Internal variation of electron density in galactic Hbt II regions

Details Internal variation of electron density in galactic Hbt II regions Internal variation of electron density in galactic Hbt II regions

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...357..621c&link_type=abstract

Astronomy and Astrophysics, v.357, p.621-636 (2000)

Astronomy and Astrophysics

Astrophysics

24

Ism: General, Ism: H Ii Regions

Scientific paper

A study on the internal variation of the electron density in galactic H Ii regions has been conducted on a sample of 15 objects of different sizes and evolutionary stages. The [S Ii] lambda 6716/lambda 6731 line ratio was adopted as electron density indicator. Long slit spectrophotometry of high signal-to-noise ratio with spectral dispersion of 0.75 Ä,pxl-1 and spatial scale of 0\farcs90 pxl-1 were obtained at different slit positions and orientations. No systematic spatial variation of electron density was detected in nearly half of the objects studied (S 255, S 257, S 271, S 285, S 301, S 305, NGC 3372 and IC 1275). They are in general the most diffuse and probably evolved objects with low mean densities in the range Ne ~ 20-140 cm-3. The remaining objects (S 288, S 307, NGC 2579, NGC 3503, Gum 62, Gum 64a and M 20) with mean densities Ne ~ 80-360 cm-3, have shown a statistically significant electron density dependence on position. In most of these cases, the spatial variation of density may be interpreted as a radial gradient with the density decreasing from the centre to the edges. M 20 shows a systematic non-radial variation of electron density with maximum values occurring at its prominent dark lanes. A mean filling factor of the order of phi = 0.1 was found compatible with the data. Based on their density profiles, NGC 2579, Gum 62, Gum 64a and possibly NGC 3503 were indicated as candidates of showing a `champagne flow'.

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