What Next-Generation 21 cm Power Spectrum Measurements Can Teach Us About the Epoch of Reionization

Дата и время публикации : 2013-10-25T20:01:24Z

Авторы публикации и институты :
Jonathan C. Pober
Adrian Liu
Joshua S. Dillon
James E. Aguirre
Judd D. Bowman
Richard F. Bradley
Chris L. Carilli
David R. DeBoer
Jacqueline N. Hewitt
Daniel C. Jacobs
Matthew McQuinn
Miguel F. Morales
Aaron R. Parsons
Max Tegmark
Dan J. Werthimer

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 24 pages, 17 figures, submitted to ApJ
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO

Краткий обзор статьи: A number of experiments are currently working towards a measurement of the 21 cm signal from the Epoch of Reionization. Whether or not these experiments deliver a detection of cosmological emission, their limited sensitivity will prevent them from providing detailed information about the astrophysics of reionization. In this work, we consider what types of measurements will be enabled by a next-generation of larger 21 cm EoR telescopes. To calculate the type of constraints that will be possible with such arrays, we use simple models for the instrument, foreground emission, and the reionization history. We consider an instrument modeled after the $sim 0.1 rm{km}^2$ collecting area Hydrogen Epoch of Reionization Array (HERA) concept design, and parameterize the uncertainties with regard to foreground emission by considering different limits to the recently described "wedge" footprint in $k$-space. Uncertainties in the reionization history are accounted for using a series of simulations which vary the ionizing efficiency and minimum virial temperature of the galaxies responsible for reionization, as well as the mean free path of ionizing photons through the IGM. Given various combinations of models, we consider the significance of the possible power spectrum detections, the ability to trace the power spectrum evolution versus redshift, the detectability of salient power spectrum features, and the achievable level of quantitative constraints on astrophysical parameters. Ultimately, we find that $0.1 rm{km}^2$ of collecting area is enough to ensure a very high significance ($gtrsim30sigma$) detection of the reionization power spectrum in even the most pessimistic scenarios. This sensitivity should allow for meaningful constraints on the reionization history and astrophysical parameters, especially if foreground subtraction techniques can be improved and successfully implemented.

Category: Physics