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NGC 1528, SH2-209 LRGB (Perseus)
LBN 640 (Perseus)
Vdb 47 (SH2-243) (Taurus)
vdB 4,NGC 225  (Cassiopeia)
vdB 18,LDN 1434,LBN 720,LBN 721 (Perseus)
  B35,GN 05.42.06,LDN 1596, V FU Ori.jpg - AAPOD,October 10th,2015* Barnard 35,GN 05.42.05,LDN 1596, V* FU Orionis (Orion) * November-December 2013 * ASA N12 astrograph (f/3.6,1078mm) * ASA DDM85 mount * FLI ML8300 at -25ºC * Optec LRGB filter set * L: 570m R:190m G:180m B.200m * This is my personal tribute to one of my most admired astronomers: Edward Emerson Barnard *  http://en.wikipedia.org/wiki/Edward_Emerson_Barnard   * Young stars in bright-rimmed or comet-shaped clouds are likely to havebeen formed by triggering, which would result in an age spread of several Myrsbetween the member stars or star groups formed in the sequence.In the Orion star-forming region for example, there is concrete evidence of triggeredstar formation as manifested by the bright-rimmed clouds (BRCs) in the vicinity of O stars(Lee et al. 2005, I). These BRCs are considered the remnant of molecularclouds that have been photoionized by a nearby massive star (Sugitani et al. 1991, 1994). B35 is a  BRC  associated with an H II region excited by the O8 III starLambda  Ori and surrounded by a ring-shaped molecular cloud (Lang et al. 2000). (1982) find some 80 Ha stars in the Lambda  Ori region.structure extending from either side of Lambda Ori to B35.It is likely that Lambda  Ori is the triggering source responsible for the star formation in B35. It is found that photoevaporative flows (Hester et al. 1996) stream out of thesurfaces of them; this is a demonstration of the interaction between a massive star and amolecular cloud.Credits: Hsu-Tai LeeW. P. ChenInstitute of Astronomy, National Central University, 300 Jungda Road, Jungli 32054, Taiwan  
Vdb 75,DG 99,IC 444 (Gemini)
NGC 3642-3610 LRGB (Ursa Major)
M85 ,NGC 4394, IC 3292, MCG 3-32-38  (Coma Berenices)
Hickson 68,NGC 5371,PGC 49480 (Canes Venatici)
Messier 3 and NGC 5253(Canes Venatici)

AAPOD,October 10th,2015* Barnard 35,GN 05.42.05,LDN 1596, V* FU Orionis (Orion) * November-December 2013 * ASA N12 astrograph (f/3.6,1078mm) * ASA DDM85 mount * FLI ML8300 at -25ºC * Optec LRGB filter set * L: 570m R:190m G:180m B.200m * This is my personal tribute to one of my most admired astronomers: Edward Emerson Barnard * http://en.wikipedia.org/wiki/Edward_Emerson_Barnard * Young stars in bright-rimmed or comet-shaped clouds are likely to have been formed by triggering, which would result in an age spread of several Myrs between the member stars or star groups formed in the sequence. In the Orion star-forming region for example, there is concrete evidence of triggered star formation as manifested by the bright-rimmed clouds (BRCs) in the vicinity of O stars (Lee et al. 2005, I). These BRCs are considered the remnant of molecular clouds that have been photoionized by a nearby massive star (Sugitani et al. 1991, 1994). B35 is a BRC associated with an H II region excited by the O8 III star Lambda Ori and surrounded by a ring-shaped molecular cloud (Lang et al. 2000). (1982) find some 80 Ha stars in the Lambda Ori region. structure extending from either side of Lambda Ori to B35. It is likely that Lambda Ori is the triggering source responsible for the star formation in B35. It is found that photoevaporative flows (Hester et al. 1996) stream out of the surfaces of them; this is a demonstration of the interaction between a massive star and a molecular cloud. Credits: Hsu-Tai Lee W. P. Chen Institute of Astronomy, National Central University, 300 Jungda Road, Jungli 32054, Taiwan Download Imagen original
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