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Centaurus_done.jpg
Centaurus_done.jpgCentaurus A.602 viewsThe Centaurus A/M83 Group is a complex group of galaxies in the constellations Hydra, Centaurus, and Virgo. The group may be roughly divided into two subgroups. The Cen A Subgroup, at a distance of 11.9 Mly (3.66 Mpc), is centered around Centaurus A, a nearby radio galaxy.[3] The M83 Subgroup, at a distance of 14.9 Mly (4.56 Mpc), is centered around the Messier 83 (M83), a face-on spiral galaxy.[3]

This group is sometimes identified as one group[4][5] and sometimes identified as two groups.[6] Hence, some references will refer to two objects named the Centaurus A Group and the M83 Group. However, the galaxies around Centaurus A and the galaxies around M83 are physically close to each other, and both subgroups appear not to be moving relative to each other.[3]

The Centaurus A/M83 Group is part of the Virgo Supercluster, the local supercluster of which the Local Group is an outlying member.
Martin
M48-done2M.jpg
M48-done2M.jpgM48.564 viewsMessier 48 (also known as M 48 or NGC 2548) is an open cluster in the Hydra constellation. It was discovered by Charles Messier in 1771.

There is actually no cluster in the position indicated by Messier. The value that he gave for the right ascension matches that of NGC 2548, however, his declination is off by five degrees.Credit for discovery is sometimes given instead to Caroline Herschel in 1783.
Martin
Leodone2G.jpg
Leodone2G.jpgLeo triplet510 viewsJust testing the guiding on the G11 with Gemini 2Martin
m42done.jpg
m42done.jpgM42.838 viewsThe Orion Nebula (also known as Messier 42, M42, or NGC 1976) is a diffuse nebula situated south of Orion's Belt. It is one of the brightest nebulae, and is visible to the naked eye in the night sky. M42 is located at a distance of 1,344 ± 20 light years[2][5] and is the closest region of massive star formation to Earth. The M42 nebula is estimated to be 24 light years across. Older texts frequently referred to the Orion Nebula as the Great Nebula in Orion or the Great Orion Nebula.

The Orion Nebula is one of the most scrutinized and photographed objects in the night sky, and is among the most intensely studied celestial features.[6] The nebula has revealed much about the process of how stars and planetary systems are formed from collapsing clouds of gas and dust. Astronomers have directly observed protoplanetary disks, brown dwarfs, intense and turbulent motions of the gas, and the photo-ionizing effects of massive nearby stars in the nebula. There are also supersonic "bullets" of gas piercing the dense hydrogen clouds of the Orion Nebula. Each bullet is ten times the diameter of Pluto's orbit and tipped with iron atoms glowing bright blue. They were probably formed one thousand years ago from an unknown violent event.
Martin
Eagle_done-1.jpg
Eagle_done-1.jpgEagle nebula.541 viewsThe Eagle Nebula is part of a diffuse emission nebula, or H II region, which is catalogued as IC 4703. This region of active current star formation is about 6,500 light-years distant. The tower of gas that can be seen coming off the nebula is approximately 57 trillion miles (97 trillion km) high.

The brightest star in the nebula has an apparent magnitude of +8.24, easily visible with good binoculars.
Martin
etacrop.jpg
etacrop.jpgEta Carinae nebula.562 viewsThis stellar system is currently one of the most massive that can be studied in great detail. Until recently, Eta Carinae was thought to be the most massive single star, but it was recently demoted to a binary system.[7] The most massive star in the Eta Carinae multiple star system has more than 100 times the mass of the Sun. Other known massive stars are more luminous and more massive.

Stars in the mass class of Eta Carinae, with more than 100 times the mass of the Sun, produce more than a million times as much light as the Sun. They are quite rare — only a few dozen in a galaxy as big as the Milky Way. They are assumed to approach (or potentially exceed) the Eddington limit, i.e., the outward pressure of their radiation is almost strong enough to counteract gravity. Stars that are more than 120 solar masses exceed the theoretical Eddington limit, and their gravity is barely strong enough to hold in their radiation and gas.

Eta Carinae's chief significance for astrophysics is based on its giant eruption or supernova impostor event, which was observed around 1843. In a few years, Eta Carinae produced almost as much visible light as a supernova explosion, but it survived. Other supernova impostors have been seen in other galaxies, for example the false supernovae SN 1961v in NGC 1058[8] and SN 2006jc in UGC 4904,[9] which produced a false supernova, noted in October 2004. Significantly, SN 2006jc was destroyed in a supernova explosion two years later, observed on October 9, 2006.[10] The supernova impostor phenomenon may represent a surface instability[11] or a failed supernova. Eta Carinae's giant eruption was the prototype for this phenomenon, and after nearly 170 years the star's internal structure has not fully recovered.
Martin
Tarantula-done.jpg
Tarantula-done.jpgTarantula nebula.781 viewsThe Tarantula Nebula (also known as 30 Doradus, or NGC 2070) is an H II region in the Large Magellanic Cloud. It was originally thought to be a star, but in 1751 Nicolas Louis de Lacaille recognized its nebular nature.

The Tarantula Nebula has an apparent magnitude of 8. Considering its distance of about 49 kpc[2] (160,000 light years), this is an extremely luminous non-stellar object. Its luminosity is so great that if it were as close to Earth as the Orion Nebula, the Tarantula Nebula would cast shadows. In fact, it is the most active starburst region known in the Local Group of galaxies. It is also the largest such region in the Local Group with an estimated diameter of 200 pc.[3] The nebula resides on the leading edge of the LMC, where ram pressure stripping, and the compression of the interstellar medium likely resulting from this, is at a maximum. At its core lies the compact star cluster R136 (approx diameter 35 light years)[4] that produces most of the energy that makes the nebula visible. The estimated mass of the cluster is 450,000 solar masses, suggesting it will likely become a globular cluster in the future.
Martin
Dazza_and_my_scope_on_right.jpg
Dazza_and_my_scope_on_right.jpg4782 viewsMartin

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rosette_done_ha2Mb.jpg
rosette_done_ha2Mb.jpgRosetta in HA.512 viewsStill lots of noise in the surroundings so will need more exposures.MartinDec 28, 2014
Eta_Carinae_done_ha2Mb.jpg
Eta_Carinae_done_ha2Mb.jpgEta Carinae with the EQ8 mount.823 viewsMartinDec 28, 2014
Eta_Carina.jpg
Eta_Carina.jpgEta Carinae543 viewstest image with OAG.MartinFeb 12, 2014
Lagoondone2Mb.jpg
Lagoondone2Mb.jpgLagoon nebula680 viewsDone with the ED100 and Hutech FR/FF.MartinMay 15, 2013
triffid_done2MB.jpg
triffid_done2MB.jpgTriffid nebula747 viewsDone with the ED100 and Hutech FR/FF.MartinMay 15, 2013
testing.jpg
testing.jpgtestimage984 views2X30Seconds at ISO1600MartinMay 12, 2012
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Sombrerocropdone.jpgSombrero galaxy1561 viewsThe Sombrero Galaxy (also known as M104 or NGC 4594) is an unbarred spiral galaxy in the constellation Virgo located 28 million light years from Earth. It has a bright nucleus, an unusually large central bulge, and a prominent dust lane in its inclined disk. The dark dust lane and the bulge give this galaxy the appearance of a sombrero. Astronomers initially thought that the halo was small and light, indicative of a spiral galaxy. But Spitzer found that halo around the Sombrero Galaxy is larger and more massive than previously thought, indicative of a giant elliptical galaxy. [5] The galaxy has an apparent magnitude of +9.0, making it easily visible with amateur telescopes. The large bulge, the central supermassive black hole, and the dust lane all attract the attention of professional astronomers.MartinMay 11, 2012
NGC4945.jpg
NGC4945.jpgNGC4945.1084 viewsNGC4945 with the Supernova.MartinApr 11, 2012