Issue |
A&A
Volume 428, Number 2, December III 2004
|
|
---|---|---|
Page(s) | 445 - 450 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20041650 | |
Published online | 26 November 2004 |
Mm-wave HCO+, HCN and CO absorption toward NGC 1052
1
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA, 22903-2475, USA e-mail: hliszt@nrao.edu
2
Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 Saint Martin d'Hères, France
Received:
12
July
2004
Accepted:
26
August
2004
We used the Plateau de Bure Interferometer to observe λ3 mm
absorption lines of HCO+, HCN and CO toward the core of
the nearby elliptical, megamaser-host galaxy NGC 1052. The lines
are relatively weak, with peak optical depths 0.03 for HCO+ and
HCN and 0.1 for CO. Nonetheless the inferred column density of
molecular gas 2N(H2)
5
is consistent
with the degree of reddening inferred toward the nucleus from
observations of the Balmer series of hydrogen. Mm-wave absorption
line profiles are somewhat broader than those of H I and OH, perhaps
because lower free-free opacity at mm-wavelengths exposes higher-velocity
material nearer the nucleus. Overall, the OH/HCO+ ratio in NGC 1052 is
as expected from the strong relationship established in local diffuse
clouds but the optical depth ratio varies strongly over the line
profiles. Similar variations are also seen toward Cen A, which has
very different line ratios among H I, OH and HCO+ for very nearly
the same amount of OH absorption.
Key words: galaxies: ISM / ISM: molecules / galaxies: elliptical and lenticular, cD
© ESO, 2004
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.