Observation by Mike Foylan: The Eskimo Planetary Nebula

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Mike Foylan


Mike Foylan


2016 Nov 06 - 23:40


2019 Feb 16 - 19:48


The Clown Nebula (NGC2392)

Planetarium overlay



Field centre

RA: 07h29m
Dec: +20°56'
Position angle: -89°13'

Field size

0°32' × 0°25'

  • 0.2-m SCT @ f7.6
  • Field of View 46 x 37 arcmins
  • CG5-GT Modified EQ Mount
  • Image acquisition and processing: CCD Soft v5, Mira Pro-7, TheSky6 Professional
  • SBIG STL-1301E CCD Camera, Image Scale 2.17 arcsec/pixel

Blue filter image of 377 seconds, Green filter image of 173 seconds, Red filter image of 90 seconds, all unbinned.


Cherryvalley Observatory (I83) Ireland.

Target name

NGC 2392


The Eskimo Planetary Nebula

About this image

This beautiful planetary nebula is designated NGC 2392, Caldwell 39, but it is perhaps better known as the Eskimo Nebula or Clown Face Nebula, the youngest such planetary nebula discovered in our galaxy. Astronomer William Herschel discovered it in 1787.

 A star like our Sun some three thousand light years distant came to the end of its normal life of converting hydrogen to heavier elements by means of nuclear fusion and about 10,000 years ago, when Ireland and UK were still in the grips of the end of the last ice age this old star shed its thicker outer layers during its red giant phase at about 50,000 kilometres per hour. At its centre all that will remain in time is a stellar core known as a white dwarf about the size of the Earth but very dense and very hot were no nuclear fusion takes place but is able to shine due to stored thermal energy. Its lifetime measured in many billions of years. 

Looking at the structure of the nebula one can see distinct rings or doughnut shaped structures surrounding the central star. We see only two dimensions as in this image from our vantage point on Earth but in fact, the Eskimo nebula is double lobed (bipolar structure) in nature. The extended filaments are thought to be a light year across with the inner filaments of material (ejected later) at a much greater velocity of about six million kilometres per hour thus eventually catching up with the slower moving material causing the material to become very hot and glow at high temperatures. This will closely approximate the fate of our Sun in the very distant future.

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