H i as a probe of the large-scale structure in the post-reionization universe
2010 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 407, no 1, 567-580 p.Article in journal (Refereed) Published
We model the distribution of neutral hydrogen (H i) in the post-reionization universe. This model uses gravity-only N-body simulations and an ansatz to assign H i to dark matter haloes that is consistent with observational constraints and theoretical models. We resolve the smallest haloes that are likely to host H i in the simulations; care is also taken to ensure that any errors due to the finite size of the simulation box are small. We then compute the smoothed one-point probability distribution function and the power spectrum of fluctuations in H i. This is compared with other predictions that have been made using different techniques. We highlight the significantly high bias for the H i distribution at small scales. This aspect has not been discussed before. We then discuss the prospects of the detection with the Murchison Widefield Array (MWA), Giant Meterwave Radio Telescope (GMRT) and the hypothetical MWA5000. The MWA5000 can detect visibility correlations at large angular scales at all redshifts in the post-reionization era. The GMRT can detect visibility correlations at lower redshifts; specifically there is a strong case for a survey at z similar or equal to 1.3. We also discuss prospects for direct detection of rare peaks in the H i distribution using the GMRT. We show that direct detection should be possible with an integration time that is comparable to, or even less than, the time required for a statistical detection. Specifically, it is possible to make a statistical detection of the H i distribution by measuring the visibility correlation and direct detection of rare peaks in the H i distribution at z similar or equal to 1.3 with the GMRT in less than 1000 h of observations.
Place, publisher, year, edition, pages
2010. Vol. 407, no 1, 567-580 p.
methods: numerical, galaxies: evolution, galaxies: ISM, large-scale structure of Universe, radio lines: galaxies
Astronomy, Astrophysics and Cosmology
IdentifiersURN: urn:nbn:se:su:diva-49449DOI: 10.1111/j.1365-2966.2010.16933.xISI: 000281140900047OAI: oai:DiVA.org:su-49449DiVA: diva2:378359
authorCount :32010-12-152010-12-142011-04-18Bibliographically approved