Simulating the [CII] emission of high redshift galaxies
Research output: Chapter in Book/Report/Conference proceeding › Article in proceedings › Research
Standard
Simulating the [CII] emission of high redshift galaxies. / Olsen, Karen Pardos; Greve, Thomas Rodriguez; Narayanan, Desika; Brinch, Christian; Rasmussen, Jesper; Sommer-Larsen, Jesper; Zirm, Andrew Wasmuth; Toft, Sune; Thompson, Robert; Rios, Luis; Stawinski, Stephanie Mae.
American Astronomical Society, Meeting. Vol. 228 USA, 2016. 318.06.Research output: Chapter in Book/Report/Conference proceeding › Article in proceedings › Research
Harvard
APA
Vancouver
Author
Bibtex
}
RIS
TY - GEN
T1 - Simulating the [CII] emission of high redshift galaxies
AU - Olsen, Karen Pardos
AU - Greve, Thomas Rodriguez
AU - Narayanan, Desika
AU - Brinch, Christian
AU - Rasmussen, Jesper
AU - Sommer-Larsen, Jesper
AU - Zirm, Andrew Wasmuth
AU - Toft, Sune
AU - Thompson, Robert
AU - Rios, Luis
AU - Stawinski, Stephanie Mae
PY - 2016/6/1
Y1 - 2016/6/1
N2 - 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.
AB - 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.
UR - http://adsabs.harvard.edu/abs/2016AAS...22831806P
M3 - Article in proceedings
VL - 228
BT - American Astronomical Society, Meeting
CY - USA
ER -
ID: 185475683