### Finalized PhD theses

Número de entradas: 78

### Theory and observations of the PWN-SNR complex

Estudiante: Jonatan Martín Rodríguez
Supervisada por: Diego F. Torres ; Nanda Rea
Universidad: Universitat Autònoma de Barcelona

In this work, we study theoretical and observational issues about pulsars (PSRs), pulsar wind nebulae (PWNe) and supernova remnants (SNRs). In particular, the spectral modeling of young PWNe and the X-ray analysis of SNRs with magnetars comparing their characteristics with those remnants surrounding…
Estudiante: Jonatan Martín Rodríguez
Supervisada por: Diego F. Torres ; Nanda Rea
Universidad: Universitat Autònoma de Barcelona

In this work, we study theoretical and observational issues about pulsars (PSRs), pulsar wind nebulae (PWNe) and supernova remnants (SNRs). In particular, the spectral modeling of young PWNe and the X-ray analysis of SNRs with magnetars comparing their characteristics with those remnants surrounding canonical pulsars. The spectra of PWNe range from radio to $\gamma$-rays. They are the largest class of identified Galactic sources in $\gamma$-rays increasing the number from 1 to $\sim$30 during the last years. We have developed a detailed spectral code which reproduces the electromagnetic spectrum of PWNe in free expansion ($t_{age} \lesssim$10 kyr). We shed light and try to understand issues on time evolution of the spectra, the synchrotron self-Compton dominance in the Crab Nebula, the particle dominance in PWNe detected at TeV energies and how physical parameters constrain the detectability of PWNe at TeV. We make a systematic study of all Galactic, TeV-detected, young PWNe which allows to find correlations and trends between parameters. We also discuss about the spectrum of those PWNe not detected at TeV and if models with low magnetized nebulae can explain the lack of detection or, on the contrary, high-magnetization models are more favorable. Regarding the X-ray analysis of SNRs, we use X-ray spectroscopy in SNRs with magnetars to discuss about the formation mechanism of such extremely magnetized PSRs. The alpha-dynamo mechanism proposed in the 1990's produces an energy release that should have influence in the energy of the SN explosion. We extend the work done previously done by \cite{vink06} about the energetics of the SN explosion looking for this energy release and we look for the element ionization and the X-ray luminosity and we compare our results with other SNRs with an associated central source.

### Weak Lensing Analysis of an All-Sky Simulation

Estudiante: Carlos Lopez Arenillas
Supervisada por: Pablo Fosalba Vela; Enrique Gaztañaga
Universidad: Universitat de Barcelona

This Thesis is concerned with one of the most promising probes to constrain the "Dark Universe", and, particularly, the dark matter distribution. Based on MICE cosmological simulation, and the all-sky convergence maps generated by Fosalba, Gaztanaga, Castander & Manera (2003) we perform a mass calibration…
Estudiante: Carlos Lopez Arenillas
Supervisada por: Pablo Fosalba Vela; Enrique Gaztañaga
Universidad: Universitat de Barcelona

This Thesis is concerned with one of the most promising probes to constrain the "Dark Universe", and, particularly, the dark matter distribution. Based on MICE cosmological simulation, and the all-sky convergence maps generated by Fosalba, Gaztanaga, Castander & Manera (2003) we perform a mass calibration of the dark matter halos there contained up to z=1. In order to do that, we analyse the average halo density proÖles of all the halos with masses ranging from 5E13 to 4E14 Msol/h , divided into four mass bins and three redshift bins. Through this analysis we address two main issues: the relatively low mass resolution of the simulation (mp=2.34 1011 h1M ) and the relatively high softening length (lsoft=50 h1 Kpc). We do that by using a two-step procedure. First, we simulate analytical pure NFW density profiles (with di§erent mass resolutions) using two input values: the virial radii of MICE halos and the expected concentrations, according to the Öxed mass-concentration relation from Oguri and Hamana [130]. Second, we model the e§ect of the softening length with a Gaussian Ölter, smoothing the halo core. The results show that MICE halos are, in average, NFW halos. Best-O NFW radii are in very good agreement with the average radii of our samples, overestimating the data by  1%, but best-fit NFW concentrations are in average 50% lower than the expected values. It is possible to account for part of this deviation by distinguishing between relaxed and unrelaxed halos, finding that, depending on the degree of relaxedness, the improvement can be as high as 30%. We also find that the analytical NFW halos simulated with MICE mass resolution have an overall concentration 40% lower than the input concentration, in the case of 3D proÖles, and 25% lower in that of the projected proÖles. The Gaussian-smoothed NFW profile is a good approximation for our projected halos. Additionally, we analyse the morphology of the halos, characterizing their triaxiality at R200 and calculating their orientation with respect to the line-of-sight (LOS). MICE halos tend to adopt a more prolate morphology, as might be expected from a  CDM simulation (Shaw et al. [159]), and the percentage of prolate halos grows as their mass grows. The mass resolution is, nonetheless, not good enough to draw conclusive inferences from the shape analysis, but it allows us to discern a trend and estimate the e§ect of halo shape and orientation on the weak lensing masses. Finally, we use the all-sky convergence maps to study the scatter in mass measurements of MICE halos. We determine the intrinsic scatter in the recovered masses by assuming the smoothed NFW profile as the ìtrueî profile, and creating two new convergence maps from different mass cuts. We estimate also the scatter due to the correlated structure by studying the angles between the major axes of the halos and the LOS, and also that due to projection e§ects (i.e. all the dark matter between observer and source). We find an irreducible scatter (intrinsic) of 10-14%, a scatter around a 30% of the intrinsic one due to correlated structure, and a scatter around 40-70% of the intrinsic one due to projection e§ects. The size of our halo sample allows us to improve the characterization of the cosmic noise, of great importance for present and future surveys.

### CROSS-CORRELATING SPECTROSCOPIC AND PHOTOMETRIC GALAXY SURVEYS

Estudiante: Martin B. Eriksen
Supervisada por: Enrique Gaztañaga
Universidad: Universitat Autònoma de Barcelona

CROSS-CORRELATING SPECTROSCOPIC AND PHOTOMETRIC GALAXY SURVEYS
Estudiante: Martin B. Eriksen
Supervisada por: Enrique Gaztañaga
Universidad: Universitat Autònoma de Barcelona

CROSS-CORRELATING SPECTROSCOPIC AND PHOTOMETRIC GALAXY SURVEYS

### Dynamically-generated baryon resonances with heavy flavor

Estudiante: Romanets, O. (KVI, University of Groningen)
Supervisada por: Tolos, L.; Timmermans, R. (KVI, University of Groningen)

To study the properties of exotic hadrons with charm and strange content under extreme conditions of density and temperature, with applications for astrophysical observables in neutron stars and supernovae as well as for the future FAIR project at GSI.
Study the properties of dynamically-generated baryon resonaces with strange and charm content
Estudiante: Romanets, O. (KVI, University of Groningen)
Supervisada por: Tolos, L.; Timmermans, R. (KVI, University of Groningen)

Study the properties of dynamically-generated baryon resonaces with strange and charm content

### Theories of modified gravity and reconstruction schemes of cosmological models

Estudiante: Antonio Jesús López Revelles
Supervisada por: Emilio Elizalde ; Sergei D Odintsov
Universidad: Universitat de Barcelona

The present thesis, aimed at obtaining the title of Philosophy Doctor in Physics, is based on the following papers published in referred journals, pre-prints and conference proceedings:  S. Capozziello, M. De Laurentis and A. J. Lopez-Revelles. Weak eld limit for F(R; G) modi ed gravities. In preparation. …
Estudiante: Antonio Jesús López Revelles
Supervisada por: Emilio Elizalde ; Sergei D Odintsov
Universidad: Universitat de Barcelona

The present thesis, aimed at obtaining the title of Philosophy Doctor in Physics, is based on the
following papers published in referred journals, pre-prints and conference proceedings:
 S. Capozziello, M. De Laurentis and A. J. Lopez-Revelles. Weak eld limit for F(R; G) modi ed
gravities. In preparation.
 K. Bamba, A. J. Lopez-Revelles, R. Myrzakulov, S. D. Odintsov, and L. Sebastiani. Cosmic history
of viable exponential gravity: Equation of state oscillations and growth index from in
ation to dark
energy era. Class. Quant. Grav. 30:015008 (2013).
 K. Bamba, A. J. Lopez-Revelles, R. Myrzakulov, S. D. Odintsov, and L. Sebastiani. The universe
evolution in exponential F(R) -gravity. Proceedings of QFTG2013, published in TSPU Bulletin 3
(128), 2012, n 13 p.19-24.
 E. Elizalde and A. J. Lopez-Revelles.Reconstructing cosmic acceleration from modi ed and nonmin-
imal gravity: The Yang-Mills case. Phys. Rev. D, 82:063504 (2010).
 E. Elizalde, A. J. Lopez-Revelles, S. D. Odintsov, and S. Yu. Vernov. Cosmological models with
Yang-Mills elds. Phys.Atom.Nucl., 76:996 (2013).
 A. J. Lopez-Revelles. Growth of matter perturbations for realistic F(R) models. Phys. Rev. D,
87:024021 (2013).
 A. J. Lopez-Revelles. Reconstructing cosmic acceleration from f(R) modi ed gravity. Proceedings
of ERE2011, Madrid. ArXiv: 1301.2190.
 A. J. Lopez-Revelles and E. Elizalde. Universal procedure to cure future singularities of dark energy
models. Gen. Rel. Grav., 44:751 (2012).
 A. J. Lopez-Revelles, R. Myrzakulov and D. Saez-Gomez. Ekpyrotic universes in F(R) Horava-
Lifshitz gravity. Phys. Rev. D, 85:103521 (2012).

### Measuring Large Scale Structure using angular cross-correlations

Estudiante: Jacobo Asorey Barreiro
Supervisada por: Enrique Gaztañaga ; Martin Crocce
Universidad: Universitat Autònoma de Barcelona

In this thesis we propose to use galaxy clustering, more concretely angular cross-correlations, as a tool to understand the late-time expansion of the Universe and the growth of large-scale structure. Galaxy surveys measure the position of galaxies (what traces the dark- matter field) in spherical coordinates…
Estudiante: Jacobo Asorey Barreiro
Supervisada por: Enrique Gaztañaga ; Martin Crocce
Universidad: Universitat Autònoma de Barcelona

In this thesis we propose to use galaxy clustering, more concretely angular cross-correlations, as a tool to understand the late-time expansion of the Universe and the growth of large-scale structure. Galaxy surveys measure the position of galaxies (what traces the dark- matter field) in spherical coordinates (z,θ,φ). Most galaxy clustering analyses convert these positions to distances assuming a background cosmology. This approach thus requires doing the full data analysis for each background cosmological model one wants to test. Instead we propose to select galaxies in radial shells, according to their redshifts, and then measure and analyse the angular (2D) correlations in each bin circumventing the model assumption. Remarkably, we find that if we include in the analysis also the angular cross-correlations between different shells, we can recover the radial modes corresponding to the separations between radial bins. We extend this analysis to photometric galaxy surveys, such as Physics of the Accelerating Universe (PAU) and Dark Energy Survey (DES). Angular analysis in redshift bins is then the natural framework for such surveys. We show that we can obtain competitive constraints on the growth history of the Universe at high redshifts (z~1). Finally, we built galaxy survey mocks from the MICE simulations, including non-linear gravitational effects and observational ones such as redshift-space distortions and photo-z errors.  We found a good agreement between theory and simulation measurements. In the future, we expect to apply this framework for cosmological parameter estimation, especially focusing on DES and PAU surveys.

### Gamma-ray emission of young stellar objects and discovery of superorbital variability at high energies

Supervisada por: Diego F. Torres ; Font, Ll. (UAB)
Universidad: Universitat Autònoma de Barcelona

UAB Abstract - Department of Physics - Doctor of Physics   Gamma-ray emission of young stellar objects and discovery of super orbital variability at high energies   by Daniela Hadasch   This thesis is structured in three parts: 1.) Observations of binary systems with the Fermi…
Supervisada por: Diego F. Torres ; Font, Ll. (UAB)
Universidad: Universitat Autònoma de Barcelona

UAB Abstract - Department of Physics - Doctor of Physics   Gamma-ray emission of young stellar objects and discovery of super orbital variability at high energies   by Daniela Hadasch   This thesis is structured in three parts: 1.) Observations of binary systems with the Fermi satellite and first discovery of superorbital modulation at high energies in the system LS I +61 ◦303, 2.) Studies of magnetars at high and at very high energies and deriving first upper limits on their γ-ray emission and 3.) Studies of the prospects forobservations of binary systems with the forthcoming Cherenkov Telescope Array.

### GNSS-R as a Source of Opportunity for Remote Sensing of the Cryosphere

Estudiante: Fran Fabra Cervellera
Supervisada por: Estel Cardellach Galí
Universidad: Universitat Politècnica de Catalunya

This work evaluates the potential use of signals from the Global Navigation Satellite Systems (GNSS) that scatter off the Earth surface for the retrieval of geophysical information from the cryosphere. For this purpose, the present study is based on data collected with a dedicated reflectometry GNSS…
Estudiante: Fran Fabra Cervellera
Supervisada por: Estel Cardellach Galí
Universidad: Universitat Politècnica de Catalunya

This work evaluates the potential use of signals from the Global Navigation Satellite Systems (GNSS) that scatter off the Earth surface for the retrieval of geophysical information from the cryosphere. For this purpose, the present study is based on data collected with a dedicated reflectometry GNSS receiver during two field campaigns, which were focused on two types of characteristic surfaces of the cryosphere: thin sea ice covers and thick dry snow accumulations. During the first experiment, the complete process of formation, evolution and melting of sea ice was monitorized for more than seven months in a bay located in Greenland. This type of ice is typically characterized by its thickness, concentration and roughness. Different observables from GNSS reflections are analyzed to try to infer these properties. The ice thickness is linked to the free-board level, defined as the height of the sea ice
surface. Accurate phase altimetry is achieved, showing good agreement with an Arctic tide model. In addition, the long term results of ellipsoidal height retrievals are consistent with the evolution of the ice surface temperature product given by MODIS, which is a key parameter in the rate of growth of sea ice. On the other hand, the presence of salinity in the sea ice modifies its dielectric properties, resulting in different amplitude and phase for the co- and cross-polar components of the complex Fresnel coefficients. The polarimetric measurements obtained show good agreement with visual inspections of ice concentration from an Arctic weather station. Finally, the shape of the reflected signals and its phase dispersion are tested as potential signatures of surface roughness. For comparison, ice charts of the experimental area are employed. In particular, maximums in roughness given by the GNSS observables coincide with fast ice events. Fast ice is defined as ice anchored to the coast, where the tidal movements contribute to the development of strange patterns, cracks, and fissures on its surface, thus consistent with the GNSS-R roughness retrievals. The second experiment took place on Antarctica, monitoring a pristine snow area which is well-known for the calibration of remote sensing instruments. Due to the relative stability of the snow layers, the data acquisition was limited to ten continuous days. Interferometric beats were found after a first analysis of the amplitude from the collected signals, which were consistent with a multipath model where the reflector lies below the surface level. Motivated by these results, a forward model is developed that reconstructs the complex received signal as a sum of a finite number of reflections, coming from different snow layers (a snow density profile obtained from in-situ measurements). The interferometric information is then retrieved from the spectral analysis applied to time series from both real and modeled signals (lag-holograms). We find that the frequency bands predicted by the model are in general consistent with the data and the lag-holograms show repeatability for different days. Then, we attempt a proper inversion of the collected data to determine the dominant layers of the dry snow profile that contribute to L-band reflections, which are related to significant gradients of snow density/permittivity.

### Populating cosmological simulations with galaxy using the HOD model

Estudiante: Jorge Carretero Palacios
Supervisada por: Francisco Javier Castander Serentill; Enrique Gaztañaga
Universidad: Universitat Autònoma de Barcelona

We want to produce galaxy catalogs from N-body dark matter simulations. Those catalogs should be compare to real data and in this way we will learn about the process of galaxy formation.
Populating cosmological simulations with galaxy using the HOD model
Estudiante: Jorge Carretero Palacios
Supervisada por: Francisco Javier Castander Serentill; Enrique Gaztañaga
Universidad: Universitat Autònoma de Barcelona

Populating cosmological simulations with galaxy using the HOD model

### The role of magnetic fields in the formation of low and high mass stars

Estudiante: Frau, P.
Supervisada por: Josep Miquel Girart Medina; Beltrán, M. T.
Universidad: Universitat de Barcelona

The complex interplay among self-gravity, thermal support, turbulence, rotation, and magnetic fields, and ultimately the observable features that arise from them, are not well characterized observationally and, therefore, not well understood theoretically. The fact that the starless cores are diffuse and cold objects, makes them very difficult of observing because their emission is very faint. Our goal in this work is to deepen into the understanding of the formation, survival and evolution of low-mass dense cores. We doubly face this objective since we aim: Firstly, to characterize observationally the physical and chemical properties of magnetized starless dense cores in the earliest stages of evolution to derive the initial conditions for star-formation, and to check whether the magnetic field is playing a role in the evolution of the cores and; Secondly, to compare observations of more evolved Class 0 sources with models of collapse of magnetized clouds to find the most likely initial conditions and dominant physical processes. In order to achieve the first goal, we have selected a sample of starless cores of the Pipe Nebula. This nearby dark molecular cloud complex has a very low star formation efficiency, which makes it an ideal target to study the properties and evolution of pristine starless dense cores. For the second goal, we have selected NGC 1333 IRAS 4A. It is probably the best studied low-mass protostellar dense core, not only through molecular and dust emission, but also through high angular resolution polarimetric observations of the dust emission.
The complex interplay among self-gravity, thermal support, turbulence, rotation, and magnetic fields, and ultimately the observable features that arise from them, are not well characterized observationally and, therefore, not well understood theoretically. The fact that the starless cores are diffuse…
Estudiante: Frau, P.
Supervisada por: Josep Miquel Girart Medina; Beltrán, M. T.
Universidad: Universitat de Barcelona

The complex interplay among self-gravity, thermal support, turbulence, rotation, and magnetic fields, and ultimately the observable features that arise from them, are not well characterized observationally and, therefore, not well understood theoretically. The fact that the starless cores are diffuse and cold objects, makes them very difficult of observing because their emission is very faint. Our goal in this work is to deepen into the understanding of the formation, survival and evolution of low-mass dense cores. We doubly face this objective since we aim: Firstly, to characterize observationally the physical and chemical properties of magnetized starless dense cores in the earliest stages of evolution to derive the initial conditions for star-formation, and to check whether the magnetic field is playing a role in the evolution of the cores and; Secondly, to compare observations of more evolved Class 0 sources with models of collapse of magnetized clouds to find the most likely initial conditions and dominant physical processes. In order to achieve the first goal, we have selected a sample of starless cores of the Pipe Nebula. This nearby dark molecular cloud complex has a very low star formation efficiency, which makes it an ideal target to study the properties and evolution of pristine starless dense cores. For the second goal, we have selected NGC 1333 IRAS 4A. It is probably the best studied low-mass protostellar dense core, not only through molecular and dust emission, but also through high angular resolution polarimetric observations of the dust emission.
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