M17, also called the Swan Nebula and sometimes the Omega Nebula, is a region of star formation and shines by excited emissions caused by the high-energy radiation of young stars.  However, unlike many other emission nebula, these stars are not obvious in optical images, but are hidden within the nebula.  Star formation is either still active in this nebula, or has ceased very recently.  A small cluster of about 35 bright, but obscured, stars seems to be imbedded in the nebulosity.

The color of the nebula is predominately reddish, with some graduation to pink.  This color comes from hot hydrogen gas excited to shine by stars lying within the nebula.  The nebula also radiates strongly from ionized oxygen.  This is evident by a 'bluish' hue in, and around, the brighter portions of the nebula.  The nebula contains a large amount of dark obscuring material comprised of dust and cold gas.  The mass of the gas and dust in the Swan Nebula is estimated to be about 800 times that of the Sun.

While the bright nebula seems to be roughly 15 light years across, the total gaseous cloud, including low-luminosity material, extends to at least 40 light years.  M17 lies in the constellation Sagittarius at an estimated distance of 5,000 to 6,000 light years.

This image was assembled from narrowband data obtained through Hydrogen Alpha (Ha) and narrow band III (OIII) emission line filters. It was assembled as a Bi-Color, or false color,image. Ha was mapped to the Red channel and OIII was mapped to the Blue channel. The Green channel was created by combining the Ha and OIII data using Neal Carboni's Photoshop actions. This is refered to as a Synthetic Green channel.

¹http://messier.seds.org/m/m017.html