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The halo-to-stellar mass ratio in the S4G

Published online by Cambridge University Press:  21 March 2017

Simón Díaz-García ,
Heikki Salo  and
Eija Laurikainen
Simón Díaz-García
Affiliation:
Astronomy Research Group, University of Oulu, FI-90014 Finland, email: simon.diazgarcia@oulu.fi
Heikki Salo
Affiliation:
Astronomy Research Group, University of Oulu, FI-90014 Finland, email: simon.diazgarcia@oulu.fi
Eija Laurikainen
Affiliation:
Astronomy Research Group, University of Oulu, FI-90014 Finland, email: simon.diazgarcia@oulu.fi
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Abstract

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We use 3.6 μm photometry for 1154 disk galaxies (i < 65°) in the S4G (Sheth et al. 2010). We obtain the average stellar component of the circular velocity (V disk) and the mean (dark matter) halo-to-stellar mass ratio (M halo/M *) inside the optical radius (R opt) in bins of total stellar mass (M *, from Muñoz-Mateos et al. 2015), providing observational constraints for galaxy formation models to be tested against. We find the M halo/M * − M * relation in good agreement with the best-fit model at z ≈ 0 in ΛCDM cosmological simulations (e.g. Moster 2010), assuming that the dark matter halo within R opt comprises a constant fraction (~ 4%) of its total mass.

Keywords

galaxies: structure - galaxies: dark matter - galaxies: statistics

References

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