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12CO(J = 1-0) Mapping of the Merging Galaxy NGC 3310

Published online by Cambridge University Press:  12 April 2016

T. Kikumoto ,
Y. Taniguchi ,
M. Suzuki  and
K. Tomisaka
T. Kikumoto
Affiliation:
Astronomical Institute, Tohoku University, Aoba, Sendai, Miyagi 980
Y. Taniguchi
Affiliation:
Astronomical Institute, Tohoku University, Aoba, Sendai, Miyagi 980
M. Suzuki
Affiliation:
The Graduate University for Advanced Students and Nobeyama Radio Observatory, National Astronomical Observatory, Nobeyama, Minamimaki, Minamisaku, Nagano 384-13
K. Tomisaka
Affiliation:
Faculty of Education, Niigata University, 8050 Ikarashi 2, Niigata 950-21

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Since molecular gas clouds in nuclear regions play important roles on both the intense star formation and fueling active galactic nuclei, a large number of molecular-line observations have been made for starburst, Seyfert, and merging galaxies. Recently, millimeter-wave arrays have been used to study circumnuclear molecular gas in merging galaxies. Most of them, however, have been devoted to the observations of more luminous objects such as ultra-luminous merging galaxies (ULMGs) discovered by IRAS (Sanders et al. 1988). In order to obtain a comprehensive understanding, it is necessary to study less-luminous merging galaxies. With this motivation, we present results of CO mapping of NGC 3310 which is one of less luminous merger candidates (LFIR = 2.5 × 1010Lʘ).

The central region (5.1 kpc in diameter) of NGC 3310 was observed in CO(J = 1 − 0) using the Nobeyama Millimeter Array. The synthesized beam size was 6″.3 × 6″.1, which corresponds to 500 × 480 pc at the distance 16.3 Mpc. Our main results and conclusions are summarized as follows.

Type
3. Astronomical Results and Prospects
Information
International Astronomical Union Colloquium , Volume 140: Astronomy with Millimeter and Submillimeter Wave Interferometry , 1994 , pp. 374 - 375
Copyright
Copyright © Astronomical Society of the Pacific 1994

References

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