Physical Conditions in Photodissociation Regions - M17 Northern Bar

Details Physical Conditions in Photodissociation Regions - M17 Northern Bar Physical Conditions in Photodissociation Regions - M17 Northern Bar

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.265..329c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 265, NO. 2/NOV15, P. 329, 1993

Astronomy and Astrophysics

Astronomy

45

H Ii Regions - Ism: Individual: M17 - Ism: Molecules - Infrared: Interstellar: Lines

Scientific paper

We present results of long-slit spectroscopy, from 2.0 to 2.5 m, of the photodissociation region in the northern bar of the H II region M17. The emission from ionized material peaks to the south of that from molecular gas, in agreement with previous measurements. The diagnostic 1-O S(1) to 2-1 S(1) line ratio is approximately 3, larger than the ratio for pure fluorescence, implying that the H2 is slightly thermalized. The ratio does not change along the extent of the molecular emission which fills the slit (approximately 60 arcsec), suggesting that the collisional de-excitation rate is constant. We take this to mean that the physical conditions are constant across the region, implying that in the northern bar of M17 we are viewing the face of the molecular cloud. A model is proposed, which describes the geometry.
16 H2 lines are detected, and the column densities of the upper levels of the transitions show clearly that UV excitation is responsible for the emission. We model the physical conditions in the region by fitting six line ratios with a two-component PI)R model. This modelling suggests that the gas is clumpy and that the observations are consistent with 76 per cent of the beam area being filled by gas at a density of 10r cm-3 and 16 per cent by gas of density 106 cm-3. It is shown that a lower limit to the critical density for de-excitation of the υ = 1, J =3 level is 105 cm-3. We also find that the ratio of the ortho- and para- states of H2 cannot be equal to the LTE value of 3. We introduce two physical models, which may explain the low value of the ortho-to-para ratio that is observed.

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