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Faint extended OH emission from the local interstellar medium in the direction l ≈ 108°, b ≈ 5°

Ronald J. Allen ; Mónica Ivette Rodríguez ; John H. Black (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; Roy Booth (Institutionen för rymd- och geovetenskap)
The Astronomical Journal (0004-6256). Vol. 143 (2012), 4, p. Article 97, pp. 1-8.
[Artikel, refereegranskad vetenskaplig]

We have mapped faint 1667 OH line emission (TA ≈ 20-40 mK in our ≈30' beam) along many lines of sight in the Galaxy covering an area of ≈4° × 4° in the general direction of l ≈ 108°, b ≈ 5°. The OH emission is widespread, similar in extent to the local H I (r lsim 2 kpc) both in space and in velocity. The OH profile amplitudes show a good general correlation with those of H I in spectral channels of ≈1 km s–1; this relation is described by TA (OH) ≈1.50 × 10–4 TB (H I) for values of TB (H I) lsim 60-70 K. Beyond this the H I line appears to "saturate," and few values are recorded above ≈90 K. However, the OH brightness continues to rise, by a further factor ≈3. The OH velocity profiles show multiple features with widths typically 2-3 km s–1, but less than 10% of these features are associated with CO(1-0) emission in existing surveys of the area smoothed to comparable resolution.

Nyckelord: interstellar matter, interstellar molecules

An erratum has been published: http://stacks.iop.org/1538-3881/145/85 , and it should be cited as Astronomical Journal, vol. 145, page 85 (2013).

Denna post skapades 2012-03-20. Senast ändrad 2014-09-02.
CPL Pubid: 156021


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