– Niels Bohr Institute - University of Copenhagen

Simulating the [CII] emission of high redshift galaxies

Research output: Chapter in Book/Report/Conference proceedingArticle in proceedingsResearch

Karen Pardos Olsen, Thomas Rodriguez Greve, Desika Narayanan, Christian Brinch, Jesper Rasmussen, Jesper Sommer-Larsen, Andrew Wasmuth Zirm, Sune Toft, Robert Thompson, Luis Rios, Stephanie Mae Stawinski

he fine structure line of [CII] at 158 microns can arise throughout theinterstellar medium (ISM) and has been proposed as a tracer of starformation rate (SFR). But the origin of [CII] and how it depends on e.g.metallicity and radiation field of a galaxy remain uncertain.Simulating[CII] can be done by combining the output from galaxy simulations withprescriptions for the subgrid physics, as has now been demonstrated byseveral groups. However, these models are either built on analyticaldiscs or contain other simplifying assumptions. SÍGAME (Simulatorof GAlaxy Millimeter/submillimeter emission) avoids these issues byusing cosmological simulations and calculates [CII] emission reliably onresolved scales within each galaxy. The local metallicity is that of thesimulation, whereas the far-ultraviolet radiation field and cosmic rayintensity are both scaled with local star formation rate density. Forthe chemistry and radiative transfer, the photoionization code CLOUDY isimplemented. I will show results for z=2 star-forming galaxies yet to beobserved, as well as preliminary results for galaxies at z~6-7 whereobservations have presented contradictory detections and non-detectionsof star-forming galaxies.
Original languageEnglish
Title of host publicationAmerican Astronomical Society, Meeting
Place of PublicationUSA
Publication date1 Jun 2016
Article number318.06
StatePublished - 1 Jun 2016

ID: 185475683