Exploring the thermal state of the low-density intergalactic medium at z = 3 with an ultra-high signal-to-noise QSO spectrum

Rorai, A. and Becker, George D. and Haehnelt, Martin G. and Carswell, R.F. and Bolton, James S. and Cristiani, S. and D'Odorico, V. and Cupani, G. and Barai, P. and Calura, F. and Kim, T.-S. and Pomante, E. and Tescari, E. and Viel, Matteo (2016) Exploring the thermal state of the low-density intergalactic medium at z = 3 with an ultra-high signal-to-noise QSO spectrum. Monthly Notices of the Royal Astronomical Society, 466 (3). pp. 2690-2709. ISSN 1365-2966

[img]
Preview
PDF - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Download (3MB) | Preview

Abstract

At low densities, the standard ionization history of the intergalactic medium (IGM) predicts a decreasing temperature of the IGM with decreasing density once hydrogen (and helium) reionization is complete. Heating the high-redshift, low-density IGM above the temperature expected from photoheating is difficult, and previous claims of high/rising temperatures in low-density regions of the Universe based on the probability density function (PDF) of the opacity in Ly α forest data at 2 < z < 4 have been met with considerable scepticism, particularly since they appear to be in tension with other constraints on the temperature–density relation (TDR). We utilize here an ultrahigh signal-to-noise spectrum of the Quasi-stellar object HE0940-1050 and a novel technique to study the low opacity part of the PDF. We show that there is indeed evidence (at 90 per cent confidence level) that a significant volume fraction of the underdense regions at z ∼ 3 has temperatures as high or higher than those at densities comparable to the mean and above. We further demonstrate that this conclusion is nevertheless consistent with measurements of a slope of the TDR in overdense regions that imply a decreasing temperature with decreasing density, as expected if photoheating of ionized hydrogen is the dominant heating process. We briefly discuss implications of our findings for the need to invoke either spatial temperature fluctuations, as expected during helium reionization, or additional processes that heat a significant volume fraction of the low-density IGM.

Item Type: Article
Additional Information: © 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society
Keywords: intergalactic medium, quasars: absorption lines
Schools/Departments: University of Nottingham, UK > Faculty of Science > School of Physics and Astronomy
Identification Number: 10.1093/mnras/stw2917
Depositing User: Bolton, James
Date Deposited: 04 May 2017 14:24
Last Modified: 04 May 2017 23:50
URI: http://eprints.nottingham.ac.uk/id/eprint/42517

Actions (Archive Staff Only)

Edit View Edit View