Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos

By Andrey V. Kravtsov, A. Vikhlinin, Alexander Meshscheryakov. Astronomy letters, 2014

186 citations recorded by the source corpus.

We study relation between stellar mass and halo mass for high-mass halos using a sample of galaxy clusters with accurate measurements of stellar masses from optical and ifrared data and total masses from X-ray observations. We find that stellar mass of the brightest cluster galaxies (BCGs) scales as M*,BCG ∝ M500αBCG with the best fit slope of αBCG ≈ 0.4 ± 0.1. We measure scatter of M*,BCG at a fixed M500 of ≈0.2 dex. We show that stellar mass-halo mass relations from abundance matching or halo modelling reported in recent studies underestimate masses of BCGs by a factor of ∼2−4. We argue that this is because these studies used stellar mass functions (SMF) based on photometry that severely underestimates the outer surface brightness profiles of massive galaxies. We show that M*−M relation derived using abundance matching with the recent SMF calibration by Bernardi et al. (2013) based on improved photometry is in a much better agreement with the relation we derive via direct calibration for observed clusters. The total stellar mass of galaxies correlates with total mass M500 with the slope of ≈0.6 ± 0.1 and scatter of 0.1 dex. This indicates that efficiency with which baryons are converted into stars decreases with increasing cluster mass. The low scatter is due to large contribution of satellite galaxies: the stellar mass in satellite galaxies correlates with M500 with scatter of ≈0.1 dex and best fit slope of αsat ≈ 0.8 ± 0.1. We show that for a fixed choice of the initial mass function (IMF) total stellar fraction in clusters is only a factor of 3−5 lower than the peak stellar fraction reached in M ≈ 1012M⊙ halos. The difference is only a factor of ∼1.5−3 if the IMF becomes progressively more bottom heavy with increasing mass in early type galaxies, as indicated by recent observational analyses. This means that the overall efficiency of star formation in massive halos is only moderately suppressed compared to L* galaxies and is considerably less suppressed than previously thought. The larger normalization and slope of the M*−M relation derived in this study shows that feedback and associated suppression of star formation in massive halos should be weaker than assumed in most of the current semi-analytic models and simulations.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/32957ca75c1851f8438ed02f41083af3e9b1f660

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Citations in the corpus

The Romulus cosmological simulations: a physical approach to the formation, dynamics and accretion models of SMBHs (2016, methodology): “…galaxies with stellar masses less than 108 M , a regime where the observed luminosity function is not well constrained (Anderson et al. 2017). et al. (2013), which our model has been calibrated to reproduce, as well as Kravtsov et al. (2014) for halos spanning more than three decades in mass.”
Simulating galaxy formation with black hole driven thermal and kinetic feedback (2016, result): “At the high halo-mass end, the data shown here are in reasonable agreement with Kravtsov et al. (2014) who pointed out the importance of outer stellar profiles in high-mass haloes in this type of analysis.”
First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies (2017, methodology): “1011M in stellar mass, above this limit our preliminary comparisons to observational data indicates that the TNG relation between centrals stellar mass (< 30 kpc) and halo mass at z = 0 is steeper than the one inferred by e.g. Kravtsov et al. (2014).”
EMERGE – an empirical model for the formation of galaxies since z ∼ 10 (2017, methodology): “While the SMFs, sSFRs, and the CSFRD are still reproduced very well, this new addition significantly improves the fit to the quenched fractions of low-mass galaxies, as low-mass satellites keep forming stars longer.”
NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time (2015, methodology): “2013; Kravtsov et al. 2014), and hence our halo contraction is not due to unphysical overcooling as it happened in older simulations (e.g. Gnedin et al. 2004) and it is consistent with recent results from other groups on the same mass scale (Schaller et al. 2015).”