The Galaxy Clustering Crisis in Abundance Matching

Abstract

Galaxy clustering on small scales is significantly under-predicted by sub-halo abundance matching (SHAM) models that populate (sub-)haloes with galaxies based on peak halo mass, $M_{\mathrm{peak}}$. SHAM models based on the peak maximum circular velocity, $V_{\mathrm{peak}}$, have had much better success. The primary reason $M_{\mathrm{peak}}$ based models fail is the relatively low abundance of satellite galaxies produced in these models compared to those based on $V_{\mathrm{peak}}$. Despite success in predicting clustering, a simple $V_{\mathrm{peak}}$ based SHAM model results in predictions for galaxy growth that are at odds with observations. We evaluate three possible remedies that could "save" mass-based SHAM: (1) SHAM models require a significant population of "orphan" galaxies as a result of artificial disruption/merging of sub-haloes in modern high resolution dark matter simulations; (2) satellites must grow significantly after their accretion; and (3) stellar mass is significantly affected by halo assembly history. No solution is entirely satisfactory. However, regardless of the particulars, we show that popular SHAM models based on $M_{\mathrm{peak}}$ cannot be complete physical models as presented. Either $V_{\mathrm{peak}}$ truly is a better predictor of stellar mass at $z\sim 0$ and it remains to be seen how the correlation between stellar mass and $V_{\mathrm{peak}}$ comes about, or SHAM models are missing vital component(s) that significantly affect galaxy clustering.

25 pages, 22 figures, submitted to MNRAS, comments welcome

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