Baryon Resonances

In this talk I show recent results on how many excited baryon resonances appear as systems of one meson and one baryon, or two mesons and one baryon, with the mesons being either pseudoscalar or vectors. Connection with experiment is made including a discussion on old predictions and recent results for the photoproduction of the $\Lambda(1405)$ resonance, as well as the prediction of one $1/2^+$ baryon state around 1920 MeV which might have been seen in the $\gamma p \to K^+ \Lambda$ reaction.Comment: Talk given at the 10th International Conference on Hypernuclear and Strange Particle Physics, Tokai, Japan, Sptember 200

Dynamically generated resonances from the vector octet-baryon decuplet interaction

We study the interaction of the octet of vector mesons with the decuplet of baryons using Lagrangians of the hidden gauge theory for vector interactions. The unitary amplitudes in coupled channels develop poles that can be associated with some known baryonic resonances, while there are predictions for new ones at the energy frontier of the experimental research. The work offers guidelines on how to search for these resonances

Meson and Baryon resonances

In this talk I review recent advances on the structure of the meson and baryon resonances which can be dynamically generated from the interaction of mesons or mesons and baryons. Particular emphasis is put on results involving vector mesons, which bring new light into the nature of some of the observed higher mass mesons and baryons and make predictions for new states.Comment: 6 pages, Talk at the PANIC2008 Conferenc

ESPAI GEA: A new platform for promoting Geology in Catalonia

X Congreso Geológico de España, 5-7 Julio 2021, Vitoria - GasteizESPAI GEA es una comunidad abierta que nace con el objetivo de promover las Ciencias de la Tierra y divulgar la importancia del conocimiento geológico entre la ciudadanía. La voluntad de ESPAI GEA es la de conectar a todas las instituciones, asociaciones, entidades, museos, centros de interpretación, etc., que realizan actividades relacionadas con las Ciencias de la Tierra y la Geología en el territorio catalán. La primera acción que se está llevando a cabo desde ESPAI GEA es la de crear una agenda con el objetivo de centralizar las actividades de divulgación en una única plataforma que sirva al mismo tiempo de escaparate y altavoz. Con estas premisas se está implementando la agenda en un visor web, en el que se mostrarán principalmente dos tipos de información: i) por una parte, actividades y eventos de carácter temporal, y ii) por otra parte, la geolocalización de información geológica disponible permanentemente (paneles informativos, itinerarios geológicos, área geográfica de las guías publicadas, centros de interpretación, museos, centros de investigación, u otras instalaciones singulares relacionadas) así como otra información de interés complementaria. ESPAI GEA también quiere incidir de una manera muy especial en la comunidad educativa, realizando actividades formativas, proporcionando recursos didácticos y favoreciendo la actualización científica del profesorado.ESPAI GEA is an open community that is born with the aim of promoting Earth Sciences and to disseminate the importance of geological knowledge among citizens. The goal of ESPAI GEA is to connect all the institutions, associations, entities, museums, interpretation centres, etc., that carry out activities related to Earth Sciences and Geology in the Catalan territory. The first action undertaken within ESPAI GEA is to create an agenda to assemble all the dissemination activities in a common platform that works both as a showcase and as amplifier of the activities. Under these premises, the agenda is being implemented into a web viewer, this will display two main types of data; i) on the one hand, temporary activities and events, and ii) on the other hand, the location of existing permanent geological data (information boards, geological itineraries, geographical areas of published guides, interpretation centres, museums, research centres, etc.) along with other information. ESPAI GEA wants to pay special attention to the educational community, carrying out training activities, providing instructional resources and promoting continuing education in Geology for teacher community.Peer reviewe

AGILE detection of extreme gamma-ray activity from the blazar PKS 1510-089 during March 2009. Multifrequency analysis

We report on the extreme gamma-ray activity from the FSRQ PKS 1510-089 observed by AGILE in March 2009. In the same period a radio-to-optical monitoring of the source was provided by the GASP-WEBT and REM. Moreover, several Swift ToO observations were triggered, adding important information on the source behaviour from optical/UV to hard X-rays. We paid particular attention to the calibration of the Swift/UVOT data to make it suitable to the blazars spectra. Simultaneous observations from radio to gamma rays allowed us to study in detail the correlation among the emission variability at different frequencies and to investigate the mechanisms at work. In the period 9-30 March 2009, AGILE detected an average gamma-ray flux of (311+/-21)x10^-8 ph cm^-2 s^-1 for E>100 MeV, and a peak level of (702+/-131)x10^-8 ph cm^-2 s^-1 on daily integration. The gamma-ray activity occurred during a period of increasing activity from near-IR to UV, with a flaring episode detected on 26-27 March 2009, suggesting that a single mechanism is responsible for the flux enhancement observed from near-IR to UV. By contrast, Swift/XRT observations seem to show no clear correlation of the X-ray fluxes with the optical and gamma-ray ones. However, the X-ray observations show a harder photon index (1.3-1.6) with respect to most FSRQs and a hint of harder-when-brighter behaviour, indicating the possible presence of a second emission component at soft X-ray energies. Moreover, the broad band spectrum from radio-to-UV confirmed the evidence of thermal features in the optical/UV spectrum of PKS 1510-089 also during high gamma-ray state. On the other hand, during 25-26 March 2009 a flat spectrum in the optical/UV energy band was observed, suggesting an important contribution of the synchrotron emission in this part of the spectrum during the brightest gamma-ray flare, therefore a significant shift of the synchrotron peak.Comment: 13 pages, 7 figures, 3 tables. Accepted for publication in Astronomy and Astrophysic

Highlights from the Pierre Auger Observatory

The Pierre Auger Observatory is the world's largest cosmic ray observatory. Our current exposure reaches nearly 40,000 km$^2$ str and provides us with an unprecedented quality data set. The performance and stability of the detectors and their enhancements are described. Data analyses have led to a number of major breakthroughs. Among these we discuss the energy spectrum and the searches for large-scale anisotropies. We present analyses of our X$_{max}$ data and show how it can be interpreted in terms of mass composition. We also describe some new analyses that extract mass sensitive parameters from the 100% duty cycle SD data. A coherent interpretation of all these recent results opens new directions. The consequences regarding the cosmic ray composition and the properties of UHECR sources are briefly discussed.Comment: 9 pages, 12 figures, talk given at the 33rd International Cosmic Ray Conference, Rio de Janeiro 201

A search for point sources of EeV photons

Measurements of air showers made using the hybrid technique developed with the fluorescence and surface detectors of the Pierre Auger Observatory allow a sensitive search for point sources of EeV photons anywhere in the exposed sky. A multivariate analysis reduces the background of hadronic cosmic rays. The search is sensitive to a declination band from -85{\deg} to +20{\deg}, in an energy range from 10^17.3 eV to 10^18.5 eV. No photon point source has been detected. An upper limit on the photon flux has been derived for every direction. The mean value of the energy flux limit that results from this, assuming a photon spectral index of -2, is 0.06 eV cm^-2 s^-1, and no celestial direction exceeds 0.25 eV cm^-2 s^-1. These upper limits constrain scenarios in which EeV cosmic ray protons are emitted by non-transient sources in the Galaxy.Comment: 28 pages, 10 figures, accepted for publication in The Astrophysical Journa