Satoki Matsushita et al 2004 ApJ 616 L55 doi:10.1086/424798
Submillimeter Array 12CO (J = 3-2) Interferometric Observations of the Central Region of M51
FREESatoki Matsushita1, Kazushi Sakamoto2, Cheng-Yu Kuo1, Pei-Ying Hsieh3, Dinh-V- Trung1, Rui-Qing Mao4, Daisuke Iono2,5, Alison B. Peck2, Martina C. Wiedner2,6, Sheng-Yuan Liu1, Nagayoshi Ohashi1 and Jeremy Lim1
Show affiliationsWe present the first interferometric 12CO (J = 3-2) observations (beam size of 3
9 × 16 or 160 × 65 pc) with the Submillimeter Array (SMA) toward the center of the Seyfert 2 galaxy M51. The image shows a strong concentration at the nucleus and weak emission from the spiral arm to the northwest. The integrated intensity of the central component in 12CO (J = 3-2) is almost twice as high as that in 12CO (J = 1-0), indicating that the molecular gas within an ~80 pc radius of the nucleus is warm (
100 K) and dense (~104 cm-3). Similar intensity ratios are seen in shocked regions in our Galaxy, suggesting that these gas properties may be related to active galactic nucleus or starburst activity. The central component shows a linear velocity gradient (~1.4 km s-1 pc-1) perpendicular to the radio continuum jet, similar to that seen in previous observations and interpreted as a circumnuclear molecular disk/torus around the Seyfert 2 nucleus. In addition, we identify a linear velocity gradient (0.7 km s-1 pc-1) along the jet. Judging from the energetics, the velocity gradient can be explained by supernova explosions or energy and momentum transfer from the jet to the molecular gas via interaction, which is consistent with the high-intensity ratio.
- Subject headings
galaxies: individual (M51, NGC 5194); galaxies: ISM; galaxies: nuclei; galaxies: Seyfert; ISM: jets and outflows
- Dates
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Issue 1 (2004 November 20)
Received 2004 March 7, accepted for publication 2004 July 23
Published 2004 October 28
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Submillimeter Array 12CO (J = 3-2) Interferometric Observations of the Central Region of M51
Satoki Matsushita et al 2004 ApJ 616 L55
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