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CoCo 2o23: Cosmology in Colombia

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Unicentro Cali. Salón Caracolí

Unicentro Cali. Salón Caracolí

Unicentro Cali. Salón Caracolí
Alejandro Guarnizo (Universidad Antonio Nariño), Cesar A. Valenzuela-Toledo (Departamento de Física, Universidad del Valle), JOHN BAYRON ORJUELA-QUINTANA, Juan Pablo Beltran (Universidad Nacional de Colombia), Leonardo Castañeda Colorado (Universidad Nacional de Colombia), Luz Ángela García (Universidad ECCI), Yeinzon Rodríguez García
Description
The fifth CoCo meeting (Cosmología en Colombia) will be held from the 21st and 22nd of September 2023 at Ciudad Universitaria Meléndez -Universidad del Valle, Cali - Colombia

The goal of this meeting is to bring together cosmologists to discuss the current state of cosmology at the interface of theory and observations.
The main topics include:
  • Inflation and the early Universe,
  • Cosmic microwave background,
  • Large-scale structures of the Universe,
  • Dark matter and neutrino astrophysics,
  • Dark energy and modified gravity,
  • Gravitational waves and multi-messenger astronomy.

We expect this event to provide a platform for maximizing interactions and creating new collaborations.

 
In-person conference: The workshop will be held in Cali (Colombia).
 
 

 

 

 
 
 
 

 

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  • Thursday 21 September
    • 09:00 → 09:45
      A neural network approach for approximating the local mass in general relativity 45m

      Within the framework of general relativity, the concept of local mass (or quasi-local mass) aims to quantify the amount of mass contained within a particular region of space-time. Nevertheless, the precise definition of such mass in accordance with the theory of general relativity continues to be an unresolved matter. Over the past few decades, numerous proposals have emerged in an attempt to address this issue. One particular proposal that has garnered significant attention from the scientific community in recent years is Bartnik's mass proposal, which builds upon a specific instance of the well-established ADM-mass concept. Unfortunately, performing numerical calculations of this mass for specific situations using conventional numerical methods presents a formidable challenge due to the inherent complexity of the coupled system of partial differential equations that must be solved. Motivated by this challenge, our presentation aims to introduce a deep learning approach for approximating Bartnik's mass for a two-dimensional hypersurface. We will showcase several numerical results and discuss the advantages and disadvantages associated with this method.

      Speaker: Dr LEON DARIO ESCOBAR DIAZ (Universidad del Valle)
    • 09:45 → 10:15
      Machine learning unveils the linear matter power spectrum of modified gravity 30m

      The matter power spectrum $P(k)$ is one of the main quantities connecting observational and theoretical cosmology. Although for a fixed redshift this can be numerically computed very efficiently by Boltzmann solvers, an analytical description is always desirable. However, accurate fitting functions for $P(k)$ are only available for the concordance model. Taking into account that forthcoming surveys will further constrain the parameter space of cosmological models, it is also of interest to have analytical formulations for $P(k)$ when alternative models are considered. Here, we use the genetic algorithms, a machine learning technique, to find a parametric function for $P(k)$ considering several possible effects imprinted by modifications of gravity. Our expression for the $P(k)$ of modified gravity shows a mean accuracy of around $1$-$2\%$ when compared with numerical data obtained via modified versions of the Boltzmann solver CLASS, and thus it represents a competitive formulation given the target accuracy of forthcoming surveys.

      Speaker: JOHN BAYRON ORJUELA-QUINTANA (UNIVERSIDAD DEL VALLE)
      coco 3.pdf
      coco 3.pptx
    • 10:45 → 11:05
      Coffee break 20m
    • 11:05 → 11:35
      Reconstruyendo el perfil de masa de cúmulos de galaxias a partir del efecto de lente gravitacional 30m

      En este trabajo presentamos relensing, un método que busca modelar cúmulos de galaxias haciendo uso del efecto de lente gravitacional. Hemos implementado un método no paramétrico (o de forma-libre) el cual determina el potencial deflector sobre una red irregular adaptativa. Para poder modelar un cúmulo de galaxias, relensing hace uso de sistemas de múltiples imágenes (régimen fuerte), al igual que utiliza la elipticidad de fuentes de fondo que han sido débilmente deformadas (régimen débil). Con relensing introducimos un suavizado en el potencial deflector, el cual reduce el ruido presente en la reconstrucción y por tanto, se obtienen perfiles de masa menos irregulares y más cercanos a la distribución real. Esta mejora se extiende a los mapas de magnificación, y con ello, a la estimación de las curvas críticas y cáusticas. Para validar el poder del suavizado, aplicamos relensing a Ares y Hera, los cuales son dos cúmulos de galaxias simulados que buscan asemejar las observaciones dadas por el telescopio espacial Hubble. Nuestros resultados muestran una mejora respecto a reconstrucciones realizadas con métodos que se basan en los mismos principios que relensing. El suavizado del potencial introduce además un aumentando la estabilidad y una reducción del tiempo de cómputo en nuestra implementación.

      Esta presentación está basada en nuestro paper titulado “relensing: Reconstructing the mass profile of galaxy clusters from gravitational lensing”.

      Speakers: Daniel Alexdy Torres Ballesteros (Universidad Nacional de Colombia), Prof. Leonardo Castañeda Colorado (Universidad Nacional de Colombia)
      Reconstruyendo el perfil de masa de cúmulos de galaxias a partir del efecto de lente gravitacional.pdf
    • 11:35 → 12:05
      Discs of satellites in the Illustris-TNG simulations I: identification of flattened systems 30m

      The Local Group, dominated by the main galaxies: the Milky Way and the Andromeda galaxy, presents a scenario where a set of satellite galaxies orbiting around one of these two galaxies is observed. These satellites do not present an isotropic distribution, but rather the majority are located on a plane almost perpendicular to the plane of the galaxy’s disk. In the case of the Milky Way, the distribution of dwarf galaxies presents a structure that has a radius ∼ 200 kpc, where most of them is found, and a thickness of ∼50 kpc, which has been called the disk of satellites or Vast Polar Structure of Satellite Galaxies (VPOS). For the Andromeda satellite disk, the radial extension is like that of the Milky Way, but with a slightly thinner width.
      The study of the disks of dwarf satellites is important due to the discrepancy in the way in which dwarf galaxies are distributed around larger galaxies, since theoretically they should have a nearly isotropic distribution around their host galaxies, contrary to observations. Currently there is no theoretical model that correctly explains the spatial distribution of these objects within the Local Group or in other galactic systems.
      This paper presents the results of a study on the identification of galaxy satellite disks in IllustrisTNG simulations at z = 0. From a total of 64066 systems made up of a central galaxy and several galaxies that orbit around it, we have detected 5393 flattened systems resembling the VPOS. The method used for detecting flattened distributions of galaxies and some statistics of the found systems are presented.

      Speaker: Rigoberto Angel Casas Miranda (Universidad Nacional de Colombia)
      IdenFlatSystems.pdf
    • 12:05 → 14:00
      Lunch 1h 55m
    • 14:00 → 14:30
      Frame dragging effect around slowly rotating stars in modified gravity theories 30m

      We study the frame-dragging effect in the context of slowly rotating stars in Horndeski theory (HT), Generalized Proca theory (GPT) and Generalized SU(2) Proca theory (GSU2P). The last two differ in that while GPT does not have internal simmetries, the GSU2P is invariant under SU(2) group of global transformations. The frame-dragging effect occurs when a rotating compact object distorts spacetime and inertial observers are dragged along when they are in free fall from infinity. James Hartle developed a methodology to study this effect for slowly rotating stars in General Relativity (GR) through a perturbative treatment of the GR’s field equations in powers of $Ω^2$ , being $Ω$ the angular velocity of the star. Applying the same methodology, we find that deviations from GR are very tiny in HT; these results holds for both, the interior and exterior regions of the star. For the GPT and GSU2P, we find important deviations from GR which exhibit the role that the vector field plays in the gravitational interaction for both theories. We also find constraints in the relevant modified gravity couplings which could be compared with possible future results from multimessenger astronomy.

      Speaker: William Jaimes
    • 14:30 → 15:00
      Scalar-Vector Multifield Anisotropic Dark Energy 30m

      We present partial results from a model constructed using conventional components found in string compactification as well as in general supersymmetric theories. The model entails a pair of scalar fields coupled through non-trivial kinetic mixing and incorporates a $U(1)$ vector field with a field dependent gauge kinetic function. The system unveils a novel fixed point within a Bianchi I spacetime background, exhibiting characteristics that could potentially describe a late accelerated epoch in the universe. Additionally, we expound on potential ultraviolet (UV) completions that give rise to such a model.

      Speaker: Diego Mauricio Gallego Mahecha (Universidad Pedagógica y Tecnológica de Colombia.)
      DGallegoCoCo2023.pdf
    • 15:00 → 15:30
      Tracking the validity of the quasi-static and sub-horizon approximations in modified gravity 30m

      Within the framework of modified gravity, the quasi-static and sub-horizon approximations are widely used in analyses aiming to identify departures from the concordance model at late-times. In general, it is assumed that time derivatives are subdominant with respect to spatial derivatives given that the relevant physical modes are those well inside the Hubble radius. In practice, the perturbation equations under these approximations are reduced to a tractable algebraic system in terms of the gravitational potentials and the perturbations of involved matter fields. Here, in the framework of $f(R)$ theories, we revisit standard results when these approximations are invoked using a new parameterization scheme that allows us to track the relevance of each time-derivative term in the perturbation equations. This new approach unveils correction terms which are neglected in the standard procedure. We assess the relevance of these differences by comparing results from both approaches against full numerical solutions for two well-known toy-models: the designer $f(R)$ model and the Hu-Sawicki model. We find that: $i)$ the sub-horizon approximation can be safely applied to linear perturbation equations for scales $0.06 \, h/\text{Mpc} \lesssim k \lesssim 0.2 \, h/\text{Mpc}$, $ii)$ in this ``safety region'', the quasi-static approximation provides a very accurate description of the late-time cosmological dynamics even when dark energy significantly contribute to the cosmic budget, and $iii)$ our new methodology performs better than the standard procedure, even for several orders of magnitude in some cases. Although, the impact of this major improvement on the linear observables is minimal for the studied cases, this does not represent an invalidation for our approach. Instead, our findings indicate that the perturbation expressions derived under these approximations in more general modified gravity theories, such as Horndeski, should be also revisited.

      Speaker: JOHN BAYRON ORJUELA-QUINTANA (UNIVERSIDAD DEL VALLE)
      QSASHA.pdf
    • 15:30 → 15:50
      Coffee break 20m
    • 15:50 → 16:20
      Some astrophysical properties of compact object solutions in the Generalized SU(2) Proca theory 30m

      In this work, we studied some compact object solutions in the Generalized SU(2) Proca theory. This modified gravity model is a vector-tensor theory whose action is invariant under global transformations of the SU(2) group and includes second-order derivative self-interactions of the vector field beyond the massive Yang-Mills theory. First, we studied two Lagrangian pieces consisting of four gauge fields minimally coupled to metric tensor. These pieces give rise to an exact Reissner-Nordstrom black hole solution endowed with two different non-Abelian effective charges that depend on the free parameters of the theory. We analyzed the spacetime structure and found the parameter space that preserves the weak cosmic censorship conjecture. The joint analysis of observations of the EHT's first images of Sagittarius A$^{\star}$ of our Galaxy and the Keck telescope set the first constraint on the free parameters of the theory beyond the theoretical bounds found. Also, we present some numerical solutions in the Generalized SU(2) Proca theory which describes a spherical and static black hole. We constructed equilibrium sequences and studied some thermodynamic properties. Finally, we studied the effective potential of soliton solutions in the Generalized SU(2) Proca theory. These objects are compact enough to generate a photon sphere making them black hole mimickers.

      Speaker: Jose Fernando Rodriguez Ruiz (Universidad Industrial de Santander)
    • 16:20 → 16:50
      Colapso esférico en diversos modelos de energía oscura 30m

      Se presentará un estudio del proceso de formación de estructuras a gran escala en el Universo, en el marco del modelo del colapso esférico, para diferentes escenarios de energía oscura. Se consideran modelos de energía oscura con ecuaciones de estado dinámicas construidas a partir del análisis fenomenológico y otras construidas a partir de campos, con el objetivo de evaluar los efectos del componente de energía oscura en el proceso de formación de estructuras. Primero se mostrará la evolución de las perturbaciones de materia tanto en el régimen no lineal como en el régimen lineal. Luego, se mostrará el cálculo de los parámetros que caracterizan el modelo del colapso esférico, es decir, la sobredensidad crítica $\delta_c$, el parámetro de sobredensidad virial $\Delta_v$ y el factor de crecimiento $D_+$. Finalmente, mediante el formalismo Press Schecter, se mostrará cómo la energía oscura afecta el proceso de formación de estructuras a gran escala.

      Speaker: Mr PEDRO MARTIN IBARBO PERLAZA (Universidad del Valle)
      LSSF_CoCo2023.pdf
  • Friday 22 September
    • 09:00 → 09:45
      Broad absorption lines in DESI Y1 QSO spectra 45m

      Accurate quasar classifications and redshift measurements are increasingly important to precision cosmology experiments. Broad absorption line (BAL) features are present in 15-20% of all quasars, and these features can introduce systematic redshift errors, and in extreme cases produce misclassifications. We quantitatively investigate the impact of BAL features on quasar classifications and redshift measurements with synthetic spectra that were designed to match observations by the Dark Energy Spectroscopic Instrument (DESI) survey. Over the course of five years, DESI aims to measure spectra for 40 million galaxies and quasars, including nearly three million quasars. Our synthetic quasar spectra match the signal-to-noise ratio and redshift distributions of the first year of DESI observations and include the same synthetic quasar spectra both with and without BAL features. We demonstrate that masking the locations of the BAL features decreases the redshift errors by about 1% and reduces the number of catastrophic redshift errors by about 80%. We conclude that identifying and masking BAL troughs should be a standard part of the redshift determination step for DESI and other large-scale spectroscopic surveys of quasars.

      Speaker: Luz Ángela García (Universidad ECCI)
      BALs_talk_2023.pptx.pdf
    • 09:45 → 10:15
      Scaling Solutions in Generalized Proca Theory and its Cosmological Implications 30m

      In the framework of the generalized Proca theories, we derive for the first time the most general Lagrangian allowing for scaling solutions between dark energy and cold dark matter. At background level, we highlight two interesting features for this novel model. Firstly, although its equation of state of is exactly $-1$, the dark energy component has a dynamical behaviour due to its coupling with the cold dark matter. Secondly, the existence of an attractor point where the scaling condition holds and the universe can undergo accelerated expansion. At the perturbative level, we derive the growth equation for cold dark matter under the sub-horizon and quasi-static approximations. The solutions of this equation show that the strength of gravity can vary at late times, where the differences with respect to the concordance model depend on the parameters of the novel model.

      Speaker: SANTIAGO GARCIA SERNA
      Talk CoCo.pptx
    • 10:15 → 10:45
      Particle-like solutions in the generalized SU(2) Proca theory 30m

      The generalized SU(2) Proca theory is a vector-tensor modified gravity theory where the action is invariant under both diffeomorphisms and global internal transformations of the SU(2) group. This work constitutes the first approach to investigate the physical properties of the theory at astrophysical scales. We have found solutions that naturally generalize the particle-like solutions of the Einstein-Yang-Mills equations, also known as gauge boson stars. Under the requirement that the solutions must be static, asymptotically flat, and globally regular, the t'Hooft-Polyakov magnetic monopole configuration for the vector field rises as one viable possibility. The solutions have been obtained analytically through asymptotic expansions and numerically by solving the boundary value problem. We have found new features in the solutions such as regions with negative effective energy density and imaginary effective charge. We have also obtained a new kind of globally charged solutions for some region in the parameter space of the theory. Furthermore, we have constructed equilibrium sequences and found turning points in some cases. These results hint towards the existence of stable solutions which are absent in the Einstein-Yang-Mills case.

      Speaker: Jhan Nicolás Martínez Lobo (Universidad Industrial de Santander)
      CoCo (1).pdf
    • 10:45 → 11:05
      Coffee break 20m
    • 11:05 → 11:35
      Time Travel Paradoxes and Entangled Timelines 30m

      It seems that if time travel is possible, it is inevitable to encounter paradoxes. These paradoxes include consistency paradoxes, such as the famous grandfather paradox, and bootstrap paradoxes, in which something is created out of nothing. The concept of parallel timelines is suggested to address these paradoxes, and a model called "Entangled Timelines" or E-CTCs is proposed to explain the mechanism by which timelines can be created. This mechanism is based on the Everett or "many-worlds" interpretation. In this research, we endeavor to expand upon the existing model by exploring various scenarios, including multiple time machines, an infinite number of timelines, non-cyclical timelines. Additionally, we investigate the consequences of a part of an entangled system and particles in superposition accessing the time machine.

      Speaker: Ms GABRIELA ALEJANDRA VALENCIA ZUÑIGA (Universidad del Valle)
      TTP.pdf
    • 11:35 → 12:05
      Las teorías gravitacionales en el contexto de geometrías no Riemannianas al filo de la navaja de Ockham 30m

      La teoría newtoniana de la gravedad puede ser reformulada en el lenguaje de geometría diferencial como una teoría no relativista en espaciotiempo curvo, en donde la fuente de la curvatura está asociada con el potencial gravitacional newtoniano estándar. Ésta es conocida como la teoría de Newton-Cartan (NC), y aunque a nivel dinámico es absolutamente equivalente a la teoría newtoniana estándar, la interpretación de los objetos geométricos y de la estructura misma del espaciotiempo newtoniano es diferente. Un factor determinante de esta reformulación es que permite hacer una comparación en paralelo, y en el mismo lenguaje geométrico, de los postulados necesarios para construir la teoría de NC y la teoría de la Relatividad General (RG) de Einstein. Se concluye que la teoría de RG es más simple que la teoría de NC ya que requiere menos postulados para su construcción. Con base en estas conclusión y adhiriéndose al principio de la navaja de Ockham, es razonable pensar que la RG sea la mejor opción que ha tenido la naturaleza para describir la gravedad. No obstante, se ha mostrado que, a nivel dinámico, la RG es indistinguible de sus versiones teleparalela y simétrica teleparalela en el contexto de geometrías no Riemannianas. Por lo anterior, en este trabajo se plantea la pregunta ¿cuál teoría gravitacional sería la preferida por la Naturaleza teniendo como base su simplicidad y el número de postulados requeridos para su construcción?

      Speaker: William Jaimes
      Documento de William Jaimes
    • 12:05 → 14:00
      Lunch 1h 55m
    • 14:00 → 14:30
      Spherical collapse model for a non-Abelian Gauge-field cosmology 30m

      In this talk, we investigate the spherical collapse model within the framework of dynamical dark energy cosmologies. We present a versatile code that allows for the implementation of various dark energy models, providing a powerful tool for studying their effects on structure formation. To demonstrate the capabilities of our code, we focus on a cosmology where a non-abelian gauge SU(2) vector field is the sole source of dark energy. This choice allows us to explore the unique characteristics of this model and investigate its implications for the formation of cosmic structures. By incorporating the dynamics of the non-abelian gauge field into the spherical collapse model, we analyze the growth of density perturbations and the formation of collapsed objects in this cosmological scenario. We observe distinct deviations from the LCDM result, highlighting the importance of considering alternative sources of dark energy in cosmological investigations of structure formation.

      Speaker: William Esteban Salazar (Centre for Bioinformatics and Photonics (CIBioFi), Universidad del Valle, Edificio E20 No. 1069, 760032 Cali, Colombia)
    • 14:30 → 15:00
      DARK AND BARYONIC MATTER IN EULERIAN COSMOLOGICAL PERTURBATION THEORY TO FIRST ORDER 30m

      In modern cosmology, the problem of large-scale structure formation has been studied through various analytical and computational methods and has become a cornerstone of astrophysics. The complexity of the equations that describe the evolution of small fluctuations in the matter field, with respect to the Friedmann - Lemaître - Robertson - Walker (FLRW) universe, commonly known as the theory linearized gravitational perturbations, makes it a valuable framework for describing the problem. Specifically, the approximation of sub-horizon scale allows us to explore scenarios where semi-analytical tools play a significant role in gaining a better understanding of how significant structures in our universe have evolved and how the cosmic web structure is formed. In this sense, these types of techniques have allowed for comparisons with extensive simulations and have provided a basis for contrasting with high-precision observations in this context. Therefore, in this lecture, we present a semi-analytical description of the evolution of contrast density in cold dark matter (CDM), including baryonic matter, in a linear regime in Fourier space. We achieve this by using the Jeans filtering function (JFF), considering only proportional solutions, and then comparing them with the numerical solutions calculated for the JFF equations to zero and first order. Finally, we discuss and elaborate upon some of the results obtained for various initial conditions in redshift.

      Speaker: Diego Fernando Fonseca Moreno (Universidad Nacional de Colombia/ Universidad Antonio Nariño)
      PRESENTACIÓN CoCo 2023.pdf
    • 15:00 → 15:20
      Coffee break 20m
    • 15:20 → 15:50
      Energía oscura y campos vectoriales inhomogéneos 30m

      Con frecuencia, se ha recurrido a campos escalares como potenciales fuentes de inflación y energía oscura, dado que son capaces de generar presiones negativas requeridas para este tipo de fenómenos. Sin embargo, en esta ocasión, se ha explorado un enfoque diferente al considerar campos vectoriales no homogéneos como posibles fuentes de energía oscura.

      En esta investigación, se ha empleado un lagrangiano que se origina a partir de una triada de campos vectoriales no homogéneos donde, en este caso en particular, se ha adoptado una configuración de campo conocida como configuración magnética. A partir de esta formulación lagrangiana se ha derivado el tensor momento-energía con el cual se describe la dinámica del sistema y, de esta manera, se encontró un conjunto de ecuaciones autónomas fundamentales para hacer un debido análisis de la estabilidad del sistema, centrado en sus puntos críticos.

      Finalmente, se encontró que los resultados obtenidos son consistentes con las observaciones relacionadas con la expansión del universo.

      Speaker: EDUARDO JOSE ORDOÑEZ HURTADO
      COCO2023.pdf
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