Astrometric and photometric initial mass functions from the UKIDSS Galactic Clusters Survey: II The Alpha Persei open cluster
Astrometric and photometric initial mass functions from the UKIDSS Galactic Clusters Survey: II The Alpha Persei open cluster
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来自 UKIDSS 银河星团巡天的天体测量和光度初始质量函数：II 英仙座阿尔法疏散星团
DOI：
10.1111/j.1365-2966.2012.21811.x
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发表时间：
2012
影响因子：
4.8
通讯作者：
UK.
中科院分区：
文献类型：
--
作者：
N. Lodieu;N. Deacon;N. Hambly;S. Iac;Tenerife;Spain.;Ull;La Laguna;Mpia Heidelberg;H Germany;R. Edinburgh;UK.
我们给出了对每个开放星系团的完整�的深(J=19.1MAG)红外(ZY JHK)调查结果，该调查是从UKIRT红外深空调查数据发布的第9版中提取的。我们通过结合五个近红外频段的光度测定和由UKIDSS GCS DR9提供的多个历元得出的自行，选择了�700星团成员候选者，�为56平方度/Per。我们还根据DR9提供的新光度和天体测量学，为在GCS中发现的所有先前公布的Per低质量恒星和棕矮星提供了修订的成员资格。在离散度小于0.06-0.09 MAG的Per中，我们没有发现K带可变性的证据。我们使用了两种独立但互补的方法来推导星系团的光度和质量函数：一种是概率分析，另一种是更标准的方法，包括更严格的天文测量和光度学切割。我们发现由两种方法得到的光度函数和质量函数是一致的。我们发现，Per质量函数的形状与昂宿星团的形状相似，尽管在包含了早期研究的更高质量数据后，特征质量可能更高(色散是可比的)。我们的结论是，Per、昂宿星和Praesepe的质量函数最好用类似于系统场质量函数的对数正态表示来再现，尽管特征质量和色散值有一些变化。
We present the results of a deep (J = 19.1 mag) infrared (ZY JHK) survey over the full � Per open cluster extracted from the Data Release 9 of the UKIRT Infrared Deep Sky Survey Galactic Clusters Survey. We have selected � 700 cluster member candidates in �56 square degrees inPer by combining photometry in five near-infrared passbands and proper motions derived from the multiple epochs provided by the UKIDSS GCS DR9. We also provide revised membership for all previously publishedPer low-mass stars and brown dwarfs recovered in GCS based on the new photometry and astrometry provided by DR9. We find no evidence of K-band variability in members ofPer with dispersion less than 0.06-0.09 mag. We employed two independent but complementary methods to derive the cluster luminosity and mass functions: a probabilistic analysis and a more standard approach consisting of stricter astrometric and photometric cuts. We find that the resulting luminosity and mass functions obtained from both methods are consistent. We find that the shape of thePer mass function is similar to that of the Pleiades although the characteristic mass may be higher after including higher mass data from earlier studies (the dispersion is comparable). We conclude that the mass functions ofPer, the Pleiades, and Praesepe are best reproduced by a log- normal representation similar to the system field mass function although with some variation in the characteristic mass and dispersion values.