Moderadores
Wednesday morning
- Eusebio Sánchez Álvaro (CIEMAT)
Materiales de la presentación
A generic modified gravity theory, that generates a dynamical dark energy, will produce a different evolution at the background level, determined by the DE equation of state, as well as different cosmological perturbations with respect to LCDM. An effect that is completely general to modified gravity models is that the propagation of tensor perturbations is modified so that it emerges a notion...
The PAU Survey (PAUS) is an innovative photometric survey with 40 narrow bands at the William Herschel Telescope (WHT). The narrow bands are spaced at 100A intervals covering the range 4500A to 8500A and, in combination with standard broad bands, enable excellent redshift precision. Using BCNz2, a new photometric redshift code developed for this purpose, we characterise the photometric...
In this work we have considered the gravitational production as the mechanism responsible for the creation of dark matter during the early epochs of the Universe. This mechanism imposes some constrains in the parameter space of the candidate field as it abundance is bounded by the observations. We have considered the dark matter field as a scalar one not minimally coupled to gravity. The...
I will summarize the progress on image simulations on LSST-DESC and their relevance for next generation cosmological surveys.
Strong lenses are systems in which the light from a background source is deflected by a foreground galaxy or group of galaxies, resulting in multiple images of the background source. These images are also usually heavily distorted, acquiring the shape of rings or arcs. Study of these images provides us unique information about the distribution of matter (baryonic plus dark) within the...
The late time acceleration of the Universe can be characterized in terms of an extra, time dependent, component of the universe -- dark energy. The simplest proposal for dark energy is quintessence, a scalar field, phi, whose dynamics is solely dictated by its potential, V(phi). In this simple case, just an extra function of the background is necessary to describe the evolution of the dark...
The late time acceleration of the Universe can be characterized in terms of an extra, time dependent, component of the universe -- dark energy. The simplest proposal for dark energy is quintessence, a scalar field, phi, whose dynamics is solely dictated by its potential, V(phi). In this simple case, just an extra function of the background is necessary to describe the evolution of the dark...
Galaxy clustering is one of the main cosmological probes used by the Dark Energy Survey to investigate the nature of the Dark Energy. In order to avoid biasing our measurements derived from galaxy clustering, the impact of observing conditions must be taken into account, since they can imprint a non-cosmological clustering signal. These observing conditions are characterized through the...
The QUIJOTE (Q U I JOint TEnerife) CMB Experiment operates from the Teide Observatory, providing a novel view of the northern sky in the frequency range from 10 to 20 GHz with the Multi Frequency Instrument (MFI). Moreover, it is targeting the detection of the B-modes in the polarization of the CMB at 30 and 40 GHz with the Thirty-Forty GHz Instrument (TFGI), with a tensor to scalar ratio goal...
The nature of dark matter (DM) is still an open question for modern physics. In the particle DM paradigm, this elusive kind of matter cannot be made of any of the known particles of the Standard Model (SM). Many efforts have been made in order to model the nature of the DM. Among others, and beyond the SM of particle physics, we focus on brane world theory as a prospective framework for DM...
In this talk, we present our studies of the discovery potential of low-mass Galactic dark matter (DM) subhalos for indirect searches of DM. In particular, we analyzed the properties of DM halo substructure in a galaxy like our own. To do so, we have used data from the Via Lactea II (VL-II) N-body cosmological simulation, that resolves subhalos down to one million solar masses. First, we...
As high redshift galaxies cannot be resolved, it is necessary to have the information of the whole stellar population in order to interpret correctly the data. Thus, templates of spectra of simple stellar populations (SSPs) are needed to extract information about the stellar populations. We present our new high resolution spectra of SSPs. We have tested the application of the spectra testing...
A prediction of the standard LCDM cosmological model is that dark matter (DM) halos are teeming with numerous self-bound substructure, or subhalos. The most massive ones host the observed dwarf satellite galaxies, while smaller subhalos may host no stars/gas at all and thus may have no visible astrophysical counterparts and would remain completely dark. Yet, some of these ‘dark satellites’ are...
