Astrophysics and Observational Cosmology with Galaxy Clusters.
Grant number: | 22/16790-0 |
Support Opportunities: | Scholarships in Brazil - Scientific Initiation |
Start date until: | April 01, 2023 |
End date until: | December 31, 2023 |
Field of knowledge: | Physical Sciences and Mathematics - Astronomy - Extragalactic Astrophysics |
Principal Investigator: | Luis Raul Weber Abramo |
Grantee: | Victor Roberto Soares da Silva |
Host Institution: | Instituto de Física (IF). Universidade de São Paulo (USP). São Paulo , SP, Brazil |
Abstract The $H_0$ problem is the present tension between local (direct) measurementes of the Hubble-Lemaître parameter, and high-redshift (indirect) measurements.The so-called ``$H_0$ tension'' is becoming one of the main challenges (perhaps even an embarassment) of modern cosmology.In this Scientific Initiation project the student will first get started on the basics of Relativistic Cosmology.After this initial, formative phase, the student will acquire a deeper understanding about the local measurements of $H_0$ by means of standard candles and the ``cosmic distance ladder''. In the next phase, the student will learn about the Cosmic Microwave Background radiation (CMB), to the extent that he understands how that observable can also constrain the Hubble parameter, with a precision even greater than the local measurements.In particular, the student must be able to compute $\theta_{dec}$, the angular scale of the acoustic horizon at matter/radiation decoupling (around $z\simeq 1089$), which is one of the most precisely determined parameters from the CMB, and which constrains rather strongly the history of cosmic expansion before and after decoupling.At a later stage, the student will learn how the observations of electromagnetic counterparts of gravitational wave events, such as neutron star-neutron star collisions (Kilonovas), can also serve as a type of standard candle that constrains the value of the expansion rate.In the final phase of the project the student will determine, on his own, how the $H_0$ tension can be alleviated in some scenarios, such as, e.g., the {\it Early Dark Energy} (EDE) models. | |
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