Número de entradas: **37**

### The Lambdac(2940)+ as a molecular D*N (Ds*Lambda) state

**Estado:** defended (25/07/2017)

**Estudiante:** Montaña, G.

**Supervisada por:** Laura Tolos ; Ramos, A.

**Universidad:** Universitat de Barcelona

**Estado:** defended (25/07/2017)

**Estudiante:** Montaña, G.

**Supervisada por:** Laura Tolos ; Ramos, A.

**Universidad:** Universitat de Barcelona

Upon the assumption of being a resonance with spin-parity J=3/2-, the Lambda_c(2940)+ is described

in this thesis as a vector meson-baryon molecule. Also, a visible signal of this resonance

is found in the invariant mass spectrum of the Lambda_b -> pi D0 p decay. This is achieved after a

complete study of the interaction of pseudoscalar mesons and vector mesons with baryons in

the charm C = 1 sector within a coupled-channel approach in SU(4), using the hidden gauge

formalism to implement the interaction through a vector meson exchange model. The results of

the model presented here predict the Lambdac(2940)+ as a state with basically rho Sigma_c and K*Xi'c components,

but also coupling to the D*N and D*sLambda channels. It is the coupling to these latter

vector meson-baryon systems which allows the appearance of a peak in the D0p invariant mass

distribution of the b decay, signalling the presence of the Lambdac(2940)+. The study of the details

of the weak decay and the hadronization process leads to a clear signal of this resonance, as well

as other interesting features, which make the Lambda_b -> pi D0 p decay an interesting process to be

observed experimentally, both for validating the molecular nature of the Lambdac(2940)+ and for the

observation of new exotic hadron states.
### Inflation from fluid models

**Estado:** defended (15/02/2017)

**Estudiante:** Kerim Demirel

**Supervisada por:** Sergei D Odintsov ; Emilio Elizalde

**Universidad:** Universitat Autònoma de Barcelona

**Estado:** defended (15/02/2017)

**Estudiante:** Kerim Demirel

**Supervisada por:** Sergei D Odintsov ; Emilio Elizalde

**Universidad:** Universitat Autònoma de Barcelona

Fluid inflation is proposed and studied.
### The J/Psi interaction with nucleons and baryons within a unitarized SU(6)x HQSS meson-baryon model

**Estado:** defended (24/10/2016)

**Estudiante:** Elisabet Galiana Baldo

**Supervisada por:** Laura Tolos

**Universidad:** Universitat de Barcelona

**Estado:** defended (24/10/2016)

**Estudiante:** Elisabet Galiana Baldo

**Supervisada por:** Laura Tolos

**Universidad:** Universitat de Barcelona

We present a detailed analysis of the hidden charm sector (i.e. with cc pairs),

with C = 0. In particular, we study the interaction between J/Y and nucleons and

baryons. For this purpose, we use a theoretical model that has been built in previous

works, that is based on a suitable extension of the Weinberg Tomozawa term

to include, beside Chiral Symmetry, Spin Flavour Symmetry in the light sector and

Heavy Quark Spin Symmetry in the heavy sector. Within this model we obtain the

interaction between J=1/2+, J=3/2+ baryons and pseudoscalar and vector mesons which

contain light and heavy quarks. We carry out the calculation of some scattering observables,

such as cross sections and scattering lengths, while comparing the results

with other works. Moreover, we analyze the existence of the two new states recently

discovered by the LHCb Collaboration, the P+c (4380) and P+c (4450) pentaquarks.

We find that we can only reproduce one of the state, the Pc(4450) pentaquark, if we

modify considerably the subtraction point.
### Correlations between Cosmic Voids and CMB Lensing in the MICE Simulation

**Estado:** defended (14/09/2016)

**Estudiante:** Umut Emek Demirbozan

**Supervisada por:** Pablo Fosalba Vela; Kovacs, A.

**Estado:** defended (14/09/2016)

**Estudiante:** Umut Emek Demirbozan

**Supervisada por:** Pablo Fosalba Vela; Kovacs, A.

In this Master Thesis we investigate the correlation between Cosmic Microwave Background(CMB) lensing with cosmic voids in the large scale structure in the universe by using MICE-Grand Challenge(GC) simulation. We use the convergence map generated from MICE-Grand Challange simula- tion to search for correlation between CMB lensing convergence with cosmic voids. We identify the voids in MICE-GC simulation by using the void finder algorithm in Sanchez et al. (2016) and use different samples of input galaxies from MICE-GC and measure CMB lensing effect in these samples. One recent study Cai et al. (2016) found a significant correlation between Planck convergence data and BOSS-CMASS voids and we were developing our work in parallel to this study. In our study, we find ≈ 3σ correlation by using similar input sample (0.4<z<0.7) as in Cai et al. (2016). Furthermore, we found that the voids which are deeper (very underdense) signifi- cantly more likely to have CMB lensing imprint. However, these underdense voids are generally smaller. Since there are much more smaller voids than large voids, it follows that small voids are more likely to have imprint on the CMB lensing map. Our findings are consistent with the results by Cai et al. (2016). In addition to this, we show that there is a special region on cen- tral underdensity vs general underdensity plane where voids are very likely to have imprint on the CMB lensing map. We measure radial convergence profile as a function void radius and discuss the potential usage of this technique to derive cosmological parameters.
### GAMMA RAY EMISSION STUDY OF PSR J2022+3842 WITH FERMILAT

**Estado:** defended (14/09/2016)

**Estudiante:** Mariona Caixach

**Supervisada por:** Emma de Ona Wilhelmi

**Universidad:** Universitat Autònoma de Barcelona

**Estado:** defended (14/09/2016)

**Estudiante:** Mariona Caixach

**Supervisada por:** Emma de Ona Wilhelmi

**Universidad:** Universitat Autònoma de Barcelona

This project presents the analysis of the pulsar PSR J2022+3842 which has been previously identified as one of the most energetic pulsars in radio and X-rays. Here we analyse the source 3FGL J2022.2+3840 identifying it with the pulsar. The analysis has been taken from data observed by the LAT, on board of the NASA satellite Fermi Gamma-ray Space Telescope, in order to study its gamma radiation from 60 MeV to 50GeV. Previously, in order to make the project more understandable, some theoretical aspects about very high energy radiation and pulsars are explained.
### Analyzing the photometric performance of the PAU survey

**Estado:** defended (14/09/2016)

**Estudiante:** Andrea Pocino Yuste

**Supervisada por:** Francisco Javier Castander Serentill

**Universidad:** Universitat Autònoma de Barcelona

**Estado:** defended (14/09/2016)

**Estudiante:** Andrea Pocino Yuste

**Supervisada por:** Francisco Javier Castander Serentill

**Universidad:** Universitat Autònoma de Barcelona

Using the Bayesian Photometric Redshift, a template-fitting based code, we compute the expected photometric accuracy for the Physics of the Accelerating Universe (PAU) sur- vey through simulations. We check its real performance by computing the photometric redshift using observed data through PAUCam from a period of observations during the first semester of 2016. Then we validate the photo-z by comparing it to the highly reliable photometric and spectroscopic redshift from COSMOS survey. At the end we obtain a photometric accuracy of σ ∼ 0.0019(1 + z) for real data of PAU.
### Clues on protoplanetary disk components from the meteorite evidence

**Estado:** defended (07/09/2016)

**Estudiante:** Tanbakouei, S.

**Supervisada por:** Josep M. Trigo-Rodríguez

**Universidad:** Universitat Autònoma de Barcelona

**Estado:** defended (07/09/2016)

**Estudiante:** Tanbakouei, S.

**Supervisada por:** Josep M. Trigo-Rodríguez

**Universidad:** Universitat Autònoma de Barcelona

Complementary to observations of protoplanetary disks, the remnant solid bodies

of our planetary system provide valuable clues on the conditions of the solar system

during its formation as well on planet formation, which could be applicable to

study other systems as well. Undifferentiated bodies preserved their internal structure,

because they were the ones that did not melt or were not involved in large-scale

differentiation processes. From time-to-time meteorites fall on Earth and preserve

clues on these early processes. Contrarily of what is commonly believed, they are

only affected by atmospheric entry in a thin outer layer known as fusion crust. Their

interior below that outer layer is preserved, and if the meteorite was not largely affected

by impact metamorphism in the parent body, the study of its basic chemistry

and mineralogy with modern equipment allow to unveil the first accretionary processes

occurred in our solar system. Meteorites, especially chondriticmeteorites, are

therefore, a way to provide observational constraints on the physical scenarios regarding

primary accretion: having formed within the first few million years after the

origin of the solar system, in a disk that was still gas-reach, they are real fossils of the

protoplanetary disk-forming materials. The dominant components of these chondrites

are chondrules: ~100 micrometers to mm-sized stony spherules composed primarily of

the silicate minerals olivine and pyroxene. Here a short introduction

to the origin of chondrules, and the implications for the composition of chondrites

will be given to demonstrate the importance that meteorite studies have to validate

astrophysicalmodels and observations of protoplanetary disks.
### Simulación y ánalisis del experimento de la ventana óptica en la misión LISA Pathnder

**Estado:** defended (21/09/2015)

**Estudiante:** Francisco Rivas García

**Supervisada por:** Carlos Sopuerta ; Miquel Nofrarias Serra

**Universidad:** Universidad de Granada

**Url:** https://www.ugr.es

**Estado:** defended (21/09/2015)

**Estudiante:** Francisco Rivas García

**Supervisada por:** Carlos Sopuerta ; Miquel Nofrarias Serra

**Universidad:** Universidad de Granada

**Url:** https://www.ugr.es

En este trabajo se va a dar una visión general sobre ondas gravitacionales (fundamentos matemáticos, detectores, etc) que introducirá qué es y el por qué de la misión espacial LISA Pathnder (LPF), poniendo especial atención en uno de los experimentos que llevará a cabo una vez en su órbita, el experimento de la Optical Window (OW).
### Modeling and Analysis of the Galaxy Clustering

**Estado:** defended (18/09/2015)

**Estudiante:** Anna Maria Porredon Díez de Tejada

**Supervisada por:** Martin Crocce ; Pablo Fosalba Vela

**Universidad:** Universitat Autònoma de Barcelona

**Estado:** defended (18/09/2015)

**Estudiante:** Anna Maria Porredon Díez de Tejada

**Supervisada por:** Martin Crocce ; Pablo Fosalba Vela

**Universidad:** Universitat Autònoma de Barcelona

Splitting the different calculations of a pipeline into interchangeable modular units seems to be a promising method for analyzing samples of data in a large scientific collaboration. Here, we develop a stable code that models the two-point correlation function of galaxies, as this observable is a powerful tool to derive cosmological constraints. Then, we simulate mock data from this model assuming that the data points are uncorrelated and follow a Poisson distribution centered at the theoretical values. Last, from the expected theoretical values and the mock data, we take a modular approach to perform a Markov Chain Monte-Carlo (MCMC) likelihood analysis on some cosmological parameters. The resulting values of these parameters are in agreement with the true ones used to generate the mock data, thus we conclude that the pipeline is consistent.
### BOUND GEODESIC ORBITS IN KERR SPACETIME

**Estado:** defended (16/09/2015)

**Estudiante:** Massimiliano Baravelli

**Supervisada por:** Carlos Sopuerta

**Universidad:** Universitat Autònoma de Barcelona

**Estado:** defended (16/09/2015)

**Estudiante:** Massimiliano Baravelli

**Supervisada por:** Carlos Sopuerta

**Universidad:** Universitat Autònoma de Barcelona

This work is based on the derivation of the analytical solution of the bound timelike geodesic orbits of a particle in Kerr spacetime done by Ryuichi Fujita and Wataru Hikida [1]. I wrote a code to compute these solutions expressed in terms of elliptic integrals using Mino time as the independent variable. These papers are structured as follows: in the introduction is explained the importance of the study of the geodesic motion to investigate the properties of a Kerr black hole; in the first section there are the details of the theory used in this work, the Kerr spacetime, the Mino time and the bound geodesic orbits; in section two I talk about the project itself, how the code has been done and the main procedure, also the results and plots are showed with a comparison with previous works; finally, in section three, there are the main conclusions and how and where this kind of project could be applied.

Upon the assumption of being a resonance with spin-parity J=3/2-, the Lambda_c(2940)+ is described in this thesis as a vector meson-baryon molecule. Also, a visible signal of this resonance is found in the invariant mass spectrum of the Lambda_b -> pi D0 p decay. This is achieved after a complete…

Upon the assumption of being a resonance with spin-parity J=3/2-, the Lambda_c(2940)+ is described

in this thesis as a vector meson-baryon molecule. Also, a visible signal of this resonance

is found in the invariant mass spectrum of the Lambda_b -> pi D0 p decay. This is achieved after a

complete study of the interaction of pseudoscalar mesons and vector mesons with baryons in

the charm C = 1 sector within a coupled-channel approach in SU(4), using the hidden gauge

formalism to implement the interaction through a vector meson exchange model. The results of

the model presented here predict the Lambdac(2940)+ as a state with basically rho Sigma_c and K*Xi'c components,

but also coupling to the D*N and D*sLambda channels. It is the coupling to these latter

vector meson-baryon systems which allows the appearance of a peak in the D0p invariant mass

distribution of the b decay, signalling the presence of the Lambdac(2940)+. The study of the details

of the weak decay and the hadronization process leads to a clear signal of this resonance, as well

as other interesting features, which make the Lambda_b -> pi D0 p decay an interesting process to be

observed experimentally, both for validating the molecular nature of the Lambdac(2940)+ and for the

observation of new exotic hadron states.

Fluid inflation is proposed and studied.

Fluid inflation is proposed and studied.

We present a detailed analysis of the hidden charm sector (i.e. with cc pairs), with C = 0. In particular, we study the interaction between J/Y and nucleons and baryons. For this purpose, we use a theoretical model that has been built in previous works, that is based on a suitable extension of the…

We present a detailed analysis of the hidden charm sector (i.e. with cc pairs),

with C = 0. In particular, we study the interaction between J/Y and nucleons and

baryons. For this purpose, we use a theoretical model that has been built in previous

works, that is based on a suitable extension of the Weinberg Tomozawa term

to include, beside Chiral Symmetry, Spin Flavour Symmetry in the light sector and

Heavy Quark Spin Symmetry in the heavy sector. Within this model we obtain the

interaction between J=1/2+, J=3/2+ baryons and pseudoscalar and vector mesons which

contain light and heavy quarks. We carry out the calculation of some scattering observables,

such as cross sections and scattering lengths, while comparing the results

with other works. Moreover, we analyze the existence of the two new states recently

discovered by the LHCb Collaboration, the P+c (4380) and P+c (4450) pentaquarks.

We find that we can only reproduce one of the state, the Pc(4450) pentaquark, if we

modify considerably the subtraction point.

In this Master Thesis we investigate the correlation between Cosmic Microwave Background(CMB) lensing with cosmic voids in the large scale structure in the universe by using MICE-Grand Challenge(GC) simulation. We use the convergence map generated from MICE-Grand Challange simula- tion to search…

In this Master Thesis we investigate the correlation between Cosmic Microwave Background(CMB) lensing with cosmic voids in the large scale structure in the universe by using MICE-Grand Challenge(GC) simulation. We use the convergence map generated from MICE-Grand Challange simula- tion to search for correlation between CMB lensing convergence with cosmic voids. We identify the voids in MICE-GC simulation by using the void finder algorithm in Sanchez et al. (2016) and use different samples of input galaxies from MICE-GC and measure CMB lensing effect in these samples. One recent study Cai et al. (2016) found a significant correlation between Planck convergence data and BOSS-CMASS voids and we were developing our work in parallel to this study. In our study, we find ≈ 3σ correlation by using similar input sample (0.4<z<0.7) as in Cai et al. (2016). Furthermore, we found that the voids which are deeper (very underdense) signifi- cantly more likely to have CMB lensing imprint. However, these underdense voids are generally smaller. Since there are much more smaller voids than large voids, it follows that small voids are more likely to have imprint on the CMB lensing map. Our findings are consistent with the results by Cai et al. (2016). In addition to this, we show that there is a special region on cen- tral underdensity vs general underdensity plane where voids are very likely to have imprint on the CMB lensing map. We measure radial convergence profile as a function void radius and discuss the potential usage of this technique to derive cosmological parameters.

This project presents the analysis of the pulsar PSR J2022+3842 which has been previously identified as one of the most energetic pulsars in radio and X-rays. Here we analyse the source 3FGL J2022.2+3840 identifying it with the pulsar. The analysis has been taken from data observed by the LAT,…

This project presents the analysis of the pulsar PSR J2022+3842 which has been previously identified as one of the most energetic pulsars in radio and X-rays. Here we analyse the source 3FGL J2022.2+3840 identifying it with the pulsar. The analysis has been taken from data observed by the LAT, on board of the NASA satellite Fermi Gamma-ray Space Telescope, in order to study its gamma radiation from 60 MeV to 50GeV. Previously, in order to make the project more understandable, some theoretical aspects about very high energy radiation and pulsars are explained.

Using the Bayesian Photometric Redshift, a template-fitting based code, we compute the expected photometric accuracy for the Physics of the Accelerating Universe (PAU) sur- vey through simulations. We check its real performance by computing the photometric redshift using observed data through PAUCam…

Using the Bayesian Photometric Redshift, a template-fitting based code, we compute the expected photometric accuracy for the Physics of the Accelerating Universe (PAU) sur- vey through simulations. We check its real performance by computing the photometric redshift using observed data through PAUCam from a period of observations during the first semester of 2016. Then we validate the photo-z by comparing it to the highly reliable photometric and spectroscopic redshift from COSMOS survey. At the end we obtain a photometric accuracy of σ ∼ 0.0019(1 + z) for real data of PAU.

Complementary to observations of protoplanetary disks, the remnant solid bodies of our planetary system provide valuable clues on the conditions of the solar system during its formation as well on planet formation, which could be applicable to study other systems as well. Undifferentiated bodies preserved…

Complementary to observations of protoplanetary disks, the remnant solid bodies

of our planetary system provide valuable clues on the conditions of the solar system

during its formation as well on planet formation, which could be applicable to

study other systems as well. Undifferentiated bodies preserved their internal structure,

because they were the ones that did not melt or were not involved in large-scale

differentiation processes. From time-to-time meteorites fall on Earth and preserve

clues on these early processes. Contrarily of what is commonly believed, they are

only affected by atmospheric entry in a thin outer layer known as fusion crust. Their

interior below that outer layer is preserved, and if the meteorite was not largely affected

by impact metamorphism in the parent body, the study of its basic chemistry

and mineralogy with modern equipment allow to unveil the first accretionary processes

occurred in our solar system. Meteorites, especially chondriticmeteorites, are

therefore, a way to provide observational constraints on the physical scenarios regarding

primary accretion: having formed within the first few million years after the

origin of the solar system, in a disk that was still gas-reach, they are real fossils of the

protoplanetary disk-forming materials. The dominant components of these chondrites

are chondrules: ~100 micrometers to mm-sized stony spherules composed primarily of

the silicate minerals olivine and pyroxene. Here a short introduction

to the origin of chondrules, and the implications for the composition of chondrites

will be given to demonstrate the importance that meteorite studies have to validate

astrophysicalmodels and observations of protoplanetary disks.

En este trabajo se va a dar una visión general sobre ondas gravitacionales (fundamentos matemáticos, detectores, etc) que introducirá qué es y el por qué de la misión espacial LISA Pathnder (LPF), poniendo especial atención en uno de los experimentos que llevará a cabo una vez en su órbita,…

En este trabajo se va a dar una visión general sobre ondas gravitacionales (fundamentos matemáticos, detectores, etc) que introducirá qué es y el por qué de la misión espacial LISA Pathnder (LPF), poniendo especial atención en uno de los experimentos que llevará a cabo una vez en su órbita, el experimento de la Optical Window (OW).

Splitting the different calculations of a pipeline into interchangeable modular units seems to be a promising method for analyzing samples of data in a large scientific collaboration. Here, we develop a stable code that models the two-point correlation function of galaxies, as this observable is…

Splitting the different calculations of a pipeline into interchangeable modular units seems to be a promising method for analyzing samples of data in a large scientific collaboration. Here, we develop a stable code that models the two-point correlation function of galaxies, as this observable is a powerful tool to derive cosmological constraints. Then, we simulate mock data from this model assuming that the data points are uncorrelated and follow a Poisson distribution centered at the theoretical values. Last, from the expected theoretical values and the mock data, we take a modular approach to perform a Markov Chain Monte-Carlo (MCMC) likelihood analysis on some cosmological parameters. The resulting values of these parameters are in agreement with the true ones used to generate the mock data, thus we conclude that the pipeline is consistent.

This work is based on the derivation of the analytical solution of the bound timelike geodesic orbits of a particle in Kerr spacetime done by Ryuichi Fujita and Wataru Hikida [1]. I wrote a code to compute these solutions expressed in terms of elliptic integrals using Mino time as the independent variable.…

This work is based on the derivation of the analytical solution of the bound timelike geodesic orbits of a particle in Kerr spacetime done by Ryuichi Fujita and Wataru Hikida [1]. I wrote a code to compute these solutions expressed in terms of elliptic integrals using Mino time as the independent variable. These papers are structured as follows: in the introduction is explained the importance of the study of the geodesic motion to investigate the properties of a Kerr black hole; in the first section there are the details of the theory used in this work, the Kerr spacetime, the Mino time and the bound geodesic orbits; in section two I talk about the project itself, how the code has been done and the main procedure, also the results and plots are showed with a comparison with previous works; finally, in section three, there are the main conclusions and how and where this kind of project could be applied.

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