Efectos de la fecha de siembra sobre el rendimiento y calidad comercial del maíz dulce (Zea Mays L., var. saccharata körn)

El efecto de la fecha de siembra sobre la producción y calidad del cultivo de maíz dulce en el norte de la provincia de Buenos Aires no ha sido estudiado y su conocimiento resulta de suma importancia para la planificación y obtención de resultados óptimos y viabilidad comercial para los productores de dicha zona. En base a esta problemática se estudió el efecto de tres fechas de siembra: 28 de octubre, 9 de noviembre y 5 de diciembre 2009 (fecha 1, 2 y 3, respectivamente) sobre el rendimiento y calidad comercial de Maíz Dulce (Zea Mays L., var. saccharata körn). La hipótesis principal que guió este trabajo fue que el atraso de la fecha de siembra reduciría el tamaño y peso de la espiga de maíz dulce afectando sus parámetros comerciales. Para poner a prueba esta hipótesis, se realizó un ensayo a campo en la localidad de Capilla del Señor, provincia de Buenos Aires. En las tres fechas mencionadas se sembró el híbrido Cahill (P) de un ciclo en fecha de siembra óptima de 75 días. El manejo de los cultivos respondió a un manejo convencional de la zona. Durante el ciclo del cultivo se llevaron a cabo determinaciones densidad y área foliar por planta. El momento de la cosecha se determinó por el método de apreciación visual del grano lechoso. Se tomaron muestras de espigas para la determinación de rendimiento y calidad comercial. El área foliar por planta no presentó diferencias significativas entre la fecha 2 y3, sin embargo hubo una tendencia hacia una mayor área foliar en la fecha 2 (2826 cm2 ± 256) que en la fecha 3 (2596 cm2 ± 256). Además, fue la fecha en la que la radiación acumulada incidente fue mayor (1605 mj/m2) en el ciclo de cultivo, ya que ésta fue en aumento desde principios de octubre hasta fines de enero; a partir de ese momento la radiación cayó marcadamente, coincidiendo con el ciclo del cultivo de la fecha 3 (1555 mj/m2). La mayor radiación incidente y la mayor capacidad de captura de la misma (Área Foliar) se tradujo en un mayor peso de la espiga (270 ± 58 gr) para los cultivos sembrados en la fecha 2 respecto de los de la fecha 3 (204 ± 58) y la fecha 1 (190 ± 58). Por otro lado, los cultivos en la fecha 2 presentaron mejor relación grano/marlo (2,57 ± 0,29) y mayor cantidad de granos comerciales (446 ± 45 granos/espiga) diferenciándose significativamente de los cultivos sembrados en la fecha 3 (1,97 ± 0,29) y la fecha 1 (0,92 ± 0,29) para la relación grano/marlo y también para los granos comerciales, 384 ± 45 y 394 ± 45 en los cultivos de la fecha 3 y 1, respectivamente. En vista de los resultados obtenidos se recomienda la fecha de principios de noviembre como fecha óptima de siembra ya que fue en la que se obtuvo el mayor rendimiento y mejor calidad de producto

FACT - Long-term stability and observations during strong Moon light

The First G-APD Cherenkov Telescope (FACT) is the first Cherenkov telescope equipped with a camera made of silicon photon detectors (G-APD aka. SiPM). Since October 2011, it is regularly taking data on the Canary Island of La Palma. G-APDs are ideal detectors for Cherenkov telescopes as they are robust and stable. Furthermore, the insensitivity of G-APDs towards strong ambient light allows to conduct observations during bright Moon and twilight. This gain in observation time is essential for the long-term monitoring of bright TeV blazars. During the commissioning phase, hundreds of hours of data (including data from the the Crab Nebula) were taken in order to understand the performance and sensitivity of the instrument. The data cover a wide range of observation conditions including different weather conditions, different zenith angles and different light conditions (ranging from dark night to direct full Moon). We use a new parmetrisation of the Moon light background to enhance our scheduling and to monitor the atmosphere. With the data from 1.5 years, the long-term stability and the performance of the camera during Moon light is studied and compared to that achieved with photomultiplier tubes so far.Comment: 3 pages, 3 figures, FACT Contribution to the 33rd International Cosmic Ray Conference (ICRC), Rio de Janeir

FACT - Threshold prediction for higher duty cycle and improved scheduling

The First G-APD Cherenkov telescope (FACT) is the first telescope using silicon photon detectors (G-APD aka. SiPM). The use of Silicon devices promise a higher photon detection efficiency, more robustness and higher precision than photo-multiplier tubes. Being operated during different light-conditions, the threshold settings of a Cherenkov telescope have to be adapted to feature the lowest possible threshold but also an efficient suppression of triggers from night-sky background photons. Usually this threshold is set either by experience or a mini-ratescan. Since the measured current through the sensors is directly correlated with the noise level, the current can be used to set the best threshold at any time. Due to the correlation between the physical threshold and the final energy threshold, the current can also be used as a measure for the energy threshold of any observation. This presentation introduces a method which uses the properties of the moon and the source position to predict the currents and the corresponding energy threshold for every upcoming observation allowing to adapt the observation schedule accordingly

FACT - Long-term Monitoring of Bright TeV-Blazars

Since October 2011, the First G-APD Cherenkov Telescope (FACT) is operated successfully on the Canary Island of La Palma. Apart from the proof of principle for the use of G-APDs in Cherenkov telescopes, the major goal of the project is the dedicated long-term monitoring of a small sample of bright TeV blazars. The unique properties of G-APDs permit stable observations also during strong moon light. Thus a superior sampling density is provided on time scales at which the blazar variability amplitudes are expected to be largest, as exemplified by the spectacular variations of Mrk 501 observed in June 2012. While still in commissioning, FACT monitored bright blazars like Mrk 421 and Mrk 501 during the past 1.5 years so far. Preliminary results including the Mrk 501 flare from June 2012 will be presented.Comment: 4 pages, 4 figures, presented at the 33rd ICRC (2013

FACT - How stable are the silicon photon detectors?

The First G-APD Cherenkov telescope (FACT) is the first telescope using silicon photon detectors (G-APD aka. SiPM). The use of Silicon devices promise a higher photon detection efficiency, more robustness and higher precision than photo-multiplier tubes. Since the properties of G-APDs depend on auxiliary parameters like temperature, a feedback system adapting the applied voltage accordingly is mandatory. In this presentation, the feedback system, developed and in operation for FACT, is presented. Using the extraction of a single photon-equivalent (pe) spectrum as a reference, it can be proven that the sensors can be operated with very high precision. The extraction of the single-pe, its spectrum up to 10\,pe, its properties and their precision, as well as their long-term behavior during operation are discussed. As a by product a single pulse template is obtained. It is shown that with the presented method, an additional external calibration device can be omitted. The presented method is essential for the application of G-APDs in future projects in Cherenkov astronomy and is supposed to result in a more stable and precise operation than possible with photo-multiplier tubes

FACT - Monitoring Blazars at Very High Energies

The First G-APD Cherenkov Telescope (FACT) was built on the Canary Island of La Palma in October 2011 as a proof of principle for silicon based photosensors in Cherenkov Astronomy. The scientific goal of the project is to study the variability of active galatic nuclei (AGN) at TeV energies. Observing a small sample of TeV blazars whenever possible, an unbiased data sample is collected. This allows to study the variability of the selected objects on timescales from hours to years. Results from the first three years of monitoring will be presented. To provide quick flare alerts to the community and trigger multi-wavelength observations, a quick look analysis has been installed on-site providing results publicly online within the same night. In summer 2014, several flare alerts were issued. Results of the quick look analysis are summarized.Comment: 2014 Fermi Symposium proceedings - eConf C14102.