The regional network capital index in Mexico from 2012 to 2016

Abstract Based-off the regional development theory developed from knowledge and innovation, Huggins & Thompson [1] have proposed the concept of Network Capital, which aims to explain the importance of knowledge flow, knowledge absorptive capacity and investments on associations between firms and Universities or Scientific Centers or other firms in order to increase regional development. This paper used empirical data from Mexico for the period 2012–2016 to propose an alternative to the calculation of Network Capital at State level as an alternative to the Huggins and Thompson proposal. The data used cover all the 32 Mexican States about innovation activities. On this paper is shown the deep differences between Mexican States about the knowledge qualities, the absorptive capacity of knowledge and the investments on strategic associations, it that might be typical at non-innovation Nations. Although the proposal on this paper cannot be directly compared to that of Huggins and Thompson, both shows evidence that, the greater network capital, the greater the potential development based on knowledge

PROGRAMAS DE ESTIMULOS A LA INNOVACION EMPRESARIAL EN MEXICO, PRINCIPALES CIFRAS Y RESULTADOS

México se encuentra en el lugar 56 de 126 países en el Global Innovation Index 2018, un índice elaborado en conjunto por la Universidad de Cornell y Organización Mundial de Propiedad Intelectual, el indicador identifica como muy débil el aspecto de inversión y financiamiento a la innovación en México, pilar donde se sitúa en el lugar 102 de 126 países. El gasto en actividades de Innovación y Desarrollo en México proviene en su mayoría del gobierno federal, el cual lleva a cabo programas para incentivar la inversión del sector privado, que tan solo contribuye con un 22 por ciento, mientras que el resto proviene tanto de los gobiernos estatales a través de universidades y diversas fuentes de índole internacional. Este documento plantea hacer uso de un análisis descriptivo para obtener un balance del estado actual de las principales cifras y resultados que permitan identificar los sectores de actividad económica, los estados y las empresas más beneficiadas por los dos principales programas de estímulos a la innovación empresarial en México en el periodo de 2009 a 2018, con el fin de destacar elementos importantes en la operación de éstos en el contexto de las empresas mexicanas. Estos programas son el Programa de Estímulos a la Innovación (PEI) y el Estímulo Fiscal a la investigación y Desarrollo de la Tecnología (EFIDT). El tema de ésta investigación resulta de interés en el momento actual, ya que ha sido motivo de controversia de los actuales cambios en el marco de la política de la nueva administración federal, en el caso concreto el Programa de Estímulos a la innovación que recientemente ha sido cancelado. Los resultados del análisis descriptivo del programa también nos alertan de la necesidad de seguir profundizando en un diseño de políticas públicas en materia de CTI en mejorar la correcta distribución de los recursos de los programas de apoyo a las actividades de innovación de las empresas con una perspectiva local, regional y sectorial que considere las áreas de oportunidad respectivas. El reto, radica en este sentido en las brechas entre los estados, los sectores y las empresas más desarrolladas y el resto parece que se está ampliando y no reduciendo. El balance de las cifras a casi 20 años de operación de los programas de estímulos directos e indirectos a la innovación en las empresas desde 2001 a 2018, nos muestran una alta concentración tanto en el número de proyectos aprobados como en el monto de los recursos otorgados a un grupo de regiones, sectores industriales y grandes empresas beneficiarias de los programas

Measurement of the cosmic ray spectrum above 4×10184{\times}10^{18} eV using inclined events detected with the Pierre Auger Observatory

A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\gamma}$ with index $\gamma=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV.Comment: Replaced with published version. Added journal reference and DO

Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy deposit per area is determined from the radio pulses at each observer position and is interpolated using a two-dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge-excess emission components. The spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy -- corrected for geometrical effects -- is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. We find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal.Comment: Replaced with published version. Added journal reference and DO

Measurement of the Radiation Energy in the Radio Signal of Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy

We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 \pm 0.7 (stat) \pm 6.7 (sys) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cosmic-ray energy. A comparison with predictions from state-of-the-art first-principle calculations shows agreement with our measurement. The radiation energy provides direct access to the calorimetric energy in the electromagnetic cascade of extensive air showers. Comparison with our result thus allows the direct calibration of any cosmic-ray radio detector against the well-established energy scale of the Pierre Auger Observatory.Comment: Replaced with published version. Added journal reference and DOI. Supplemental material in the ancillary file

A search for ultra-high-energy photons at the Pierre Auger Observatory exploiting air-shower universality

The Pierre Auger Observatory is the most sensitive detector to primary photons with energies above ∼0.2 EeV. It measures extensive air showers using a hybrid technique that combines a fluorescence detector (FD) with a ground array of particle detectors (SD). The signatures of a photon-induced air shower are a larger atmospheric depth at the shower maximum (X$_{max}$) and a steeper lateral distribution function, along with a lower number of muons with respect to the bulk of hadron-induced background. Using observables measured by the FD and SD, three photon searches in different energy bands are performed. In particular, between threshold energies of 1-10 EeV, a new analysis technique has been developed by combining the FD-based measurement of X$_{max}$ with the SD signal through a parameter related to its muon content, derived from the universality of the air showers. This technique has led to a better photon/hadron separation and, consequently, to a higher search sensitivity, resulting in a tighter upper limit than before. The outcome of this new analysis is presented here, along with previous results in the energy ranges below 1 EeV and above 10 EeV. From the data collected by the Pierre Auger Observatory in about 15 years of operation, the most stringent constraints on the fraction of photons in the cosmic flux are set over almost three decades in energy

Study on multi-ELVES in the Pierre Auger Observatory

Since 2013, the four sites of the Fluorescence Detector (FD) of the Pierre Auger Observatory record ELVES with a dedicated trigger. These UV light emissions are correlated to distant lightning strikes. The length of recorded traces has been increased from 100 μs (2013), to 300 μs (2014-16), to 900 μs (2017-present), to progressively extend the observation of the light emission towards the vertical of the causative lightning and beyond. A large fraction of the observed events shows double ELVES within the time window, and, in some cases, even more complex structures are observed. The nature of the multi-ELVES is not completely understood but may be related to the different types of lightning in which they are originated. For example, it is known that Narrow Bipolar Events can produce double ELVES, and Energetic In-cloud Pulses, occurring between the main negative and upper positive charge layer of clouds, can induce double and even quadruple ELVES in the ionosphere. This report shows the seasonal and daily dependence of the time gap, amplitude ratio, and correlation between the pulse widths of the peaks in a sample of 1000+ multi-ELVES events recorded during the period 2014-20. The events have been compared with data from other satellite and ground-based sensing devices to study the correlation of their properties with lightning observables such as altitude and polarity