The Galaxy-Halo Connection for $1.5\lesssim z\lesssim 5$ as revealed by the \emph{Spitzer} Matching survey of the UltraVISTA ultra-deep Stripes

Abstract

The \emph{Spitzer} Matching Survey of the UltraVISTA ultra-deep Stripes (SMUVS) provides unparalleled depth at $3.6$ and $4.5$~$\mu$m over $\sim 0.66$~deg${}^2$ of the COSMOS field, allowing precise photometric determinations of redshift and stellar mass. From this unique dataset we can connect galaxy samples, selected by stellar mass, to their host dark matter halos for $1.5<z<5.0$, filling in a large hitherto unexplored region of the parameter space. To interpret the observed galaxy clustering we utilize a phenomenological halo model, combined with a novel method to account for uncertainties arising from the use of photometric redshifts. We find that the satellite fraction decreases with increasing redshift and that the clustering amplitude (e.g., comoving correlation length / large-scale bias) displays monotonic trends with redshift and stellar mass. Applying $\Lambda$CDM halo mass accretion histories and cumulative abundance arguments for the evolution of stellar mass content we propose pathways for the coevolution of dark matter and stellar mass assembly. Additionally, we are able to estimate that the halo mass at which the ratio of stellar to halo mass is maximized is $10^{12.5_{-0.08}^{+0.10}}$~M${}_{\odot }$ at $z\sim 2.5$. This peak halo mass is here inferred for the first time from stellar mass-selected clustering measurements at $z\gtrsim 2$, and implies mild evolution of this quantity for $z\lesssim 3$, consistent with constraints from abundance-matching techniques.

22 pages (14 pages in main body + appendices). 17 Figures. 3 Tables. Accepted for publication in ApJ

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• CONCERTO: High-fidelity simulation of millimeter line emissions of galaxies and [CII] intensity mapping
• The COSMOS-UltraVISTA stellar-to-halo mass relationship: new insights on galaxy formation efficiency out to $z\sim 5$
• Exploring the halo occupation of AGN using dark-matter cosmological simulations
• How to Optimally Constrain Galaxy Assembly Bias: Supplement Projected Correlation Functions with Count-in-cells Statistics
• First Identification of a CMB Lensing Signal Produced by $1.5$ Million Galaxies at $z\sim$4: Constraints on Matter Density Fluctuations at High Redshift
• The Spitzer Matching Survey of the UltraVISTA Ultra-deep Stripes (SMUVS): the Evolution of Dusty and Non-Dusty Galaxies with Stellar Mass at z=2-6
• The Subaru HSC Galaxy Clustering with Photometric Redshift I: Dark Halo Masses Versus Baryonic Properties of Galaxies at 0.3<z<1.4
• Bright Lyman $\alpha$ emitters among Spitzer SMUVS galaxies in the MUSE/COSMOS field
• How feedback shapes galaxies: an analytic model
• The Stellar-to-Halo Mass Ratios of Passive and Star-Forming Galaxies at z~2-3 from the SMUVS survey
• Tracing the galaxy-halo connection with galaxy clustering in COSMOS-Web from z = 0.1 to z ~ 12
• Accurate Modeling of the Projected Galaxy Clustering in Photometric Surveys: I. Tests with Mock Catalogs