“HII region”的版本间差异

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*PHANGS-JWST
*PHANGS-JWST
:4个星系:Two galaxies (NGC 1365 and NGC 7496) host active galactic nuclei (AGNs) and strong bars. NGC 628 is a prototypical grand-design spiral, while IC 5332 shows a flocculent spiral morphology. Based on MUSE Hα emission line maps, a catalog of ∼ 30, 000 nebulae has been constructed. The nebulae were selected using HIIphot.
:4个星系:Two galaxies (NGC 1365 and NGC 7496) host active galactic nuclei (AGNs) and strong bars. NGC 628 is a prototypical grand-design spiral, while IC 5332 shows a flocculent spiral morphology. Based on MUSE Hα emission line maps, a catalog of ∼ 30, 000 nebulae has been constructed. The nebulae were selected using HIIphot.
*采用 galaxy mixture density network (GMDN,一种高斯混合模型)的方法来推断星系中不可分辨HII区的发射线 [https://github.com/Sheng-Qi-Yang/GMDN] [https://arxiv.org/pdf/2409.03997]



:arXiv:2212.09159: 利用JWST/MIRI images in the F770W, F1000W and F1130W来计算q(PAH)=(F770+F1130)/F2100来计算PAH在尘埃中的比例,F2100是用来表示非常小的尘埃颗粒的发射,从而代表总尘埃。SIII/SII表征电离参数,发现q(PAH)最主要和电离参数相关,而和金属丰度关系不大
:arXiv:2212.09159: 利用JWST/MIRI images in the F770W, F1000W and F1130W来计算q(PAH)=(F770+F1130)/F2100来计算PAH在尘埃中的比例,F2100是用来表示非常小的尘埃颗粒的发射,从而代表总尘埃。SIII/SII表征电离参数,发现q(PAH)最主要和电离参数相关,而和金属丰度关系不大

2024年9月9日 (一) 09:18的最新版本

  • PHANGS-MUSE survey
  • PHANGS-JWST
4个星系:Two galaxies (NGC 1365 and NGC 7496) host active galactic nuclei (AGNs) and strong bars. NGC 628 is a prototypical grand-design spiral, while IC 5332 shows a flocculent spiral morphology. Based on MUSE Hα emission line maps, a catalog of ∼ 30, 000 nebulae has been constructed. The nebulae were selected using HIIphot.
  • 采用 galaxy mixture density network (GMDN,一种高斯混合模型)的方法来推断星系中不可分辨HII区的发射线 [1] [2]


arXiv:2212.09159: 利用JWST/MIRI images in the F770W, F1000W and F1130W来计算q(PAH)=(F770+F1130)/F2100来计算PAH在尘埃中的比例,F2100是用来表示非常小的尘埃颗粒的发射,从而代表总尘埃。SIII/SII表征电离参数,发现q(PAH)最主要和电离参数相关,而和金属丰度关系不大
  • HII区和分子云区域的转换非常的sharp [3]
  • 利用IFS数据来搜寻HII区的软件 pyHIIexplorer [4] arXiv:2204.04252
  • 利用发射线来算金属丰度