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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
Vdb 75,DG 99,IC 444 (Gemini)
  NGC 3642-3610 LRGB (Ursa Major).jpg - NGC 3642,NGC 3610, PGC 34666 ( Ursa Major) * February- March 2014 * ASA N12 astrograph ( f/3.6, 1078mm ) * ASA DDM85 mount * FLI Ml 8300 ar-25ºC * Optec LRGB filter set * L: 540m R: 190m G 160m B: 190m * Unguided *NGC 3642, a galaxy disturbed by a past interaction, while classified as type SBc it displays a warped outer ring undergoing star formation at 1.5 times the rate on the inner area. Distance is 79 Mly.Star formation in the warped outer parts might be linked to the fact that NGC 3642 is located in a rich environment, where its close neighbors show clear signs of merging. Our suggestion is that NGC 3642 has captured recently a low-mass, gas-rich dwarf, and star formation was triggered in this infalling external gas that produced also a pronounced warp in the gaseous disk.Verdes-Montenegro, L.; Bosma, A.; Athanassoula, E.NGC 3610 is a member of the NGC 3642 Group (LGG 234), with ?ve cataloged members. The NGC 3642 Group itself is a subgroup of the rich (N = 170) Group 94 of Geller.The optical peculiarities include two or three shells,a central X-structure, plumes, and extraordinarily boxy outer isophotes (Forbes & Thomson 1992; Whitmore et al(1997)The idea of this image was to show NGC 3610 not just as an elliptical galaxy, but show the shells all aorund it...¡¡Studies in this galaxy, suggest the presence of a small stellar edge-on disk imbedded into its spheroid.The disk modelling , allows to derive strong constraints on the inclination of the galaxy.Residuals image obtained form ths substraction of disk-model reveals the presence of an additional weak outer disk and a shell. Latter features suggest an interaction process in the more recent history of this galaxy. http://www.spacetelescope.org/images/opo9734r/http://www.cv.nrao.edu/~jhibbard/HIinEs/2003AJv125p667.pdfhttp://articles.adsabs.harvard.edu//full/1990A%26A...235...49S/0000049.000.html  
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)
NGC 4631, NGC 4656  Full resolution test (Canes Venatici)
IC 4954,4955 (Vulpecula)

NGC 3642,NGC 3610, PGC 34666 ( Ursa Major) * February- March 2014 * ASA N12 astrograph ( f/3.6, 1078mm ) * ASA DDM85 mount * FLI Ml 8300 ar-25ºC * Optec LRGB filter set * L: 540m R: 190m G 160m B: 190m * Unguided * NGC 3642, a galaxy disturbed by a past interaction, while classified as type SBc it displays a warped outer ring undergoing star formation at 1.5 times the rate on the inner area. Distance is 79 Mly. Star formation in the warped outer parts might be linked to the fact that NGC 3642 is located in a rich environment, where its close neighbors show clear signs of merging. Our suggestion is that NGC 3642 has captured recently a low- mass, gas-rich dwarf, and star formation was triggered in this infalling external gas that produced also a pronounced warp in the gaseous disk. Verdes-Montenegro, L.; Bosma, A.; Athanassoula, E. NGC 3610 is a member of the NGC 3642 Group (LGG 234), with ?ve cataloged members. The NGC 3642 Group itself is a subgroup of the rich (N = 170) Group 94 of Geller. The optical peculiarities include two or three shells,a central X-structure, plumes, and extraordinarily boxy outer isophotes (Forbes & Thomson 1992; Whitmore et al(1997) The idea of this image was to show NGC 3610 not just as an elliptical galaxy, but show the shells all aorund it...¡¡ Studies in this galaxy, suggest the presence of a small stellar edge-on disk imbedded into its spheroid.The disk modelling , allows to derive strong constraints on the inclination of the galaxy.Residuals image obtained form ths substraction of disk-model reveals the presence of an additional weak outer disk and a shell. Latter features suggest an interaction process in the more recent history of this galaxy. http://www.spacetelescope.org/images/opo9734r/ http://www.cv.nrao.edu/~jhibbard/HIinEs/2003AJv125p667.pdf http://articles.adsabs.harvard.edu//full/1990A%26A...235...49S/0000049.000.html Download Imagen original
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