Discovering young stars in the Gum 31 region with infrared observations
Discovering young stars in the Gum 31 region with infrared observations
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DOI：
10.1051/0004-6361/201220218
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发表时间：
2013-01
影响因子：
6.5
通讯作者：
H. Ohlendorf;T. Preibisch;B. Gaczkowski;T. Ratzka;J. Ngoumou;V. Roccatagliata;R. Grellmann
中科院分区：
文献类型：
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作者：
H. Ohlendorf;T. Preibisch;B. Gaczkowski;T. Ratzka;J. Ngoumou;V. Roccatagliata;R. Grellmann
上下文。包含星团NGC3324的Gum 31气泡是靠近船底座星云的一个很少被研究的年轻区域。目标。我们的目标是描述31号胶及其周围的年轻恒星和原生恒星群的特征，并研究该地区的恒星形成过程。方法：研究方法。我们从斯皮策、WISE和赫歇尔的数据中识别出候选的年轻恒星。结合这些结果，我们分析了候选年轻恒星天体的光谱能量分布。通过从赫歇尔数据获得的密度和温度图，以及与该地区“收集和坍塌”情景的比较，我们能够进一步限制该地区作为一个整体的特征。结果。从WISE数据中发现了6 6 1个候选年轻恒星天体，在1.0◦×1.1◦区域内通过赫歇尔观测探测到91个原恒星候选天体。这些天体大多分布在较小的星团中，或者与H II气泡排列得很好。我们还确定了赫比格-哈罗喷气式飞机的来源。该区域的红外形态表明，它是更大的汽车星云复合体的一部分。结论。候选年轻恒星天体在H II泡的RIM中的位置暗示它们是由“收集和坍塌”情景触发的，这与该区域的观测参数很好地吻合。在柱子的顶部发现了一些候选的年轻恒星物体，这指向了恒星形成的辐射触发。因此，我们发现在该区域不同的触发恒星形成机制在起作用。纠正了候选年轻恒星天体的污染数量，我们在31号胶中发现了∼600个年轻恒星天体，高于我们约1M⊙的完备性限制。根据初始质量函数向下推算到0.1M⊙，我们估计该区域的年轻恒星总数为∼5000。
Context. The Gum 31 bubble containing the stellar cluster NGC 3324 is a poorly-studied young region close to the Carina Nebula. Aims. We are aiming to characterise the young stellar and protoste llar population in and around Gum 31 and to investigate the starformation process in this region. Methods. We identify candidate young stellar objects from Spitzer, WISE, and Herschel data. Combining these, we analyse the spectral energy distributions of the candidate young stell ar objects. With density and temperature maps obtained from Herschel data and comparisons to a ‘collect and collapse’ scenario for the region we are able to further constrain the characteristics of the region as a whole. Results. 661 candidate young stellar objects are found from WISE data, 91 protostar candidates are detected through Herschel observations in a 1.0 ◦ × 1.1 ◦ area. Most of these objects are found in small clusters or are well aligned with the H II bubble. We also identify the sources of Herbig-Haro jets. The infrared morp hology of the region suggests that it is part of the larger Car ina Nebula complex. Conclusions. The location of the candidate young stellar objects in the ri m of the H II bubble is suggestive of their being triggered by a ‘collect and collapse’ scenario, which agrees well with the observed parameters of the region. Some candidate young stellar objects are found in the heads of pillars, which points towar ds radiative triggering of star formation. Thus, we find evid ence that in the region different mechanisms of triggered star formation are at work. Correcting the number of candidate young stellar objects for contamination we find ∼ 600 young stellar objects in Gum 31 above our completeness limit of about 1 M⊙. Extrapolating the intital mass function down to 0.1 M⊙, we estimate a total population of∼ 5000 young stars for the region.