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The [CII] line: a window on the ISM of high-z galaxies Livia Vallini, 6-10-2015 David Meeting X, Scuola Normale Superiore, Pisa
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The photoevaporation of molecular clumps
The [CII] line: a window on the ISM of high-z galaxiesLivia Vallini, 6-10-2015David Meeting X, Scuola Normale Superiore, Pisa 1Motivation
2Motivation
it is a key diagnostic of the ISM because:[CII] is the dominant cooling line of the ISM3Motivation
it is a key diagnostic of the ISM because:[CII] is the dominant cooling line of the ISM[CII] arises from different componentsproviding a wide picture of the ISM- diffuse ionized gas (?)- diffuse neutral gas (CNM, WNM)- dense neutral gas (PDR)4
Capak+2015, Nature[CII] emissionin LAEs and LBGs at z~7
Maiolino+2015Motivation
5Maiolino+2015Open issues
Capak+2015Willott+2015[CII] detectionLAEs/LBGs at 5
![The Distribution of the Milky Way ISM as revealed by the [CII] 158um line.](https://static.documents.pub/doc/80x56/568164e5550346895dd7499c/the-distribution-of-the-milky-way-ism-as-revealed-by-the-cii-158um-line-56ccdd8e3585e.jpg)
