IC 1795, knows also as Fish head Nebula is a part of a larger nebula Named Heart Nebula (also known as the Running dog nebula, IC 1805, Sharpless 2-190). It is an emission nebula located about 7500 light years away from Earth the Perseus Arm of the Galaxy in the constellation Cassiopeia.
M 52 or Messier 52 (also known as NGC 7654 or the “Salt and Pepper” cluster) is an open cluster in the constellation Cassiopeia. The exact distance of this cluster from our system is estimated between 3900 and 4900 light years, although an accepted value is around 4500 light years.
Messier 92 known as M92 or NGC 6341, is a globular cluster of stars in the northern constellation of Hercules. A globular cluster is a spheroidal conglomeration of stars. Globular clusters are bound together by gravity, with a higher concentration of stars towards their centers. They can contain anywhere from tens of thousands to many millions of member stars. Their name is derived from Latin globulus (small sphere). Globular clusters are occasionally known simply as “globulars”.
The Crescent Nebula, known as NGC 6888 is an emission nebula in the constellation Cygnus, about 5000 light-years away from Earth. It was discovered by William Herschel in 1792. It is formed by the fast stellar wind from the Wolf-Rayet star WR 136 (HD 192163) colliding with and energizing the slower moving wind ejected by the star when it became a red giant around 250,000 to 400,000 years ago. The result of the collision is a shell and two shock waves, one moving outward and one moving inward. The inward moving shock wave heats the stellar wind to X-ray-emitting temperatures.
The Cat’s Eye Nebula (also known as NGC 6543 and Caldwell 6) is a planetary nebula in the northern constellation of Draco, discovered by William Herschel on February 15, 1786. It was the first planetary nebula whose spectrum was investigated by the English amateur astronomer William Huggins, demonstrating that planetary nebulae were gaseous and not stellar in nature. Structurally, the object has had high-resolution images by the Hubble Space Telescope revealing knots, jets, bubbles and complex arcs, being illuminated by the central hot planetary nebula nucleus (PNN). It is a well-studied object that has been observed from radio to X-ray wavelengths.
The Pinwheel Galaxy, known as Messier 101, is a face-on spiral galaxy 21 million light-years away from Earth in the constellation Ursa Major. It was discovered by Pierre Méchain in 1781 and was communicated that year to Charles Messier, who verified its position for inclusion in the Messier Catalogue as one of its final entries. M101 is a large galaxy, with a diameter of 170,000 light-years. By comparison, the Milky Way has a diameter of between 100,000 and 120,000 light-years. It has around a trillion stars. It has a disk mass on the order of 100 billion solar masses, along with a small central bulge of about 3 billion solar masses. Its characteristics can be compared to those of Andromeda Galaxy.
M101 has a high population of H II regions, many of which are very large and bright. H II regions usually accompany the enormous clouds of high density molecular hydrogen gas contracting under their own gravitational force where stars form. H II regions are ionized by large numbers of extremely bright and hot young stars; those in M101 are capable of creating hot superbubbles. In a 1990 study, 1,264 H II regions were cataloged in the galaxy. Three are prominent enough to receive New General Catalogue numbers—NGC 5461, NGC 5462, and NGC 5471.
60x300s (5 hours) Skywatcher PDS250 – EQ6R – Asi 533 – in Bortle 6
It’s not always easy … Sometimes the most beautiful evenings in winter are also the coldest ones. And the instrumentation has to withstand conditions that are not exactly “ideal”. But also this time, everything went well and I managed to bring home a very interesting session …
M 13 – Great Globular Cluster in Hercules
M13 was discovered by Edmond Halley in 1714, and cataloged by Charles Messier on June 1, 1764, into his list of objects not to mistake for comets; Messier’s list, including Messier 13, eventually became known as the Messier Catalog.
About one third of the way from Vega to Arcturus, four bright stars in Herculēs form the Keystone asterism, the broad torso of the hero. M13 can be seen in this asterism 2⁄3 of the way north (by west) from Zeta to Eta Herculis. Although only telescopes with great light-gathering capability fully resolve the stars of the cluster, M13 may be visible to the naked eye depending on circumstances.
M81 Bode’s Galaxy – M82 Cigar Galaxy
Messier 81, the galaxy on the bottom left of the photo, (aka NGC 3031 or Bode’s Galaxy) is a grand design spiral galaxy about 12 million light-years away, with a diameter of 90,000 light years, in the constellation Ursa Major. Messier 81 was first discovered by Johann Elert Bode on 31 December 1774. In 1779, Pierre Méchain and Charles Messier reidentified Bode’s object, hence listed it in the Messier Catalogue.
Messier 82, the galaxy on the upper right of the photo, (also known as NGC 3034, Cigar Galaxy or M82) is a Starburst galaxy approximately 12 million light-years away in the constellation Ursa Major. A member of the M81 Group, it is about five times more luminous than the Milky Way and has a center one hundred times more luminous. The starburst activity is thought to have been triggered by interaction with neighboring galaxy M81. As the closest starburst galaxy to Earth, M82 is the prototypical example of this galaxy type. M82, with M81, was discovered by Johann Elert Bode in 1774; he described it as a “nebulous patch”, this one about 3⁄4 degree away from the other, “very pale and of elongated shape”. In 1779, Pierre Méchain independently rediscovered both objects and reported them to Charles Messier, who added them to his catalog
NGC 6995 – The Bat Nebula is a portion of a bigger nebula called Veil Nebula,. a supernova remnant (SNR) is the structure resulting from the explosion of a star in a supernova. The Veil Nebula consists of two loops, called Eastern Veil and Western Veil Nebula. The Bat nebula is part of the Eastern Veil Nebula
The nebula was discovered on 5 September 1784 by William Herschel. He described the western end of the nebula as “Extended; passes thro’ 52 Cygni… near 2 degree in length”, and described the eastern end as “Branching nebulosity … The following part divides into several streams uniting again towards the south.” When finely resolved, some parts of the nebula appear to be rope-like filaments. The standard explanation is that the shock waves are so thin, less than one part in 50,000 of the radius, that the shell is visible only when viewed exactly edge-on, giving the shell the appearance of a filament. At the estimated distance of 2400 light-years, the nebula has a radius of 65 light-years (a diameter of 130 light-years). The thickness of each filament is 1⁄50,000th of the radius, or about 4 billion miles, roughly the distance from Earth to Pluto. Undulations in the surface of the shell lead to multiple filamentary images, which appear to be intertwined.
Shooting data: Taken on 2022/090/05 – 16 shots of 300 ″ – Temp -10º – Dark Frames – Bias Frames – Flat Frames
Processing: Processing done entirely with PixInsight