CO(2-1) survey at 9 parsec resolution in the Small Magellanic Clouds
CO(2-1) survey at 9 parsec resolution in the Small Magellanic Clouds
复制标题
在小麦哲伦星云中以 9 秒差距分辨率进行 CO(2-1) 勘测
DOI：
10.1051/0004-6361/202142217
复制
发表时间：
2022
期刊：
影响因子：
--
通讯作者：
A. Leroy
中科院分区：
文献类型：
--
作者：
H. Saldaño;M. Rubio;A. Bolatto;C. Verdugo;K. Jameson;A. Leroy
The Small Magellanic Cloud (SMC) is the closest low-metallicity galaxy to the Milky Way where the dynamical state of molecular clouds can be analyzed. We present a CO(2-1) survey at 9 pc resolution obtained with the APEX telescope in an extensive region of the SMC and characterize the properties of the molecular clouds. We study the dynamical state and stability of these clouds uniformly. We identify 177 molecular clouds within the SMC by using CPROPS, of which 124 clouds are fully resolved with signal-to-noise ratio $>$ 5. The scaling relationships show that the SMC clouds are (on average) less turbulent and less luminous than their inner Milky Way counterparts of similar size by a factor of 2 and 3, respectively, while for a fixed linewidth, the SMC clouds are over-luminous by a factor of 3.5. Using the virial masses, we derive a CO-to-H2 conversion factor for the SMC CO clouds of 10.5 M$_{\odot}(K km s^{-1} pc^{2})^{-1}$, measured at 9 pc resolution. We also determine a dust-based conversion factor of 28 M$_{\odot}(K km s^{-1} pc^{2})^{-1}$, obtained at 12 pc resolution. We find that the SMC clouds appear to be in approximate gravitational virial equilibrium. We find that the cumulative mass functions based on both the luminous mass and the virial mass are steeper than $\frac{dN}{dM} \propto M^{-2}$, suggesting that most of the molecular mass of the SMC is contained in low-mass clouds.
The Small Magellanic Cloud (SMC) is the closest low-metallicity galaxy to the Milky Way where the dynamical state of molecular clouds can be analyzed. We present a CO(2-1) survey at 9 pc resolution obtained with the APEX telescope in an extensive region of the SMC and characterize the properties of the molecular clouds. We study the dynamical state and stability of these clouds uniformly. We identify 177 molecular clouds within the SMC by using CPROPS, of which 124 clouds are fully resolved with signal-to-noise ratio $>$ 5. The scaling relationships show that the SMC clouds are (on average) less turbulent and less luminous than their inner Milky Way counterparts of similar size by a factor of 2 and 3, respectively, while for a fixed linewidth, the SMC clouds are over-luminous by a factor of 3.5. Using the virial masses, we derive a CO-to-H2 conversion factor for the SMC CO clouds of 10.5 M$_{\odot}(K km s^{-1} pc^{2})^{-1}$, measured at 9 pc resolution. We also determine a dust-based conversion factor of 28 M$_{\odot}(K km s^{-1} pc^{2})^{-1}$, obtained at 12 pc resolution. We find that the SMC clouds appear to be in approximate gravitational virial equilibrium. We find that the cumulative mass functions based on both the luminous mass and the virial mass are steeper than $\frac{dN}{dM} \propto M^{-2}$, suggesting that most of the molecular mass of the SMC is contained in low-mass clouds.