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arXiv · 0904.3121

Determining Star Formation Timescale and Pattern Speed in Nearby Spiral Galaxies

Fumi Egusa·Kotaro Kohno·Yoshiaki Sofue·Hiroyuki Nakanishi·Shinya Komugi
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Abstract

We present a revised method for simultaneous determination of the pattern speed and star formation timescale of spiral galaxies, its application, and results for CO and Ha images of nearby spiral galaxies. Out of 13 galaxies, we were able to derive the 2 parameters for 5 galaxies. We categorize them as "C" galaxies, and find (1) The corotation radius is close to the edge of the CO data, and is about half of the optical radius for 3 galaxies. (2) The star formation timescale is roughly consistent with the free-fall time of typical molecular clouds, which indicates that the gravitational instability is the dominant mechanism triggering star formation in spiral arms. (3) The timescale is found to be almost independent of surface density of molecular gas, metallicity, or spiral arm strengths. The number of "C" galaxies and the quality of CO data, however, are not enough to confirm these relationships. We also find that 2 other galaxies show no offsets between CO and Ha, although their arms are clearly traced, and categorize them as "N" galaxies. The presence of a bar could account for this feature, since these 2 galaxies are both barred. With one galaxy excluded from our analysis due to its poor rotation curve, offsets of the remaining 5 galaxies are found to be ambiguous. We categorize them as "A" galaxies. The possible reasons for this ambiguity are (1) the density wave is weaker, and/or (2) observational resolution and sensitivity are not enough to detect the spiral arms and their offsets clearly. The former is supported by our finding that the arm strengths of "A" galaxies are slightly weaker than that of "C" galaxies. [abridged]

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Fumi Egusa, Kotaro Kohno, Yoshiaki Sofue, Hiroyuki Nakanishi, Shinya Komugi. 2009-04-20. Determining Star Formation Timescale and Pattern Speed in Nearby Spiral Galaxies. https://doi.org/10.1088/0004-637x%2F697%2F2%2F1870

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