Very Large Array

The most likely explanation for these results is that simple phenolics inhibit a very large array of enzymes in vitro. The most likely explanation for the CNS effects of Uncaria rynchophylla would be that indole alkaloids, such as dihydrocorynanteine or hirsutine (32), interact with the central neurotransmission and possibly the serotonin ergic system. 

Abstract. We discuss new observations of 3He towards planetary nebulae (PNe) using the Very Large Array (VLA), the 305 m Arecibo telescope, which is now capable of observing the 3He+ spectral transition, and the recently commissioned 100 m Green Bank Telescope (GBT). 

Although the development of field-effect transistors (FETs) has already reached a high level of perfection in crystalline silicon (c-Si), a-Si H offers the advantage that very large arrays of a-Si H FETs are feasible. Hence, even if their performance level is much lower than that of c-Si FETs, there are still many applications where their characteristics may be adequate. In Chapter 6, LeComber and Spear review the design, fabrication, and performance of a-Si H FETs. They point out the need for good ohmic connec-... 

Numerical evaluations, with A = 0.01, show that very large arrays (Nm > 1000) can be addressed for n > 10. 

Array detectors scintillators coupled to very large arrays of semiconductor detectors that have largely replaced film in medical diagnostics... 

In Table 2 the columns are (1) Source name, (2) distance, (3) radio core flux we use intercontinental radio interferometry or radio data from the Very Large Array, (4) maximum energy, (5) cosmic rays flux relative to M87 and at some reasonably low particle energy such as 1018 eV. 

Perhaps the most interesting and surprising discovery about Mercury s surface is the possible presence of ice caps at the planet s north and south poles. The first evidence for this discovery came as the result of studies conducted by researchers at NASA s Jet Propulsion Laboratory in Pasadena, California. The researchers bounced radar signals off the planet s north polar region and analyzed the reflected beams at the Very Large Array radio telescope system in New Mexico. They found that the spectra of the reflected beams were very similar to those for water ice. Since they first reported this result in 1991, further studies have been conducted to determine whether the poles really do contain water ice, although final confirmation has not yet been obtained. 

The nature of H-transfer in these reactions is intrinsically linked to the identity of the oxygen species capable of C-H activation. The mechanism of PHM and DySM has been subjected to extensive investigations, including an X-ray structure for PHM that shows the two coppers per subunit located at a distance of ca. 10 A across a solvent interface [118]. This structure has raised questions regarding how electrons are transferred between the metal centers and how the chemically difficult O2 and C-H activation reactions can occur at a solvent interface. Recently, Evans et al. have put forth a mechanism that is able to accommodate the very large array of experimental data for both PHM and DySM [119]. 

Solar Power Satellite - A solar power station investigated by NASA that entailed a satellite in geosynchronous orbit that would consist of a very large array of solar photovoltaic modules that would convert solar generated electricity to microwaves and beam them to a fixed point on the earth. 

Basically we will consider arrays of infinite extent in both the X and Z directions. However, the fundamental concept discussed here will also apply to very large arrays (in terms of wavelength) as long as we disregard edge effects. These will be discussed later in Chapter 5 and focus on the variation of the element impedance. 

Such systems often employ very large arrays of cells of the order of lOx the size of an electric vehicle s battery. Examples from A123 Systems contain 2 MWh within a semitractor-trailer sized platform—a combination of over 80,000 cells. 

National Radio Astronomy Observatory Very Large Array http //www.vla.nrao.edu... 

A very large array of methods have been proposed to accelerate the convergence rate of successive substitution. These include the use of the Dominant Eigenvalue Method of Crowe and Nishio (1975). In spite of significant increase in the rate of convergence, such methods may cause the loss of basic stability of successive substitution. 

Many point-spread functions, however, are far less well-behaved. For example. Fig. 1 shows an Airy disk and the point-spread functions of particular observations of the Hubble Space Telescope and the Very Large Array (a radio telescope) are shown in Figs. 3 and 4. 

FIGURE 4 The Fourier plane sampling pattern (top) and the resulant point-spread functions (bottom) for an observation with the Very large Array (near Socorro, New Mexico). The first sampling pattern corresponds to a very brief observation (a so-called snapshot). The second corresponds to a 6-hr observation, where the earth s rotation has been used to improve the sampling pattern in the Fourier plane. 

The development of self-calibration algorithms in the 1980s led to the realization that they could be employed to remove ionospheric phase fluctuations. Subsequently, interferometer baselines have been extended to tens of kilometers, and the success of these relatively long baseline interferometers (particularly the 74 MHz system on the Very Large Array, cf. Table I) have spurred plans for a Low Frequency Array (LOFAR, Fig. 4B). This instrument will have baselines of order 100 km and a collecting area of order 10 m at 15 MHz, leading to a sensitivity that will be competitive with centimeter-wavelength interferometers. 

Napier, P. J., Thompson, R. T, and Ekers, R. D. (1983). The very large array Design and performance of a modem synthesis radio telescope, Pmc. lEEEll, 1295-1320. 

The Very Large Array consists of 27 radio antennas in a Y-shaped configuration fifty miles west of Socorro, New Mexico. Each antenna is 25 meters in diameter. 

---