. Prova disso é o grande numero de estrelas jovens e quentes - gigantes azuis - que trazem à Nuvem esta sua coloração azulada.

Em 1984, radio-astronomos australianos descobriram que a Pequena Nuvem de Magalhães consiste, na verdade, de duas galáxias separadas, uma atrás da outra, uma sendo ocultada de forma que vemos apenas um único objeto no céu. Estas duas galáxias estão se separando uma da outra e foi exatamente a diferença de velocidade entre ambas que revelou o fato de a Pequena Nuvem ser, na verdade, duas galáxias separadas.

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

Localizada ao sul de Tucana, a Pequena Nuvem de Magalhães é uma galáxia anã que é uma das vizinhas mais próximas da Via Láctea a uma distância de 210 mil anos-luz. Embora provavelmente tenha tido o formato de disco, as forças de maré da Via Láctea a distorceram. Juntamente com a Grande Nuvem de Magalhães, ela está na corrente de Magalhães, uma nuvem de gás que conecta as duas galáxias8 . NGC 346 é uma região de formação de estrelas na Pequena Nuvem de Magalhães. Ela tem magnitude aparente de 10,311 . Dentro dela está o sistema estelar triplo HD 5980, sendo cada um de seus membros as estrelas mais luminosas conhecidas12 .

http://pt.wikipedia.org/wiki/Tucana

Hubble finds source of Magellanic Stream

Astronomers explore origin of gas ribbon wrapped around our galaxy

http://www.spacetelescope.org/news/heic1314/

Image credit: David L. Nidever, et al., NRAO/AUI/NSF and Mellinger, LAB Survey, Parkes Observatory, Westerbork Observatory, and Arecibo Observatory.

Astronomers using the NASA/ESA Hubble Space Telescope have solved the 40-year-old mystery of the origin of the Magellanic Stream, a long ribbon of gas stretching nearly halfway around the Milky Way. New Hubble observations reveal that most of this stream was stripped from the Small Magellanic Cloud some two billion years ago, with a smaller portion originating more recently from its larger neighbour.

The Magellanic Clouds, two dwarf galaxies orbiting our galaxy, are at the head of a huge gaseous filament known as the Magellanic Stream. Since the Stream's discovery in the early 1970s, astronomers have wondered whether this gas comes from one or both of the satellite galaxies. Now, new Hubble observations show that most of the gas was stripped from the Small Magellanic Cloud about two billion years ago — but surprisingly, a second region of the stream was formed more recently from the Large Magellanic Cloud.

LEIA MAIS EM
http://www.spacetelescope.org/news/heic1314/

AGLOMERADOS LOCALIZADOS

NA PEQUENA NUVEM DE MAGALHÃES

NGC 121 é um aglomerado globular na direção da constelação de Tucana. O objeto foi descoberto pelo astrônomo John Herschel em 1835, usando um telescópio refletor com abertura de 18,6 polegadas.

http://pt.wikipedia.org/wiki/NGC_121

http://pt.wikipedia.org/wiki/NGC_121#mediaviewer/Ficheiro:NGC_121_Hubble_WikiSky.jpg

NGC 121 Hubble WikiSkyDomínio público

en:NASA, en:STScI, en:WikiSky - en:WikiSky's snapshot tool - [1]

Credit:

ESA/Hubble & NASA
Acknowlegement: Stefano Campani

This image shows NGC 121, a globular cluster in the constellation of Tucana (The Toucan). Globular clusters are big balls of old stars that orbit the centres of their galaxies like satellites — the Milky Way, for example, has around 150.

NGC 121 belongs to one of our neighbouring galaxies, the Small Magellanic Cloud (SMC). It was discovered in 1835 by English astronomer John Herschel, and in recent years it has been studied in detail by astronomers wishing to learn more about how stars form and evolve.

Stars do not live forever — they develop differently depending on their original mass. In many clusters, all the stars seem to have formed at the same time, although in others we see distinct populations of stars that are different ages. By studying old stellar populations in globular clusters, astronomers can effectively use them as tracers for the stellar population of their host galaxies. With an object like NGC 121, which lies close to the Milky Way, Hubble is able to resolve individual stars and get a very detailed insight.

Image: Hubble Observes Infant Stars in Nearby Galaxy

http://hubblesite.org/newscenter/archive/releases/2007/04/image/a/format/web_print/

Zooming on NGC 602

http://www.spacetelescope.org/videos/heic0702a/

Credit:

Akira Fujii, Digitized Sky Survey 2 and ESA/Hubble

http://heritage.stsci.edu/2007/04/images/NGC602_AAS209_lg.jpg

NGC 602: Ongoing Star Formation in a Young SMC Cluster

http://heritage.stsci.edu/2007/04/supplemental.html

NGC 265 is an open cluster in the Small Magellanic Cloud,^[3] which is located in the constellation Tucana.

http://en.wikipedia.org/wiki/NGC_265

NGC 290 is an open cluster. It lies some 200,000 light years away in the Small Magellanic Cloud,^[2] which is located in the constellation Tucana. It spans 65 light years across.^[3]

http://en.wikipedia.org/wiki/NGC_290

http://www.spacetelescope.org/images/heic0603a/

Hubble has captured the most detailed images to date of the open star clusters NGC 265 and NGC 290 in the Small Magellanic Cloud - two sparkling sets of gemstones in the southern sky.

Two new composite images taken with the Advanced Camera for Surveys onboard the NASA/ESA Hubble Space Telescope show a myriad of stars in crystal clear detail. The brilliant open star clusters, NGC 265 and NGC 290, are located about 200,000 light-years away and are roughly 65 light-years across.

Credit:

European Space Agency & NASA

Acknowledgements:

Davide De Martin (ESA/Hubble) and Edward W. Olszewski (University of Arizona, USA)

NGC 346 is an open cluster with associated nebula located in the Small Magellanic Cloud that appears in the constellation Tucana. It contains HD 5980, the brightest star in the SMC.

http://en.wikipedia.org/wiki/NGC_346

http://en.wikipedia.org/wiki/NGC_346#mediaviewer/File:Ngc346.jpg

Ngc346Public Domain

NASA, ESA and A. Nota (ESA/STScI, STScI/AURA) - http://www.spacetelescope.org/images/html/heic0514a.html (direct link)

http://apod.nasa.gov/apod/ap110509.html

Wonder and Mystery above the Very Large Telescopes
Credit: Yuri Beletsky (ESO)

Explanation: What's that bright orange dot above the large telescope on the right? Even seasoned sky enthusiasts might ponder the origin of the orange orb seen by scrolling across this panoramic image, taken last December. Perhaps identifying known objects will help. To start, on the far left is a diagonal band of light known as zodiacal light, sunlight reflected off of dust orbiting in the inner Solar System. The bright white spot on the left, just above the horizon, is Venus, which also glows by reflected sunlight. Rising diagonally from the ground to the right of Venus is the band of our Milky Way Galaxy. In the image, the band, which usually stretches dramatically overhead, appears to arch above the elevated Chilean landscape. Under the Milky Way arch, toward the left, lie both the Largeand Small Magellanic Cloud galaxies, while toward the right lies the constellation of Orion surrounded by the red ring of Barnard's Loop. On the ground, each of the four Very Large Telescopes is busy keeping an eye on the distant universe. The orange spot -- it's the Moon. The image was taken during a total lunar eclipse when the normally bright full moon turned into a faint orb tinted orange by the intervening Earth's atmosphere.

http://www.raremaps.com/gallery/enlarge/33613

http://www.raremaps.com/gallery/detail/33613/Celestial_Map_of_the_Southern_Hemisphere/Pardies.html

Title: [Celestial Map of the Southern Hemisphere] Map Maker: Ignace Gaston Pardies

A GRANDE NUVEM DE MAGALHÃES

Duas Constelações compartilham
a maravilhosa Grande Nuvem de Magalhães:
MONS MENSA E DORADO
- A MONTANHA DA MESA E O PEIXE DOURADO

A Montanha

chamada de Montanha da Mesa

(Table Mountain)

e que é situada na Cidade do Cabo, África do Sul,

na Terra,

mas que também é acolhida nos céus estrelados do sul:

a constelação Mensa, Mons Mensa,

que compartilha, juntamente com a constelação Dorado, Dourado,

o direcionamento da Grande Nuvem de Magalhães!

http://en.wikipedia.org/wiki/Table_Mountain#mediaviewer/File:Table_Mountain_DanieVDM.jpg

Table Mountain DanieVDM

Danie van der Merwe from Cape Town, South Africa - View of Table Mountain from Bloubergstrand

"Mensa" constellation

Table Mountain is the only terrestrial feature to give its name to a constellation: Mensa, meaning The Table. The constellation is seen in the Southern Hemisphere, below Orion, around midnight in mid-July. It was named by the French astronomer Nicolas de Lacaille during his stay at the Cape in the mid 18th century.^[

http://en.wikipedia.org/wiki/Table_Mountain

A Montanha da Mesa é a única característica terrestre a nomear uma constelação: Mensa - significando A Mesa. .................. Esta constelação foi nomeada pelo astrônomo francês Nicolas de Lacaille, durante sua estada na Cidade do Cabo, em meados do século XVIII.

http://www.stellarium.org/pt/

http://en.wikipedia.org/wiki/Table_Mountain#mediaviewer/File:Tablemountain_capetown.jpg

Tablemountain capetown

Original uploader was Coda.coza at en.wikipedia

http://www.amazon.com/dp/0486210790/ref=rdr_ext_tmb

- Richard Hinckley Allen, Star Names, Their Lore and Meaning, Dover Publications, Inc, New York, USA

Richard Hinckley Allen, em seu famoso e importantíssimo livro
Star Names — Their Lore and Meaning -,

nos fala bem sinteticamente sobre Mons Mensa:

Mons Mensae, the Table Mountain,

now abbreviated by astronomers to Mensa, is translated by the French as Montagne de la Table; by the Italians, as Monte Tavola; and by the Germans, as Tafelberg.

La Caille, who did so much for our knowledge of the southern heavens, formed the figure from stars under the Greater Cloud, between the poles of the equator and the ecliptic, just north of the polar Octans; the title being suggested by the fact that the Table Mountain, back of Cape Town, "which had witnessed his nightly vigils and daily toils," also was frequently capped by a cloud.

Gould found in the constellation 44 naked-eye stars, the brightest being of 5.3 magnitude; but within its borders is a portion of the Nubecula Major.

http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Mons_Mensae*.html

.......................................

La Caille, que tanto fez para nosso conhecimento sobre os céus do sul, formou esta constelação sob A Grande Nuvem, ........................................, ao norte da constelação polar Octans. A nomeação foi sugerida pelo fato de que a Montanha da Mesa, na Cidade do Cabo, "havia testemunhado as vigílias noturnas e as labutas diárias". bem como frequentemente sendo envolvida por uma nuvem.

...................................

"Mensa" constellation

http://en.wikipedia.org/wiki/Table_Mountain

Mario Jaci Monteiro - As Constelações, Cartas Celestes - CARJ

Abbé Nicolas Louis de La Caille, comumente chamado de Lacaille, (Rumigny, 15 de março de 1713 — 21 de março de 1762) foi um astrônomo francês conhecido principalmente pelo seu trabalho de catalogação de estrelas (cerca de 10 000) e por ter nomeado 14 constelações das 88 atuais. Calculou e tabulou uma lista de eclipses para 1800 anos.

.........................................

Durante os anos de 1750-1754 se dedicou a estudar as estrelas e constelações do hemisfério austral, com este intuito viajou até o Cabo da Boa Esperança na parte mais austral do continente africano. Com base nestas observações publicou o Coelum Australe Stelliferum sua obra mais importante.

...........................................

Lacaille nomeou as seguintes constelações austrais:

Antlia, Caelum, Circinus, Fornax, Horologium, Mensa, Microscopium, Norma, Octans, Pictor, Pyxis, Reticulum, Sculptor, Telescopium.

E ainda dividiu o Navio Argus em Carina, Vela e Puppis.

http://pt.wikipedia.org/wiki/Nicolas_Louis_de_Lacaille

Voyage to the Cape of Good Hope

His desire to determine the distances of the planets trigonometrically, using the longest possible baseline, led him to propose, in 1750, an expedition to the Cape of Good Hope. This was officially sanctioned by Roland-Michel Barrin de La Galissonière. There he constructed an observatory on the shore of Table Bay with the support of the Dutch Governor Ryk Tulbagh. The primary result of his two-year stay was a catalogue of nearly 10,000 southern stars, the production of which required observing every night for over a year. In the course of his survey he took note of 42 nebulous objects. He also achieved his aim of determining the lunar and solar parallaxes (Mars serving as an intermediary). This work required near-simultaneous observations from Europe which were carried out by Jérôme Lalande.

His southern catalogue, called Coelum Australe Stelliferum, was published posthumously in 1763. He found it necessary to introduce 14 new constellations which have since become standard.^[4] One of these was Mons Mensa, the only constellation named after a terrestrial feature (Table Mountain).

http://en.wikipedia.org/wiki/Nicolas_Louis_de_Lacaille

http://www.iau.org/static/public/constellations/gif/MEN.gif

Mensa (Men), a Meseta, é uma constelação do hemisfério celestial sul. O genitivo, usado para formar nomes de estrelas, é Mensae. O nome se originou do Monte Mesa, na Cidade do Cabo, África do Sul. Esta constelação contém parte da Grande Nuvem de Magalhães, a outra parte está em Dorado.

As constelações vizinhas, são Volans, Dorado, Hydrus, Octans e Chamaeleon.

Esta constelação, além de outras 13, foram criadas pelo astrônomo francês Nicolas Louis de Lacaille, que passou os anos de 1751-1752 catalogando as estrelas do hemisfério sul na Cidade do Cabo, que observava os céus do alto da Table Mountain, ou Monte Mesa (Mons Mensa). Em homenagem a esta montanha, Lacaille acabou por batizar uma de suas constelações com este nome, que é a única que não se refere a instrumento científico ou artístico. De referir que Mons Mensa pertence a uma cadeia de promontórios que termina, junto à costa, no famoso "Adamastor" da lenda Portuguesa ligada ao próprio Cabo da Boa Esperança, onde se situa a Cidade do Cabo.

É uma constelação com estrelas muitas fracas. A estrela mais brilhante α Mansae possui magnitude 5.

http://pt.wikipedia.org/wiki/Mensa

History

Mensa was created by Nicolas Louis de Lacaille out of dim Southern Hemisphere stars in honor of Table Mountain, a South African mountain. Although the stars of Mensa do not feature in any ancient mythology, the mountain it is named after has a rich mythology. Called "Tafelberg" in Dutch and German, the mesa has two neighboring mountains called "Devil's Peak" and "Lion's Head". Table Mountain features in the mythology of the Cape of Good Hope, notorious for its storms—the explorer Bartolomeu Dias saw the mesa as a mythical anvil for storms. Another myth relating to its dangers comes from Sinbad the Sailor, an Arabic folk hero who saw the mountain as a magnet pulling his ships to the bottom of the sea.^[1]

Notable features

Stars

Mensa contains no bright stars, with Alpha Mensae its brightest star at a barely visible magnitude 5.09, making it the faintest constellation in the entire sky. Alpha Mensaeis a solar-type star (class G5 V) 33 light-years from Earth, and is considered a good prospect for harboring an Earth-like planet. Pi Mensae, on the other hand, while also solar-type (G1) and at 59 light-years, has been found to have a large gas giant in an eccentric orbit crossing the habitable zone, which would effectively rule out the existence of any habitable planets.

Deep-sky objects

Mensa contains part of the Large Magellanic Cloud (the rest being in Dorado).

The first images taken by the Chandra X-Ray Observatory were of PKS 0637-752, a quasar in Mensa with a large gas jet visible in both optical and x-ray wavelengths.^{[citation needed]}

^{http://en.wikipedia.org/wiki/Mensa_(constellation)}

http://pt.wikipedia.org/wiki/Mensa#mediaviewer/Ficheiro:Mensa_constellation_map.png

MONS MENSA, A MONTANHA DA MESA, A MESA

Posicionamento:

Ascensão Reta 3h20m / 7h37m Declinação -69^o.9 / 85^o.0

História:

Constelação formada por La Caille, 1752.

Algumas Informações Interessantes acerca esta Constelação:

Esta constelação foi assim nomeada - A Montanha da Mesa - em função do fato de que La Caille trabalhou em um Observatório na Cidade do Cabo, na África do Sul, onde existe um complexo de montanhas e uma delas é assim nomeada.

Nesta constelação nos chama a atenção a presença da Grande Nuvem de Magalhães
- que também faz parte da constelação de Dorado, o Peixe Dourado
(que acolhe a tão conhecida Nebulosa Tarântula, ainda dentro da Grande Nuvem de Magalhães).

É uma constelação de estrelas que vão além de magnitude 5, portanto pouco visíveis.

No entanto, a estrela Beta Mensae situa-se bem ao centro da Nebulosa Tarântula.

Fronteiras:

Dorado, Hydrus, Octantis, Chamaleon, Volans

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

Alpha Mensae (33 Mensae) é uma estrela na direção da Mensa. Possui uma ascensão reta de 06h 10m 14.20s e uma declinação de −74° 45′ 09.1″. Sua magnitude aparente é igual a 5.08. Considerando sua distância de 33 anos-luz em relação à Terra, sua magnitude absoluta é igual a 5.05. Pertence à classe espectral G5V.

http://pt.wikipedia.org/wiki/Alpha_Mensae

Beta Mensae (17 Mensae) é uma estrela na direção da Mensa. Possui uma ascensão reta de 05h 02m 43.00s e uma declinação de −71° 18′ 51.6″. Sua magnitude aparente é igual a 5.30. Considerando sua distância de 642 anos-luz em relação à Terra, sua magnitude absoluta é igual a −1.17. Pertence à classe espectral G8III.

http://pt.wikipedia.org/wiki/Beta_Mensae

Gamma Mensae (25 Mensae) é uma estrela dupla na direção da constelação de Mensa. Possui uma ascensão reta de 05h 31m 52.66s e uma declinação de −76° 20′ 30.0″. Sua magnitude aparente é igual a 5.18. Considerando sua distância de 101 anos-luz em relação à Terra, sua magnitude absoluta é igual a 2.73. Pertence àclasse espectral K4III.

http://pt.wikipedia.org/wiki/Gamma_Mensae

Eta Mensae (16 Mensae) é uma estrela na direção da constelação de Mensa. Possui uma ascensão reta de 04h 55m 11.14s e uma declinação de −74° 56′ 13.2″. Suamagnitude aparente é igual a 5.47. Considerando sua distância de 712 anos-luz em relação à Terra, sua magnitude absoluta é igual a −1.23. Pertence à classe espectral K6III.

http://pt.wikipedia.org/wiki/Eta_Mensae

As Nuvens de Magalhães nos trazem imensa felicidade

por morarmos no hemisfério sul e podermos, então,

usufruir da maravilhosa observação a olho nu

dessas Nuvens que não são nuvens e sim galáxias

e que escondem um verdadeiro mundo de tesouros....

Tesouros que vão sendo, vagarosamente,

descobertos e trazidos ao nosso conhecimento!

http://en.wikipedia.org/wiki/Magellanic_Clouds#mediaviewer/File:Magellanic_Clouds_%E2%80%95_Irregular_Dwarf_Galaxies.jpg

Magellanic Clouds ― Irregular Dwarf Galaxies

ESO/S. Brunier - ESO

DORADO, O PEIXE DOURADO

Mario Jaci Monteiro - As Constelações, Cartas Celestes - CARJ

DORADO, O PEIXE DOURADO

Posicionamento:

Ascensão Reta 3h52m / 6h36m Declinação -48^o.8 / -70^o.1

(Dados referentes à época 1980, coletados no Atlas Celeste de R.R.de Freitas Mourão, 6^a. edição)

História:

Constelação adicionada por Bayer em 1604.

Fronteiras:

Pictor, Caelum, Horologium, Reticulum, Hydra Macho, Mensa, Volans

http://www.stellarium.org/pt/

Dorado (Dor), o dourado,1 2 é uma constelação do hemisfério celestial sul.

O genitivo, usado para formar nomes de estrelas, é Doradus.

Nesta constelação e estendendo-se até a Meseta,

encontra-se a Grande Nuvem de Magalhães.

http://pt.wikipedia.org/wiki/Dorado

http://pt.wikipedia.org/wiki/NGC_1722

Estrelas e Objetos Interessantes, em Dourado:

R Doradus - Estrela Variável

Ascensão Reta 04h36m Declinação -62^o.10

Magnitudes: Max 4,5 Min 7,0 Período 335,0

Tipo PLG Espectro M7

(Dados referentes à época 1980, coletados no Atlas Celeste de R.R.de Freitas Mourão, 6^a. edição)

R Doradus (also called HD 29712) is the name of a red giant Mira variable star in the far-southern constellation Dorado, although visually it appears more closely associated with the constellation Reticulum. Its distance from Earth is 178 ± 10 light-years (54.6 ± 3.1 parsecs).^[1] Having a uniform disk diameter of 0.057 ± 0.005arcsec,^[8] it is currently believed to be the star with the second largest apparent size as viewed from Earth (right after the Sun). The estimated diameter of R Doradus is 515 ± 70 million km (3.46 AU) or 370 ± 50^[7] times the diameter of the Sun. If placed at the centre of the Solar System, the orbit of Mars and most of the main asteroid belt would be contained within the star.

The visible magnitude of R Doradus varies between 4.8 and 6.6, which makes it usually just visible to the naked eye, but in the infrared it is one of the brightest stars in the sky and its total luminosity is 6500 ± 1400 times that of the Sun.^[9] With a near-infrared J band magnitude of −2.6,^[4] only Betelgeuse at −2.9 is brighter.

http://en.wikipedia.org/wiki/R_Doradus

http://en.wikipedia.org/wiki/Milky_Way#mediaviewer/File:6_Virgo_Supercluster_(ELitU).png

6 Virgo Supercluster (ELitU)CC BY-SA 3.0

Andrew Z. Colvin - Own work

The Dorado Group is a loose concentration of galaxies^[2] containing both spirals and ellipticals.^[3] It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'.^[6] It lies primarily in the southern constellation Dorado and is one of the richest galaxy groups of the Southern Hemisphere.^[7] Gérard de Vaucouleurs was the first to identify it in 1975 as a large complex nebulae II in the Dorado region,^[2] designating it as G16.^[3]
....................................................

At the center of the cluster lie interacting galaxies^[11] NGC 1549 and NGC 1553. The dominant group members, ordered by luminosity, are: spiral NGC 1566,lenticular NGC 1553, and elliptical NGC 1549.^[6] The group spans an area of the sky 10° square which represents around 3 Mpc square.^[2] The group exhibits a relatively small harmonic mean radius (230 ± 40 kpc) due to the concentration at its core of more luminous galaxies.^[6] All together, the group has an overall luminosity of 7.8 ± 1.6 ×10¹⁰ L_⊙.^[6]

The Dorado Group contains three dominant smaller groups within itself, NGC 1672 Group, NGC 1566 Group and the NGC 1433 Group, as evidenced by the H Idistribution of the region.^[5] The Dorado Group is in the Fornax Wall that connects these three groups.^[5] Because it is in the Fornax Wall, it is at a similar distance as the Fornax Cluster.^[10] The Dorado Group is interesting for being richer than the Local Group, while still being dominated by disk types of galaxies (i.e. its two brightest members are spiral NGC 1566 and lenticular NGC 1553) and its member galaxies have H I masses on par with non-interacting galaxies of the same morphological type.^[10] With the group's apparent crossing time being 12.6 ± 0.6^[6] % of the universe's age, recent analyses deduce that the group is unvirialized, and thus this may explain the abundance of spirals and H I.^[10]

http://en.wikipedia.org/wiki/Dorado_Group

http://www.iau.org/static/public/constellations/gif/DOR.gif

NGC 1566 is an intermediate spiral galaxy in the constellation Dorado. It is the dominant^[3] member of the Dorado Group and also its brightest member.^[4]^[5] It is one of the brightest Seyfert galaxies in the sky.^[3] Its absolute luminosity is 3.7×10¹⁰ L_☉.^[6] It contains 1.4×10¹⁰ M_☉ of H I.^[6]
http://en.wikipedia.org/wiki/NGC_1566

http://en.wikipedia.org/wiki/NGC_1566#mediaviewer/File:Grand_Swirls_NGC_1566.jpg

Grand Swirls NGC 1566CC BY 2.0

NASA Goddard Space Flight Center - http://www.flickr.com/photos/gsfc/14172908657/

This new Hubble image shows NGC 1566, a beautiful galaxy located approximately 40 million light-years away in the constellation of Dorado (The Dolphinfish). NGC 1566 is an intermediate spiral galaxy, meaning that while it does not have a well-defined bar-shaped region of stars at its center — like barred spirals — it is not quite an unbarred spiral either. The small but extremely bright nucleus of NGC 1566 is clearly visible in this image, a telltale sign of its membership of the Seyfert class of galaxies. The centers of such galaxies are very active and luminous, emitting strong bursts of radiation and potentially harboring supermassive black holes that are many millions of times the mass of the sun. NGC 1566 is not just any Seyfert galaxy; it is the second brightest Seyfert galaxy known. It is also the brightest and most dominant member of the Dorado Group, a loose concentration of galaxies that together comprise one of the richest galaxy groups of the southern hemisphere. This image highlights the beauty and awe-inspiring nature of this unique galaxy group, with NGC 1566 glittering and glowing, its bright nucleus framed by swirling and symmetrical lavender arms. This image was taken by Hubble’s Wide Field Camera 3 (WFC3) in the near-infrared part of the spectrum. European Space Agency Credit: ESA/Hubble & NASA, Acknowledgement: Flickr user Det58 NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

http://en.wikipedia.org/wiki/NGC_1566

NGC 1553 is a prototypical^[3] lenticular galaxy in the constellation Dorado. It is the second brightest member of the Dorado Group of galaxies.^[4]^[5]^[6] British astronomerJohn Herschel discovered NGC 1553 on December 5, 1834 using an 18.7 inch reflector.^[7]
.................................
It forms a pair of interacting galaxies together with elliptical NGC 1549^[8] which lies 11′.8 away from it in the sky.^[2] Their interaction appears to be in the early stage and can be seen in optical wavelengths by faint but distinct irregular shells of emission and a curious jet on the northwest side.^[2]^[3] Together, these two galaxies comprise the center of the Dorado group.^[8]

http://en.wikipedia.org/wiki/NGC_1553

http://en.wikipedia.org/wiki/NGC_1553#mediaviewer/File:NGC_1553_Hubble.jpg

NGC 1553 HubblePublic Domain

The original uploader was Friendlystar at English Wikipedia - Transferred from en.wikipedia to Commons by Mike Peel using CommonsHelper.

The Dorado Group contains three dominant smaller groups within itself, NGC 1672 Group, NGC 1566 Group and the NGC 1433 Group, as evidenced by the H Idistribution of the region.^[5] The Dorado Group is in the Fornax Wall that connects these three groups.^[5] Because it is in the Fornax Wall, it is at a similar distance as the Fornax Cluster.^[10] The Dorado Group is interesting for being richer than the Local Group, while still being dominated by disk types of galaxies (i.e. its two brightest members are spiral NGC 1566 and lenticular NGC 1553) and its member galaxies have H I masses on par with non-interacting galaxies of the same morphological type.^[10] With the group's apparent crossing time being 12.6 ± 0.6^[6] % of the universe's age, recent analyses deduce that the group is unvirialized, and thus this may explain the abundance of spirals and H I.^[10]

http://en.wikipedia.org/wiki/Dorado_Group

http://en.wikipedia.org/wiki/Galaxy_filament#mediaviewer/File:2MASS_LSS_chart-NEW_Nasa.jpg

2MASS LSS chart-NEW NasaPublic Domain

IPAC/Caltech, by Thomas Jarrett - "Large Scale Structure in the Local Universe: The 2MASS Galaxy Catalog", Jarrett, T.H. 2004, PASA, 21, 396

A Grande Nuvem de Magalhães

http://en.wikipedia.org/wiki/Large_Magellanic_Cloud#mediaviewer/File:Large_Magellanic_Cloud-8sec.jpg

Large Magellanic Cloud-8secView license

Skatebiker - Taken from South Africa

http://en.wikipedia.org/wiki/Large_Magellanic_Cloud#mediaviewer/File:Large.mc.arp.750pix.jpg

Observation data (J2000 epoch)
The Large Magellanic Cloud
Constellation	Dorado/Mensa
Right ascension	05^h 23^m 34.5^s^[1]
Declination	−69° 45′ 22″^[1]
Distance	162.98 kly (49.97 kpc)^[2]^[3]^[4]^[5]
Type	SB(s)m^[1]
Apparent dimensions (V)	10.75° × 9.17°^[1]
Apparent magnitude (V)	0.9^[1]
Other designations
LMC, ESO 56- G 115, PGC 17223,^[1] Nubecula Major^[6]

http://en.wikipedia.org/wiki/Large_Magellanic_Cloud

A Grande Nuvem de Magalhães

Ascensão Reta 05h23m Declinação -69^o.46

Tipo I - Galáxia Irregular Magnitude fotográfica aparente 0,86

Dimensões Angulares 432 X432 Distância (milhões de anos-luz) 0,2

(Dados referentes à época 1980, coletados no Atlas Celeste de R.R.de Freitas Mourão, 6^a. edição)

Inicialmente, a Grande Nuvem de Magalhães foi classificada como uma galáxia irregular.
No entanto, mais tarde foram descobertos sinais de estrutura espiralada
e alguma relação com espirais barrados.
A barra é a parte mais interessante da galáxia
e se parece com uma nuvem estelar brilhante e alongada
e ao longo dessa barra, existem numerosas nebulosas
avermelhadas por hidrogênio ionizado,
e estimuladas pela radiação de estrelas quentes e jovens.
Nestas regiões são formadas novas estrelas.

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

http://en.wikipedia.org/wiki/Large_Magellanic_Cloud#mediaviewer/File:Satellite_Galaxies.JPG

Large Magellanic Cloud
	The largest of the satellite galaxies and also the fourth largest galaxy in the Local Group. This galaxy is a large bright object in southern hemisphere skies and it is the brightest galaxy in the sky. It contains several billion stars and many stars are still forming in it, most notably in the Tarantula nebula, a huge concentration of gas and dust over 2000 light years in diameter. A supernova exploded in the Large Magellanic Cloud in 1987 and observations of the expanding supernova remnant provided accurate distance measurements to the galaxy.
Small Magellanic Cloud
	Despite its name, this galaxy is fairly large for a dwarf galaxy. It contains at least several hundred million stars and is easily visible with the naked eye from the southern hemisphere. Like the Large Magellanic Cloud, there is still a lot star formation taking place within it.

Satellite Galaxies

Richard Powell - http://www.atlasoftheuniverse.com

http://pt.wikipedia.org/wiki/NGC_1722

CARO LEITOR,
CONHEÇA MUITÍSSIMO MAIS
SOBRE A GRANDE NUVEM DE MAGALHÃES
em Imagens maravilhosamente bem detalhadas
acessando
http://www.astrosurf.com/comolli/d144.htm

http://www.astrosurf.com/comolli/d144.htm

http://apod.nasa.gov/apod/ap130528.html
The Large Cloud of Magellan
Image Credit & Copyright: L. Comolli, L. Fontana, G. Ghioldi & E. Sordini

Explanation:

The 16th century Portuguese navigator Ferdinand Magellan and his crew had plenty of time to study the southern sky during the first circumnavigation of planet Earth. As a result, two fuzzy cloud-like objects easily visible to southern hemisphereskygazers are known as the Clouds of Magellan, now understood to be satellite galaxies of our much larger, spiral Milky Way galaxy. About 160,000 light-years distant in the constellation Dorado, the Large Magellanic Cloud (LMC) is seen here in a remarkably deep, colorful, and annotated composite image. Spanning about 15,000 light-years or so, it is the most massive of the Milky Way's satellite galaxies and is the home of the closest supernova in modern times, SN 1987A. The prominent patch just left of center is 30 Doradus, also known as the magnificent Tarantula Nebula, is a giant star-forming region about 1,000 light-years across.

NGC 2070 - A Nebulosa Tarântula

Esta nebulosa difusa é reconhecida como a maior do céu em sua espécie. Se acaso ela ocupasse a grande nebulosa em Orion, seria cerca de três vezes mais brilhante do que Vênus e cobriria toda a constelação do Gigante Caçador.

É o objeto mais brilhante e mais facilmente visível a olho nú dentro da Grande Nuvem de Magalhães.

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

http://www.30doradus.org/images/30dor/phot-05a-00-normal.jpg

A Nebulosa da Tarântula (também conhecida como 30 Doradus ou NGC 2070) é uma região HII na Grande Nuvem de Magalhães, localizada na constelação de Dorado. Ela foi inicialmente considerada uma estrela, mas em 1751 Nicolas Louis de Lacaille identificou-a como uma nebulosa.1 Está a uma distância de cerca de 49 kiloparsecs(160 mil anos-luz) da Terra.3

A Nebulosa da Tarântula é a maior e mais massiva região de formação estelar conhecida no Grupo Local, com um diâmetro de cerca de 200 parsecs (650 anos-luz).3Apesar de ter uma magnitude aparente de 8,1 é um objeto extremamente luminoso, e se estivesse tão perto da Terra quanto a Nebulosa de Órion, cobriria uma área de 60 luas cheias no céu e seu brilho seria suficiente para causar sombras.4 Em seu centro, está localizado o aglomerado estelar R136, que produz grande parte da energia que torna a nebulosa visível. R136 é um jovem aglomerado (idade de 1-2 milhões de anos) de estrelas extremamente quentes e luminosas, a maioria de classe espectral O3.5 A massa estimada do aglomerado é de 450 000 massas solares, sugerindo que ele se torne um aglomerado globular no futuro.6

Além de R136, a Nebulosa da Tarântula contém um aglomerado estelar mais velho, catalogado como Hodge 301, com uma idade de 20–25 milhões de anos. Estima-se que pelo menos 40 estrelas desse aglomerado já explodiram em supernovas, o que provavelmente é a causa de movimentos violentos de gás e emissão de raios-X na região do aglomerado.7

A supernova mais próxima já detectada desde a invenção do telescópio, Supernova 1987A, ocorreu nos arredores da Nebulosa da Tarântula.8

http://pt.wikipedia.org/wiki/Nebulosa_da_Tar%C3%A2ntula

http://pt.wikipedia.org/wiki/Nebulosa_da_Tar%C3%A2ntula#mediaviewer/Ficheiro:Spitzer-TarantulaNebula.jpg

Spitzer-TarantulaNebulaDomínio público

NASA/JPL-Caltech/B. Brandl (Cornell & University of Leiden) - http://photojournal.jpl.nasa.gov/catalog/PIA05062 http://www.spitzer.caltech.edu/Media/releases/ssc2004-01/ssc2004-01a.shtml

NASA's new Spitzer Space Telescope, formerly known as the Space Infrared Telescope Facility, has captured in stunning detail the spidery filaments and newborn stars of the Tarantula Nebula, a rich star-forming region also known as 30 Doradus. This cloud of glowing dust and gas is located in the Large Magellanic Cloud, the nearest galaxy to our own Milky Way, and is visible primarily from the Southern Hemisphere. This image of an interstellar cauldron provides a snapshot of the complex physical processes and chemistry that govern the birth - and death - of stars. At the heart of the nebula is a compact cluster of stars, known as R136, which contains very massive and young stars. The brightest of these blue supergiant stars are up to 100 times more massive than the Sun, and are at least 100,000 times more luminous. These stars will live fast and die young, at least by astronomical standards, exhausting their nuclear fuel in a few million years. The Spitzer Space Telescope image was obtained with an infrared array camera that is sensitive to invisible infrared light at wavelengths that are about ten times longer than visible light. In this four-color composite, emission at 3.6 microns is depicted in blue, 4.5 microns in green, 5.8 microns in orange, and 8.0 microns in red. The image covers a region that is three-quarters the size of the full moon. The Spitzer observations penetrate the dust clouds throughout the Tarantula to reveal previously hidden sites of star formation. Within the luminescent nebula, many holes are also apparent. These voids are produced by highly energetic winds originating from the massive stars in the central star cluster. The structures at the edges of these voids are particularly interesting. Dense pillars of gas and dust, sculpted by the stellar radiation, denote the birthplace of future generations of stars. The Spitzer image provides information about the composition of the material at the edges of the voids. The surface layers closest to the massive stars are subject to the most intense stellar radiation. Here, the atoms are stripped of their electrons, and the green color of these regions is indicative of the radiation from this highly excited, or 'ionized,' material. The ubiquitous red filaments seen throughout the image reveal the presence of molecular material thought to be rich in hydrocarbons. The Tarantula Nebula is the nearest example of a 'starburst' phenomenon, in which intense episodes of star formation occur on massive scales. Most starbursts, however, are associated with dusty and distant galaxies. Spitzer infrared observations of the Tarantula provide astronomers with an unprecedented view of the lifecycle of massive stars and their vital role in regulating the birth of future stellar and planetary systems.

http://www.30doradus.org/images/30dor/30dor_hst_big.jpg

http://www.30doradus.org/index.html

30 Doradus is a huge star-formation complex in the Large Magellanic Cloud. It is the most active starburst region in the entire Local Group of galaxies.

http://www.30doradus.org/30dor_images.html

Supernova 1987 A, na vizinhança da Nebulosa Tarântula

Esta foi a primeira supernova visível a olho nú desde os tempos da estrela de Kepler, em 1604, e o primeiro objeto de seu tipo suficientemente brilhante para ser observado por todos os tipos de equipamento astronômico, bem como, pela primeira vez, através detectores de neutrinos (que são partículas espraiadas pelo colapso gravitacional do núcleo de uma estrela que se tornou uma supernova em seu estágio final de desenvolvimento).

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

SN 1987A was a supernova in the outskirts of the Tarantula Nebula in the Large Magellanic Cloud, a nearby dwarf galaxy. It occurred approximately 51.4kiloparsecs from Earth, approximately 168,000 light-years,^[3] close enough that it was visible to the naked eye. It could be seen from the Southern Hemisphere. It was the closest observed supernova since SN 1604, which occurred in the Milky Way itself. The light from the new supernova reached Earth on February 23, 1987.^[6] As it was the first supernova discovered in 1987, it was labeled “1987A”. Its brightness peaked in May with an apparent magnitude of about 3 and slowly declined in the following months. It was the first opportunity for modern astronomers to see a supernova up close and observations have provided much insight intocore-collapse supernovae.

http://en.wikipedia.org/wiki/SN_1987A

http://en.wikipedia.org/wiki/SN_1987A#mediaviewer/File:SN_1987A_HST.jpg

SN 1987A HSTCC BY 3.0

ESA/Hubble & NASA - http://www.spacetelescope.org/images/potw1142a/

SN 1987A, one of the brightest stellar explosions detected since the invention of the telescope more than 400 years ago[8]

Supernova SN 1987A, one of the brightest stellar explosions since the invention of the telescope more than 400 years ago, is no stranger to the NASA/ESA Hubble Space Telescope. The observatory has been on the frontline of studies into this brilliant dying star since its launch in 1990, three years after the supernova exploded on 23 February 1987. This image of Hubble’s old friend, retreived from the telescope’s data archive, may be the best ever of this object, and reminds us of the many mysteries still surrounding it. Dominating this picture are two glowing loops of stellar material and a very bright ring surrounding the dying star at the centre of the frame. Although Hubble has provided important clues on the nature of these structures, their origin is still largely unknown. Another mystery is that of the missing neutron star. The violent death of a high-mass star, such as SN 1987A, leaves behind a stellar remnant — a neutron star or a black hole. Astronomers expect to find a neutron star in the remnants of this supernova, but they have not yet been able to peer through the dense dust to confirm it is there. The supernova belongs to the Large Magellanic Cloud, a nearby galaxy about 168 000 light-years away. Even though the stellar explosion took place around 166 000 BC, its light arrived here less than 25 years ago. This picture is based on observations done with the High Resolution Channel of Hubble’s Advanced Camera for Surveys. The field of view is approximately 25 by 25 arcseconds.

A SN 1987A foi a primeira supernova estudada com aparelhagem moderna. Através dela, astrônomos de todo mundo puderam fortalecer ou eliminar as teorias que estudam a expansão do universo, tendo as supernovas como material de estudo.

A Shelton Sn 1987A ocorreu na Nebulosa da Tarântula, na Grande Nuvem de Magalhães, uma galáxia anã a aproximadamente 170 mil anos-luz da Terra, tendo como progenitora (a que sofreu o colapso) uma estrela conhecida como Sanduleak -69º 202, uma supergigante azul. Pode ser vista a partir do hemisfério sul. Foi a mais próxima supernova observada desde 1604, que ocorreu na própria Via Láctea.

Ela foi descoberta em 24 de fevereiro de 1987, por Ian Shelton da Universidade de Toronto, no Canadá, através do observatório Las Campanas, no Chile. Seu brilho pico em maio, com uma magnitude aparente de cerca de três e diminuiu lentamente nos meses seguintes. Foi a primeira oportunidade para os astrônomos modernos para verem de perto uma supernova.

http://pt.wikipedia.org/wiki/SN_1987A

http://pt.wikipedia.org/wiki/SN_1987A#mediaviewer/Ficheiro:Supernova-1987a.jpg

Supernova-1987a

First image: Dr. Christopher Burrows, ESA/STScI and NASA; Second image: Hubble Heritage team. - Supernova 1987A: Halo for a Vanished Star, Mosaic of Supernova 1987A.

http://en.wikipedia.org/wiki/SN_1987A#mediaviewer/File:Composite_image_of_Supernova_1987A.jpg

Remnant of SN 1987A seen in light overlays of different spectra. ALMA data (radio, in red) shows newly formed dust in the center of the remnant. Hubble (visible, in green) and Chandra (X-ray, in blue) data show the expanding shock wave.^[1]

http://en.wikipedia.org/wiki/SN_1987A#mediaviewer/File:SN1987a_debris_evolution_animation.gif

SN1987a debris evolution animationCC BY-SA 3.0

Mark McDonald - Larsson, J. et al. (2011). "X-ray illumination of the ejecta of supernova 1987A". Nature 474 (7352): 484–486., video compilation: Mark McDonald

A time sequence of Hubble Space Telescope images, taken in the 15 years from 1994 to 2009, showing the collision of the expanding supernova remnant with a ring of dense material ejected by the progenitor star 20,000 years before the supernova.^[5]

Massive Infant Stars Rock their Cradle

http://images.astronet.ru/pubd/2001/04/04/0001167168/ngc1748_hst_big.jpg

Extremely intense radiation from newly born, ultra-bright stars has blown a glowing spherical bubble in the nebula N83B, also known as NGC 1748. A new NASA Hubble Space Telescope image has helped to decipher the complex interplay of gas and radiation of a star-forming region in a nearby galaxy. The image graphically illustrates just how these massive stars sculpt their environment by generating powerful winds that alter the shape of the parent gaseous nebula. These processes are also seen in our Milky Way in regions like the Orion Nebula.

The Hubble telescope is famous for its contribution to our knowledge about star formation in very distant galaxies. Although most of the stars in the Universe were born several billions of years ago, when the Universe was young, star formation still continues today. This new Hubble image shows a very compact star-forming region in a small part of one of our neighboring galaxies - the Large Magellanic Cloud. This galaxy lies only 165,000 light-years from our Milky Way and can easily be seen with the naked eye from the Southern Hemisphere.

Object Names: N83B, NGC 1748

Image Type: Astronomical

Credit: NASA, ESA, Mohammad Heydari-Malayeri (Observatoire de Paris, France)

LHA 120-N11 in the Large Magellanic Cloud

http://www.spacetelescope.org/images/heic1301a/

Nearly 200 000 light-years from Earth, the Large Magellanic Cloud, a satellite galaxy of the Milky Way, floats in space, in a long and slow dance around our galaxy. As the Milky Way’s gravity gently tugs on its neighbour’s gas clouds, they collapse to form new stars. In turn, these light up the gas clouds in a kaleidoscope of colours, visible in this image from the NASA/ESA Hubble Space Telescope.

Credit:

NASA, ESA. Acknowledgement: Josh Lake

http://www.spacetelescope.org/images/heic1301a/

Zoom into LHA 120-N11

This video zooms in from a view of the night sky into the Large Magellanic Cloud, and focuses in on part of LHA 120-N11, a region of glowing dust and gas with ongoing star formation.

Credit:

NASA, ESA, Digitized Sky Survey 2

http://www.spacetelescope.org/videos/heic1301a/

NGC 2035 é uma nebulosa na direção da constelação de Dorado. O objeto foi descoberto pelo astrônomo James Dunlop em 1826, usando um telescópio refletor com abertura de 9 polegadas.
http://pt.wikipedia.org/wiki/NGC_2035

https://www.eso.org/public/archives/images/screen/eso1348a.jpg

A Grande Nuvem de Magalhães é uma das galáxias mais próximas da nossa. Os astrónomos usaram o poder do Very Large Telescope do ESO para explorar com grande detalhe a NGC 2035, umas das suas regiões menos bem conhecidas. Esta nova imagem mostra nuvens de gás e poeira onde estrelas quentes se estão a formar, ao mesmo tempo que esculpem formas estranhas no seu meio circundante. Mas a imagem mostra também os efeitos da morte das estrelas - filamentos criados por uma explosão de supernova (à esquerda da imagem).

Crédito:

ESO

Situada a apenas 160 000 anos-luz de distância da Terra (eso1311) na constelação do Espadarte, a Grande Nuvem de Magalhães é uma das nossas vizinhas galácticas mais próximas. Encontra-se a formar estrelas de forma ativa em regiões que são tão brilhantes que algumas podem ser vistas a olho nu a partir da Terra, tais como a Nebulosa da Tarântula (eso1033). Esta nova imagem, obtida com o Very Large Telescope do ESO, instalado no Observatório do Paranal no Chile, explora uma região chamada NGC 2035 ou Nebulosa da Cabeça de Dragão (à direita na imagem).

A NGC 2035 é uma região HII, ou nebulosa de emissão, constituída por nuvens de gás que brilham devido à radiação intensa emitida por estrelas jovens. Esta radiação arranca electrões dos átomos do gás, que eventualmente se recombinam com outros átomos emitindo radiação. Misturados com o gás estão nodos densos escuros de poeira que absorvem a radiação em vez de a emitirem, criando assim ao longo da nebulosa troços estreitos intrincados e formas escuras.

LEIA MAIS EM

http://www.eso.org/public/brazil/news/eso1348/

ESO. Zooming in on the star formation region NGC 2035. HD

http://www.youtube.com/watch?v=GzrBolB4KjQ

http://apod.nasa.gov/apod/ap060206.html
The N44 Superbubble
Credit & Copyright: Gemini Obs., AURA, NSF
Explanation: What created this gigantic hole? The vast emission nebula N44 in our neighboring galaxy the Large Magellanic Cloud has a large, 250 light-year hole and astronomers are trying to figure out why. One possibility is particle winds expelled by massive stars in the bubble's interior that are pushing out the glowing gas. This answer has been recently found to be inconsistent with measured wind velocities, however. Another possibility is that the expanding shells of old supernovas have sculpted the unusual space cavern. An unexpected clue of hot X-ray emitting gas was recently been detected escaping the N44 superbubble. The above image, here digitally sharpened, was taken in three very specific colors by the huge 8-meter Gemini South Telescope on Cerro Pachonin Chile.

DEM L 159 Nebula and KMHK 840 and 831 Starclusters in the LMC

http://www.eso.org/public/usa/images/eso0332c/

The ionised region DEM L 159 and two clusters with hot stars named KMHK 840 (top left) and KMHK 831 (bottom right). The colours have been enhanced compared to ESO Press Photo eso0332a to clearly show the different shades.

Credit:

ESO

SNR B0544-6910 in the LMC

http://www.eso.org/public/unitedkingdom/images/eso0437d/

Young supernova remnant, B0544-6910 located in the South-East of the ringshaped nebula DEM L 299 in the Large Magellanic Cloud. The sky field measures 3.7 x 3.6 arcmin. North is up and East is left.

Credit:

ESO

http://archive.today/7ASc#selection-2361.0-2377.3

http://en.wikipedia.org/wiki/Large_Magellanic_Cloud#mediaviewer/File:Large_and_small_magellanic_cloud_from_new_zealand.jpg

Large and small magellanic cloud from new zealand

Markrosenrosen - Own work

Os desenhos formados pelas estrelas – As Constelações - são como janelas que se abrem para a infinitude do universo e que possibilitam nossa mente a ir percebendo que existe mais, bem mais, entre o céu e a terra bem como percebendo que o caos, vagarosamente, vai se tornando Cosmos e sendo por nossa mente conscientizado. Quer dizer, nossa mente é tão infinita quanto infinito é o Cosmos.

COM UM ABRAÇO ESTRELADO,

Janine Milward

- 6^a. Edição do Atlas Celeste

de autoria de Ronaldo Rogério de Freitas Mourão,

Editora Vozes, Petrópolis, ano de 1986

(com dedicatória do próprio autor para mim

em evento realizado no Museu de Astronomia do Rio de Janeiro,

em 16/06/1989)

- Mario Jaci Monteiro , As Constelações, Cartas Celestes -

Apoio: CARJ/MEC/CAPES/PADCT-SPEC - com dedicatória do autor para mim, em março de 2004 (quando Mário Jaci generosamente me presenteou com um instrumento de observação (kepleriano) artesanalmente construído por ele).

Da Terra ao Céu

e ao Infinito

Constelações, Estrelas e Objetos Celestes

(sob o ponto de vista do Mundo Ocidental)

Suas histórias, seus mitos, seus significados e suas sintetizadas descrições

Reunião das Informações e Compilação,

Tradução para a língua portuguesa (em alguns momentos)

bem como Comentários Pessoais:

Janine Milward

Visitando os Sites abaixo,

você conseguirá informações atualizadas e preciosas

sobre os Objetos Celestiais de seu interesse:

NASA/IPAC EXTRAGALACTIC DATABASE –

http://ned.ipac.caltech.edu/

http://ned.ipac.caltech.edu/forms/byname.html

NASA/IPAC Extragalactic Database (NED) - operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

THE NIGHT SKY ATLAS

http://www.nightskyatlas.com/index.jsp

The night sky atlas creates images of any part of the night sky, allowing easy location of any object. Detailed chart images show all stars visible to the naked eye, the constellations, Messier objects, and names of the brightest stars.

The Internet STELLAR DATABASE

http://www.stellar-database.com/

- stars within 75 light-years. (Plus some of the more well-known "name brand" stars farther away.)

Estrela mãe
Exoplaneta		Lista de exoplanetas

Estrela		HD 4308
Constelação		Tucana
Ascensão reta		00h 44m 39,3s
Declinação		-65° 38′ 58,3″
Magnitude aparente		6,54
Distância		71,39 anos-luz (21,9 pc)
Elementos orbitais
Semieixo maior		0,115 ± 0,096 UA
Periastro		0,115 UA
Apoastro		0,115 UA
Excentricidade		0,00 ± 0,01
Período orbital		15,56 ± 0,02 dias
Argumento do periastro		359 ± 47°
Semi-amplitude		4,07 ± 0,2 m/s m/s
Características físicas
Massa		>0,0442 MJ >14 M⊕
Descoberta
Data da descoberta		22 de agosto de 2005
Descobridores		Udry et al.
Método de detecção		Espectroscopia Doppler
Estado da descoberta		Publicada

Estrela mãe
Exoplaneta		Lista de exoplanetas

Estrela		HD 215497
Constelação		Tucana
Ascensão reta		22h 46m 36,7s
Declinação		-56° 35′ 58,3″
Magnitude aparente		8,97
Distância		142 ± 7,8 anos-luz(43,5 ± 2,4 pc)
Elementos orbitais
Semieixo maior		0,044 UA
Período orbital		3,93 dias (0,0108 anos)
Características físicas
Massa		>0,017 MJ >5,4 M⊕
Descoberta
Data da descoberta		19 de outubro de 2009
Descobridores		Lo Curto et al.
Método de detecção		Velocidade radial (HARPS)

Estrela mãe
Exoplaneta		Lista de exoplanetas

Estrela		HD 215497
Constelação		Tucana
Ascensão reta		22h 46m 36,7s
Declinação		-56° 35′ 58,3″
Magnitude aparente		8,97
Distância		142 ± 7,8 anos-luz(43,5 ±2,4 pc)
Elementos orbitais
Semieixo maior		1,282 UA
Excentricidade		0,49 ± 0,04
Período orbital		569,94 dias (1,56 anos)
Argumento do periastro		45 ± 4°
Semi-amplitude		10,10 ± 0,65 m/s m/s
Características físicas
Massa		>0,33 MJ >104,3 M⊕
Descoberta
Data da descoberta		19 de outubro de 2009
Descobridores		Lo Curto et al.
Método de detecção		Velocidade radial (HARPS)
Estado da descoberta		Publicada

Estrela mãe
Exoplaneta		Lista de exoplanetas

Estrela		HD 221287
Constelação		Tucana
Ascensão reta		23h 31m 20,3s
Declinação		-58° 12′ 35,0″
Magnitude aparente		7,82
Distância		172,5 anos-luz (52,9 pc)
Elementos orbitais
Semieixo maior		1,25 ± 0,04 UA
Periastro		1,15 UA
Apoastro		1,35 UA
Excentricidade		0,08 ± 0,11
Período orbital		456,1 ± 6,5 dias(1,2487 anos)
Argumento do periastro		98 ± 72°
Semi-amplitude		71 ± 13 m/s m/s
Características físicas
Massa		>3,12 ± 0,78 MJ >992 M⊕
Descoberta
Data da descoberta		5 de março de 2007
Descobridores		Naef et al.
Método de detecção		Espectrógrafo HARPS
Estado da descoberta		Publicada

English: The local group of galaxies surrounding the Milky Way
Date	21 September 2006
Source	Re-drawn from File:Local Group.JPG, originally from http://www.atlasoftheuniverse.com
Author	Richard Powell

Da Terra ao Céu e ao Infinito - Algumas das 88 Constelações

AS NUVENS DE MAGALHÃES

Da Terra ao Céu ....

.....e ao Infinito

- As 88 Constelações

Globular cluster 47 Tucanae and the Small Magellanic Cloud (ground-based image)

Image: Hubble Observes Infant Stars in Nearby Galaxy

Zooming on NGC 602

Hubble finds source of Magellanic Stream

Astronomers explore origin of gas ribbon wrapped around our galaxy

Image: Hubble Observes Infant Stars in Nearby Galaxy

Zooming on NGC 602

"Mensa" constellation

Mons Mensae, the Table Mountain,

"Mensa" constellation

Durante os anos de 1750-1754 se dedicou a estudar as estrelas e constelações do hemisfério austral, com este intuito viajou até o Cabo da Boa Esperança na parte mais austral do continente africano. Com base nestas observações publicou o Coelum Australe Stelliferum sua obra mais importante.

Voyage to the Cape of Good Hope

http://en.wikipedia.org/wiki/Nicolas_Louis_de_Lacaille

History

Notable features

Stars

Deep-sky objects

Massive Infant Stars Rock their Cradle

LHA 120-N11 in the Large Magellanic Cloud

Zoom into LHA 120-N11

ESO. Zooming in on the star formation region NGC 2035. HD

DEM L 159 Nebula and KMHK 840 and 831 Starclusters in the LMC

http://www.eso.org/public/usa/images/eso0332c/

The ionised region DEM L 159 and two clusters with hot stars named KMHK 840 (top left) and KMHK 831 (bottom right). The colours have been enhanced compared to ESO Press Photo eso0332a to clearly show the different shades.

Credit:

ESO

SNR B0544-6910 in the LMC

AS NUVENS DE MAGALHÃES

Da Terra ao Céu ....

.....e ao Infinito

- As 88 Constelações

Globular cluster 47 Tucanae and the Small Magellanic Cloud (ground-based image)

Image: Hubble Observes Infant Stars in Nearby Galaxy

Zooming on NGC 602

Hubble finds source of Magellanic Stream

Astronomers explore origin of gas ribbon wrapped around our galaxy

Image: Hubble Observes Infant Stars in Nearby Galaxy

Zooming on NGC 602

"Mensa" constellation

Mons Mensae, the Table Mountain,

"Mensa" constellation

Durante os anos de 1750-1754 se dedicou a estudar as estrelas e constelações do hemisfério austral, com este intuito viajou até o Cabo da Boa Esperança na parte mais austral do continente africano. Com base nestas observações publicou o Coelum Australe Stelliferum sua obra mais importante.

Voyage to the Cape of Good Hope

http://en.wikipedia.org/wiki/Nicolas_Louis_de_Lacaille

History

Notable features

Stars

Deep-sky objects

Massive Infant Stars Rock their Cradle

LHA 120-N11 in the Large Magellanic Cloud

Zoom into LHA 120-N11

ESO. Zooming in on the star formation region NGC 2035. HD

DEM L 159 Nebula and KMHK 840 and 831 Starclusters in the LMC

http://www.eso.org/public/usa/images/eso0332c/ The ionised region DEM L 159 and two clusters with hot stars named KMHK 840 (top left) and KMHK 831 (bottom right). The colours have been enhanced compared to ESO Press Photo eso0332a to clearly show the different shades. Credit: ESO

SNR B0544-6910 in the LMC

http://www.eso.org/public/usa/images/eso0332c/

The ionised region DEM L 159 and two clusters with hot stars named KMHK 840 (top left) and KMHK 831 (bottom right). The colours have been enhanced compared to ESO Press Photo eso0332a to clearly show the different shades.

Credit:

ESO