The growth of the first galaxies

Duncan, Kenneth James (2015) The growth of the first galaxies. PhD thesis, University of Nottingham.

[img]
Preview
PDF (Thesis - as examined) - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Download (15MB) | Preview

Abstract

This thesis explores the growth of galaxies during the first few billion years of galaxy formation and their potential role as the sources which powered the process of reionization. The data used throughout the thesis is taken from the Cosmic Assembly Near-infrared Extragalactic Legacy Survey (CANDELS).

First, we measure new estimates for the galaxy stellar mass function and star formation rates for samples of galaxies at z ~ 4, 5, 6 &7 using data in the CANDELS GOODS South field. The deep near-infrared observations allow us to construct the stellar mass function at z > 6 directly for the first time. We estimate stellar masses for our sample by fitting the observed spectral energy distributions with synthetic stellar populations, including the contributions from nebular line and continuum emission. The observed UV luminosity functions for the samples are consistent with previous observations, however we find that the observed M(UV) - stellar mass relation has a shallow slope more consistent with a constant mass to light ratio and a normalisation which evolves with redshift.

We observe stellar mass functions which have steep low-mass slopes (alpha ~ -1.9), steeper than previously observed at these redshifts and closer to that of the UV luminosity function. Integrating our new mass functions, we find the observed stellar mass density evolves from log10(rho) = 6.64 +0.58/-0.89 at z ~ 7 to 7.36 +/- 0.06 solar masses per Mpc^-3 at z ~ 4. Combining the measured UV continuum slopes (beta) with their rest-frame UV luminosities, we calculate dust corrected star-formation rates (SFR) for our sample. We find the specific star-formation rate for a fixed stellar mass increases with redshift whilst the global SFR density falls rapidly over this period. Our new SFR density estimates are higher than previously observed at this redshift.

Next, we utilise the same dataset to test a new method for estimating the merger fraction of galaxies in photometric surveys. Using a probabilistic method for estimating close galaxy pairs using photometric redshift probability distributions, we estimate the merger fraction of galaxies at z > 2. For projected separations of 5 <= r <= 20 kpc and 5 <= r <= 30 kpc we measure the merger fraction for mass selected samples of log(M) > 9.5 and log(M)> 10 and merger ratios of 1:4 or less (major mergers).

For assumed merger timescales based on hydrodynamical simulations, we estimate the average time between mergers per galaxy (Gamma, Gyr) and the comoving merger rate (R, /Gyr/Mpc^-3). Over the redshift range 2 < z < 4 we find that the average time between mergers per galaxy is approximately constant. Compared to the star-formation rates measured for galaxies at these masses, we conclude that star-formation is the dominant form of growth (by a factor ~10 times) during this epoch. Although we find that the methodology performs well at z ~ 4, more data is required to make robust estimations of the merger fraction at z ~5 or z ~ 6. Similarly, tighter constraints on the observed stellar mass functions are required before we can draw meaningful conclusions from the observed comoving merger rates.

Finally, we present a new analysis of the ionizing emissivity (N_ion, /s/Mpc^-3 for galaxies during the epoch of reionization and their potential for completing and maintaining reionization. We use extensive SED modelling -- incorporating two plausible mechanisms for the escape of Lyman continuum photon -- to explore the range and evolution of ionizing efficiencies consistent with new results on galaxy colours (beta) during this epoch. We estimate N_ion for the latest observations of the luminosity and star-formation rate density at z < 10, outlining the range of emissivity histories consistent with our new model.

Given the growing observational evidence for a UV colour-magnitude relation in high-redshift galaxies, we find that for any plausible evolution in galaxy properties, red (brighter) galaxies are less efficient at producing ionizing photons than their blue (fainter) counterparts. The assumption of a redshift and luminosity evolution in beta leads to two important conclusions. Firstly, the ionizing efficiency of galaxies naturally increases with redshift.

Secondly, for a luminosity dependent ionizing efficiency, we find that galaxies down to a rest-frame magnitude of M_uv ~ -15 alone can potentially produce sufficient numbers of ionizing photons to maintain reionization as early as z ~ 8 for a clumping factor of C = 3.

Item Type: Thesis (University of Nottingham only) (PhD)
Supervisors: Conselice, Christopher
Almaini, Omar
Subjects: Q Science > QB Astronomy
Faculties/Schools: UK Campuses > Faculty of Science > School of Physics and Astronomy
Item ID: 30609
Depositing User: Duncan, Kenneth
Date Deposited: 14 Jan 2016 11:32
Last Modified: 26 Oct 2016 13:51
URI: http://eprints.nottingham.ac.uk/id/eprint/30609

Actions (Archive Staff Only)

Edit View Edit View