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NGC6914 & Gamma Cygni Nebula (Sadr Region)

Classification: Reflection Nebula NGC6914, LBN247-280
Constellation: Cygnus (CYG)
Object Location: Ra 20h 24m 13s Dec +41° 21’50” (current) (centered)
Size & Distance: NGC6914 3.0 x 3.0 Apx 6000 light years

Date & Location: 08-27-2022 Lockwood Observatory, Descanso,CA
Exposure: HaLRGB, Ha 2 @ 15min. LRGB 9 x 10min ea. (bin 1x1)
Optics: Telescope Engineering Company APO110FL w/ TEC FF @ f/5.74, 631mm, FLI-Atlas focuser.
Mount: Astro-Physics Mach 1 GTOCP4 / ATS 8x36 Pier.
Camera: FLI-PL16803 @-25c / FLI CFW5-7 / FLI-Atlas focuser / Guided by SBIG ST-I / w OAG.
Filters: Astrodon 3nm Ha, G2 LRGB
Software: MaxImDL 6, CCDStack Photoshop CC, Topaz Studio.

Notes: Sky conditions: Above average seeing, No wind, Temp low 60’s
Image Field of view is 198x198 arcmin. Image Scale 2.94 arcsec/pix
Ha was combined with both red and luminance channels to make an HaRed and a HaLum layer.
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NGC 6914 is a reflection nebula located in the constellation Cygnus, it was discovered by Édouard Stephan on August 29, 1881.[3] Ultraviolet radiation from stars in the Cygnus OB2 association ionize the nebula's hydrogen.

The Gamma Cygni Nebula, also known as the Sadr Region or IC 1318, is a diffuse emission nebula that can be seen around Sadr (Gamma Cygni), the star at the center of the Northern Cross, which marks the heart of Cygnus, the Swan. Despite the name, the star and the nebula are unrelated. Even though it looks embedded in the nebulosity, Sadr is approximately 1,800 light years distant, while the nebula is much further away, at 4,900 light years.

The Gamma Cygni Nebula is considered an emission nebula because it is ionized by the radiation of the nearby stars and it emits visible light as a result. The visible portion of the H II region stretches over an area more than 100 light years across. The nebula is illuminated by an O9-class star which is visually obscured by interstellar material.
Sadr It is a white supergiant star with an apparent magnitude of 2.23. With 12 solar masses and 150 times the Sun’s radius, the star is about 33,000 times more luminous than the Sun.

The Gamma Cygni Nebula has three distinct parts, designated as IC 1318 A, B and C. The dark cloud about 20 light years thick that divides IC 1318 B and C is a dark nebula known as LDN 889. It is physically related to the emission nebula and the surrounding molecular cloud complex. The dark dust lane is responsible for the nebula’s distinctive shape, resembling that of a butterfly, which is why IC 1318 is sometimes also known as the Butterfly Nebula. The components IC 1318 B and C are not separate parts of the nebula, but a single cloud visually separated by LDN 889.
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