Science Results from the Long Wavelength Demonstrator Array

Details Science Results from the Long Wavelength Demonstrator Array Science Results from the Long Wavelength Demonstrator Array

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21544205h&link_type=abstract

American Astronomical Society, AAS Meeting #215, #442.05; Bulletin of the American Astronomical Society, Vol. 42, p.407

Astronomy and Astrophysics

Astronomy

Scientific paper

We present recent scientific results from the Long Wavelength Demonstrator Array (LWDA), a 16 element, full polarization, active dipole antenna array located near the Very Large Array (VLA) in New Mexico. The LWDA is a technology pathfinder for the Long Wavelength Array (LWA, http://lwa.unm.edu) operating over a frequency range of 60-80 MHz, and has been used in two principal scientific investigations.
First, LWDA interferometer measurements contributed to a recent study of the secular decrease of the low frequency intensity of Cassiopeia A ("Cas A"). LWDA data was combined with archival 74 MHz VLA data together with data in the literature to confirm (1) the secular decrease is slower than originally predicted, (2) the rate of decrease has been relatively stable for the last 50 years, and (3) the rate of secular decrease between 38 and 74 MHz is nearly identical. The results also demonstrated that there are significant fluctuations about the secular decrease with periods between 3 and 20 years. Further monitoring is needed to search for oscillations on shorter time scales and to explore the frequency dependence (if any) of the fluctuations to constrain their physical origin(s).
The second project was an all-sky search for low frequency transient sources. A data processing pipeline was developed to use LWDA observations to construct all-sky images, exploiting the near all-sky field-of-view of the individual antennas and to detect sources within them. A total of 83 hours of "on-sky" time over a six month period was searched for transient sources, and no candidates were found. We compare our results with various transient classes to assess their detectability and place our results in context to previous searches.
These studies serve as scientific pathfinders for the emerging much larger dipole-based arrays including the LWA, Low Frequency Array (LOFAR), and Murchison Wide-field Array (MWA).

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