A Search for Intermediate-separation Low-mass Binaries in the Orion Nebula Cluster
A Search for Intermediate-separation Low-mass Binaries in the Orion Nebula Cluster
复制标题
猎户座星云团中中等分离低质量双星的搜索
作者：
Matthew De Furio;M. Reiter;M. Meyer;A. Greenbaum;T. Dupuy;A. Kraus
我们利用哈勃空间望远镜（HST）的存档数据，在约翰逊V滤光片中（HST提案10246，PI M）获得了猎户座星云团（ONC）中的二元种群研究结果。Robberto）。年轻的星团和星协为多星星系统的起源和性质提供了线索。间距小于100 Au的双星可以作为初始双星群体的示踪剂，因为它们不太可能通过动力学相互作用而被破坏。低质量，低恒星密度，恒星形成区域，如金牛座-御夫座，与银河系相比，揭示了过量的倍数。研究像ONC这样的高质量、高恒星密度恒星形成区的双星种群，可以提供有关银河场星星种群起源的有用信息。在这项调查中，我们以前未探索（和不完整）的分离参数空间的二进制ONC（15-160 Au）通过拟合双点扩散函数（PSF）模型建立经验PSF。我们确定了14个候选双星（11个新的探测），发现我们观测到的样品是在双星系统中，完全超过质量比，分离度为0.6 < q < 1.0和30 < a < 160 Au。这与在相同参数范围（6.5% ± 3%）内银河场M矮星群是一致的。因此，像ONC这样的大质量恒星形成区不需要进一步的动力学演化，就可以使它们的双星群类似于银河场，就像一些模型对年轻星团所假设的那样。
We present the results of a binary population study in the Orion Nebula Cluster (ONC) using archival Hubble Space Telescope (HST) data obtained with the Advanced Camera for Surveys in Johnson V filter (HST Proposal 10246, PI M. Robberto). Young clusters and associations hold clues to the origin and properties of multiple star systems. Binaries with separations <100 au are useful as tracers of the initial binary population because they are not as likely to be destroyed through dynamical interactions. Low-mass, low stellar density, star-forming regions such as Taurus–Auriga, reveal an excess of multiples compared to the Galactic field. Studying the binary population of higher mass, higher stellar density star-forming regions like the ONC provides useful information concerning the origin of the Galactic field star population. In this survey, we characterize the previously unexplored (and incomplete) separation parameter space of binaries in the ONC (15–160 au) by fitting a double-point-spread function (PSF) model built from empirical PSFs. We identified 14 candidate binaries (11 new detections) and find that of our observed sample are in binary systems, complete over mass ratios and separations of 0.6 < q < 1.0 and 30 < a < 160 au. This is consistent with the Galactic field M-dwarf population over the same parameter ranges, 6.5% ± 3%. Therefore, high-mass star-forming regions like the ONC would not require further dynamical evolution for their binary population to resemble the Galactic field, as some models have hypothesized for young clusters.
影响因子：
4.8
作者：
De Rosa R
通讯作者：
De Rosa R