Allen Telescope Array & Radio Frequency Interference. Geoffrey C. Bower UC Berkeley
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1 Allen Telescope Array & Radio Frequency Interference Geoffrey C. Bower UC Berkeley
2 Allen Telescope Array Large N design 350 x 6.1m antennas Sensitivity of the VLA Unprecedented imaging capabilities Continuous frequency coverage 0.5 to 11.2 GHz Wide field of view 3.5 degrees at 1 GHz Excellent survey instrument Compact Configuration 1 arcmin at 1.4 GHz (350), 1 arcmin at 5 GHz (42) Simultaneous observing with multiple backends Correlator: 2 x 100 MHz x full Stokes x 1024 channels Phased array beams: 32 indepent at 4 frequencies Joint project of UC Berkeley/SETI Inst. Privately funded construction $30M from PGAF and others NSF support for correlator & operations ($2.2M) USNO support for construction ($4M)
3 EVLA
4 ATA Science All Frequencies Transient Signals SETI GC survey: 20 sq. deg, GHz, 6 months 10 6 stars over 1-10 GHz Arecibo radar detectable at 300 pc Simultaneous with correlator Radio continuum science Static & transient surveys Extragalactic HI survey Neutral gas SDSS equivalent L* at z=0.1 over the entire sky Galactic magnetic fields, HI, long-chain molecules Pulsars Can Confine to Protected Bands Transient Signals Deep integrations Out of band observations Deep integrations Out of band observations Deep integrations Out of band observations Transient signals
5 ATA 42 Commissioning Construction Complete July 2007 Commissioning Summer 2007 Internal science Summer Public call for proposals early 2008
6
7 Wide Field Mosaic >30 antennas 7 pointing mosaic ~20 square degrees >170 sources 15 mjy minimum source flux
8 First 12 Antennas Phased Up By Beamformer 7/19/07 Inmarsat Coarse resolution ~1kHz Fine resolution ~1 Hz
9 Tsys 2K-Y moon Tsys in K Frequency in GHz
10 Σ 2D FT Flexible, upgradable digital signal processing FT DSP
11 RFI Strategy Overview Know the enemy Put many arrows in the quiver No Magic Bullets Exploit large N capability Exploit flexible digital electronics Implement at all levels Antenna design Array configuration Headroom in signal path 8-bit digitization
12 RFI Modeling: Hat Creek Terrain
13 Increased Path Loss due to Terrain --- ITU-R 526
14 RFI Monitor Simple design Discone antenna Broadband amp Spectrum analyzer Linux PC on net 0.1 to 10 GHz 0.3 to 3 GHz currently Isotropic sensitivity
15 (One of) the Enemies is Us RFI generated by BIMA array Offset +25dB for clarity
16 Aircraft DME
17 Multiple Time Scales: Radar
18 Broadband Spectrum Interferometric Detection with ATA
19 Parkes 1995 Green Bank Project Phoenix MHz 10 MHz Blocked Bands Arecibo Fractional Occupancy C 48 spectral occupancy May 4-5, Prelude RFI Survey December MHz Block Bands Frequency (GHz)
20 Real Time RFI Mitigation Monitoring Artificial horizons around known interferers Real time RFI Databases Multiple beams for rejection Time Blanking Adaptive canceling Interferometric Nulling Postcorrelation Analysis
21 Time Blanking Implementation Done in backends Correlator will have 100 μsec precision External & Internal Triggers
22 Adaptive Canceling
23 Rapid Prototyping Array
24 Cancellation of Glonass
25 Cancellation of GPS
26 Phased Array Beam Nulls with the ATA
27 Multiple Nulls
28 Nulls in Frequency Space
29
30 The Costs of Nulling Requires large-n to be effective Loss in SNR with number of nulls Must be able to update complex gains at ~100 Hz Matrix inversion is computationally expensive
31 Postcorrelation Analysis Manipulate output of correlator/visibility matrix Data rate: 350x349/2 4 Stokes 1024 Channels 16 bit 100 Hz sampling 400 Gbits/sec: too much!
32 Where to Use the Tools Blanking Radar, Aircraft, intermittent signals Adaptive Canceling Reference antenna(s) on transmitter Interferometric Nulling Predictable trajectories: satellites, fixed transmitters Postcorrelation Analysis Broadly adaptable
33
34 Square Kilometer Array * 100
35 ATA & RFI We have made extensive surveys to characterize RFI We plan to use numerous tools Many of these tools are untested All carry a significant cost in engineering, observing efficiency, etc.
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