A&A 432, 1-14 (2005)
DOI: 10.1051/0004-6361:20041488
Multi-density model of the ionised gas in NGC 253 using radio recombination lines
Niruj R. Mohan1, 2, 3, W. M. Goss4 and K. R. Anantharamaiah21 Institut d'Astrophysique de Paris, 98 bis boulevard Arago, 75014 Paris, France
2 Raman Research Institute, C.V. Raman Avenue, Sadashivanagar Post Office, Bangalore 560080, India
3 Joint Astronomy Program, Department of Physics, Indian Institute of Science, Bangalore 560012, India
4 National Radio Astronomy Observatory, PO Box O, Socorro, NM 87801, USA
e-mail: mgoss@aoc.nrao.edu
(Received 17 June 2004 / Accepted 26 October 2004)
Abstract
We have imaged the H92
(8.3 GHz), H75
(15 GHz), and H166
(1.4 GHz) Radio Recombination
Lines (RRLs) from NGC 253 at resolutions of 4.5 pc (0.4
) , 2.5 pc (0.2
) and 53 pc
(4.5
) respectively. The H92
line
arises from individual compact sources, most of which possess radio continuum counterparts. The line widths
range from ~200 km s
-1 for the sources near the radio nucleus to 70-100 km s
-1 for the extranuclear
ones. These lines are emitted by gas at a density ~10
4 cm
-3. The remainder of the cm-wave RRLs
arise in lower density gas (~500 cm
-3) with a higher area filling factor and with ten times higher
mass. A third component of higher density gas (
>10
4 cm
-3) is required to explain the mm-wave RRLs.
Key words: galaxies: individual: NGC 253 -- galaxies: ISM -- galaxies: starburst -- radio lines: galaxies -- radio lines: ISM
SIMBAD Objects
© ESO 2005

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