51 research outputs found
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
First Study of Combined Blazar Light Curves with FACT and HAWC
For studying variable sources like blazars, it is crucial to achieve unbiased
monitoring, either with dedicated telescopes in pointing mode or survey
instruments. At TeV energies, the High Altitude Water Cherenkov (HAWC)
observatory monitors approximately two thirds of the sky every day. It uses the
water Cherenkov technique, which provides an excellent duty cycle independent
of weather and season. The First G-APD Cherenkov Telescope (FACT) monitors a
small sample of sources with better sensitivity, using the imaging air
Cherenkov technique. Thanks to its camera with silicon-based photosensors, FACT
features an excellent detector performance and stability and extends its
observations to times with strong moonlight, increasing the duty cycle compared
to other imaging air Cherenkov telescopes. As FACT and HAWC have overlapping
energy ranges, a joint study can exploit the longer daily coverage given that
the observatories' locations are offset by 5.3 hours. Furthermore, the better
sensitivity of FACT adds a finer resolution of features on hour-long time
scales, while the continuous duty cycle of HAWC ensures evenly sampled
long-term coverage. Thus, the two instruments complement each other to provide
a more complete picture of blazar variability. In this presentation, the first
joint study of light curves from the two instruments will be shown, correlating
long-term measurements with daily sampling between air and water Cherenkov
telescopes. The presented results focus on the study of the variability of the
bright blazars Mrk 421 and Mrk 501 during the last two years featuring various
flaring activities.Comment: 6 pages, 2 figures. Contribution to the 6th International Symposium
on High Energy Gamma-Ray Astronomy (Gamma2016), Heidelberg, Germany. To be
published in the AIP Conference Proceeding
FACT -- Operation of the First G-APD Cherenkov Telescope
Since more than two years, the First G-APD Cherenkov Telescope (FACT) is
operating successfully at the Canary Island of La Palma. Apart from its purpose
to serve as a monitoring facility for the brightest TeV blazars, it was built
as a major step to establish solid state photon counters as detectors in
Cherenkov astronomy.
The camera of the First G-APD Cherenkov Telesope comprises 1440 Geiger-mode
avalanche photo diodes (G-APD aka. MPPC or SiPM) for photon detection. Since
properties as the gain of G-APDs depend on temperature and the applied voltage,
a real-time feedback system has been developed and implemented. To correct for
the change introduced by temperature, several sensors have been placed close to
the photon detectors. Their read out is used to calculate a corresponding
voltage offset. In addition to temperature changes, changing current introduces
a voltage drop in the supporting resistor network. To correct changes in the
voltage drop introduced by varying photon flux from the night-sky background,
the current is measured and the voltage drop calculated. To check the stability
of the G-APD properties, dark count spectra with high statistics have been
taken under different environmental conditions and been evaluated.
The maximum data rate delivered by the camera is about 240 MB/s. The recorded
data, which can exceed 1 TB in a moonless night, is compressed in real-time
with a proprietary loss-less algorithm. The performance is better than gzip by
almost a factor of two in compression ratio and speed. In total, two to three
CPU cores are needed for data taking. In parallel, a quick-look analysis of the
recently recorded data is executed on a second machine. Its result is publicly
available within a few minutes after the data were taken.
[...]Comment: 19th IEEE Real-Time Conference, Nara, Japan (2014
FACT - The First G-APD Cherenkov Telescope: Status and Results
The First G-APD Cherenkov telescope (FACT) is the first telescope using
silicon photon detectors (G-APD aka. SiPM). It is built on the mount of the
HEGRA CT3 telescope, still located at the Observatorio del Roque de los
Muchachos, and it is successfully in operation since Oct. 2011. The use of
Silicon devices promises a higher photon detection efficiency, more robustness
and higher precision than photo-multiplier tubes. The FACT collaboration is
investigating with which precision these devices can be operated on the
long-term. Currently, the telescope is successfully operated from remote and
robotic operation is under development. During the past months of operation,
the foreseen monitoring program of the brightest known TeV blazars has been
carried out, and first physics results have been obtained including a strong
flare of Mrk501. An instantaneous flare alert system is already in a testing
phase. This presentation will give an overview of the project and summarize its
goals, status and first results
The extreme HBL behaviour of Markarian 501 during 2012
A multiwavelength campaign was organized to take place between March and July of 2012. Excellent temporal coverage was obtained with more than 25 instruments, including the MAGIC, FACT and VERITAS Cherenkov telescopes, the instruments on board the Swift and Fermi spacecraft, and the telescopes operated by the GASP-WEBT collaboration. Mrk 501 showed a very high energy (VHE) gamma-ray flux above 0.2 TeV of 0.5 times the Crab Nebula flux (CU) for most of the campaign. The highest activity occurred on 2012 June 9, when the VHE flux was 3 CU, and the peak of the high-energy spectral component was found to be at 2 TeV. This study reports very hard X-ray spectra, and the hardest VHE spectra measured to date for Mrk 501. The fractional variability was found to increase with energy, with the highest variability occurring at VHE, and a significant correlation between the X-ray and VHE bands. The unprecedentedly hard X-ray and VHE spectra measured imply that their low- and high-energy components peaked above 5 keV and 0.5 TeV, respectively, during a large fraction of the observing campaign, and hence that Mrk 501 behaved like an extreme high-frequency- peaked blazar (EHBL) throughout the 2012 observing season. This suggests that being an EHBL may not be a permanent characteristic of a blazar, but rather a state which may change over time. The one-zone synchrotron self-Compton (SSC) scenario can successfully describe the segments of the SED where most energy is emitted, with a significant correlation between the electron energy density and the VHE gamma-ray activity, suggesting that most of the variability may be explained by the injection of high-energy electrons. The one-zone SSC scenario used reproduces the behaviour seen between the measured X-ray and VHE gamma-ray fluxes, and predicts that the correlation becomes stronger with increasing energy of the X-rays
Searching for VHE gamma-ray emission associated with IceCube neutrino alerts using FACT, H.E.S.S., MAGIC, and VERITAS
The realtime follow-up of neutrino events is a promising approach to search for astrophysical
neutrino sources. It has so far provided compelling evidence for a neutrino point source: the
flaring gamma-ray blazar TXS 0506+056 was observed in coincidence with the high-energy neutrino IceCube-170922A detected by IceCube. The detection of very-high-energy gamma rays (VHE, E > 100 GeV) from this source helped establish the coincidence and constrained the modeling of the blazar emission at the time of the IceCube event. The four major imaging atmospheric Cherenkov telescope arrays (IACTs) - FACT, H.E.S.S., MAGIC, and VERITAS - operate an active follow-up program of target-of-opportunity observations of neutrino alerts sent by IceCube. This program has two main components. One are the observations of known gamma-ray sources around which a cluster of candidate neutrino events has been identified by IceCube (Gamma-ray Follow-Up, GFU). The second one is the follow-up of single high-energy neutrino candidate events of potential astrophysical origin such as IceCube-170922A. GFU has been recently upgraded by IceCube in collaboration with the IACT groups. We present here recent results from the IACT follow-up programs of IceCube neutrino alerts and a description of the upgraded IceCube GFU system
An intermittent extreme BL Lac: MWL study of 1ES 2344+514 in an enhanced state
Extreme high-frequency BL Lacs (EHBL) feature their synchrotron peak of the broad-band spectral energy distribution (SED) at nu(s) >= 10(17) Hz. The BL Lac object 1ES 2344+514 was included in the EHBL family because of its impressive shift of the synchrotron peak in 1996. During the following years, the source appeared to be in a low state without showing any extreme behaviours. In 2016 August, 1ES 2344+514 was detected with the groundbased gamma-ray telescope FACT during a high gamma-ray state, triggering multiwavelength (MWL) observations. We studied the MWL light curves of 1ES 2344+514 during the 2016 flaring state, using data from radio to very-high-energy (VHE) gamma-rays taken with OVRO, KAIT, KVA, NOT, some telescopes of the GASP-WEBT collaboration at the Teide, Crimean, and St. Petersburg observatories, Swift-UVOT, Swift-XRT, Fermi-LAT, FACT, and MAGIC. With simultaneous observations of the flare, we built the broad-band SED and studied it in the framework of a leptonic and a hadronic model. The VHE gamma-ray observations show a flux level of 55 per cent of the Crab Nebula flux above 300 GeV, similar to the historical maximum of 1995. The combination of MAGIC and Fermi-LAT spectra provides an unprecedented characterization of the inverse-Compton peak for this object during a flaring episode. The Gamma index of the intrinsic spectrum in the VHE gamma-ray band is 2.04 +/- 0.12(stat) +/- 0.15(sys). We find the source in an extreme state with a shift of the position of the synchrotron peak to frequencies above or equal to 1018 Hz
Flux States of Active Galactic Nuclei
Blazars are known to show variability on time scales from minutes to years covering a wide range of flux states. Studying the flux distribution of a source allows for various insights. The shape of the flux distribution can provide information on the nature of the underlying variability processes. The level of a possible quiescent state can be derived from the main part of the distribution that can be described by a Gaussian distribution. Dividing the flux states into quiescent and active, the duty cycle of a source can be calculated. Finally, this allows alerting the multi-wavelength and multi-messenger community in case a source is in an active state. To get consistent and conclusive results from flux distributions, unbiased long-term observations are crucial. Only like this is a complete picture of the variability and flux states, e.g., an all-time quiescent state, possible. In seven years of monitoring of bright TeV blazars, the first G-APD Cherenkov telescope (FACT) has collected a total of more than 11,700 hours of physics data with 1500 hours to 3000 hours per source for Mrk 421, Mrk 501, 1ES 1959+650, and 1ES 2344+51
Investigation of the correlation patterns and the Compton dominance variability of Mrk 421 in 2017
Publisher Copyright: © 2021 Georg Thieme Verlag. All rights reserved.Aims. We present a detailed characterisation and theoretical interpretation of the broadband emission of the paradigmatic TeV blazar Mrk 421, with a special focus on the multi-band flux correlations. Methods. The dataset has been collected through an extensive multi-wavelength campaign organised between 2016 December and 2017 June. The instruments involved are MAGIC, FACT, Fermi-LAT, Swift, GASP-WEBT, OVRO, Medicina, and Metsahovi. Additionally, four deep exposures (several hours long) with simultaneous MAGIC and NuSTAR observations allowed a precise measurement of the falling segments of the two spectral components. Results. The very-high-energy (VHE; E > 100 GeV) gamma rays and X-rays are positively correlated at zero time lag, but the strength and characteristics of the correlation change substantially across the various energy bands probed. The VHE versus X-ray fluxes follow different patterns, partly due to substantial changes in the Compton dominance for a few days without a simultaneous increase in the X-ray flux (i.e., orphan gamma-ray activity). Studying the broadband spectral energy distribution (SED) during the days including NuSTAR observations, we show that these changes can be explained within a one-zone leptonic model with a blob that increases its size over time. The peak frequency of the synchrotron bump varies by two orders of magnitude throughout the campaign. Our multi-band correlation study also hints at an anti-correlation between UV-optical and X-ray at a significance higher than 3 sigma. A VHE flare observed on MJD 57788 (2017 February 4) shows gamma-ray variability on multi-hour timescales, with a factor ten increase in the TeV flux but only a moderate increase in the keV flux. The related broadband SED is better described by a two-zone leptonic scenario rather than by a one-zone scenario. We find that the flare can be produced by the appearance of a compact second blob populated by high energetic electrons spanning a narrow range of Lorentz factors, from gamma(min)' = 2 x 10(4) to gamma(max)' = 6 x 10(5).Peer reviewe
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