“BPT diagram”的版本间差异
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无编辑摘要 |
无编辑摘要 |
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*高红移和低红移有一些系统的shift |
*高红移和低红移有一些系统的shift |
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:In order to explain offsets between z ∼ 0 and high- redshift galaxies in diagnostic plots such as the [O iii]/Hβ |
:In order to explain offsets between z ∼ 0 and high- redshift galaxies in diagnostic plots such as the [O iii]/Hβ vs. [N ii]/Hα diagram, it has been proposed that high-redshift galaxies may have higher ionization parameters (Kewley et al. 2015; Cullen et al. 2016), harder ionizing stellar spectra (Steidel et al. 2014), higher density/ISM pressure (Kewley et al. 2013; Sanders et al. 2016), and/or anomalous nitrogen abundance at fixed O/H (Masters 2 Sanders et al. et al. 2014; Shapley et al. 2015; Sanders et al. 2016) compared to z ∼ 0 galaxies. Depending |
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vs. [N ii]/Hα diagram, it has been proposed that high-redshift galaxies may have higher ionization parameters |
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(Kewley et al. 2015; Cullen et al. 2016), harder ionizing stellar spectra (Steidel et al. 2014), higher density/ISM |
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pressure (Kewley et al. 2013; Sanders et al. 2016), and/or anomalous nitrogen abundance at fixed O/H (Masters |
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2 Sanders et al. et al. 2014; Shapley et al. 2015; Sanders et al. 2016) compared to z ∼ 0 galaxies. Depending |
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2016年6月15日 (三) 02:59的版本
- OIII/Hbeta VS NII/Halpha
- 不一定4条线都有才能区分，3条加一个upper limit也可以
- 通常 OIII和Hbeta比较弱，更难探测，主要是一些弱的AGN或者金属丰度比较高的恒星形成星系。
- 大质量星系容易出现Hbeta强，OIII，低金属丰度容易Halpha强，NII弱；
- 有一些星系没有巴尔沫线，但是有OIII和NII，（高电离态）
- 有一个类似的图用[SII]λ6717+6713/Halpha 代替NII/Halpha，成为VO87
- 该图能区分LINER和AGN，BPT不能
- OIII/Hbeta 可能不完全能表征AGN
- Maragkoudakis et al. (2014) revealed that galaxies with extranuclear star formation can show higher [O III] λ5007/Hβ line ratios, since lower metallicity H II regions in the outer parts of galaxy discs are also capable of producing high-excitation emis- sion lines.
- 高红移和低红移有一些系统的shift
- In order to explain offsets between z ∼ 0 and high- redshift galaxies in diagnostic plots such as the [O iii]/Hβ vs. [N ii]/Hα diagram, it has been proposed that high-redshift galaxies may have higher ionization parameters (Kewley et al. 2015; Cullen et al. 2016), harder ionizing stellar spectra (Steidel et al. 2014), higher density/ISM pressure (Kewley et al. 2013; Sanders et al. 2016), and/or anomalous nitrogen abundance at fixed O/H (Masters 2 Sanders et al. et al. 2014; Shapley et al. 2015; Sanders et al. 2016) compared to z ∼ 0 galaxies. Depending