论文标题
海马红外乌云中的密集核心：从修改后的黑体拟合到远红外submillimetre光谱能量分布的物理特性
Dense cores in the Seahorse infrared dark cloud: physical properties from modified blackbody fits to the far-infrared-submillimetre spectral energy distributions
论文作者
论文摘要
我们与先前与Saboca和laboca的观察结果一起使用了Wise，IRA和Herschel的数据，并在丝状海马Indrared Indrared Indrared Indrared Inforrared Inforder Infore inder核心构建了巨大光谱分布（SED）的Far-ir构造。 For the 12 analysed cores, which include two IR dark cores (no WISE counterpart), nine IR bright cores, and one HII region, the mean dust temperature of the cold (warm) component, the mass, luminosity, H$_2$ number density, and surface density were derived to be $13.3\pm1.4$ K ($47.0\pm5.0$ K), $113\pm29$ m $ _ {\ odot} $，$ 192 \ pm94 $ l $ _ {\ odot} $，$（4.3 \ pm1.2）\ times10^5 $ cm $^{ - 3} $，$ 0.77 \ pm0.19 $ g cm $ g cm $^cm $^{ - 3} $，分别。 HII区域IRA 13039-6108A被发现是我们样本中最具发光的来源（$（1.1 \ pm0.4）\ times10^3 $ l $ _ {\ odot} $）。发现所有核心都具有重力结合（即病毒参数$α_ {\ rm vir} <2 $）。在文献中提出的高质量恒星形成的质量 - 拉迪乌斯阈值之上，有12个分析的核心中有7个（58％）位于质量拉迪乌斯阈值之上。 $σ> 0.4 $ g cm $^{ - 3} $的表面密度也超过了高质量星形成的相应阈值。五个分析的核心（42％）在Saboca 350 $μ$ M图像中显示了分裂成两个组成部分的证据。除了HII区域来源IRA 13039-6108A外，Seahorse中的其他一些核心似乎也能够生育高质量恒星。海马IRDC的密集核心人群具有与研究精通的蛇IRDC G11.11-0.12相当的平均特性。海马核心碎裂机制似乎是异质的，包括热牛仔裤不稳定性的情况。需要高分辨率的随访研究来解决核心碎片形成高质量恒星的真正潜力。
We used data from WISE, IRAS, and Herschel in conjuction with our previous observations with SABOCA and LABOCA, and constructed the far-IR to submillimetre spectral energy distributions (SEDs) of dense cores in the filamentary Seahorse infrared dark cloud (IRDC) G304.74+01.32. For the 12 analysed cores, which include two IR dark cores (no WISE counterpart), nine IR bright cores, and one HII region, the mean dust temperature of the cold (warm) component, the mass, luminosity, H$_2$ number density, and surface density were derived to be $13.3\pm1.4$ K ($47.0\pm5.0$ K), $113\pm29$ M$_{\odot}$, $192\pm94$ L$_{\odot}$, $(4.3\pm1.2)\times10^5$ cm$^{-3}$, and $0.77\pm0.19$ g cm$^{-3}$, respectively. The HII region IRAS 13039-6108a was found to be the most luminous source in our sample ($(1.1\pm0.4)\times10^3$ L$_{\odot}$). All the cores were found to be gravitationally bound (i.e. the virial parameter $α_{\rm vir}<2$). Seven out of 12 of the analysed cores (58%) were found to lie above the mass-radius thresholds of high-mass star formation proposed in the literature. The surface densities of $Σ>0.4$ g cm$^{-3}$ derived for these seven cores also exceed the corresponding threshold for high-mass star formation. Five of the analysed cores (42%) show evidence of fragmentation into two components in the SABOCA 350 $μ$m image. In addition to the HII region source IRAS 13039-6108a, some of the other cores in Seahorse also appear to be capable of giving birth to high-mass stars. The dense core population in the Seahorse IRDC has comparable average properties to the cores in the well-studied Snake IRDC G11.11-0.12. The Seahorse core fragmentation mechanisms appear to be heterogenous, including cases of both thermal and non-thermal Jeans instability. High-resolution follow-up studies are required to address the fragmented cores' genuine potential of forming high-mass stars.
