GAS SURFACE DENSITY, STAR FORMATION RATE SURFACE DENSITY, AND THE MAXIMUM MASS OF YOUNG STAR CLUSTERS IN A DISK GALAXY. I. THE FLOCCULENT GALAXY M 33

被引：11

作者：

Gonzalez-Lopezlira, Rosa A. ^{[1
]}

Pflamm-Altenburg, Jan ^{[1
]}

Kroupa, Pavel ^{[1
]}

机构：

[1] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 761卷 / 02期

关键词：

galaxies: ISM; galaxies: spiral; galaxies: star clusters: individual (M 33; NGC; 598); stars: formation; DIFFUSE IONIZED-GAS; H-ALPHA; STELLAR POPULATIONS; MOLECULAR CLOUDS; NEARBY GALAXIES; SPIRAL GALAXIES; M33; ULTRAVIOLET; STARBURST99; PHOTOMETRY;

D O I：

10.1088/0004-637X/761/2/124

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：6

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