HR: 0830h
AN: P21E-02    [Abstracts]
TI: Search for Radio Emissions from Extrasolar Planets: Recording and Software Correlation
AU: * Kuiper, T
EM: Thomas.B.Kuiper@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AU: Farrell, W
EM: William.Farrell@gsfc.nasa.gov
AF: NASA/Goddar Splace Flight Center, Code 690, Greenbelt, MD 20771 United States
AU: Lazio, J
EM: Joseph.Lazio@nrl.navy.mil
AF: Naval Research Lab, Code 7213, Washington, DC 20735 United States
AU: Majid, W
EM: Walid.A.Majid@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AU: Naudet, C
EM: Charles.J.Naudet@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AU: Treumann, R
EM: tre@mpe.mpg.de
AF: Max Planck Institute, Karl-Schwarzschildstrasse 1 D-85748, Garching, Germany
AU: Winterhalter, D
EM: Daniel.Winterhalter@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AU: Zarka, P
EM: philippe.zarka@obspm.fr
AF: Laboratoire d'Etudes Spatiales et, Observatoire de Paris Center National de la Recherche Scientifique, Meudon, France
AB: Theory and observations of solar planets show that extra-solar planets probably emit electron-cyclotron (EC) maser emission and that it may in some cases be orders of magnitude stronger than that from Jupiter. Nevertheless, at the Earth, such signals will be barely detectable. It will not be possible to observe them with university-class telescopes such as are used to study Jupiter. It will require the largest meter wavelength telescopes and antenna time will have to be used efficiently. EC emission is highly dynamic in time with time scales of milliseconds to hours and in frequency on scales of less than one to many tens of MHz. With a hardware signal processor configured to record data with a particular resolution and number of frequency bins, data with other time and frequency characters are not resolved or lost. Currently, the GMRT is the most sensitive radio telescope for extrasolar planet studies. With the availability of the Mark5 VLBI recorder, it is now possible to record both polarizations from all 30 antennas over a 12 hr observing run, with the full 4 bits per sample, on ten disk packs. Of course, various trade-offs can be made to reduce the number of disk packs but it is clear that it is possible to record the raw digited data for later processing. The only serious issue is how much of what kind of RFI is tolerable with only four bit samples. JPL has a software correlator (SoftC) now used routinely in the Deep Space Network. It runs on a Beowulf cluster. Also, JPL operates a much larger cluster for research on which SoftC can run. Besides being able to re-examine the data with different time and frequency resolutions, the baselines can also be phased or weighted to null out confusion caused by intense radio sources. We have obtained data from GMRT in this mode and the results of preliminary analysis is described in another paper at this meeting.
DE: 2756 Planetary magnetospheres (5443, 5737, 6030)
DE: 6900 RADIO SCIENCE
DE: 6954 Radio astronomy
SC: Planetary Sciences [P]
MN: 2005 Joint Assembly