Program

SCHEDULE
August 13
08h00 - 08h30 Registration
08h30 - 09h00 Opening ceremony
09h00 – 10h15 Yin-Zhe Ma
10h15 – 11h15 Coffee-break + posters
11h15 – 12h30 Marta Silva
12h30 – 14h00 Lunch
14h00 – 15h15 Jeff Petterson
15h15 - 16h00 Coffee-break + posters
16h00 - 17h15 Filipe Abdalla (Hands-on)
August 14
09h00 – 10h15 Jeff Petterson
10h15 – 11h15 Coffee-break + posters
11h15 – 12h30 Marta Silva
12h30 – 14h00 Lunch
14h00 – 15h15 Filipe Abdalla (Hands-on)
15h15 - 16h00 Coffee-break + posters
16h00 - 17h15 Yin-Zhe Ma
August 15
09h00 – 10h15 Marta Silva
10h15 – 11h15 Coffee-break + posters
11h15 – 12h30 Jeff Petterson
12h30 – 14h00 Lunch
14h00 - 14h40 Invited talk
14h40 - 15h20 Invited talk
15h20 - 16h00 Invited talk
16h00 - 17h00 Coffee-break + posters + discussions
August 16
09h00 – 10h15 Filipe Abdalla (Hands-on)
10h15 – 11h15 Coffee-break + posters
11h15 – 12h30 Yin-Zhe Ma
12h30 – 14h00 Lunch
14h00 - 16h00 Discussion / closing remarks
16h00 - 17h00 Final coffee-break


Jeff Peterson

Jeff Peterson

I will describe the thermal history of hydrogen gas from recombination to reionization., probed by its 21-cm emission line. I will explain how 21-cm all-sky and imaging experiments use this line to study cosmic history of the first stars, galaxies, X-ray sources and large scale structure.

Yin-Zhe Ma

Yin-Zhe Ma

This leture will cover 21-cm cosmology aspects. 21-cm mean temperature and introduction to perturbation theory;, then we will proceed to the relativistic perturbation to 21-cm brightness temperature. Finally, we will cover how to measure BAO from CMB and 21-cm from observations.

Marta Silva

Marta Silva

The first stars formed during the Cosmic Dawn heated the intergalactic medium (IGM) above the cosmic microwave background (CMB). Later, during the Epoch of Reionization (EoR), the radiation from the first galaxies ionized the intergalactic medium. The reionization process was the last major phase transition in our Universe and had a large impact on the subsequent galaxy formation and evolution. The 21cm line from neutral hydrogen is a direct probe of the state of the IGM in the early Universe. Therefore, this transition line is the target of multiple Cosmic Dawn missions which plan to detect this signal in absorption and of EoR missions which are competing for a first statistics detection of the signal in emission. The second generation of 21cm line missions/experiments is being planned with the aim to model the evolution of the signal amplitude and spectral fluctuations and finally to map the 3D reionization field. I will describe the physics driving the 21cm line signal and the multiple efforts for modeling the 21cm line amplitude and spatial fluctuations during the Cosmic Dawn and the EoR. Furthermore, I will discuss the several current missions targetting the high redshift Universe and aiming to probe the reionization process and the sources of ionizing radiation.

Filipe Abdalla

Filipe Abdalla

Bayesian statistics is a very important tool to the cosmologist and the radio astronomer. The examples of uses of Bayesian statistics are fast in this field. For example: the determination of the maps which reveal the large scale structure of the Universe, the determination of Cosmological parameters or the detection of sources in radio images all can be optimal performed when a model is tested via the Bayesian framework. All of these ingredients are needed when testing a cosmological model. I will review the background of Bayesian statistics and its applications to cosmology. I will also review the methodology which allows us to solve some these problems in a Bayesian framework. We will review publicly available software which can be used in the above problems.

Publicado Por: INPE
Última Modificação: Jul 16, 2018 12h05