41 research outputs found
Constraining the contribution of active galactic nuclei to reionization
Recent results have suggested that active galactic nuclei (AGN) could provide
enough photons to reionise the Universe. We assess the viability of this
scenario using a semi-numerical framework for modeling reionisation, to which
we add a quasar contribution by constructing a Quasar Halo Occupation
Distribution (QHOD) based on Giallongo et al. observations. Assuming a constant
QHOD, we find that an AGN-only model cannot simultaneously match observations
of the optical depth , neutral fraction, and ionising emissivity. Such
a model predicts too low by relative to Planck
constraints, and reionises the Universe at . Arbitrarily
increasing the AGN emissivity to match these results yields a strong mismatch
with the observed ionising emissivity at . If we instead assume a
redshift-independent AGN luminosity function yielding an emissivity evolution
like that assumed in Madau & Haardt model, then we can match albeit
with late reionisation, however such evolution is inconsistent with
observations at and poorly motivated physically. These results
arise because AGN are more biased towards massive halos than typical reionising
galaxies, resulting in stronger clustering and later formation times.
AGN-dominated models produce larger ionising bubbles that are reflected in
more 21cm power on all scales. A model with equal parts galaxies
and AGN contribution is still (barely) consistent with observations, but could
be distinguished using next-generation 21cm experiments HERA and SKA-low. We
conclude that, even with recent claims of more faint AGN than previously
thought, AGN are highly unlikely to dominate the ionising photon budget for
reionisation.Comment: 16 pages, 9 figures, matches the accepted version for publication in
MNRAS, 201
Epoch of reionization 21 cm forecasting from MCMC-constrained semi-numerical models
The recent low value of Planck (2016) integrated optical depth to Thomson
scattering suggests that the reionization occurred fairly suddenly, disfavoring
extended reionization scenarios. This will have a significant impact on the
21cm power spectrum. Using a semi-numerical framework, we improve our model
from Hassan et al. (2016) to include time-integrated ionisation and
recombination effects, and find that this leads to more sudden reionisation. It
also yields larger HII bubbles which leads to an order of magnitude more 21cm
power on large scales, while suppressing the small scale ionization power.
Local fluctuations in the neutral hydrogen density play the dominant role in
boosting the 21cm power spectrum on large scales, while recombinations are
subdominant. We use a Monte Carlo Markov Chain approach to constrain our model
to observations of the star formation rate functions at z = 6,7,8 from Bouwens
et al. (2015), the Planck (2016) optical depth measurements, and the Becker &
Bolton (2013) ionising emissivity data at z~5. We then use this constrained
model to perform 21cm forecasting for LOFAR, HERA, and SKA in order to
determine how well such data can characterise the sources driving reionisation.
We find that the 21cm power spectrum alone can somewhat constrain the halo mass
dependence of ionising sources, the photon escape fraction and ionising
amplitude, but combining the 21cm data with other current observations enables
us to separately constrain all these parameters. Our framework illustrates how
21cm data can play a key role in understanding the sources and topology of
reionisation as observations improve.Comment: 20 pages, 16 figues, matches the accepted version for publication in
MNRA