GAS KINEMATICS AND STAR FORMATION IN THE FILAMENTARY IRDC G34.43+0.24
GAS KINEMATICS AND STAR FORMATION IN THE FILAMENTARY IRDC G34.43+0.24
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DOI：
10.3847/0004-637x/819/2/117
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发表时间：
2016-02
期刊：
影响因子：
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通讯作者：
Jin-Long Xu;Di Li;Chuan-peng Zhang;Xiao-Lan Liu;Jun-jie Wang;C. Ning;B. Ju
中科院分区：
文献类型：
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作者：
Jin-Long Xu;Di Li;Chuan-peng Zhang;Xiao-Lan Liu;Jun-jie Wang;C. Ning;B. Ju
我们对红外暗云(IRDC)G34.43+0.24进行了多波长研究。从紫金山天文台(PMO)13.7m射电望远镜获得了13CO J=1-0和C18O J=1-0的新地图。在8μm处(Spitzer-irac)，IRDC G34.43+0.24是一条沿南北方向延伸18‘的暗丝。根据870μm和C18O J=1-0排放的关系，我们建议IRDCG34.43+0.24的长度不应为18‘，而应延伸到34’。IRDC G34.43+0.24包含一些大质量的原恒星、UC H II区和红外气泡。假设距离为3.7kpC，IRDC G34.43+0.24的空间扩展约为37pC。IRDC G34.43+0.24的线性质量密度为∼1.6×103M⊙PC−1，与其临界质量长度比大致一致。湍流运动可能有助于稳定细丝以防径向崩塌。红外气泡N61和N62在8μm处都表现为环状结构，特别是N61具有扩展为IRDCG34.43+0.24的双壳结构。外壳以8μm和13CO J=1-0的发射示踪，内壳以24μm和20 cm的发射示踪。我们推测外壳(9.9×105年)是由HⅡ区G34.172+0.175的膨胀形成的，而内壳(4.1∼6.3×105年)可能是由其中心大质量恒星的高能恒星风产生的。从Glimse I目录中，我们选择了一些具有∼105年历史的I类来源。这些I类源沿着丝状分子云聚集。
We performed a multiwavelength study toward the infrared dark cloud (IRDC) G34.43+0.24. New maps of 13CO J = 1–0 and C18O J = 1–0 were obtained from the Purple Mountain Observatory (PMO) 13.7 m radio telescope. At 8 μm (Spitzer-IRAC), IRDC G34.43+0.24 appears to be a dark filament extended by 18′ along the north–south direction. Based on the association with the 870 μm and C18O J = 1–0 emission, we suggest that IRDC G34.43+0.24 should not be 18′ in length, but extend to 34′. IRDC G34.43+0.24 contains some massive protostars, UC H ii regions, and infrared bubbles. The spatial extend of IRDC G34.43+0.24 is about 37 pc, assuming a distance of 3.7 kpc. IRDC G34.43+0.24 has a linear mass density of ∼1.6 × 103 M⊙ pc−1, which is roughly consistent with its critical mass to length ratio. The turbulent motion may help stabilize the filament against the radial collapse. Both infrared bubbles N61 and N62 show a ringlike structure at 8 μm. In particular, N61 has a double-shell structure that has expanded into IRDC G34.43+0.24. The outer shell is traced by 8 μm and 13CO J = 1–0 emission, while the inner shell is traced by 24 μm and 20 cm emission. We suggest that the outer shell (9.9 × 105 years) is created by the expansion of H ii region G34.172+0.175, while the inner shell (4.1 ∼ 6.3 × 105 years) may be produced by the energetic stellar wind of its central massive star. From the GLIMPSE I catalog, we selected some Class I sources with an age of ∼105 years. These Class I sources are clustered along the filamentary molecular cloud.