“Hello Giggy” is a 2304 MHz Earth Moon Earth (EME) station designed and built in order to test Earth Venus Earth (EVE) signal constructions. If the signal constructions behave as expected in an EME channel, then we have increased confidence that the signal design will work well for EVE.
The Hello Giggy station bill of materials is listed below and the costs have been tallied.
ANTENNA SYSTEM
Dish: ~1m offset dish, f/D = 0.83
Rotator: Yaesu G-5500DC (AZ/EL)
Rotator mount: ITE T6 broadcast tripod
Mast extension: Al round tube, 116 mm, custom design in EVE repository
Feed arm: Rectangular conduit, 135° mounting angle (original equipment, will need replacing)
FEEDHORN
Design: OK1DFC stepped septum polarizer,W1GHZ verified, 2304 MHz specific
Construction: 1mm 3003-H14 Al sheet, bending brake, machine screws
Pieces: 2× U-channel halves + septum + back plate
Flare: W1GHZ 1.4λ square pyramid, 15° half-angle
Connectors: SMA with long dielectric, trimmed to match feed wall, 4mm wire
Probe: 1/8 diameter brass rod, drilled and then soldered to SMA pin
Fasteners: M3 stainless bolts + nuts
RF CHAIN
TRANSMIT
SDR: USRP B210 (70 MHz–6 GHz)
IF: 144 MHz
Transverter: Kuhne MKU 23 G4 (144 MHz → 2304 MHz)
Power amp: Kuhne MKU PA 13CM-20W A2 (~20W at 2304 MHz)
Sequencer: Kuhne SEQ 4
Feed TX port: SMA bulkhead
RECEIVE
Feed RX port: SMA bulkhead
LNA: Kuhne MKU LNA 231 AH-SMA
Bias tee: Kuhne KU BT 6000 SMA
Transverter: Kuhne MKU 23 G4 (2304 MHz → 144 MHz IF)
SDR: USRP B210
POWER SUPPLIES
PA supply: Mean Well RSP-150-27 (trimmed to 28V)
12V equipment: Mean Well LRS-200-15 (trimmed to 13.5V)
Heatsink/fan: Kuhne SK 150-62 + 60×60mm 24V fan
ROTATOR CONTROLLER
Interface: Arduino Mega + 4-channel relay shield
Firmware: K3NG (GS-232B emulation)
Protocol: GS-232B to hamlib rotctld to Python
Host: Good question – anything that runs Linux
SIGNAL PROCESSING
SDR software: GNU Radio or custom modem
Waveform: Pete Wyckoff KA3WCA EVE waveform
4096-ary non-coherent orthogonal modulation
BCH(127,106) FEC, 0 dB C/N0target
Moon tracking: Open Source or Custom Python script via hamlib
ESTIMATED COSTS TO DATE
KUHNE ORDER (all ordered together)
MKU 23 G4 transverter (2304 MHz) ~$650
MKU PA 13CM-20W A2 (28V) ~$450
SEQ 4 sequencer ~$120
MKU LNA 231 AH-SMA ~$180
KU BT 6000 SMA bias tee ~$45
SK 150-62 heatsink ~$30
60×60mm 24V fan ~$15
RSP-150-27 power supply (28V) ~$65
Kuhne subtotal: ~$1,555
ROTATOR SYSTEM
Yaesu G-5500DC ~$650
DXE-YRC-10PE cables ×2 ~$80
DMV-YSU-PIGTAIL ×2 ~$30
Rotator subtotal: ~$760
OTHER RECEIVED HARDWARE
USRP B210 (already owned) $0
Mean Well LRS-200-15 ~$35
USB-DB9 FTDI adapter ~$15
ITE T6 tripod (already owned) $0
Other subtotal: ~$50
STILL TO PURCHASE (estimates)
SendCutSend San Diego Al sheet cuts ~$383
Marshall’s Hardware fasteners/wire ~$30
Arduino Mega + relay shield ~$35
Remaining subtotal: ~$448
TOTAL SPENT TO DATE: ~$2,365
TOTAL INCLUDING REMAINING: ~$2,813
the USRP B210 and ITE T6 tripod being already owned saved probably another $1,500-2,000 in startup costs.
Hello Giggy: Building a 2304 MHz EME Station for the EVE Venus Radar Campaign
The Mission
This October, Venus reaches inferior conjunction, passing between the Earth and the Sun. For a brief window, the planetary window is best to attempt something remarkable. We are going to bounce a radio signal off Venus and attempt to detect the echo. This is the Earth-Venus-Earth (EVE) experiment. ORI is a part of that effort.
The target frequency is 2304 MHz, in the amateur 13cm band. The signal will travel roughly 80 million kilometers each way, reflect off a planet, and come back. To have any hope of detecting it, we need a well-characterized station with circular polarization, a sensitive receiver, and a carefully designed waveform. The waveform comes from Pete Wyckoff KA3WCA. The signal construction is a 4096-ary non-coherent orthogonal modulation scheme with BCH(127,106) forward error correction, targeting 0 dB C/N0. The station is called Hello Giggy because it’s Hello Kitty themed and on a Gigahertz band.
The Antenna
At the heart of Hello Giggy is an approximately one-meter offset parabolic dish with a measured focal ratio of f/D = 0.83. This is a shallow dish that requires a feedhorn with an appropriately narrow beamwidth. The dish sits on an ITE T6 broadcast tripod with a Yaesu G-5500DC azimuth-elevation rotator, giving full sky coverage for Moon and Venus tracking.
The feedhorn is a stepped septum polarizer in a square waveguide. This is a design with a well-documented history in amateur EME circles. Zdenek Samek OK1DFC introduced the concept to the amateur community in 2002. He was building on earlier professional literature by Chen and Tsandoulas. Zdenek published a spreadsheet that generates the dimensions for any frequency. Paul Wade W1GHZ subsequently analyzed the design through HFSS electromagnetic simulation and published his verification in 2003, along with a variation for offset dishes, which direcly applies to Hello Giggy. Paul W1GHZ described a 1.4λ square pyramidal flare section at 15° half-angle, well matched to dishes in the f/D 0.7 to 0.85 range. Our dish, at f/D = 0.83, sits squarely in that window. Therefore, we use the flares.
Our dimensions are the OK1DFC spreadsheet values for 1296 MHz, frequency-scaled by exactly 1296/2304 = 0.5625. Nothing is independently derived. The septum profile is not something that can be adjusted piecewise. The waveguide size, the five step positions, the five step heights, and the probe placement are all a single interlocking solution. Paul W1GHZ is explicit that the septum is only valid at the Chen and Tsandoulas guide dimension. Scale all of it or none of it.
We caught an error that shows why cutoff frequency is worth checking. A mid-development parameter set specified a 73 mm waveguide with five evenly spaced septum steps topping out at 59% of the guide height. Two checks caught it. First, the cutoff was wrong. A 73 mm square guide at 2304 MHz is 0.561λ, putting the TE10 cutoff at 2053 MHz, uncomfortably close to the operating frequency. Second, and more fundamental, a septum that never reaches the top wall cannot divide the guide into two ports, which means it cannot produce circular polarization at all. The parameters were replaced with the verified OK1DFC set. When using code-based 3d modeling programs like OpenSCAD, it’s very important to make sure that the code is still specifying the mental model of the design.
As another independent cross-check, we compared against the septum profile separately optimized by Dmitry Dimitriev RA3AQ. Normalized to their respective guide dimensions, the two designs track each other closely at every step. Scaled to 2304 MHz the two guide dimensions agree to within about one millimeter. Two independent optimizations converging on the same profile is about as good a validation as an amateur project can hope for before building in metal and then testing with a network analyzer.
At 2304 MHz, the resulting dimensions are:
Waveguide inner bore: 81.5 × 81.5 mm square (0.626λ)
Septum length, tip to back wall: 208.4 mm
Probe: 3.2 mm brass rod, 24.8 mm long, 24.2 mm from the back wall
Flare aperture: 182.2 mm square inner (1.4λ), 15° half-angle
TE10 cutoff 1839 MHz, TE11 cutoff 2601 MHz. This is single-mode at 2304 MHz
The feedhorn is fabricated from 0.040 inch 3003-H14 aluminum sheet. The body is a hat-channel clamshell. This gives two identical U-shaped halves, each with four brake bends, that close around a stepped septum plate. The septum carries its own flanges, which are sandwiched between the mated body flanges and clamped by the assembly screws. One set of fasteners therefore does three jobs at once. They hold the body together, register the septum in the exact center plane of the guide, and maintain electrical continuity along the seam.
Two details in that arrangement are easy to get wrong. Because the septum sits between the flanges, it adds its own thickness to the assembled interior, so each half channel must be cut shallower by half a septum thickness for the finished guide to come out square. The OpenSCAD methodology of scripting dimensions helps here, as dimension offsets can be parameterized and then rendered in the viewer. Also, the septum’s full-height rear section, cut to exactly the guide dimension, doubles as a go/no-go gauge for the mated channel. If the septum drops in, the guide is right.
The backshort cap is a folded pan that slips over the outside of the tube. At the front, the flare attaches through collar tabs. Flares are connected together with brackets. These brackets close the flare pieces together on the outside edges of the flares. Where a joint crosses multiple bends and accumulates tolerance, holes are laser-cut in the outer part only and match-drilled through into the body at fit-up rather than being pre-cut in both parts and hoping they line up. Parts are laser-cut and brake-bent by SendCutSend. The two SMA connectors (one transmit, one receive) are four-hole SMA parts with 4mm of probe. We drill and solder 1/8 inch brass rod and then trim this rod to length for final tuning. Following W1GHZ’s guidance, the design uses a deliberately fat probe rather than tuning screws, trading adjustability for dimensional precision.
The RF Chain
The transverter chain is entirely from Kuhne Electronic, a German manufacturer that is well regarded in the amateur microwave community.
On transmit, a USRP B210 software-defined radio provides a 144 MHz IF signal. The Kuhne MKU 23 G4 transverter converts this to 2304 MHz, and the MKU PA 13CM-20W A2 amplifier brings the output to approximately 20 watts. The Kuhne SEQ 4 sequencer manages the transmit/receive switching to protect the LNA during transmit.
On receive, the signal from the feedhorn passes through the Kuhne MKU LNA 231 AH-SMA low-noise amplifier and a KU BT 6000 SMA bias tee before returning to the transverter and the B210.
Power is provided by two Mean Well supplies: an RSP-150-27 trimmed to 28V for the power amplifier, and an LRS-200-15 trimmed to 13.5V for the remaining 12V equipment.
The Rotator Interface
The Yaesu GS-232B computer interface, Yaesu’s own PC control box, was back-ordered and expensive. Rather than buy that, we’re building our own using an Arduino Mega running the open-source K3NG rotator controller firmware. The K3NG firmware emulates the GS-232B protocol natively, which means hamlib’s rotctld daemon sees it as a standard Yaesu controller. The G-5500DC controller box provides 0–5V analog position feedback on its 8-pin DIN connector for both azimuth and elevation; the Arduino Uno’s 5V ADC reads these directly without level shifting. Four relay outputs control the motor direction lines. Total hardware cost for the interface is approximately $100.
The software stack runs on a Linux host. K3NG firmware over USB serial to hamlib rotctld to an open source Python Moon-tracking script that will compute ephemeris positions and command the rotator in real time.
The Mast Adapter
The ITE T6 is a heavy-duty metal camera tripod built for professional broadcast, industrial, and educational television environments. We removed the existing pan-tilt camera plate to expose the mounting post. We measured the mounting post and machined a mast adapter for the G-5500DC. The current OpenSCAD drawing can be found at https://github.com/OpenResearchInstitute/EVE/blob/main/mechanical/mast-adapter.scad
The G-5500DC requires an anti-twist pin hole of 9 mm diameter, with the center of that hole located 50 mm below the top of the mast. Set screws were also drilled and tapped to secure the mast adapter fo the mounting post of the T6. The mast adapter was secured to the mounting post. The rotator was secured to the mast adapter.
The Design Philosophy
Every parameter in this station traces back to a primary source, and the ones that could not be traced were removed. The feedhorn dimensions come from the OK1DFC spreadsheet, verified by W1GHZ’s HFSS simulations, cross-checked against RA3AQ’s independently optimized profile and against DL4MUP’s as-built measurements. The link budget and analysis has been computed in a Jupyter notebook and published in ORI’s public EVE repository. The waveform design has been through Monte Carlo BER simulation.
The OpenSCAD source file carries its own provenance section listing every reference, every scaling factor, and every known ambiguity. This includes two places where published sources disagree by about a millimeter, along with which value we chose and why. Where a number is an estimate rather than a measurement, it says so. The sheet metal bend allowances, for instance, have a process in the document. The defaults are replaced by measured values from a test coupon before any parts are cut. That way you know what your brake or bending process does to the dimensions before you cut.
This is a fully open project. All design files, notebooks, and documentation are publicly available at github.com/OpenResearchInstitute/EVE. If our community succeeds in detecting a Venus echo, the data will be open. If we don’t, the attempt and its documentation will still be a contribution to the art, and we will continue working towards June 2028, the next inferior conjunction of Earth and Venus.
What’s Next
The feedhorn parts are on order from SendCutSend. The Arduino rotator interface has been ordered and is being assembled. The October inferior conjunction window opens around October 19 and offers several observation opportunities through early November.
We’re grateful to Pete Wyckoff KA3WCA for the waveform design, Paul Wade W1GHZ for the feedhorn guidance, Brian Yee at SBMS for CST simulation cross-validation, and the entire ORI volunteer community for making this possible.




