The bright rim is the surface of the dense cloud that is being illuminated and ionized by a very bright, massive star (HD 206267) that is just to the east of IC 1396A. The piece of the nebula shown here is the dark, dense globule IC 1396A it is commonly called the Elephant's Trunk nebula because of its appearance at visible light wavelengths, where there is a dark patch with a bright, sinuous rim. The Elephant's Trunk Nebula is a concentration of interstellar gas and dust within the much larger ionized gas region IC 1396 located in the constellation Cepheus about 2,400 light years away from Earth. The processing for this version was done by Budassi in 2021. This image combines observations performed through three different filters (B, V, R) with the 1.5-metre Danish telescope at the ESO La Silla Observatory in Chile. The Lagoon Nebula derives its name from the wide lagoon-shaped dark lane located in the middle of the nebula that divides it into two glowing sections. Messier 8 is one of the few star-forming nebulae visible to the unaided eye, and was discovered as long ago as 1747, although the full range of colours wasn’t visible until the advent of more powerful telescopes. Two of these giant stars illuminate the brightest part of the nebula, known as the Hourglass Nebula, a spiralling, funnel-like shape near its centre. It boasts many large, hot stars, whose ultraviolet radiation sculpts the gas and dust into unusual shapes. Located four to five thousand light-years away, in the constellation of Sagittarius (the Archer), the nebula is a giant interstellar cloud, one hundred light-years across. Gas and dust condense, beginning the process of creating new stars in this image of Messier 8, also known as the Lagoon Nebula. Although it is four times as large as and even brighter than the famous Orion Nebula, the Carina Nebula is much less well known due to its location in the southern sky. The nebula is one of the largest diffuse nebulae in our skies. NGC 3293 is the oldest and furthest from Trumpler 14, indicating sequential and ongoing star formation. Trumpler 15, Collinder 228, Collinder 232, NGC 3324, and NGC 3293 are also considered members of the association. Trumpler 16 is the home of WR 25, currently the most luminous star known in our Milky Way galaxy, together with the less luminous but more massive and famous Eta Carinae star system and the O2 supergiant HD 93129A. Trumpler 14 is one of the youngest known star clusters at half a million years old. Carina OB1 encompasses the star clusters Trumpler 14 and Trumpler 16. The nebula has within its boundaries the large Carina OB1 association and several related open clusters, including numerous O-type stars and several Wolf–Rayet stars. The nebula is approximately 8,500 light-years (2,600 pc) from Earth. The Carina Nebula or Eta Carinae Nebula (catalogued as NGC 3372) is a large, complex area of bright and dark nebulosity in the constellation Carina, and it is located in the Carina–Sagittarius Arm. There has been no appreciable change in this quintuple system since the first measures were made in 1875. It consists of an 8th-magnitude primary with four companions at distances between 1.4 and 15.7 arcsec. Burnham, whose bright component is identified as the highly luminous O6 spectral class star, HD 5005 or HIP 4121. Edward Emerson Barnard discovered the nebula in August 1883, describing it as "a large faint nebula, very diffuse." Multiple star 'B 1' or β 1 was later discovered by S. Colloquially, NGC 281 is also known as the Pacman Nebula for its resemblance to the video game character. A recent distance from radio parallaxes of water masers at 22 GHz made during 2014 is estimated it lies 2.82☐.20 kpc. It collectively forms Sh2-184, spanning over a larger area of 40 arcmin. This 20×30 arcmin sized nebulosity is also associated with open cluster IC 1590, several Bok globules and the multiple star, B 1. NGC 281, IC 11 or Sh2-184 is a bright emission nebula and part of an H II region in the northern constellation of Cassiopeia and is part of the Milky Way's Perseus Spiral Arm.
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