Section I: Introduction to ALFA and GALFA
The Arecibo L-band Feed Array (ALFA) is a multibeam receiver designed to provide its users with a capability to survey the sky rapidly. It is inherently a high throughput device, meaning that astronomical data are acquired rapidly at the same time that areas on the sky are surveyed rapidly. The output of the ALFA receivers are processed in special-purpose signal processors for the specific research objectives of its users. As an astronomical research system, ALFA consists of the frontend receiver that is mounted on the telescope, a signal transmission system bringing data from the receiver and the control room, and the backend signal processing instrumentation located in the control room.
At the NAIC (National Astronmy and Ionosphere Center), the ALFA Project is organized around three topical science groups or consortia of interested scientists. One of these consortia is the group seeking to survey the neutral atomic hydrogen in the Milky Way Galaxy. This Galactic ALFA consortium, or GALFA consortium, derives its scientific objectives from accurate spectral measurements of the kinematic shape of the hydrogen line. The spectral decomposition of the hydrogen radio-frequency line observed with ALFA is done by a special-purpose backend signal processor known as a spectrometer. The radio spectrum is analyzed digitally by the spectrometer and presented to the astronomer for scientific analysis.
The GALFA spectrometer is designed around the scientific requirements necessary for the study of hydrogen gas in our galaxy. Other spectrometers are being designed and fabricated for SETI and the specific scientific requirements of the two other ALFA consortia, the consortium interested in galaxies beyond the Milky Way, and the consortium interested in studying pulsars.
A detailed research plan and list of all GALFA consortia members is available at http://www.naic.edu/alfa/galfa/.
Section II: System Description
ALFA receives 7 beams, 2 polarizations per beam, each covering 1225-1525 MHz. The 14 IF signals cover nominally the 100 to 400 MHz band. Each IF signal will be split and sent to several backends for commensal observing; one of these backends will be dedicated for GALFA.
Two spectrometers pipelines are required for on each of the 14 IF signals:
The wide bandwidth spectrometer is needed to accurately measure and model
standing waves so that these corrugations can later be removed from the
high resolution spectra.
See Heiles, Nov. 25, 2003, "Good news on using Fourier Filtering for Standing Wave Removal", ALFA memo series.
The GALFA spectrometer consists of:
Section III: System Specifications
A block diagram of one of the seven GALFA beams is shown in Figure 1. First, each polarization's IF signal is downconverted to baseband via a pair of mixers and a pair of 40 MHz low-pass filters (corresponding to 100 MHz maximum-bandwidth operation, of which 80 to 90 MHz is usable bandwidth, due to low-pass filter roll off). The quadrature baseband signals are then amplified and sent to the spectrometer boards. The frequency synthesizer/LO is split to drive the 28 mixers (7 beams x 2 polarizations x 2 mixers/baseband).
Each spectrometer board handles two polarizations from one telescope beam.The baseband signals are to be digitized by four 8-bit ADCs at 100 Msamples/sec.
The narrowband spectrometer uses a programmable digital LO, digital complex mixers and FIR filters to select the sub-band. The narrowband spectrometer analyzes a 7 MHz sub-band (actually 100/14 MHz), and outputs spectra with 8192 channels covering the sub-band. Note that Figure 1 incorrectly shows a decimation of 16 (the actual decimation is 14) and shows Stokes parameters (the spectrometer does not calculate stokes parameters).
Both wide- and narrowband spectra are output at a rate of 1 Hz to a general-purpose computer or file server for archiving and subsequent analysis.
Polyphase Filter Bank: