SPECTROPHOTOMETRY OF THE HUYGENS REGION OF THE ORION NEBULA, THE EXTENDED ORION NEBULA, AND M 43: SCATTERED LIGHT SYSTEMATICALLY DISTORTS CONDITIONS DERIVED FROM EMISSION LINES

Journal Article · Fri Oct 15 04:00:00 EDT 2010 · Astronomical Journal (New York, N.Y. Online)

DOI:https://doi.org/10.1088/0004-6256/140/4/985· OSTI ID:21443226

O'Dell, C R ^[1]

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1. Department of Physics and Astronomy, Vanderbilt University, Box 1807-B, Nashville, TN 37235 (United States)

We report on medium resolution spectrophotometry of the Orion Nebula region, including for the first time the Extended Orion Nebula (EON) and the nearby M 43. The 49 long-slit observations were divided into 99 smaller samples, which have allowed determinations of the amount of extinction, extinction-corrected H{beta} surface brightness, electron temperatures (from [S II], [N II], and [O III]), and electron densities (from [S II] and [Cl III]) throughout much of this complex region. We verify an earlier conclusion from a radio/optical study that beyond about 5' from {theta}{sup 1}Ori C local emission begins to be contaminated by scattering of light from the much brighter central Huygens region of M 42, and this scattered light component becomes dominant at large distances. This contamination means that the derived properties for the outer regions are not accurate. From comparison of the light from the dominant star in M 43 with the continuum of that nebula (which is almost entirely scattered starlight), it is determined that scattered light is enhanced in the blue, which can lead to observed Balmer line ratios that are theoretically impossible and erroneous electron temperatures. This blue scattering of emission lines is important even in the Huygens region because it means that at anything except very high spectroscopic resolution the observed lines are a blend of the original and scattered light, with shorter wavelength lines being artificially enhanced. This can lead to overestimates of the electron temperatures derived from the nebular and auroral line ratios of forbidden lines. This phenomenon is probably applicable to many other H II regions. We have been able to use extinction-insensitive line ratios, the extinction-corrected surface brightness in H{beta}, and the equivalent width of the continuum to create for the first time a three-dimensional model of the entire M 42, EON, and M 43 region. This is an irregular concave blister of ionized gas bounded on the outside by apparent walls where the ionization front has curved almost to the direction of the observer. M 43 is seen to be shielded from illumination by {theta}{sup 1}Ori C by the northeast portion of the wall bounding M 42.

• OSTI ID: 21443226
• Journal Information: Astronomical Journal (New York, N.Y. Online), Journal Name: Astronomical Journal (New York, N.Y. Online) Journal Issue: 4 Vol. 140; ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
BALMER LINES
BLISTERS
BRIGHTNESS
ELECTRON DENSITY
ELECTRON TEMPERATURE
EMISSION
IONIZATION
NEBULAE
OPTICAL PROPERTIES
PHOTON EMISSION
PHYSICAL PROPERTIES
RESOLUTION
SPECTROPHOTOMETRY
STARS
THREE-DIMENSIONAL CALCULATIONS