Testing the star formation scaling relations in the clumps of the North American and Pelican nebulae cloud complex

S. Das, J. Jose, Manash R. Samal, Shaobo Zhang, N. Panwar
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引用次数: 4

Abstract

The processes which regulate the star-formation within molecular clouds are still not well understood. Various star-formation scaling relations have been proposed to explain this issue by formulating a relation between star-formation rate surface density ($\rm \Sigma_{SFR}$) and the underlying gas surface density ($\rm \Sigma_{gas}$). In this work, we test various star formation scaling relations, such as Kennicutt-Schmidt relation, volumetric star-formation relation, orbital time model, crossing time model, and multi free-fall time scale model towards the North American and Pelican Nebulae complexes and in cold clumps associated with them. Measuring stellar-mass from young stellar objects and gaseous mass from CO measurements, we estimated mean $\rm \Sigma_{SFR}$, star formation rate per free-fall time, and star formation efficiency (SFE) for clumps to be 1.5 $\rm M{_\odot}~yr^{-1}~kpc^{-2}$, 0.009, 2.0$\%$, respectively, while for the entire NAN complex the values are 0.6 $\rm M{_\odot}~yr^{-1}~kpc^{-2}$, 0.0003, and 1.6$\%$, respectively. For clumps, we notice that the observed properties are in line with the correlation obtained between $\rm \Sigma_{SFR}$ and $\rm \Sigma_{gas}$, and between $\rm \Sigma_{SFR}$ and $\rm \Sigma_{gas}$ per free-fall time and orbital time for Galactic clouds. At the same time, we do not observe any correlation with $\rm \Sigma_{gas}$ per crossing time and multi free-fall time. Even though we see correlations in former cases, however, all models agree with each other within a factor of 0.5 dex, and discriminating between these models is not possible due to the current uncertainties in the input observables. We also test the variation of $\rm \Sigma_{SFR}$ versus the dense gas, but due to low statistics, a weak correlation is seen in our analysis.
在北美和鹈鹕星云复合体的团块中测试恒星形成的尺度关系
调控分子云中恒星形成的过程仍未被很好地理解。为了解释这一问题,人们提出了各种恒星形成尺度关系,即恒星形成速率表面密度($\rm \Sigma_{SFR}$)与下垫气体表面密度($\rm \Sigma_{gas}$)之间的关系。在这项工作中,我们测试了各种恒星形成尺度关系,如kennicut - schmidt关系、体积恒星形成关系、轨道时间模型、穿越时间模型和多重自由落体时间尺度模型,针对北美和鹈鹕星云复合体及其相关的冷团。通过测量年轻恒星天体的恒星质量和CO测量的气体质量,我们估计团块的平均$\rm \Sigma_{SFR}$、每自由落体时间的恒星形成速率和恒星形成效率(SFE)分别为1.5 $\rm M{_\odot}~yr^{-1}~kpc^{-2}$、0.009、2.0 $\%$,而整个NAN复合体的值分别为0.6 $\rm M{_\odot}~yr^{-1}~kpc^{-2}$、0.0003和1.6 $\%$。对于团块,我们注意到观测到的性质与获得的$\rm \Sigma_{SFR}$和$\rm \Sigma_{gas}$之间的相关性,以及在银河系的自由落体时间和轨道时间中$\rm \Sigma_{SFR}$和$\rm \Sigma_{gas}$之间的相关性是一致的。同时,我们没有观察到与$\rm \Sigma_{gas}$每次穿越时间和多次自由落体时间的任何相关性。尽管我们在以前的情况下看到了相关性,但是,所有模型在0.5指数的因子范围内彼此一致,并且由于输入可观测值中的当前不确定性,这些模型之间的区分是不可能的。我们还测试了$\rm \Sigma_{SFR}$与致密气体的变化,但由于统计量低,在我们的分析中可以看到弱相关性。
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