Bayesian hierarchical modelling of the ${\mathrm{M}}_{\star }$-SFR relation from 1<z<6 in ASTRODEEP

Abstract

The Hubble Frontier Fields represent the opportunity to probe the high-redshift evolution of the main sequence of star-forming galaxies to lower masses than possible in blank fields thanks to foreground lensing of massive galaxy clusters. We use the BEAGLE SED-fitting code to derive stellar masses, ${\mathrm{M}}_{\star }=\log (M/{\mathrm{M}}_{\odot })$, SFRs, $\Psi =\log (\psi /{\mathrm{M}}_{\odot }{\mathrm{yr}}^{-1})$ and redshifts from galaxies within the ASTRODEEP catalogue. We fit a fully Bayesian hierarchical model of the main sequence over $1.25<z<6$ of the form $\Psi ={\alpha }_{9.7}(z)+\beta ({\mathrm{M}}_{\star }-9.7)+\mathcal{N}(0,{\sigma }^2)$ while explicitly modelling the outlier distribution. The redshift-dependent intercept at ${\mathrm{M}}_{\star }=9.7$ is parametrized as ${\alpha }_{9.7}(z)=\log [N(1+z{)}^{\gamma }]+0.7$. Our results agree with an increase in normalization of the main sequence to high redshifts that follows the redshift-dependent rate of accretion of gas onto dark matter halos with $\gamma =2.40_{-0.18}^{+0.18}$. We measure a slope and intrinsic scatter of $\beta =0.79_{-0.04}^{+0.03}$ and $\sigma =0.26_{-0.02}^{+0.02}$. We find that the sampling of the SED provided by the combination of filters (Hubble + ground-based Ks-band + Spitzer 3.6 and 4.5 $\mu \mathrm{m}$) is insufficient to constrain ${\mathrm{M}}_{\star }$ and $\Psi$ over the full dynamic range of the observed main sequence, even at the lowest redshifts studied. While this filter set represents the best current sampling of high-redshift galaxy SEDs out to $z>3$, measurements of the main sequence to low masses and high redshifts still strongly depend on priors employed in SED fitting (as well as other fitting assumptions). Future data-sets with JWST should improve this.

MNRAS published

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