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LBN 248, HH425 (Cygnus)
NS2,LDN 1299 (Cassiopeia)
TGU H774 P19,vdB 2,LBN 590,V V510 Cas (Cassiopeia)
DG 41 (GN 04.32.08, Magakian 77), HH 434,435,436,LDN 1536 (Taurus)
BSF32 (Perseus)
  NGC 4449 (Canes Venatici).jpg - * AAPOD  10th July 2016 ** NGC 4449 (Canes Venatici) * February-May 2016 * ASA N12 astrograph (f/3.6,1078mm) * ASA DDM85 * FLI ML8300 CCD * Optec LRGB filter set * L: 660m  Ha:180m R:600m G:550m B:600m * NGC 4449 (also known as Caldwell 21) is an irregular galaxy in the constellation Canes Venatici. It is located about 12 million light-years away, part of the M94 Group (the Canes Venatici I Group), a galaxy group relatively close to the Local Group containing the Milky Way.his well-studied galaxy is similar in size and brightness, and often compared to, the Milky Way's satellite galaxy, the Large Magellanic Cloud (LMC). NGC 4449 has a general bar shape, also characteristic of the LMC, with scattered young blue star clusters.Unlike the Large Magellanic Cloud, however, NGC 4449 is considered a starburst galaxy due to its high rate of star formation (twice the one of the LMC) and includes several massive and young star clusters, one of them in the galaxy's center.Near the bottom ) is the pinkish glow of atomic hydrogen gas, the telltale tracer of massive star forming region. NGC 4449 is surrounded by a large envelope of neutral hydrogen that extends over an area of 75 arc minutes (14 times larger than the optical diameter of the galaxy). The envelope shows distortions and irregularities likely caused by interactions with nearby galaxies.Interactions with nearby galaxies are thought to have influenced star formation in NGC 4449 and, in fact, in 2012 two small galaxies have been discovered interacting with this galaxy: a very low surface brightness disrupted dwarf spheroidal with the same stellar mass as NGC 4449's halo but with a ratio of dark matter to stellar matter between 5 and 10 times that of NGC 4449 and a highly flattened globular cluster with two tails of young stars that may be the nucleus of a gas-rich galaxy. Both satellites have apparently been disrupted by NGC 4449 and are now being absorbed by it.  
NGC2782 (Lynx)
SH2 140,LDN 1201,HH 251,252,253,254 (Cepheus)
vdB 155, HH 168,169,174 (Cepheus)
Barnard 18,LBN 812 (DG 37) ,Herbig-Haro 319,466,467,468 (Taurus) END
MBM 25 (Lynx)

* AAPOD 10th July 2016 ** NGC 4449 (Canes Venatici) * February-May 2016 * ASA N12 astrograph (f/3.6,1078mm) * ASA DDM85 * FLI ML8300 CCD * Optec LRGB filter set * L: 660m Ha:180m R:600m G:550m B:600m * NGC 4449 (also known as Caldwell 21) is an irregular galaxy in the constellation Canes Venatici. It is located about 12 million light-years away, part of the M94 Group (the Canes Venatici I Group), a galaxy group relatively close to the Local Group containing the Milky Way.his well-studied galaxy is similar in size and brightness, and often compared to, the Milky Way's satellite galaxy, the Large Magellanic Cloud (LMC). NGC 4449 has a general bar shape, also characteristic of the LMC, with scattered young blue star clusters.Unlike the Large Magellanic Cloud, however, NGC 4449 is considered a starburst galaxy due to its high rate of star formation (twice the one of the LMC) and includes several massive and young star clusters, one of them in the galaxy's center.Near the bottom ) is the pinkish glow of atomic hydrogen gas, the telltale tracer of massive star forming region. NGC 4449 is surrounded by a large envelope of neutral hydrogen that extends over an area of 75 arc minutes (14 times larger than the optical diameter of the galaxy). The envelope shows distortions and irregularities likely caused by interactions with nearby galaxies.Interactions with nearby galaxies are thought to have influenced star formation in NGC 4449 and, in fact, in 2012 two small galaxies have been discovered interacting with this galaxy: a very low surface brightness disrupted dwarf spheroidal with the same stellar mass as NGC 4449's halo but with a ratio of dark matter to stellar matter between 5 and 10 times that of NGC 4449 and a highly flattened globular cluster with two tails of young stars that may be the nucleus of a gas-rich galaxy. Both satellites have apparently been disrupted by NGC 4449 and are now being absorbed by it. Download Imagen original
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