HR: 0830h
AN: P21E-03    [Abstracts]
TI: Search for Radio Emission from Extrasolar Planets: Preliminary Analysis of GMRT Data
AU: * Majid, W A
EM: walid.a.majid@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91106 United States
AU: Chandra, I
EM: ishwar@ncra.tifr.res.in
AF: National Center for Radio Astrophysics, TIFR, Post Bag No. 3, Ganeshkhind, Pune, India
AU: Kuiper, T
EM: Thomas.B.Kuiper@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91106 United States
AU: Lazio, J
EM: Joseph.Lazio@nrl.navy.mil
AF: Naval Research Lab, Code 7213, Washington, DC 20735 United States
AU: Winterhalter, D
EM: Daniel.Winterhalter@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91106 United States
AU: Naudet, C
EM: Charles.J.Naudet@jpl.nasa.gov
AF: Jet Propulsion Lab/Caltech, 4800 Oak Grove Dr., Pasadena, CA 91106 United States
AU: Treumann, R
EM: tre@mpe.mpg.de
AF: Max Planck Institute, Karl-Schwarzschildstrasse 1 D-85748, Garching, Germany
AU: Zarka, P
EM: philippe.zarka@obspm.fr
AF: Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris Center National de la Recherche Scientifique, Meudon, France
AB: In 2004 we carried out a series of short calibration runs using the central square array of the GMRT. At the operating RF of 150 MHz, we have determined that the GMRT has a fantastic sensitivity of 2 mJy over a bandwidth of 5 MHz and a timescale of one hour and is relatively free of RFI between midnight and early morning hours local time. As part of the calibration runs, we have carried out brief observation of UpsAnd with various observing strategies. In early 2005, we were granted observing time on the GMRT during its Cycle 7 observation period. Our focus to date has been in characterizing the large scale structure of the dynamic spectra, identifying RFI and developing filters to remove them. We will present our results from both the short calibrations runs of 2004 as well as those obtained from the 2005 observations. We will also describe techniques for detection of chirps as present in Jupiter observations, including match filter strategies. In addition we will describe some preliminary results for detecting bursts via statistical techniques. We plan to use Jupiter and Saturn data to calibrate our detection efficiency for various strategies. We will also discuss our software package for data analysis and computing strategies that we have adopted on our Beowulf Linux cluster at JPL.
DE: 2756 Planetary magnetospheres (5443, 5737, 6030)
DE: 6900 RADIO SCIENCE
DE: 6954 Radio astronomy
SC: Planetary Sciences [P]
MN: 2005 Joint Assembly