Simulating the [CII] emission of high redshift galaxies
Abstract
The fine structure line of [CII] at 158 microns can arise throughout the interstellar medium (ISM) and has been proposed as a tracer of star formation 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 with prescriptions for the subgrid physics, as has now been demonstrated by several groups. However, these models are either built on analytical discs or contain other simplifying assumptions. SÍGAME (Simulator of GAlaxy Millimeter/submillimeter emission) avoids these issues by using cosmological simulations and calculates [CII] emission reliably on resolved scales within each galaxy. The local metallicity is that of the simulation, whereas the far-ultraviolet radiation field and cosmic ray intensity are both scaled with local star formation rate density. For the chemistry and radiative transfer, the photoionization code CLOUDY is implemented. I will show results for z=2 star-forming galaxies yet to be observed, as well as preliminary results for galaxies at z~6-7 where observations have presented contradictory detections and non-detections of star-forming galaxies.
- Publication:
-
American Astronomical Society Meeting Abstracts #228
- Pub Date:
- June 2016
- Bibcode:
- 2016AAS...22831806P