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ESTAR TO SMOS DEVELOPMENT OF
INTERFEROMETRIC RADIOMETRY FOR REMOTE SENSING FROM SPACE
David M. Le Vine Goddard Space Flight Center
Greenbelt, MD 20771
Outline
ESTAR
• Short History– Description
– Plans for Space• Hydrostar
• SMOS
– Today: 2D-STAR
• Lessons Learned– RFI
– Scene Dependent Calibration
– Null feed backESTAR image of “Delmarva” Peninsula south of NASA’s Wallops Island Facility
ESTAR
• Hybrid– Real along track
– Synthetic across track
• Antenna Array– 8-element dipole stick
– H-pol only
– 5 sticks
– 7 baselines
• Objective– Demonstrate viability of aperture
synthesis for remote sensing
– Apply to SM and OS
ESTAR Hardware
Walnut Gulch Watershed
ESTAR Image TB vs Soil Moisture
ESTAR (Solid); PBMR (open)
Remote Sensing Campaigns
• Soil Moisture– Walnut Gulch Watershed
1991– Little Washita Watershed
1992, 1994– Southern Great Plains
Experiment: SGP- 97,-99 – Soil Moisture Experiment:
SMEX-02
• Ocean Salinity– Delaware Coastal Current
Experiment, 1993– Gulf Stream Experiment,
1999
HYDROSTARESTAR in Space: Proposed to First NASA ESSP Call
1. 2.
3.
4.
DeployedResolution < 30 km( 5.8 x 9.5 m array)
Deployment of Antenna (16 Slotted Waveguide Sticks)
2D-STAR
• Synthesis in two dimensions• Array of patch antennas• Multiple configurations • V and H-pol
2D-STAR Installed on NASA P3-B Aircraft
SMEX-03: Huntsville, AL
Above: Landsat, false color image of SMEX-03 site. Tennessee River at lower right.
Right: 2D-STAR image during SMEX-03; H-pol (top) and V-pol (bottom)
Lessons Learned
RFI is a problem even in the restricted band at 1.413 GHz
ESTAR image crossing the Chesapeake Bay near Richmond, Virginia showing effects of RFI
RFI in zero spacing channel
Noise Injection is Stable
• Used for ESTAR zero spacing
• Employed Basic Correlator
• Proved to be extremely stable
ESTAR TO SMOS DEVELOPMENT OF
INTERFEROMETRIC RADIOMETRY FOR REMOTE SENSING FROM SPACE
David M. Le Vine Goddard Space Flight Center
Greenbelt, MD 20771
C. Swift, T. Jackson, A. Tanner, C. Ruf, A. Griffis, J. Isham,P. Gaiser, M. Goodberlet , M. Haken, J. Fuchs, R. Aldridge, ProSensing Staff, M. Kao, J. Good
BACK UP
Scene Dependent Artifacts
• Reconstruction noise– G-matrix (anechoic chamber)– Antenna coupling
• Scene dependence– Gibbs phenomena
• ESTAR – Coupled with incidence angle– Scene-dependent Inverse “filter”