no code implementations • 13 Apr 2020 • Abhik Ghosh, Florent Mertens, Gianni Bernardi, Mário G. Santos, Nicholas S. Kern, Christopher L. Carilli, Trienko L. Grobler, Léon V. E. Koopmans, Daniel C. Jacobs, Adrian Liu, Aaron R. Parsons, Miguel F. Morales, James E. Aguirre, Joshua S. Dillon, Bryna J. Hazelton, Oleg M. Smirnov, Bharat K. Gehlot, Siyanda Matika, Paul Alexander, Zaki S. Ali, Adam P. Beardsley, Roshan K. Benefo, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Carina Cheng, Paul M. Chichura, David R. DeBoer, Eloy de Lera Acedo, Aaron Ewall-Wice, Gcobisa Fadana, Nicolas Fagnoni, Austin F. Fortino, Randall Fritz, Steve R. Furlanetto, Samavarti Gallardo, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Jack Hickish, Alec Josaitis, Austin Julius, Amy S. Igarashi, MacCalvin Kariseb, Saul A. Kohn, Matthew Kolopanis, Telalo Lekalake, Anita Loots, David MacMahon, Lourence Malan, Cresshim Malgas, Matthys Maree, Zachary E. Martinot, Nathan Mathison, Eunice Matsetela, Andrei Mesinger, Abraham R. Neben, Bojan Nikolic, Chuneeta D. Nunhokee, Nipanjana Patra, Samantha Pieterse, Nima Razavi-Ghods, Jon Ringuette, James Robnett, Kathryn Rosie, Raddwine Sell, Craig Smith, Angelo Syce, Max Tegmark, Nithyanandan Thyagarajan, Peter K. G. Williams, Haoxuan Zheng
The key challenge in the observation of the redshifted 21-cm signal from cosmic reionization is its separation from the much brighter foreground emission.
Cosmology and Nongalactic Astrophysics
no code implementations • 6 Feb 2020 • Anson D'Aloisio, Matthew McQuinn, Hy Trac, Christopher Cain, Andrei Mesinger
The clumping factor of ionized gas (proportional to the recombination rate) rises to a peak value of $5-20$ approximately $\Delta t = 10$ Myr after ionization front passage, depending on the incident intensity, redshift, and degree to which the gas had been pre-heated by the first X-ray sources.
Cosmology and Nongalactic Astrophysics Astrophysics of Galaxies
2 code implementations • 7 May 2018 • Nicolas Gillet, Andrei Mesinger, Bradley Greig, Adrian Liu, Graziano Ucci
The 21-cm power spectrum (PS) has been shown to be a powerful discriminant of reionization and cosmic dawn astrophysical parameters.
Cosmology and Nongalactic Astrophysics
no code implementations • 5 Jan 2018 • Bradley Greig, Andrei Mesinger
Using the light-cone version of 21CMMC, we quantify the biases in the recovered astrophysical parameters if we use the 21cm power spectrum from the co-evolution approximation to fit a 3D light-cone mock observation.
Cosmology and Nongalactic Astrophysics
no code implementations • 9 May 2017 • Bradley Greig, Andrei Mesinger
The cosmic 21 cm signal is set to revolutionise our understanding of the early Universe, allowing us to probe the 3D temperature and ionisation structure of the intergalactic medium (IGM).
Cosmology and Nongalactic Astrophysics Astrophysics of Galaxies
no code implementations • 26 Jan 2015 • Bradley Greig, Andrei Mesinger
As an example, combining three observations (z=8, 9 and 10) of the 21 cm power spectrum with a conservative noise estimate and uniform model priors, we find that interferometers with specifications like the Low Frequency Array/Hydrogen Epoch of Reionization Array (HERA)/Square Kilometre Array 1 (SKA1) can constrain common reionization parameters: the ionizing efficiency (or similarly the escape fraction), the mean free path of ionizing photons and the log of the minimum virial temperature of star-forming haloes to within 45. 3/22. 0/16. 7, 33. 5/18. 4/17. 8 and 6. 3/3. 3/2. 4 per cent, ~$1\sigma$ fractional uncertainty, respectively.
Cosmology and Nongalactic Astrophysics
1 code implementation • 19 Mar 2010 • Andrei Mesinger, Steven Furlanetto, Renyue Cen
We introduce a powerful semi-numeric modeling tool, 21cmFAST, designed to efficiently simulate the cosmological 21-cm signal.
Cosmology and Nongalactic Astrophysics
no code implementations • 9 Apr 2007 • Andrei Mesinger, Steven Furlanetto
We also generate maps and power spectra of 21-cm brightness temperature fluctuations, which for the first time include corrections due to gas bulk velocities.
