Clusters, clouds, and correlations: relating young clusters to giant molecular clouds in M33 and M31
Clusters, clouds, and correlations: relating young clusters to giant molecular clouds in M33 and M31
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星团、云和相关性：将年轻星团与 M33 和 M31 中的巨型分子云联系起来
DOI：
10.1093/mnras/stad1430
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发表时间：
2023
影响因子：
4.8
通讯作者：
Leroy, Adam K.
中科院分区：
文献类型：
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作者：
Peltonen, Joshua;Rosolowsky, Erik;Johnson, L. Clifton;Seth, Anil C.;Dalcanton, Julianne;Bell, Eric F.;Braine, Jonathan;Koch, Eric W.;Lazzarini, Margaret;Leroy, Adam K.
我们利用星系M33和M31中的年轻星系团和巨分子云（GMC）来约束星星形成过程的时空尺度。在M33中，我们将全色哈勃仙女座宝藏：三角形扩展区域（PHATTER）目录中的1214个星系团（通过色星等图（CMD）拟合测量年龄）与新的35 pc分辨率阿塔卡马大型毫米/亚毫米阵列（阿尔马）识别的444个GMC进行了比较12 CO（2-1）调查。在M31中，我们比较了全色哈勃仙女座宝库（PHAT）目录的1249个集群，从毫米波天文学研究组合阵列（CARMA）12 CO（1-0）测量的251个GMC与20 pc分辨率。通过两点相关性分析，我们发现年轻的集群有很高的概率是附近的其他年轻的集群，但GMC之间的相关性被抑制的云识别算法。通过比较位置，我们发现，年轻的集群比老集群更接近GMC。通过对M33星团数据的互相关分析，我们发现当星团的年龄≤ 1000万年时，它们是统计相关的。利用高精度的年龄的集群，我们发现，集群的年龄超过1.18亿年是不相关的分子星际介质（ISM）。利用M33中最年轻的星系团和巨星系团的空间重合性，我们估计星系团在母星系团内部的寿命为1400 - 600万年。通过类似的分析，我们发现M33中的巨星系团的总寿命为1100 - 1500万年。我们还发展了一个漂移模型，并表明，上述相关性可以解释，如果在M33中的集群有一个5-10 km s-1的速度色散相对于分子ISM。
We use young clusters and giant molecular clouds (GMCs) in the galaxies M33 and M31 to constrain temporal and spatial scales in the star formation process. In M33, we compare the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) catalogue of 1214 clusters with ages measured via colour–magnitude diagram (CMD) fitting to 444 GMCs identified from a new 35 pc resolution Atacama Large Millimeter/submillimeter Array (ALMA)12CO(2–1) survey. In M31, we compare the Panchromatic Hubble Andromeda Treasury (PHAT) catalogue of 1249 clusters to 251 GMCs measured from a Combined Array for Research in Millimeter-wave Astronomy (CARMA)12CO(1–0) survey with 20 pc resolution. Through two-point correlation analysis, we find that young clusters have a high probability of being near other young clusters, but correlation between GMCs is suppressed by the cloud identification algorithm. By comparing the positions, we find that younger clusters are closer to GMCs than older clusters. Through cross-correlation analysis of the M33 cluster data, we find that clusters are statistically associated when they are ≤10 Myr old. Utilizing the high precision ages of the clusters, we find that clusters older than ≈18 Myr are uncorrelated with the molecular interstellar medium (ISM). Using the spatial coincidence of the youngest clusters and GMCs in M33, we estimate that clusters spend ≈4–6 Myr inside their parent GMC. Through similar analysis, we find that the GMCs in M33 have a total lifetime of ≈11–15 Myr. We also develop a drift model and show that the above correlations can be explained if the clusters in M33 have a 5–10 km s−1velocity dispersion relative to the molecular ISM.