PAH - 版本历史

2025年12月4日 (四) 10:39 Shen

2025-12-04T10:39:16Z

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	*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102		*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102

			* PAHs can form and survive in extremely metal-poor environments https://arxiv.org/abs/2512.04060 JWST Captures Growth of Aromatic Hydrocarbon Dust Particles in the Extremely Metal-poor Galaxy Sextans A

	*JWST中MIRI的测光数据估算PAH的流量 [https://arxiv.org/abs/2501.19397]		*JWST中MIRI的测光数据估算PAH的流量 [https://arxiv.org/abs/2501.19397]

2025年11月6日 (四) 03:03 Shen

2025-11-06T03:03:20Z

←上一版本		2025年11月6日 (四) 03:03的版本
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	*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]		*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]

	* the observed ratio in the AIBs reflects contributions from two distinct PAH populations: the smaller PAHs (∼ 30 − 50 carbon atoms) that contribute most of the 3.3 μm AIB emission and the larger PAHs (≳ 80) that contribute most of the 11.2 μm AIB emission. arXiv:2510.~~2697~~		* the observed ratio in the AIBs reflects contributions from two distinct PAH populations: the smaller PAHs (∼ 30 − 50 carbon atoms) that contribute most of the 3.3 μm AIB emission and the larger PAHs (≳ 80) that contribute most of the 11.2 μm AIB emission. arXiv:2510.2697（很好的一篇review）

	*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102		*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102

2025年11月6日 (四) 03:00 Shen

2025-11-06T03:00:34Z

←上一版本		2025年11月6日 (四) 03:00的版本
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	*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]		*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]

			* the observed ratio in the AIBs reflects contributions from two distinct PAH populations: the smaller PAHs (∼ 30 − 50 carbon atoms) that contribute most of the 3.3 μm AIB emission and the larger PAHs (≳ 80) that contribute most of the 11.2 μm AIB emission. arXiv:2510.2697

	*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102		*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102

2025年2月4日 (二) 03:42 Shen

2025-02-04T03:42:39Z

←上一版本		2025年2月4日 (二) 03:42的版本
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	*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102		*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102

			*JWST中MIRI的测光数据估算PAH的流量 [https://arxiv.org/abs/2501.19397]
	*[[PAHFIT]]		*[[PAHFIT]]

2024年9月10日 (二) 09:24 Shen

2024-09-10T09:24:49Z

←上一版本		2024年9月10日 (二) 09:24的版本
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	:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲		:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲
	:17um,C-C-C弯曲，18mu有硅的发射特征		:17um,C-C-C弯曲，18mu有硅的发射特征
			* tight correlation of PAH and CO emission from z ∼ 0 to 4 [https://arxiv.org/pdf/2409.05710]
			:* PAH和CO与IR光度的关系都是sub-linear的，MIR的光度中有AGN的贡献

	*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]		*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]

2024年5月27日 (一) 07:04 Shen

2024-05-27T07:04:35Z

←上一版本		2024年5月27日 (一) 07:04的版本
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	*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]		*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]

			*Mapping RPAH across the 19 [[PHANGS]] galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find RPAH is constant across the PHANGS sample with an average value of 3.43±0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to qPAH values of 3-6%. arXiv:2405.15102

	*[[PAHFIT]]		*[[PAHFIT]]

2024年2月28日 (三) 13:42 Shen

2024-02-28T13:42:27Z

←上一版本		2024年2月28日 (三) 13:42的版本
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	*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]		*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]

			*[[PAHFIT]]

2023年3月25日 (六) 09:18 Shen

2023-03-25T09:18:50Z

←上一版本		2023年3月25日 (六) 09:18的版本
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	:17um,C-C-C弯曲，18mu有硅的发射特征		:17um,C-C-C弯曲，18mu有硅的发射特征

	*PAHs are better suited as a tracer of B stars than as a tracer of massive		*PAHs are better suited as a tracer of B stars than as a tracer of massive SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]
	SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]

2023年3月25日 (六) 09:18 Shen

2023-03-25T09:18:25Z

←上一版本		2023年3月25日 (六) 09:18的版本
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	:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲		:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲
	:17um,C-C-C弯曲，18mu有硅的发射特征		:17um,C-C-C弯曲，18mu有硅的发射特征

			*PAHs are better suited as a tracer of B stars than as a tracer of massive
			SF. They probe star formation activity time scales of up to 100Myr. [http://astro.dur.ac.uk/AGNvsSF/Talks/AlonsoHerrero.pdf]

Shen：创建页面，内容为“*PAH 的辐射 :3.3um C-H键震动，脂肪族的C-H键震动在3.4um :6.2,7.6um是C-C拉伸震动 :7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲 :17um,C-…”

2022-03-20T09:14:03Z

创建页面，内容为“*PAH 的辐射 :3.3um C-H键震动，脂肪族的C-H键震动在3.4um :6.2,7.6um是C-C拉伸震动 :7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲 :17um,C-…”

新页面

*PAH 的辐射
:3.3um C-H键震动，脂肪族的C-H键震动在3.4um
:6.2,7.6um是C-C拉伸震动
:7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲
:17um,C-C-C弯曲，18mu有硅的发射特征

PAH - 版本历史

2025年12月4日 (四) 10:39 Shen

2025年11月6日 (四) 03:03 Shen

2025年11月6日 (四) 03:00 Shen

2025年2月4日 (二) 03:42 Shen

2024年9月10日 (二) 09:24 Shen

2024年5月27日 (一) 07:04 Shen

2024年2月28日 (三) 13:42 Shen

2023年3月25日 (六) 09:18 Shen

2023年3月25日 (六) 09:18 Shen

Shen：​创建页面，内容为“*PAH 的辐射 :3.3um C-H键震动，脂肪族的C-H键震动在3.4um :6.2,7.6um是C-C拉伸震动 :7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲 :17um,C-…”

Shen：创建页面，内容为“*PAH 的辐射 :3.3um C-H键震动，脂肪族的C-H键震动在3.4um :6.2,7.6um是C-C拉伸震动 :7.8,8.6 C-H在平面内弯曲，11.3,12.7平面外弯曲 :17um,C-…”