Cold gas in the early Universe

First detection of [CII]158um at high redshift (top), compared with a previous detection of CO in the same object (a quasar host galaxy at z=6.4) (Maiolino et al. 2005).

Tracing the formation of the first galaxies in the early Universe is one of the hottest topics in Astrophysics, but also one of the most challenging areas, since such distant (and generally low mass) galaxies are very faint at most wavelengths. I have been pioneering the use of far-IR fine structure lines to identify and characterize primordial galaxies. Far-IR fine structure lines are generally the strongest emission lines in the spectrum of any galaxy, hence the most promising tool to detect and trace galaxies at high redshift. Among these lines the [CII]158um is often the strongest.

The first detection of [CII]158um at high redshift, specifically at z=6.4, was obtained by Maiolino et al. (2005). This discovery has opened the era of using far-IR lines for searching and characterizing distant galaxies, nowadays one of the main science cases of major facilities such as the Atacama Large Millimeter/submillimeter Array (ALMA). Since the first [CII] detection at high redshift, several groups world wide have used far-IR fine structure lines to identify distant galaxies and to trace their evolutionary processes, with steadily growing detection rates and delivering exquisite maps of the interstellar medium and circum-galactic medium in these primordial systems.

Distribution of [CII]158um, [OIII]88um and UV light emission in a galaxy at z=7.1, reveaing the complex distribution of ISM, star formation and dust obscuration in these primeval systems (Carniani, Maiolino et al. 2017).

Additional highlights obtained by exploiting this technique by members of my team or collaborating groups include:

The detection of the [CII]158um transition in a large sample of more than 100 galaxies at z~5 in order to characterize their properties if the goal of the ALMA Large Programme ALPINE