Roberto Colombari
In the arms of Andromeda
This is a composition of broadband filters and narrow data with a RC 10" and Apogee U9
L: 34x900s
RGB: (22, 10, 22)x900s
Ha: 67x900s
Processing: R. Colombari
Data: C. Iaffaldano
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NGC 206 is a bright star cloud in the Andromeda Galaxy. It is notable for being the brightest star cloud in Andromeda as viewed from Earth.
Features[edit]
NGC 206 is the richest and most conspicuous star cloud in the Andromeda Galaxy as well as one of the largest and brightest star formation regions of the Local Group.[2] It contains more than 300 stars brighter than Mb=-3.6.[3] It was originally identified by Edwin Hubble as a star cluster but today, due to its size, it is classified as an OB association.[4]
NGC 206 is located in a spiral arm of the Andromeda Galaxy, in a zone free of neutral hydrogen and has a double structure, with one region that has an age of around 10 million years and includes several H II regions in one of its borders and other with an age of between 40 million years and 50 million years that includes a number of cepheids. Both parts are separated by a band of interstellar dust and include hundreds of stars of spectral type O and B.[5]
Source: Wikipedia
In the arms of Andromeda
This is a composition of broadband filters and narrow data with a RC 10" and Apogee U9
L: 34x900s
RGB: (22, 10, 22)x900s
Ha: 67x900s
Processing: R. Colombari
Data: C. Iaffaldano
____________________________________
NGC 206 is a bright star cloud in the Andromeda Galaxy. It is notable for being the brightest star cloud in Andromeda as viewed from Earth.
Features[edit]
NGC 206 is the richest and most conspicuous star cloud in the Andromeda Galaxy as well as one of the largest and brightest star formation regions of the Local Group.[2] It contains more than 300 stars brighter than Mb=-3.6.[3] It was originally identified by Edwin Hubble as a star cluster but today, due to its size, it is classified as an OB association.[4]
NGC 206 is located in a spiral arm of the Andromeda Galaxy, in a zone free of neutral hydrogen and has a double structure, with one region that has an age of around 10 million years and includes several H II regions in one of its borders and other with an age of between 40 million years and 50 million years that includes a number of cepheids. Both parts are separated by a band of interstellar dust and include hundreds of stars of spectral type O and B.[5]
Source: Wikipedia