报告题目：[CII] is all the rage at high-z - but how to make sense of it?

　　报告人：Dr. Thomas Greve (UCL)

　　摘要：In this talk I will present new SIGAME simulations of the [CII] 157.7um fine structure line emission from cosmological smoothed particle hydrodynamics (SPH) simulations of main sequence galaxies at z = 2. The gas in our galaxy simulations is modelled as a multi-phased interstellar medium (ISM) comprised of molecular gas residing in the inner regions of giant molecular clouds, an atomic gas phase associated with photodissociation regions at the surface of the clouds, and a diffuse, fully ionized gas phase. Taking into account heating by the local FUV radiation field and cosmic rays - both scaled by the local star formation rate density - we calculate the [CII] emission from each of the aforementioned ISM phases. The [CII] emission peaks in the central (<~ 1 kpc) regions of our galaxies where the star formation is most intense, and we find that the majority (>~ 60%) of the emission in this region originates in the molecular gas phase. At larger galactocentric distances (>~2 kpc), the atomic gas is the main contributor to the [CII] emission (>~ 80%), and at all radii the ionized gas provides a negligible amount (<~ 5%) to the [CII] budget. Our simulations predict a log-linear relationship between the integrated [CII] luminosity and star formation rate with a slope (0.80 +/- 0.12) in agreement with observationally determined slopes (~ 0.85 - 1.00) but with a ~ 3 times higher normalization than the observed z ~ 0 relation.

　　报告时间：2015年9月18日（星期五）上午 9：30

　　报告地点：紫台办公大楼 619 会议室

　　联系人：马红君（83332210）

欢迎大家积极参加！

　                                              　紫金山天文台学术委员会