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

The Active Mirror Control of the MAGIC Telescope

One of the main design goals of the MAGIC telescopes is the very fast repositioning in case of Gamma Ray Burst (GRB) alarms, implying a low weight of the telescope dish. This is accomplished by using a space frame made of carbon fiber epoxy tubes, resulting in a strong but not very rigid support structure. Therefore it is necessary to readjust the individual mirror tiles to correct for deformations of the dish under varying gravitational load while tracking an object. We present the concept of the Active Mirror Control (AMC) as implemented in the MAGIC telescopes and the actual performance reached. Additionally we show that also telescopes using a stiff structure can benefit from using an AMC.Comment: Contribution to the 30th ICRC, Merida, Mexico, July 2007 on behalf of the MAGIC Collaboratio

Detection of Cherenkov light from air showers with Geiger-APDs

We have detected Cherenkov light from air showers with Geiger-mode APDs (G-APDs). G-APDs are novel semiconductor photon-detectors, which offer several advantages compared to conventional photomultiplier tubes in the field of ground-based gamma-ray astronomy. In a field test with the MAGIC telescope we have tested the efficiency of a G-APD / light catcher setup to detect Cherenkov light from air showers. We estimate a detection efficiency, which is 60% higher than the efficiency of a MAGIC camera pixel. Ambient temperature dark count rates of the tested G-APDs are below the rates of the night sky light background. According to these recent tests G-APDs promise a major progress in ground-based gamma-ray astronomy.Comment: 4 pages, 5 figures, to appear in the proceedings of the 30th International Cosmic Ray Conference, Merida, July 200

FlashCam: A fully digital camera for CTA telescopes

The future Cherenkov Telescope Array (CTA) will consist of several tens of telescopes of different mirror sizes. CTA will provide next generation sensitivity to very high energy photons from few tens of GeV to >100 TeV. Several focal plane instrumentation options are currently being evaluated inside the CTA consortium. In this paper, the current status of the FlashCam prototyping project is described. FlashCam is based on a fully digital camera readout concept and features a clean separation between photon detector plane and signal digitization/triggering electronics.Comment: In Proceedings of the 2012 Heidelberg Symposium on High Energy Gamma-Ray Astronomy. All CTA contributions at arXiv:1211.184

Mirror Position Determination for the Alignment of Cherenkov Telescopes

Imaging Atmospheric Cherenkov Telescopes (IACTs) need imaging optics with large apertures to map the faint Cherenkov light emitted in extensive air showers onto their image sensors. Segmented reflectors fulfill these needs using mass produced and light weight mirror facets. However, as the overall image is the sum of the individual mirror facet images, alignment is important. Here we present a method to determine the mirror facet positions on a segmented reflector in a very direct way. Our method reconstructs the mirror facet positions from photographs and a laser distance meter measurement which goes from the center of the image sensor plane to the center of each mirror facet. We use our method to both align the mirror facet positions and to feed the measured positions into our IACT simulation. We demonstrate our implementation on the 4 m First Geiger-mode Avalanche Cherenkov Telescope (FACT).Comment: 11 figures, small ray tracing performance simulation, and implementation demonstratio

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