2011/01/18 by Taku Nakajima, T. Nakajima, S. Takano +5 · 36 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Hubble sequence #Line (geometry) #Molecule #Spectral line #Telescope #astro-ph.GA
paper · pdf · doi:10.1088/2041-8205/728/2/l38
published in The Astrophysical Journal Letters 728(2), L38 (IOP Publishing) · 10 pages, 3 figures, Accepted for publication in ApJ Letter. After the submission of this manuscript, we found two relevant papers. Snell et al. detected C2H in NGC 1068 (astro-ph 1101.0132). It was very recently published in The Astronomical Journal 141 38. Costagliola et al. detected C2H and H13CN in NGC 1068 (astro-ph 1101.2122)
arxiv created 2011/01/18 · openalex publication_date 2011/02/01 · arxiv updated 2015/05/27 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We used the Nobeyama 45 m telescope to conduct a spectral line survey in the 3 mm band (85.1–98.4 GHz) toward one of the nearest galaxies with an active galactic nucleus (AGN), NGC 1068, and the prototypical starburst galaxy NGC 253. The beam size of this telescope is ∼ 18'', which was sufficient to spatially separate the nuclear molecular emission from the emission of the circumnuclear starburst region in NGC 1068. We detected rotational transitions of C 2 H, cyclic-C 3 H 2 , and H 13 CN in NGC 1068. These are detections of carbon-chain and carbon-ring molecules in NGC 1068. In addition, the C 2 H N = 1–0 lines were detected in NGC 253. The column densities of C 2 H were determined to be 3.4 × 10 15 cm −2 in NGC 1068 and 1.8 × 10 15 cm −2 in NGC 253. The column densities of cyclic-C 3 H 2 were determined to be 1.7 × 10 13 cm −2 in NGC 1068 and 4.4 × 10 13 cm −2 in NGC 253. We calculated the abundances of these molecules relative to CS for both NGC 1068 and NGC 253, and found that there were no significant differences in the abundances between the two galaxies. This result suggests that the basic carbon-containing molecules are either insusceptible to AGN or are tracing cold ( T rot ∼ 10 K) molecular gas rather than X-ray irradiated hot gas.