Forum Springer Astron. Astrophys.
Forum Whats New Search Orders

Astron. Astrophys. 356, 705-723 (2000)

Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

ISO-SWS observations of OMC-1: H2 and fine structure lines *

D. Rosenthal 1, F. Bertoldi 2 and S. Drapatz 1

1 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85740 Garching, Germany (rosenthal@mpe.mpg.de)
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany (bertoldi@mpifr-bonn.mpg.de)

Received 21 December 1999 / Accepted 18 February 2000


Using the Short-Wavelength-Spectrometer on the Infrared Space Observatory (ISO), we obtained near- and mid-infrared spectra toward the brightest H2 emission peak of the Orion OMC-1 outflow. A wealth of emission and absorption features were detected, dominated by 56 [FORMULA] ro-vibrational and pure rotational lines reaching from H2 0-0 S(1) to 0-0 S(25). The spectra also show a number of H I recombination lines, atomic and ionic fine structure lines, and molecular lines of CO and [FORMULA]. Between 6 and 12 [FORMULA] the emission is dominated by PAH features.

The extinction toward the molecular and atomic line emitting regions is estimated from relative line intensities, and it is found that the H2 emission arises from within the OMC-1 cloud at an average K-band extinction of 1.0 mag, whereas the atomic hydrogen emission and much of the fine structure emission comes from the foreground H II region and its bounding photodissociation front.

The total H2 luminosity in the ISO-SWS aperture is estimated at [FORMULA], and extrapolated to the entire outflow, [FORMULA]. The H2 level column density distribution shows no signs of fluorescent excitation or a deviation from an ortho-to-para ratio of three. It shows an excitation temperature which increases from about 600 K for the lowest rotational and vibrational levels to about 3200 K at level energies [FORMULA] K. No single steady state shock model can reproduce the observed H2 excitation. The higher energy H2 levels may be excited either thermally in non-dissociative J-shocks, through non-thermal collisions between fast ions and molecules with H2 in C-shocks, or they are pumped by newly formed H2 molecules. The highest rotational levels may be populated by yet another mechanism, such as the gas phase formation of H2 through H-.

Key words: shock waves – ISM: abundances – ISM: individual objects: Orion Peak 1 – ISM: molecules – infrared: ISM: lines and bands

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom) and with the participation of ISAS and NASA.

Send offprint requests to: D. Rosenthal

© European Southern Observatory (ESO) 2000

Online publication: April 10, 2000