Click here for a higher resolution image (2.5 Mb)


 

 

The Details
Object
NGC 3199 and PN MeWe 1-2 in Carina
Optics
Astro-Physics 12" Mak-Cass at f/8
Platform
Astro-Physics 1600 GTO with absolute encoders
Camera
FLI Proline 16803
Filters
Tru-Balance 5nm Hydrogen-Alpha
Date
March 2015
Location
Las Campanas Observatory, Chile
Exposure
Ha 58 ea x 1800 sec, 1x1 bin (29 hours total exposure)
Software
ACP, Maxim DL/CCD, CCDStack, Photoshop CS5
Orientation
Field of View:00°51' x 00°51' centered on RA10h17m06s DEC -57°55’00” (2000.0) . North angle179.5°; east 90° CCW from north
Notes
NGC 3199, also known as RCW 48 and Gum 28, is a HII emission region lying about 12,000 light-years from Earth in the constellation Carina.  The bright western edge of this nebula is the most prominent portion of a complex shell morphology that extends southeastward to trace out an elliptical shape having an apparent dimension of about 25 arc-minutes along its major axis and 20 arc-minutes along the minor axis.  The star exciting this nebula, asymmetrically placed within the ellipse, is Wolf-Rayet star HD 89358. It can be seen in the image as the most luminous star just right of the bright western arc of the nebula and lies at nearly the dead center of the frame.

Research on NGC 3199 by Whitehead, Meaburn and Goudis, published in the journal Astronomy and Astrophysics (ref: 196, 262-265 (1988)) entitled “The Nature of the Wolf-Rayet Nebula NGC 3199”, concluded substantial stellar displacement of the Wolf-Rayet star has taken place during the time the nebular shell was forming and that radiative ionization and not the energetic stellar winds associated with the Wolf-Rayet is the dominant mechanism for the ionized gas in this nebula.

A bonus capture in the above image is the faint, slightly elliptical planetary nebula MeWe 1-2 (PN G283.4-01.3) in the upper left corner of the frame. This low surface brightness planetary is quite far along in its evolution and has been studied by Kerber, Furlan, Rauch and Roth to investigate the process by which processed nuclear material from the central star that created the nebula is returned to the interstellar medium (ISM), thus seeding the ISM for the chemical evolution of galaxies.  This research was published in the Astronomical Society of the Pacific, ASP Conference Series Vol. 199, 2000 in an article entitled “Planetary Nebula – ISM Interaction:  The Observational Evidence”.

This image is a collaborative effort between Howard Hedlund of Astro-Physics, Inc. and Dave Jurasevich, with a total exposure time of 29 hours.

 

 

 

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No reproduction of these images are permitted without prior approval of the author.