A DEEP SPITZER SURVEY OF CIRCUMSTELLAR DISKS IN THE YOUNG DOUBLE CLUSTER, h AND χ PERSEI
A DEEP SPITZER SURVEY OF CIRCUMSTELLAR DISKS IN THE YOUNG DOUBLE CLUSTER, h AND χ PERSEI
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年轻双星团 h 和 χ 英仙座中周星盘的深度斯必泽观测
DOI：
10.1088/0004-637x/796/2/127
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
R. Jayawardhana
中科院分区：
文献类型：
--
作者：
R. Cloutier;T. Currie;G. Rieke;S. Kenyon;Z. Balog;R. Jayawardhana
我们分析了非常深的红外阵列相机和斯皮策多波段成像光度计（MIPS）测光的1400万年前的双星系团，h和χ英仙座，我们早期的基础上，较浅的斯皮策周期1的研究。许多可能的成员在8 μm和24 μm处显示出过量的红外（IR），表明是星周尘埃。在我们的整个样本中，具有8 μm过量的恒星的频率至少为2%，对于B/A恒星（较晚类型，较低质量的恒星）略低（较高）。光谱学还可以在大约2%的系统中识别气体，但在尘埃和气体之间没有明确的趋势。对18个源的光谱能量分布建模，在MIPS 24 μm的光波长下进行探测，揭示了一组不同的盘演化状态，包括很高比例的过渡盘，尽管所有盘轴承成员的类似数据将提供限制。利用蒙特卡罗模拟，我们联合收割机结合我们的结果与其他年轻的集群研究全球的尘埃/气体盘的演变。对于星系团的名义年龄，热尘埃和气体的e折叠时间（τ0）分别为2.75 Myr和1.75 Myr。假设一组修订的年龄为一些集群，这些时标增加到5.75和3.75亿年，分别意味着一个显着更长的典型的原行星盘的寿命比以前认为的。在这两种情况下，过渡盘持续时间（多个进化途径的平均值）约为100万年。最后，4-6百万年恒星的24 μm过剩频率似乎低于其他10-30百万年老星团中1-2.5百万年恒星的24 μ m过剩频率。
We analyze very deep Infrared Array Camera and Multiband Imaging Photometer for Spitzer (MIPS) photometry of ∼12, 500 members of the 14 Myr old Double Cluster, h and χ Persei, building upon our earlier, shallower Spitzer Cycle 1 studies. Numerous likely members show infrared (IR) excesses at 8 μm and 24 μm, indicative of circumstellar dust. The frequency of stars with 8 μm excess is at least 2% for our entire sample, slightly lower (higher) for B/A stars (later type, lower mass stars). Optical spectroscopy also identifies gas in about 2% of systems, but with no clear trend between the presence of dust and gas. Spectral energy distribution modeling of 18 sources with detections at optical wavelengths through MIPS 24 μm reveals a diverse set of disk evolutionary states, including a high fraction of transitional disks, though similar data for all disk-bearing members would provide constraints. Using Monte Carlo simulations, we combine our results with those for other young clusters to study the global evolution of dust/gas disks. For nominal cluster ages, the e-folding times (τ0) for the frequency of warm dust and gas are 2.75 Myr and 1.75 Myr, respectively. Assuming a revised set of ages for some clusters, these timescales increase to 5.75 and 3.75 Myr, respectively, implying a significantly longer typical protoplanetary disk lifetime than previously thought. In both cases, the transitional disk duration, averaged over multiple evolutionary pathways, is ≈1 Myr. Finally, 24 μm excess frequencies for 4–6 M☉ stars appear lower than for 1–2.5 M☉ stars in other 10–30 Myr old clusters.
影响因子：
4.8
作者：
Bell, Cameron P. M.;Naylor, Tim;Littlefair, S. P.
通讯作者：
Littlefair, S. P.