The high-speed phenomena of the Orion nebula (M42, NGC 1976) - IV. Velocity imaging and spectroscopy

Details The high-speed phenomena of the Orion nebula (M42, NGC 1976) - IV. Velocity imaging and spectroscopy The high-speed phenomena of the Orion nebula (M42, NGC 1976) - IV. Velocity imaging and spectroscopy

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.273..615m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 273, Issue 3, pp. 615-624.

Astronomy and Astrophysics

Astronomy

27

Line: Profiles, Hii Regions, Ism: Individual: Orion Nebula, Ism: Jets And Outflows, Ism: Kinematics And Dynamics

Scientific paper

High-resolution, spatially resolved long-slit spectra of the [OIII] 5007-A line in the vicinity of the Trapezium group of stars in the Orion nebula have now been obtained for 17 slit positions with the Manchester Echelle Spectrometer in combination with the Isaac Newton and William Herschel telescopes. The long-slit spectra obtained from 10 of the 14 Isaac Newton slit positions have been stacked into a 'data cube' to permit imaging in various velocity ranges. A variety of new high-speed kinematical phenomena are found on a wide range of spatial scales. In particular, nearly all of the compact (<=2 arcsec across), highly ionized knots covered by these and previous observations in the core of M42 are associated with unresolved ~=100 km s^-1 mono-or bipolar flows. Extended, high-speed features connect several compact sources. Jets from embedded young stellar objects, as well as the ablation by particle winds from the Trapezium stars, are considered as the origin of these motions. A coherent structure is now found in two orthogonal position-velocity arrays of [OIII] 5007-A profiles. This feature has a 1-arcmin radius and is composed of velocity `spikes' and `loops', the extents of which in radial velocity diminish with increasing apparent distance from theta^1 OriC. Its presence is considered to be strong evidence for the predominance of wind-driven ablated flows in the creation of the high-speed phenomena. A 15-arcsec wide, high-speed filament, bright in the [OIII] 5007-A line and with a radial velocity of -90 km s^-1 (V_HEL~=-72 km s^-1) with respect to the systemic radial velocity is traced for a length of 40 arcsec. This feature is possibly associated with an as yet undetected, high-speed finger in the underlying molecular cloud and driven by the burst of massive star formation associated with the Kleinmann-Low region.

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