Luis Raul Weber Abramo.

Biblioteca municipal do sistema da Prefeitura de São Paulo, dedicada à divulgação científica e atividades afins

Cosmological applications of galaxy surveys depend on the dentification of sources and extraction of properties such as the redshifts of galaxies. We will study the combination of LSST data with different tracers (galaxies, quasars, intensity mapping) and even other messengers. In particular, we plan on combining LSST observations with a variety of other data sets, in particular (1) narrow-band surveys such as S-PLUS, J-PAS and J-PLUS; and (2) observations from present (LIGO-Virgo-Kagra) and future (Einstein Telescope and Cosmis Explorer) gravitational wave detectors. These multiple tracers will serve two goals: on one hand, we want to study large-scale effects that can only be measured on extremely large (angular or radial) distances. On the other hand, we will use these multiple tracers in order to better understand the connection between them and the halos they inhabit the so-called galaxy-halo connection.

This is a 4-year bilateral project between Brazil (FAPESP) and France (Agence National de Recherche, ANR). I am the coordinator in Brazil, and the coordinator in France is Dr. Matthew Pieri. FAPESP is investing R$ 400k , and ANR is investing EUR 400k.

WEAVE-QSO and J-PAS are two large astrophysical surveys active from 2022 to 2029, on two major observatories, supported by two international collaborations: WEAVE-QSO (European) and J-PAS (mainly Brazilian-Spanish). These two surveys are partners towards a common goal: cosmology and galaxy formation in the first half of the history of the universe using data of unprecedented quality and size. J-PAS does this by performing imaging in 56 colours and WEAVE-QSO follows this up with spectroscopy. The exploitation of this data presents a variety of challenges and opportunities that we seek to address through machine learning. In some cases, the first steps have been undertaken and preliminary results are already available, while in other cases the projects are in the cradle. The leads of these surveys propose to pool the expertise of the partners and bring together innovative methods for the fullest exploitation of our large common data set.

Projeto Temático FAPESP, 2019/26492-3. Coordenadora: Claudia L. Mendes de Oliveira

Projeto Regular de Pesquisa FAPESP - 2018/04683-9

Projeto de Auxilio Regular à Pesquisa FAPESP, Processo No. 2015/17199-0

Large galaxy surveys, either spectroscopic or photometric, are changing the landscape of Astronomy, since they are the best strategy to understand one of the most profound mysteries of contemporary cosmology: the nature of dark energy, the dominant component of the Universe, responsible for the acceleration of its expansion. From a cosmological perspective, galaxy redshift surveys are necessary to build 3-D maps of the galaxy distribution, which can then be used to estimate cosmological parameters through statistical studies of features imprinted in this distribution. The nature of dark energy is actually only one of the many scientific challenges that may be pursued with large surveys. In fact, as exemplified by the Sloan Digital Sky Survey (SDSS), which is regarded as the most productive project of all time in Astronomy, galaxy redshift or photometric surveys are powerful tools to study from asteroids in the Solar System to our own Galaxy, from galaxy evolution to the large-scale structures of the Universe. Indeed, large galaxy surveys are the most efficient way (if not the only one) to approach properly some of the big challenges of contemporary astronomy. At present, we are currently participating in the design of two new surveys: the Javalambre Physics of the Accelerating Universe Astrophysical Survey (J-PAS) and the Prime Focus Spectrograph for the Subaru Measurement of Images and Redshifts survey (PFS/SuMIRe ). Their potential is enormous from both the scientific and technological point of view. We already have graduate students and post-docs developing projects which have these surveys in mind. We also have strongparticipation in the development of instruments for these surveys: the panoramic CCD camera of J-PAS and the optical fiber sub-system for PFS/SuMIRe. The objective of this Thematic Project is twofold: i) to consolidate our scientific work with galaxy surveys, and ii) to obtain the funding in order to build the optical fiber sub-system of the PFS/SuM

Understanding how galaxies form and evolve remains one of the most significant problems in Astrophysics. To meet this challenge, our group has developed a technique of spectral synthesis, the empirical population synthesis, which allows to identify the dominant stellar populations of galaxies from the analysis of their spectra. This technique is suitable for the analysis of data produced by large surveys that cover large areas on the sky and that became essential tools to efficiently address several problems of contemporary astrophysics and cosmology. We have applied this technique to SDSS data, examining several properties of the galaxy population from studies involving nearly a million spectra. In this project we wish to extend our empirical synthesis approach to high redshift and actively participate in the design and implementation of two new spectroscopic and photometric surveys, J-PAS (Javalambre Physics of the Accelerating Universe Survey) and SuMIRe (Subaru Measurement of Images and Redshifts). The latter will be conducted with the aid of a new spectrograph, the PFS (Prime Focus Spectrograph), in which construction we were invited to participate. Our goal with this project is to obtain resources to enable the effective development of these activities and, especially, allow us to develop a preliminary study of a PFS sub-system called FOCCOS, involving the optical fibres and their connectors, which will provide the optical interface between the telescope and the spectrograph. Although the main objective of these two surveys is the study of dark energy, they must bring invaluable contributions to several areas of modern astronomy, including galaxy evolution.

J-PAS (Javalambre Physics of the Accelerating Universe Astrophysical Survey) is a large-area medium-band optical survey that will map > 200 million galaxies, millions of quasars, thousands of Supernovas and many other types of solar system, galactic and extragalactic objects. One of the main aims of J-PAS is to measure the expansion rate of the Universe using the baryonic acoustic oscillation (BAO) features to percent-level accuracy. The goal is for this project to become the first Stage III/Stage IV astrophysical survey (in the nomenclature of the Dark Energy Task Force, Albrecht et al. 2009).
I have been involved since the inception of the brazilian project to build the cameras for J-PAS, and I am presently one of the Coordinators (together witl N. Benítez and R. Dupke) of the Observational Cosmology Working Group (which coordinates the work of many Science Working Groups). I am also actively involved with the Science Working Groups on Theoretical Cosmology, on Supernovas, and on Quasars & AGNs.
In Spain, J-PAS is supported by CSIC, CEFCA and the State Government of Aragón. In Brazil, J-PAS is supported by MCT/ON, FINEP, FAPESP (Proc. 2010/17649-1, 2011/18729-1 and 2012/00800-4) and FAPERJ.

This grant served to finance a long visit (1 month) by Dr. Patrick Peter, of the Institut D'Astrophysique de Paris (IAP).

Instituto Nacional de Ciencia e Tecnologia em Astrofísica - uma rede de 144 pesquisadores. 
A missão do INCT-A é inserir a astronomia brasileira no futuro da astronomia mundial.. 
Coordenador: João Evangelista Steiner
Financiador(es): Conselho Nacional de Desenvolvimento Científico e Tecnológico - Auxílio financeiro / Fundação de Amparo à Pesquisa do Estado de São Paulo - Auxílio financeiro.

This was a grant for my group, to study the phenomenology of dark energy models.

We developed a numerical code (Q-CMBFAST) based on the existing code by Seljak & Zaldarriaga (1996) to compute the CMB anisotropies in generalized dark energy models. We also developed tools to study the observational constraints from experiments such as WMAP and Planck.