Metodologia Para Estimação Das Constantes ópticas E Da Espessura De Um Filme Fino Utilizando Minimização Irrestrita

Metodologia para estimação das constantes ópticas e da espessura de um filme fino utilizando minimização irrestrita, dita metodologia destina-se a possibilitar a estimação das constantes ópticas e da espessura de um filme fino, baseada na minimização irrestrita.BR9901600 (A)G01B11/06G01B11/06BR19999901600G01B11/06G01B11/0

Localización de zonas de cizalla y de contactos intrusivos en la Sierra de Velasco (Argentina), mediante análisis gravimétrico

Mediante la aplicación de la metodología de Deconvolución de Euler, se pueden identificar y hacer estimaciones de profundidad para una variedad de estructuras geológicas tales como fallas, contactos, diques, plutones, etc. La gran ventaja de esta técnica es que no asume ningún modelo geológico en particular, pudiendo aplicarse directamente a datos regularizados. La aplicación de este método a la carta gravimétrica de Sierra de Velasco (con índices estructurales que variaron entre 0,5, 1Y2) permitió obtener un conjunto de soluciones, en un rango de profundidades que van desde unos pocos metros hasta 24 km. Estas soluciones pueden aplicarse a discontinuidades litológicas de la corteza, tales como la zona de cizalla TIPA,o bien el plano de intrusivo entre el plutónSan Bias con el Granito Asha. Estas discontinuidades geológicas son observadas en superficie, pero la determinación y continuación en profundidad no era posiblecon herramientasgeológicas tradicionales. Se identifican además, dos sistemas de fallas inversas que elevan la sierra (por el noreste y por el noroeste), que son de tipo inverso y se hacen lístricas en profundidad. Las mismas como se sabe responden a la orogenia Andina, que levantan las Sierras Pampeanas, dándole la actual configuración morfológicaa laSierra deVelasco.By means of the Eu/er Deeonvolueión methodology, they ean be identified and depth estima te for a variety of ge%gie struetures, sueh as fau/ts, eontacts, dikes, p/utons, etc. The great advantage of this technique is that it does not assume any particular ge%gic pattem, being been ab/e to app/y directly to sprouted data. The app/ieation of this method to the gravimetric chart of the Sierra de Ve/asco (with struetura/ indexes that varied between 0.5, 1 and 2) it allowed to obtain a group of so/utions, in a range of depths that they go from some few meters to 24 km. These so/utions can be applied to the /ith%gic diseontinuities of the erust, such as the shear TlPA area, or the intrusive eontact p/ane between the San B/as p/uton and the Asha granite. These ge%gic discontinuities are observed in surface, but the determination and continuation in depth it was not possib/e. Theyare a/so idenfified, two systems of in verse faults that e/evate the mountains (for the northeast and for the northwest). These faults are of upthrust type and they are made listrie in depth. These fau/ts as ii is known they respond to the Andean orogeny that the Sierras Pampeanas get up, giving the current motpñoloqic conñquretion to the Sierra of Ve/asco.Fil: Martinez, M. Patricia. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Instituto Geofísico Sismológico Volponi; ArgentinaFil: Gimenez, Mario Ernesto. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Instituto Geofísico Sismológico Volponi; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Toselli, Alejandro Jose. Universidad Nacional de Tucumán. Facultad de Ciencias Naturales e Instituto Miguel Lillo. Departamento de Geología; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Rossi de Toselli, Juana. Universidad Nacional de Tucumán. Facultad de Ciencias Naturales e Instituto Miguel Lillo. Departamento de Geología; ArgentinaFil: Ruiz, F.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Instituto Geofísico Sismológico Volponi; ArgentinaFil: Introcaso, Antonio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Rosario. Instituto de Física de Rosario. Universidad Nacional de Rosario. Instituto de Física de Rosario; ArgentinaFil: Novara, Ivan Lionel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Rosario. Instituto de Física de Rosario. Universidad Nacional de Rosario. Instituto de Física de Rosario; Argentin

Localización de zonas de cizalla y de contactos intrusivos en la Sierra de Velasco (Argentina), mediante análisis gravimétrico

Mediante la aplicación de la metodología de Deconvolución de Euler, se pueden identificar y hacer estimaciones de profundidad para una variedad de estructuras geológicas tales como fallas, contactos, diques, plutones, etc. La gran ventaja de esta técnica es que no asume ningún modelo geológico en particular, pudiendo aplicarse directamente a datos regularizados. La aplicación de este método a la carta gravimétrica de Sierra de Velasco (con índices estructurales que variaron entre 0,5, 1Y2) permitió obtener un conjunto de soluciones, en un rango de profundidades que van desde unos pocos metros hasta 24 km. Estas soluciones pueden aplicarse a discontinuidades litológicas de la corteza, tales como la zona de cizalla TIPA,o bien el plano de intrusivo entre el plutónSan Bias con el Granito Asha. Estas discontinuidades geológicas son observadas en superficie, pero la determinación y continuación en profundidad no era posiblecon herramientasgeológicas tradicionales. Se identifican además, dos sistemas de fallas inversas que elevan la sierra (por el noreste y por el noroeste), que son de tipo inverso y se hacen lístricas en profundidad. Las mismas como se sabe responden a la orogenia Andina, que levantan las Sierras Pampeanas, dándole la actual configuración morfológicaa laSierra deVelasco.By means of the Eu/er Deeonvolueión methodology, they ean be identified and depth estima te for a variety of ge%gie struetures, sueh as fau/ts, eontacts, dikes, p/utons, etc. The great advantage of this technique is that it does not assume any particular ge%gic pattem, being been ab/e to app/y directly to sprouted data. The app/ieation of this method to the gravimetric chart of the Sierra de Ve/asco (with struetura/ indexes that varied between 0.5, 1 and 2) it allowed to obtain a group of so/utions, in a range of depths that they go from some few meters to 24 km. These so/utions can be applied to the /ith%gic diseontinuities of the erust, such as the shear TlPA area, or the intrusive eontact p/ane between the San B/as p/uton and the Asha granite. These ge%gic discontinuities are observed in surface, but the determination and continuation in depth it was not possib/e. Theyare a/so idenfified, two systems of in verse faults that e/evate the mountains (for the northeast and for the northwest). These faults are of upthrust type and they are made listrie in depth. These fau/ts as ii is known they respond to the Andean orogeny that the Sierras Pampeanas get up, giving the current motpñoloqic conñquretion to the Sierra of Ve/asco.Fil: Martinez, M. Patricia. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Instituto Geofísico Sismológico Volponi; ArgentinaFil: Gimenez, Mario Ernesto. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Instituto Geofísico Sismológico Volponi; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Toselli, Alejandro Jose. Universidad Nacional de Tucumán. Facultad de Ciencias Naturales e Instituto Miguel Lillo. Departamento de Geología; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Rossi de Toselli, Juana. Universidad Nacional de Tucumán. Facultad de Ciencias Naturales e Instituto Miguel Lillo. Departamento de Geología; ArgentinaFil: Ruiz, F.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Instituto Geofísico Sismológico Volponi; ArgentinaFil: Introcaso, Antonio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Rosario. Instituto de Física de Rosario. Universidad Nacional de Rosario. Instituto de Física de Rosario; ArgentinaFil: Novara, Ivan Lionel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Rosario. Instituto de Física de Rosario. Universidad Nacional de Rosario. Instituto de Física de Rosario; Argentin

Cancer immunotherapy in special challenging populations: recommendations of the Advisory Committee of Spanish Melanoma Group (GEM)

Cancer immunotherapy based on the use of antibodies targeting the so-called checkpoint inhibitors, such as programmed cell death-1 receptor, its ligand, or CTLA-4, has shown durable clinical benefit and survival improvement in melanoma and other tumors. However, there are some special situations that could be a challenge for clinical management. Persons with chronic infections, such as HIV-1 or viral hepatitis, latent tuberculosis, or a history of solid organ transplantation, could be candidates for cancer immunotherapy, but their management requires a multidisciplinary approach. The Spanish Melanoma Group (GEM) panel in collaboration with experts in virology and immunology from different centers in Spain reviewed the literature and developed evidence-based guidelines for cancer immunotherapy management in patients with chronic infections and immunosuppression. These are the first clinical guidelines for cancer immunotherapy treatment in special challenging populations. Cancer immunotherapy in chronically infected or immunosuppressed patients is feasible but needs a multidisciplinary approach in order to decrease the risk of complications related to the coexistent comorbidities

The Fifth Data Release of the Sloan Digital Sky Survey

This paper describes the Fifth Data Release (DR5) of the Sloan Digital Sky Survey (SDSS). DR5 includes all survey quality data taken through June 2005 and represents the completion of the SDSS-I project (whose successor, SDSS-II will continue through mid-2008). It includes five-band photometric data for 217 million objects selected over 8000 square degrees, and 1,048,960 spectra of galaxies, quasars, and stars selected from 5713 square degrees of that imaging data. These numbers represent a roughly 20% increment over those of the Fourth Data Release; all the data from previous data releases are included in the present release. In addition to "standard" SDSS observations, DR5 includes repeat scans of the southern equatorial stripe, imaging scans across M31 and the core of the Perseus cluster of galaxies, and the first spectroscopic data from SEGUE, a survey to explore the kinematics and chemical evolution of the Galaxy. The catalog database incorporates several new features, including photometric redshifts of galaxies, tables of matched objects in overlap regions of the imaging survey, and tools that allow precise computations of survey geometry for statistical investigations.Comment: ApJ Supp, in press, October 2007. This paper describes DR5. The SDSS Sixth Data Release (DR6) is now public, available from http://www.sdss.or

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