Journal
ASTROPHYSICAL JOURNAL
Volume 761, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/761/2/124
Keywords
galaxies: ISM; galaxies: spiral; galaxies: star clusters: individual (M 33, NGC 598); stars: formation
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Funding
- DGAPA, UNAM
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We analyze the relationship between maximum cluster mass M-max and surface densities of total gas (Sigma(gas)), molecular gas (Sigma(H2)), and star formation rate (Sigma(SFR)) in the flocculent galaxy M 33, using published gas data and a catalog of more than 600 young star clusters in its disk. By comparing the radial distributions of gas and most massive cluster masses, we find that M-max alpha Sigma(4.7 +/- 0.4)(gas), M-max alpha Sigma(1.3 +/- 0.1)(H2), and M-max alpha Sigma(1.0 +/- 0.1)(SFR). We rule out that these correlations result from the size of the sample; hence, the change of the maximum cluster mass must be due to physical causes.
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