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High-Sensitivity Observations for a Large Region of the Cassiopeia Molecular Cloud Complex in the Molecular Lines

对仙后座分子云复合体大区域分子线的高灵敏度观测

基本信息

批准号：
08640324
负责人：
SATO Fumio
金额：
$ 1.22万
依托单位：
Tokyo Gakugei University
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
1996
资助国家：
日本
起止时间：
1996 至 1997
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-08640324/
关键词：
Interstellar Matter Interstellar Molecular Clouds Star Formation Dark Clouds 分子雲分子線観測

项目摘要

By use of the 4m millimeter-wave telescope with the 4K cooled SIS mixer receiver at Nagoya University, we mapped the regions containing the dark clouds Khav 216, L1333, L1358, and L1394 located in the Cassiopeia molecular cloud complex in the ^<13>CO(J=1-0)line. Their high-density cores were mapped also in the C^<18>O(J=1-0)line. Khav 216 has radial velocity of -+3kms^<-1>. The ^<13>CO cloud core, with size of 0.74pc*0.67pc, has a total mass of -12M_<<of sun>>, and its mean H_2 density is -9.2*10^2cm^<-3>. The ^<13>CO cloud in the L1333 region consists fo two filamentary clouds with V_<LSR> --2kms^<-1> and+3kms^<-1>, extending nearly parallel to the galactic equator. Thirteen C^<18>O cores were found embedded in the ^<13>CO clouds. We found eithteen Halpha emission stars and five cold IRAS point sources (three of them were identified with the Halpha emission stars)there. The fact suggests that stars have been forming there. One of the IRAS point sources is associated with a C^<18>O core. We infer it is an especially young protostar from its far-infrared spectrum. Towards the source the C^<18>O linewidth is as broad as -1.6kms^<-1> (full width at the zero intensity level). This may probably indicate the outflow activity of the young star. The core has the smallest ratio of the virial mass to the LTE mass among the C^<118>O cores in the L1333 cloud, suggesting that star formation occurs preferentially in a core whose internal kinetic energy is smallest as compared with the self-gravitational energy. The ^<13>CO cloud in the L1358 region has three components with different velocities. Their total mass was estimated -2*10^3M12M_<<of sun>>. Six cold IRAS point sources are associated with the ^<13>CO cloud cores, suggesting that star formation is ongoing there.

利用名古屋大学的4米毫米波望远镜和4 K冷却SIS混合器接收机，我们绘制了位于仙后座分子云复合体中的星云Khav 216、L1333、L1358和L1394的^<13>CO（J=1-0）谱线。它们的高密度核也被绘制在C^<18>O（J=1-0）线上。Khav 216的径向速度为-+3kms ^<-1>。CO<13>云核大小为0.74pc*0.67pc，总质量为-12M <<of sun>>，平均H_2密度为-9.2 10 ^2cm ^<-3>。L1333<13>区的^ CO云由两个V_<LSR>--2kms ^<-1>和+3kms ^<-1>的对流云组成，几乎平行于银河赤道延伸。在<18>^ CO云中发现了13个C^ O核<13>。我们在那里发现了18颗Halpha发射星和5个冷IRAS点源（其中3个被确认为Halpha发射星）。这一事实表明，恒星一直在那里形成。其中一个IRAS点源与一个C^<18>O核有关。我们从它的远红外光谱推断它是一颗特别年轻的原恒星。朝向源的C^<18>O线宽为-1.6kms ^<-1>（零强度水平的全宽）。这可能表明年轻星星的外流活动。在L1333云的C^ O核中，该核的维里质量与LTE质量之比最小<118>，这表明星星的形成优先发生在内部动能与自引力能相比最小的核中。L1358<13>区的^ CO云有三个不同速度的分量。它们的总质量估计为-2 10 ^3 M12 M_<<of sun>>。六个冷IRAS点源与^<13>CO云核有关，表明那里正在形成星星。