Galaxy And Mass Assembly (GAMA): The galaxy stellar mass function to $z=0.1$ from the r-band selected equatorial regions

Abstract

We derive the low redshift galaxy stellar mass function (GSMF), inclusive of dust corrections, for the equatorial Galaxy And Mass Assembly (GAMA) dataset covering 180 deg${}^2$. We construct the mass function using a density-corrected maximum volume method, using masses corrected for the impact of optically thick and thin dust. We explore the galactic bivariate brightness plane ($M_{\star }-\mu$), demonstrating that surface brightness effects do not systematically bias our mass function measurement above 10${}^{7.5}$ M${}_{\odot }$. The galaxy distribution in the $M-\mu$-plane appears well bounded, indicating that no substantial population of massive but diffuse or highly compact galaxies are systematically missed due to the GAMA selection criteria. The GSMF is {fit with} a double Schechter function, with ${\mathcal{M}}^{\star }=10^{10.78\pm 0.01\pm 0.20}{M}_{\odot }$, ${\varphi }_1^{\star }=(2.93\pm 0.40)\times 10^{-3}{h}_{70}^3$Mpc${}^{-3}$, ${\alpha }_1=-0.62\pm 0.03\pm 0.15$, ${\varphi }_2^{\star }=(0.63\pm 0.10)\times 10^{-3}{h}_{70}^3$Mpc${}^{-3}$, and ${\alpha }_2=-1.50\pm 0.01\pm 0.15$. We find the equivalent faint end slope as previously estimated using the GAMA-I sample, although we find a higher value of ${\mathcal{M}}^{\star }$. Using the full GAMA-II sample, we are able to fit the mass function to masses as low as $10^{7.5}$ $M_{\odot }$, and assess limits to $10^{6.5}$ $M_{\odot }$. Combining GAMA-II with data from G10-COSMOS we are able to comment qualitatively on the shape of the GSMF down to masses as low as $10^6$ $M_{\odot }$. Beyond the well known upturn seen in the GSMF at $10^{9.5}$ the distribution appears to maintain a single power-law slope from $10^9$ to $10^{6.5}$. We calculate the stellar mass density parameter given our best-estimate GSMF, finding ${\Omega }_{\star }=1.66_{-0.23}^{+0.24}\pm 0.97h_{70}^{-1}\times 10^{-3}$, inclusive of random and systematic uncertainties.

arXiv comment22 pages; 15 figures; Accepted for publication in MNRAS

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