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Contains:  NGC 2244, Rosette nebula, NGC 2239, The star 12Mon
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NGC2237 Rosette Nebula - SHO, 





    
        

            Jerry Macon
NGC2237 Rosette Nebula - SHO

NGC2237 Rosette Nebula - SHO

Technical card

Resolution: 2957x2509

Dates:Feb. 1, 2017

Frames:
Ha: 30x240" -30C bin 1x1
Baader OIII: 30x240" -30C bin 1x1
Baader SII: 30x240" -30C bin 1x1

Integration: 6.0 hours

Avg. Moon age: 4.55 days

Avg. Moon phase: 21.65%

Bortle Dark-Sky Scale: 4.00

Astrometry.net job: 1914667

RA center: 97.961 degrees

DEC center: 4.974 degrees

Pixel scale: 1.917 arcsec/pixel

Orientation: 270.696 degrees

Field radius: 1.032 degrees

Locations: Dark Star Observatory, Taos, New Mexico, United States

Description

The Rosette Nebula is a large, spherical, H II region located near one end of a giant molecular cloud in the Monoceros region of the Milky Way Galaxy. The open cluster NGC 2244 (Caldwell 50) is closely associated with the nebulosity, the stars of the cluster having been formed from the nebula's matter.

The cluster and nebula lie at a distance of some 5,000 light-years from Earth and measure roughly 50 light years in diameter. The radiation from the young stars excites the atoms in the nebula, causing them to emit radiation themselves producing the emission nebula we see. The mass of the nebula is estimated to be around 10,000 solar masses.

A survey of the nebula with the Chandra X-ray Observatory has revealed the presence of numerous new-born stars inside optical Rosette Nebula and studded within a dense molecular cloud. Altogether, approximately 2500 young stars lie in this star-forming complex, including the massive O-type stars HD 46223 and HD 46150, which are primarily responsible for blowing the ionized bubble. Most of the ongoing star-formation activity is occurring in the dense molecular cloud to the south east of the bubble.

A diffuse X-ray glow is also seen between the stars in the bubble, which has been attributed to a super-hot plasma with temperatures ranging from 1 to 10 million K. This is significantly hotter than the 10,000 K plasmas seen in HII regions, and is likely attributed to the shock-heated winds from the massive O-type stars. (Wikipedia)

Comments

Author

jmacon
Jerry Macon
License: Attribution Creative Commons
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NGC2237 Rosette Nebula - SHO, 





    
        

            Jerry Macon