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Epoch of Cosmic Reionization

In the framework of the hot big bang model, our Universe is expected to become almost neutral around 400,000 years after the big bang. On the other hand, we know from observations of quasar absorption spectra that the same Universe has become highly ionized by the time it is one Gigayear old. The reionization of the Universe is driven by radiation from first luminous sources (galaxies, stars, supermassive accreting black holes). Studying reionization will thus tell us how the first galaxies formed and how they looked like.

There are  various ongoing and planned observational projects probing various apsects of reionization.  One promising method is to detect the fluctuations in the neutral hydrogen density during the reionization era through its hyperfine transition using facilities like LOFAR, MWAGMRTCMA, HERASKA.

Researchers at IoA/KICC are using numerical simulations to study how reionization proceeds. The simulations are used to model the effect of reionization on the absorption spectra and the Lya emission from high-redshift QSOs and galaxies and to generate realistic maps of 21 cm emission arising from the hyperfine transition. The neutral hydrogen distribution before reionization is expected to be complex and patchy and is thus best modelled with numerical simulations. Since very little is known about the detailed physical processes at such early epochs, we have to make different assumptions and then verify the assumptions by comparing with the data. Hence, we generate maps for various scenarios and try to get an idea how to distinguish between them from the data. The figures below illustrate some of this work.

Figure 1: Radiative transfer simulation calibrated to fit Lya forest data at z<6 based on the Sherwood simulation suite post-processesed with the radiative transfer code ATON  (Kulkarni et al. 2018). The top panel shows  the neutral hydrogen fraction in  a  ‘light cone’ stretching from z=5 to z=8. The middle  panel shows the temperature of the Intergalactic Medium and the bottom panel shows the  hydrogen photo-ionization rate.

 

Figure 2: Simulations of the prominent near-zones in high-redshift QSO absorption spectra with the radiative transfer code RADAMESH  from Keating et al. (2015). The left panel shows mock absorption spectra for different assumptions of the neutral state of the surrounding IGM while the middle and right panel show the dependence of near-zone size on QSO lifetime and mass of the QSO host halo.

 

Figure 3: The left panel shows a high-resolution  simulation resolving the escape of ionising radiation from galaxies in a simulation with a realistic reionization history. The simulation was  performed with the RAMSES-RT code as part  of the SPHINX project (Rosdahl et al. 2018). The right two panels  show a comparison of CII and OIII observations from the ISM in galaxies during  the epoch of reionization  with ALMA (Carniani et al. 2017) with our Ramses RT simulations of such galaxies (Katz et al. 2017).  Observed and simulated galaxies show similar offsets between  CII and OIII emission. In the simulation CII is tracing star forming  regions while  (some of the) OIII is produced by collisional ionised gas  expelled from star forming regions by supernova feedback which causes the spatial offset.

 

Figure 4: The three light cones on the left contrast the evolution of the 21cm brightness for models where hydrogen reionization is driven by QSOs with models where hydrogen reionization is driven by galaxies for two different reionization histories. The three panels on the right show the evolution of the 21cm power spectrum for the three models (Kulkarni et al. 2017). Note the much larger 21cm signal in the model where reionization is driven by QSOs (solid coloured curves, galaxies are in black) that should soon be in reach of LOFAR, HERA and perhaps MWA.

Through the tight links with the Battcock Centre for Experimental Astrophysics, research in this area at KICC is tightly linked to major 21cm reionization projects such as HERA and SKA.

People involved in this area are:

References
Carniani et al. , 2017, A&A, 605, 42
Katz et al., 2017, MNRAS, 468, 4831
Keating L. C., Haehnelt M.G., Cantalupo S., Puchwein E., 2015, MNRAS, 454, 681
Kulkarni G., Keating L.C., Haehnelt M.G., Bosman S E.I.,Puchwein E.,  Chardin J.,  Aubert D., submitted to MNRAS, arXiv1809.0637
Kulkarni G., Choudhury T. R., Puchwein E., Haehnelt M.G., 2017, MNRAS, 469, 4283
Rosdahl J.et al. , 2018,  arXiv:180107259