THE STAR CLUSTER MASS-GALACTOCENTRIC RADIUS RELATION: IMPLICATIONS FOR CLUSTER FORMATION
文献类型：期刊论文
| 作者 | Sun, Weijia1; de Grijs, Richard2,3,4; Fan, Zhou5 ; Cameron, Ewan6
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| 刊名 | ASTROPHYSICAL JOURNAL
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| 出版日期 | 2016 |
| 卷号 | 816期号:1 |
| 关键词 | galaxies: evolution galaxies: individual (M33, M51, M83, LMC) galaxies: star clusters: general |
| 英文摘要 | Whether or not the initial star cluster mass function is established through a universal, galactocentric-distance-independent stochastic process, on the scales of individual galaxies, remains an unsolved problem. This debate has recently gained new impetus through the publication of a study that concluded that the maximum cluster mass in a given population is not solely determined by size-of-sample effects. Here, we revisit the evidence in favor and against stochastic cluster formation by examining the young (less than or similar to a few x 10(8) year old) star cluster mass-galactocentric radius relation in M33, M51, M83, and the Large Magellanic Cloud. To eliminate size-of-sample effects, we first adopt radial bin sizes containing constant numbers of clusters, which we use to quantify the radial distribution of the first-to fifth-ranked most massive clusters using ordinary least-squares fitting. We supplement this analysis with an application of quantile regression, a binless approach to rank-based regression taking an absolute-value-distance penalty. Both methods yield, within the 1s to 3s uncertainties, near-zero slopes in the diagnostic plane, largely irrespective of the maximum age or minimum mass imposed on our sample selection, or of the radial bin size adopted. We conclude that, at least in our four well-studied sample galaxies, star cluster formation does not necessarily require an environment-dependent cluster formation scenario, which thus supports the notion of stochastic star cluster formation as the dominant star cluster-formation process within a given galaxy. |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000368225100009 |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/5483]  |
| 专题 | 国家天文台_光学天文研究部 |
| 作者单位 | 1.Peking Univ, Sch Phys, Beijing 100871, Peoples R China 2.Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China 3.Peking Univ, Dept Astron, Beijing 100871, Peoples R China 4.Int Space Sci Inst Beijing, Beijing 100190, Peoples R China 5.Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100012, Peoples R China 6.Univ Oxford, Dept Zool, SEEG, Oxford OX1 3PS, England |
| 推荐引用方式 GB/T 7714 | Sun, Weijia,de Grijs, Richard,Fan, Zhou,et al. THE STAR CLUSTER MASS-GALACTOCENTRIC RADIUS RELATION: IMPLICATIONS FOR CLUSTER FORMATION[J]. ASTROPHYSICAL JOURNAL,2016,816(1). |
| APA | Sun, Weijia,de Grijs, Richard,Fan, Zhou,&Cameron, Ewan.(2016).THE STAR CLUSTER MASS-GALACTOCENTRIC RADIUS RELATION: IMPLICATIONS FOR CLUSTER FORMATION.ASTROPHYSICAL JOURNAL,816(1). |
| MLA | Sun, Weijia,et al."THE STAR CLUSTER MASS-GALACTOCENTRIC RADIUS RELATION: IMPLICATIONS FOR CLUSTER FORMATION".ASTROPHYSICAL JOURNAL 816.1(2016). |
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来源：国家天文台
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