M17 - The Swan or Omega Nebula in H-Alpha+RGB (plus Sh2-40 and Messier 18)

Image Data:

Scope: AP155EDF w FT focuser and 4" FF
Camera: Moravian G4 (16803 chip) w Astrodon Gen II HaRGB filters
Mount: Paramount MX
Guiding: ST402ME + Borg 60mm achromat
9 x 20 minutes H-Alpha
12/9/12  x 10 minutes RGB
Lucknow, Ontario, Canada
July 2020
Images captured with CCD-Commander and TheSkyX
Each channel processed in PixInsight; RGB combined in PixInsight and PhotometricColourCalibration applied; some additional processing
H-Alpha combined with RGB in Photoshop 2020

M17 The Swan or Omega Nebula: Bottom left of image. Upper right of image is IC 4701 aka Sharpless 44 (Sh2-44), a large faint emission nebula



Discovered by Philippe Loys de Chéseaux in 1745-46.

The Omega Nebula, Messier 17 (M17, NGC 6618), also called the Swan Nebula, the Horseshoe Nebula, or (especially on the southern hemisphere) the Lobster Nebula, is a region of star formation and shines by excited emission, caused by the higher energy radiation of young stars. Unlike in many other emission nebulae, however, these stars are not obvious in optical images, but hidden in the nebula. Star formation is either still active in this nebula, or ceased very recently. A small cluster of about 35 bright but obscurred stars seems to be imbedded in the nebulosity.

This object was discovered by Philippe Loys de Chéseaux and is one of only six "nebulae properly so called" in his catalog. De Chéseaux's discovery didn't get widely known, thus Charles Messier independently rediscovered it and cataloged it on June 3, 1764.

The color of the Omega Nebula is reddish, with some graduation to pink. This color comes from the hot hydrogen gas which is excited to shine by the hottest stars which have just formed within the nebula. However, the brightest region is actually of white color, not overexposed as one might think. This phenomenon is apparently a result of a mixture of emission light from the hottest gas, together with reflections of the bright star light from the dust in this region. The nebula contains a large amount of dark obscurring material, which is obvious in its remarkable features. This matter has been heated by the hidden young stars, and shines brightly in infrared light.

The mass of the gas has been estimated to amount about 800 times that of the Sun, enough for forming a conspicuous cluster, and a good deal more than that of the Orion nebula M42. While the bright nebula seems to be roughly 15 light years in extension, the total gaseous cloud, including low-luminosity material, seems to extend to at least 40 light years. Distance estimates are spread over a wide range, but modern values are between 5,000 and 6,000 light years, thus little less than that of its apparent neighbor, M16 with the Eagle nebula - apparently, these two star forming regions are indeed close together, in the same spiral arm (the Sagittarius or Sagittarius-Carina arm) of the Milky Way galaxy, and perhaps part of the same giant complex of cosmic clouds of interstellar matter.

Under very favorable conditions, M17 is just visible to the naked eye at its apparent visual brightness of 6.0 magnitudes.


Here is the H-Alpha data channel:

M17 and Sh2 40 in H-Alpha

And here is the pure RGB to which the h-alpha was added:

M17 in RGB