Present and Future of the Arecibo Observatory Instrumentation · Present and Future of the Arecibo Observatory Instrumentation ... - Radar Interface ... PowerPoint Presentation

Present and Future of the Arecibo Observatory

InstrumentationLuis A. Quintero

Cornell University / NAICNational Astronomy and Inonosphere Center

CASPER 2010 Workshop17 August 2010

Outline

CASPER 2010 WorkshopAugust 17, 2010

• The Arecibo Observatory• Backends at the Arecibo Observatory

- Interim Correlator - WAPP- Mock Spectrometer - Galspect- VLBA Mark4 & Mark5B (continuum)- Radar Interface (continuum)

• Future Backends- rDBE & Mark5C- Arecibo GUPPI- ROACH Based Radar Interface

• Questions

Arecibo Observatory

305m

It is part of the National Astronomy and Ionosphere Center (NAIC) at Cornell University and funded by the National Science Foundation (NSF)

~100m~80m

~900Ton


Transmitters & Receivers

Goldsmith, P. et al. “Multi-feed Systems for the Arecibo Gregorian”, ASP, 1995


Transmitter – 430 MHz

2 x klystrons for 2MW of pulsed powerAeronomy: Incoherent Ionosphere scattering


430MHz Radar - Ionosphere


Moonhttp://www.naic.edu

Venushttp://www.naic.edu

SaturnRings

http://www.naic.edu

Transmitter – S-band 2380MHz

2 x klystrons for 1MW CW power

Ganesan, R. “Telescope Electronics”, May 2006

Asteroidshttp://www.naic.edu


2380MHz Planetary Radar


Backends at the Arecibo Observatory


Spectrometers• Interim Correlator• WAPP• Galspect• Mock Spectrometer

Continuum Observations• VLBA Mark4 & Mark5B• Radar Interface (continuum)

Interim Correlator

50MHz BW – ASIC Correlator ChipJon Hagen (NAIC), John Canaris (U. New Mexico / NASA SERC - Space Engineering Research Center)


Wideband Arecibo Pulsar Processors (WAPP)

• 4 WAPPs• 1 WAPP = 2 IF Channels

2 Correlators1 Multiplexer

• 50/100 MHz BW• auto / crosscorrelations• Step attenuators• Technical issues:

Difficult to troubleshootObsolete parts


Wideband Arecibo Pulsar Processors (WAPP)


WAPPs Corralators (~1995)

High Performance CMOS Correlator Chip (ASIC)

• 16 Chips per board • Autocorrelation / Crosscorrelation

• 1024 Lags / chip• 100MSPS each• “Low Power”• TTL compatible

http://www.naic.edu/~astro/general_info/correlator/cmos.html


GALFA Spec, / GALSPECT (~2004)

• Backend built by UCB for theArecibo L-band Feed Array (ALFA) multibeam receiver • 7 beams, dual polarization• Outputs*:

Narrrowband: 8192channels, 7MHz BW

Wideband: 512 channels,100MHz BW

* http://seti.ssl.berkeley.edu/galfa/


Mock Spect. / PDEV (~2007)

Digital BoardDigitizers

Designed and developed by Jeff Mock• 8 x AD9430, 12bits ADCs• 2 x Xilinx Virtex II Pro FPGA• 2 QDR Mem, 2M x 36• 1x PowerPC Processor• Flash & SRAM mems• 2 x 1GbE, 2 x RS232• 5 x SMA (clk, PPS, etc)• LCD 128x64 pixels


PDEV – Digitizers / Programming

Digitizers:• 2 Digitizers / PDEV • 4 x AD9430 / Digitizer• ADC 12bits, 170MSPS

Programming:• Linux kernel v2.6.15• VHDL/Verilog (FPGAs)• C/C++, Perl (client/server)


PDEV – Architecture

ADCADCADCADC GX2VP70

PPC440GX

GX2VP70

QDR2Mx36

QDR2Mx36

2 x GbE

2 x RS232

4 x SMA

Flash /SRAM


ADCADCADCADC

PCIe x8MGT

PCIe x8MGT

PDEV – Mock Spectrometer


PFB

/FFT

16-

8k

ADC0

ADC0

ADC0

ADC0

GA

IN/O

FFS

ET

SW

ITC

H

TEST SIGNAL

12

12

12

12 DD

C (D

DS

, LP

F)

STO

KE

S

AC

CU

MU

LATO

R

PAC

KE

TIZE

CONFIGURATION REGISTERS

PR

OC

. IN

T.

CW, Noise,CW + Noise

EALFA / PALFA Backend

14 PDEVs*

7 for 7 ALFA pixels (primary)7 for 7 ALFA pixels (commensal)

14 File servers (4TB)We own in total 24 PDEVs

DDC (DDS, Mixer, DLPF)PFB (up to 8192 channels)Stokes parametersAccumulation, Packing* http://www.naic.edu/~phil/talks/vc09/tel_Perf_datatking_09.ppt


Other PDEV Projects

Aeronomy:• Tamara Hall (consultant)

S-Band Radar (Planetary Datataking):• Doppler correction, DDC

Single pixel baseband sampling (Phil Perillat)


Our Experience with Tools

• Summer 2009 we received: ADC2x1000-8 &iBOB, Dan Werthimer• Summer 2009, Andrew Siemion, tricks!• Summer 2010, Jayanth Chennamangalam, WVU. Histogrammer, 10GbE.


VLBA Mark IV & Mark5A

VLBI – Very Large Baseline Interferometry

Data Recorders

•Mark IV Data Acquisition Terminal (AO, 90s)• Mark5A Recorder


Radar Interface (80s & 90s)


• Triggered by external signals •4xADC, 12bits, 10MHz• 24x8k FIFO• Computer control via 5MHz serial lines• Bit selection

Future Backends


• 2 x (rDBE & Mark5C) / 305m & 12m antennas

• Arecibo GUPPI

• ROACH Based Radar Interface

RDBE - Haystack/NRAO (2010)

ROACH Digital Backend• Polyphase-Filter-Bank (PFB)• Emulate several VLBA BBCs on a ROACH board (VDBE)

CASPER 2010 TalksRuss McWhirter, Haystack, Haystack/NRAO

Digital Backend on the ROACH PlatformKeith Morris, NRAO, RDBE Implementation for

VLBAWed, Aug 18, 2010


Phase Reference Antenna

Patriot Antenna Systems - 12m Aperture S/X receivers for geodesy : 2.25GHz (S-band), 8.5GHz (X-band); wideband VLBI2010 Rx in the future


RDBE Connected to the Telescopes

IF/LO IF/LO

rDBE

Mark5C

rDBE

Mark5C

Hydrogen Maser


Arecibo GUPPI

GUPPI: Green Bank Ultimate Pulsar Processing Instrument• Coherent de-dispersion mode

CASPER 2010 Talk, Paul Demorest, Pulsar Science with GUPPI, Thu, Aug 19, 2010, 9:30a.m.


ROACH Based Radar Interface


• Baseband Converter, I/Q with Doppler Correction, 2.5hours

• 25MHz (50MHz) maximum continuous bandwidth for two IF channels (polA/polB)

• DDS/Clock drifting • Programmable digital filters• Bit selection, max 8bits (12bits)

ADC2x1000-8, v1.1, 8bit, 2x1GspsROACH I, Virtex 5

Questions?

Documents

Present and Future of the Arecibo Observatory Instrumentation · Present and Future of the Arecibo Observatory Instrumentation ... - Radar Interface ... PowerPoint Presentation