the green bank telescope frank ghigo, national radio astronomy observatory 7 th us vlbi technical...
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National Radio Quiet ZoneTRANSCRIPT
The Green Bank Telescope
Frank Ghigo,National Radio Astronomy Observatory
7th US VLBI Technical Meeting,Haystack, Nov 2009
Panoramic View of Green Bank Telescopes
National Radio Quiet Zone
• 100 x 110 m section of a parent parabola 208 m in diameter• Cantilevered feed arm is at focus of the parent parabola
Unblocked Aperture
Subreflector and receiver room
Receiver turret
On the receiver turret
Inside the receiver room
GBT active surface system• Surface has
2004 panels– average
panel rms: 68
• 2209 precision actuators
One of 2209 actuators.• Actuators are located
under each set of surface panel corners
Actuator Control Room• 26,508 control and supply wires
terminated in this room
Surface Panel Actuators
Track Replacement - summer 2007
Present receivers
Future Receivers
1 7-beam 18-26GHz - being constructed2 Mustang expansion to 100 pixels - in progress
3 Expand 7-beam 18-26GHz array to 64 or 1004 Expand 4-6GHz receiver to include Methanol line at 6.7GHz.5 Dual-beam, dual polarization 3mm receiver for spectroscopy and
VLBI6 3mm many beam array (single polarization)
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CICADA• Configurable Instrument Collection for Agile
Data Acquisition– FPGA based data acquisition and processing– Uses CASPER tools and hardware
• Umbrella program for organizing FPGA projects– Purchase/obtain boards, software, development
systems– 3 ROACH, 2 BEE2, 5 iBOB, 6 ADC, 3 ADC-2, 10
GbE switches, servers, etc.
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CICADA Projects• Pulsar machines
– Green Bank Ultimate Pulsar Processing Instrument (GUPPI)– West Virginia University Pulsar Processing Instrument (WUPPI)– Coherent dedispersion machine GUPPI-2
• Event capture machines– Used for transient events
• Spectrometers– KFPA backend (for 7-beam K-band receiver)– Replacement for GBT Spectrometer
GUPPI specs
• Two IF inputs (RCP,LCP), up to 800 MHz bw each• Each input sampled at 1.6 GS/s• 8-bit samples• 128 to 4096 channel spectra• Auto- and cross-correlation spectra computed• Averaged to 50usec per output spectrum• Output rate (4096 size spectra):• (1/50usec)*4*4096 = 330 Mbytes/sec• Data flows to storage (spigot mode)• Data folded at pulsar period (timing mode)
GUPPI
GUPPI Status
• Currently available GUPPI Modes– 128 to 4096 channels– 2 polarizations– 100 to 800 MHz bandwidth– Full Stokes or Total Intensity Only– Decimation in frequency and time in CPU– Records up to ~250 MB/S continuously– Disk space is a considerable problem
• Fully integrated into the GBT Observing System
GUPPI-2
• Uses GUPPI to feed a 9-machine cluster of GPU’s via 4 10 GbE ports.
• 128, 256, or 512 coarse channels will be supported• 100 MHz processed per GPU at “reasonable” DM’s.• Only modification to GUPPI is a new output FPGA
personality and software to control the nodes
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K band Feedhorn Array Spectrometer
• 7 pixels, dual polarization– 21 ROACH boards, 14 ADC's – Needs to be in receiver room
• 3 GHz bandwidth• Cross correlation between polarizations on a single pixel• “Zoom” mode for multiple narrow windows in a bandpass• Fast dump mode for pulsar use on a few polarizations• Normal dump times of 1 ms
Array Spectrometer design
Reconfigurable Open
ArchitectureComputingHardware
Reconfigurable Open
ArchitectureComputingHardware
Front-endElectronics
Reconfigurable Open
ArchitectureComputingHardware
IF 0
Pixel 0
Pixel 1
Pixel 7Pixel 6
Pixel 5P ix el 4
Pixel 3Pixel 2
Front-endElectronics
IF 1
10 Gb Switch
10 GB X 210 GB X 2
10 Gb Switch
32 Core Pipeline Processor
Disk Controller
Disk Controller
Dual10 GbLinks
Fibers FromGBT
40 TB
40 TB
Up to 500 MB/sec to disks ,
sustained
Fibers To Jansky Lab Equipment
Room
Signal Processors
Signal Combiner /Accumulator
To existing GB Network infrastructure
The Green Bank Telescope
Frank Ghigo7th US VLBI Technical Meeting,
Haystack
VLBI usage:
About 15% of GBT time goes to VLBI projects.
Including 2 Large projects;
Also HSA, globals, EVN
The Megamaser Cosmology
project
Braatz, Condon,
Greenhill, et al
200 hours
NGC4258
Radio Interferometric Planet Search (RIPL)
Geoff Bower, Alberto Bolatto, et al; U.C. Berkeley
Search for planetsaround M-dwarfs
29 stars, 4 epochs per year.
1392 hours
~ 170 8-hr sessions
GBT_VLBI software
Improving the surface for High-Frequency Performance:
• Surface• Mechanical adjustments• Photogrammetry• FEM (finite element model)• OOF (“out of focus” holography) model - global• AutoOOF - correct thermal errors short term• “Traditional” holography
Mechanical adjustment of the panels.
Surface efficiency -- Ruze formula
John Ruze of MIT -- Proc. IEEE vol 54, no. 4, p.633, April 1966.
Effect of surface efficiency
⋅⋅⋅= surfpatap εεε€
εsurf = e−(4πσ / λ )2
= rms surface error
OOF: out of focus “holography”
Zernike polynomials
Auto-OOF corrections
“Traditional Holography”
Reduction of small-scale surface features
43 GHz Moon scans
Beam pattern improvement
Theoretical beam patterns
43 GHz Measured Aperture Efficiency
43 GHz comparisons
Aperture Efficiency at high frequencies
• For illumination pattern efficiency of 75%• And surface rms of 225u
• Peak Aperture efficiency at 43.12 GHz is ~63%– At 85 GHz: 40%– At 110 GHz: 25%|