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Harel Boren | all galleries >> Galleries >> International Acknowledgements - APODs and Publications > vdB 133, LBN 219, Sh2-106 (The Celestial Snow Angel) in Cygnus
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5,6 and 7 June, 2013 Harel Boren

vdB 133, LBN 219, Sh2-106 (The Celestial Snow Angel) in Cygnus

Negev Desert, Israel

Total Exposure Time: 10:00 hours L(bin1); RGB(bin2),
LRGB 180:140:120:160 // 60 frames of 10 minutes each
RA 20h 30m 00s, Dec +37 03' 44"
Pos Angle +88 44', FL 600.4 mm, 1.85"/Pixel
This image is 1570x1164 pixels

Officina Stellare Riccardi-Honders Veloce RH 200 OTA
Officina Stellare -
On my site -
Deeper technical informaiton on the Riccardi-Honders design -
SBIG ST8300M, LRGB Astrodon Gen II filters
NEQ6 mount, guided w/PHD

vdB 133 is a nebula surrounding and lit by 44 Cygni, a 6th magnitude star. It consists of both a reflection nebula GN 20.29.1 and the HII region LBN 076.41-01.45.

44 Cygni is a F5Iab star. Much whiter than most stars that illuminate reflection nebula. It may be in front of the nebula as the color is about that of the star rather than blue that is usually seen due to scattering from starlight passing through the dust and gas. F5 tells us it is a somewhat hotter star than our sun. The Iab means it is in the super giant class and the ab that it is of intermediate luminosity, a means luminous while b less luminous so ab is in the middle someplace. A famous Iab is Betelgeuse. 44 Cygni is listed at about 1600 light-years so that is likely the distance to the nebula as well. (ref.

The Celestial Snow Angel (catalogued as Sharpless 2-106 or Sh2-106), is an emission nebula and a star formation region in the constellation Cygnus. It is a H II region estimated to be around 2,000 ly (600 pc) from Earth, in an isolated area of the Milky Way.

In the center of the nebula is a young and massive star that emits jets of hot gas from its poles, forming the bipolar structure. Dust surrounding the star is also ionized by the star. The nebula spans about 2 light-years across.

The central star, a source of infrared radiation usually referred to as S106 IR or S106 IRS 4, is believed to have been formed only 100,000 years ago. It is a massive star, approximately 15 solar masses. Two jets of matter streaming from its poles heat surrounding matter to a temperature of around 10,000C. Dust that is not ionized by the star's jets reflect light from the star. With an estimated surface temperature of 37,000K, it is classified as a type O8 star. It loses around 10−6 per year in solar winds, ejecting material at around 100 km/s. (ref.

Studies of images has revealed that the star-forming region has also created hundreds of low-mass brown dwarf stars[4] and protostar.[6]

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