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SH2 104,LBN 195,DWB 18, GM 1-27 (Cygnus)
M101 (Ursa Major)
IC5146 ,vdB 147,CGN 185 (Cygnus)B
IC5076 (vdB 137),vdB 138,LDN 958,GN 20.57.4,LDN 955 (Cygnus)
PGCC Clouds,NGC 7223 (Lacerta)
  Mean SH 241, vdB 65 (Auriga).jpg - SH 241,vdB 65, LDN 1557 (Auriga) * December 2019-January 2020 *  CFF 135 mm telescope (f/6.7, 930mm) * ASA DDM 85 mount * G3 16200 EC Moravian CCD* Baader LRGB filter set * L: 700 minutes R:483min G:441 min B:637 min * The SH 241 emission nebula has a bright core to which a less bright region is connected...the star responsible for the ionisation of the gas appears to be a blue star of spectral class O9V, known as LSV+30 31. The presence of high-speed jets of gas coming out of the cloud suggests that massive star formation phenomena occur in the region; these jets would be pushed outwards by the action of massive stars located in the deepest regions of the cloud. The distance has not been well defined: according to some studies it would be around 4700 parsecs, while according to others the distance would be slightly less, around 4500 parsecs; in both cases, the cloud is in the Perseus arm.The reflection nebula vdB 65 is located in the southern part of the constellation, on the border with GeminivdB 65 is a small part of the large molecular cloud LDN 1557, which in turn is part of a large complex of dark molecular nebulae that includes other nearby clouds, such as LDN 1550, LDN 1555 and LDN 1560. The central star that lights the nebula has an apparent magnitude of 10.63; the distance has been estimated at 1100 parsecs (about 3600 light years).  
 NGC 918 ,MBM8,MBM7 (Aries)
 
 
 
 

SH 241,vdB 65, LDN 1557 (Auriga) * December 2019-January 2020 * CFF 135 mm telescope (f/6.7, 930mm) * ASA DDM 85 mount * G3 16200 EC Moravian CCD* Baader LRGB filter set * L: 700 minutes R:483min G:441 min B:637 min * The SH 241 emission nebula has a bright core to which a less bright region is connected...the star responsible for the ionisation of the gas appears to be a blue star of spectral class O9V, known as LSV+30 31. The presence of high-speed jets of gas coming out of the cloud suggests that massive star formation phenomena occur in the region; these jets would be pushed outwards by the action of massive stars located in the deepest regions of the cloud. The distance has not been well defined: according to some studies it would be around 4700 parsecs, while according to others the distance would be slightly less, around 4500 parsecs; in both cases, the cloud is in the Perseus arm. The reflection nebula vdB 65 is located in the southern part of the constellation, on the border with Gemini vdB 65 is a small part of the large molecular cloud LDN 1557, which in turn is part of a large complex of dark molecular nebulae that includes other nearby clouds, such as LDN 1550, LDN 1555 and LDN 1560. The central star that lights the nebula has an apparent magnitude of 10.63; the distance has been estimated at 1100 parsecs (about 3600 light years). Download Imagen original
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