Top 10 similar words or synonyms for widefield

macroscope    0.748952

tirf    0.744334

epifluorescent    0.730710

lensless    0.727784

darkfield    0.714419

sted    0.706179

spim    0.703214

lensfree    0.702788

cslo    0.698847

brightfield    0.696348

Top 30 analogous words or synonyms for widefield

Article Example
Murchison Widefield Array An MWA antenna comprises four by four regular grid of dual-polarisation dipole elements arranged on a 4m x 4m steel mesh ground plane. Each antenna (with its 16 dipoles) is known as a "tile". Signals from each dipole pass through a low noise amplifier (LNA) and are combined in an analogue beamformer to produce tile beams on the sky. Beamformers sit next to the tiles in the field. The radio frequency (RF) signals for the tile-beams are transmitted to a receiver, each receiver being able to process the signals from a group of eight tiles. Receivers therefore sit in the field, close to groups of eight tiles; cables between receivers and beamformers carry data, power and control signals. Power for the receivers is provided from a central generator. The receiver contains analogue elements to condition the signals in preparation for sampling and digitisation. The frequency range 80–300 MHz is Nyquist-sampled at high precision. Digital elements in the receiver (after the digitiser) are used to transform the time-series data to the frequency domain with a 1.28 MHz resolution – 5 bits real and 5 bits imaginary for each resolution element. Sets of 1.28 MHz coarse frequency channels are transmitted via an optical fibre connection to the correlator subsystem, located in the CSIRO Data Processing Facility near the MWA site. MWA shares the CSIRO facility with the ASKAP program.
Murchison Widefield Array The correlator subsystem comprises Poly-phase Filter Bank (PFB) boards that convert the 1.28 MHz coarse frequency channels into channels with 10 kHz frequency resolution in preparation for cross-correlation. Correlator boards then cross-multiply signals from all tiles to form visibility data. A distributed clock signal drives the coherence of receivers in the field and maintains timing for the correlator.
Murchison Widefield Array Data will be transferred from the RTC storage disks to the MWA archive located at the end of a high-bandwidth network connection. The primary MWA data archive(s) will likely be located in Perth, with copies in other locations in Australia and the US. The resultant qualified data will then be provided to, and stored by, the various scientific databases for subsequent distribution to the respective scientific communities for analysis and interpretation.
Murchison Widefield Array A 32-tile prototype (MWA-32T) was constructed and operated with increasing capability over the period 2007–2011, testing telescope hardware and making preliminary science observations, including initial observations of EoR fields. A 512-tile instrument (512T) was planned but de-scoped due to funding issues. The 128-tile instrument (MWA) was constructed in 2012, commencing science operations in early 2013. The infrastructure on-site at MRO will allow an eventual build-out to 256 tiles, increasing the sensitivity and resolution of the instrument.
Murchison Widefield Array The "GaLactic and Extragalactic All-sky MWA" (or "GLEAM" is a survey of 300,000 extragalactic sources at 20 frequencies between 70 and 230 MHz that was carried out by the MWA.