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Dimensions3252 x 2224
Original file size881 KB
Image typeJPEG
Color spaceUncalibrated
NGC 2237 HaRGB

NGC 2237 HaRGB

Other Names: Rosette Nebula, Caldwell 49, SH2-275
Optics: Borg Astrograph 101ED at f/4.1
Mount: Atlas EQG using The Sky6, EQMOD, & MaxPilote
Camera: QSI 583WS
Filters: Astrodon Ha 3nm, Gen II RGB
Exposure: 305 Mins, [61 x 300s] 200 mins Ha, 40 mins each of R&B, 25 mins G
Accessories: Auto guided with Borg 45ED and Orion Starshoot Auto Guider using Maxim DL guiding
Location: Rodeo, NM
Date: November 12th, 2012
Notes: Processing: Image acquisition with Maxim DL Pro using MaxPilote automation. Image calibration, align, and combine in Maxim DL Pro. Levels, curves, Ha RGB Starizona method #2, crop and resize in Photoshop.
Calibrated w/25 Darks, 93 Bias, 100 Flats of each filter using light box, CCD temperature was -30C. Image was taken near the Arizona Sky Village near Portal, AZ.

High Res Version: http://astromarina.zenfolio.com/img/s8/v79/p1374383562-6.jpg
Ha Version: http://astromarina.zenfolio.com/p264248004/h51ebe514#h51ebe514
Original RGB Version: http://astromarina.zenfolio.com/p14536770/h51EC196C#h51ec196c

The Rosette Nebula (also known as Caldwell 49) is a large, circular 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 complex has the following NGC designations:
  • NGC 2237 – Part of the nebulous region (Also used to denote whole nebula)
  • NGC 2238 – Part of the nebulous region
  • NGC 2239 – Part of the nebulous region (Discovered by John Herschel)
  • NGC 2244 – The open cluster within the nebula (Discovered by John Flamsteed in 1690)
  • NGC 2246 – Part of the nebulous region

The cluster and nebula lie at a distance of some 5,200 light-years from Earth (although estimates of the distance vary considerably, down to 4,900 light-years.[3]) and measure roughly 130 light years in diameter. The radiation from the young stars excite 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.
It is believed that stellar winds from a group of O and B stars are exerting pressure on interstellar clouds to cause compression, followed by star formation in the nebula. This star formation is currently still ongoing.