BHEX Mini
Direct Imaging Black Holes from LEO
Ref Bari | Update to Ben (07/04)
BHEX Mini
BHEX Mini
Size
Weight
Power
Power
Cost
\sim 2.5m
\sim 25-50kg
22 kg
300W
400mW @15^{\circ}K
\$10 \text{mln}
754 mm \times \\ 146 mm \times \\ 300 mm
\$2-5 \text{Mln}
\$4-11 \text{Mln}
10-20W
\text{(deployment)}
5-7 kg
\sim 10W
\sim \$ 1 \text{mln}
\sim0.02m^3
\sim 1 kg
\sim 3W
\sim \$1\text{mln}^*
60 mm\times \\60mm \times \\32 mm
1U (100 mm\times \\100 mm \times \\100 mm)
1.2 kg
1.2 kg
100W
\sim \$100\text{k}
3U (300 mm\times \\300 mm \times \\300 mm)
100W
3 kg
\sim \$1\text{mln}^*
\sim 4W
\sim 4W
12 mm \times \\12 mm
\sim \$1\text{mln}^*
BHEX Mini
Size
Weight
Power
Power
Cost
\sim 2.5m
\sim 25-50kg
22 kg
300W
400mW @15^{\circ}K
\$10 \text{mln}
754 mm \times \\ 146 mm \times \\ 300 mm
\$2-5 \text{Mln}
\$4-11 \text{Mln}
10-20W
\text{(deployment)}
5-7 kg
\sim 10W
\sim \$ 1 \text{mln}
\sim0.02m^3
\sim 1 kg
\sim 3W
\sim \$1\text{mln}^*
60 mm\times \\60mm \times \\32 mm
1U (100 mm\times \\100 mm \times \\100 mm)
1.2 kg
1.2 kg
100W\\\text{generated}
\sim \$100\text{k}
3U (300 mm\times \\300 mm \times \\300 mm)
100W
3 kg
\sim \$1\text{mln}^*
\sim 4W
\sim 1 kg^*
12 mm \times \\12 mm
\sim \$1\text{mln}^*
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
BHEX Mini
Ron Turner (NASA NIAC)
NASA Pioneers
Aspera
Pandora
StarBurst
PUEO
(Galaxy Evolution via UV)
(Exoplanet Explorer)
(Neutron Stars via Gamma Rays)
(Particle Physics via High-Energy Neutrinos)
BHEX Mini Coverage
(u,v)
Antenna
\text{At } 86\text{ GHz} \to \lambda= 3.5 mm
\text{Minimum Surface Accuracy: }λ/20 = 3.49 mm / 20 = 0.175 mm
\text{Good Surface Accuracy: }λ/16 = 3.49 mm / 16 = 0.218 mm
\text{Excellent Surface Accuracy: }λ/8 = 3.49 mm / 8 = 0.436 mm
Antenna
Cryocooler
Cryocooler
HiPTC Heat Intercepted Pulse Tube Cooler
- Cost: $10 Million
- Mass: 22kg
-
Cooling power
- 400 mW at 15K
- 5.2 W at 100K
- Electric power: 300 W
Cryocooler
HiPTC Heat Intercepted Pulse Tube Cooler
- Cost: $10 Million
- Mass: 22 kg
-
Cooling power
- 400 mW at 15K
- 5.2 W at 100K
- Electric power: 300 W
Raytheon RSP2: Sterling PT-Hybrid
- Cost: ~$6-8 Million
- Mass: 25 kg
-
Cooling power
- 2.1W at 20K
- 6 W at 60K
- Electric power: 450 W
BHEX Mini
BHEX Mini
NIAC Phase I
Step 1: 100/300 ~ 33% Acceptance
Step 2: 12/100 ~ 12% Acceptance
Step 3: $175,000 for 9 Months
Our Competition
Fluidic Telescope (FLUTE): Enabling the Next Generation of Large Space Observatories
Our Competition
Bend-Forming of Large Electrostatically Actuated Space Structures
Our Competition
Hybrid Observatory for Earth-like Exoplanets (HOEE)
Our Competition
SCOPE: ScienceCraft for Outer Planet Exploration
Our Competition
Kilometer-Scale Space Structures from a Single Launch
Our Competition
Beholding Black Hole Power with the Accretion Explorer Interferometer
Our Competition
Solar System-Scale VLBI to Dramatically Improve Cosmological Distance Measurements
Our Competition
Swarming Proxima Centauri: Coherent Picospacecraft Swarms Over Interstellar Distances
Our Competition
LIFA: Lightweight Fiber-based Antenna for Small Sat-Compatible Radiometry
Our Competition
Water Telescope
50m Antenna
Self-Assembling Telescope
Large antennas
Starshade Telescope
Directly image exoplanets
Quantum-dot propelled sails
Explore exoplanets
Retractable structure to enable artificial gravity
Enable long-term human living in space
Create a swarm of X-Ray Interferometers
Enable studies of black hole jets and accretion disks
Lightsail swarms
Explore exoplanets
Solar system scale VLBI
Advance Precision-based Cosmology
Large RF Antennas
Enable salinity measurements
Our Competition
Water Telescope
50m Antenna
Self-Assembling Telescope
Large antennas
Starshade Telescope
Directly image exoplanets
Quantum-dot propelled sails
Explore exoplanets
Quantum-Assisted VLBI Network in LEO
Enable time-resolved imaging of Sgr A* & M87 ("black hole video")
Create a swarm of X-Ray Interferometers
Enable studies of black hole jets and accretion disks
Lightsail swarms
Explore exoplanets
Solar system scale VLBI
Advance Precision-based Cosmology
Large RF Antennas
Enable salinity measurements
\text{MEO} (20000 \text{ km})
\text{LEO} (400 \text{ km})
BHEX Mini
An AI-Assisted Modular VLBI Constellation in LEO
\text{MEO} (20000 \text{ km})
BHEX Mini
An AI-Assisted Modular VLBI Constellation in LEO
NASA NIAC
Quinn Morley (Boeing)
NASA NIAC
Quinn Morley (Boeing)
NASA NIAC
Quinn Morley (Boeing)
TITAN Air Proposal (NIAC Phase I Selection, 2021)
NASA NIAC
NASA NIAC
BHEX Mini
Partner Satellite to BHEX
Stand-alone Satellite
Pathfinder Mission
BHEX Mini
Partner Satellite to BHEX
Stand-alone Satellite
Pathfinder Mission
Supplement (u,v) coverage at 86 GHz
Enable parameter estimation of Sgr A*/M87
Achieve Space-Space VLBI
20,200\text{ km}
400\text{ km}
BHEX Mini
Pathfinder Mission
Partner Satellite to BHEX
Stand-alone Satellite
Supplement (u,v) coverage at 86 GHz
Enable parameter estimation of Sgr A*/M87
Achieve Space-Space VLBI
Supplement (u,v) coverage at 86 GHz
Enable parameter estimation of Sgr A*/M87
Achieve Space-Space VLBI
Survey of >25 AGN+BH Targets @86 GHz
Enable Population Modeling of SMBHs
Enable real-time imaging of dynamical accretion disk around Sgr A*
Enable multi-messenger gravitational astronomy w/ LIGO + LISA
BHEX Mini
Partner Satellite to BHEX
Stand-alone Satellite
Pathfinder Mission
Supplement (u,v) coverage at 86 GHz
Enable parameter estimation of Sgr A*/M87
Achieve Space-Space VLBI
Supplement (u,v) coverage at 86 GHz
Enable parameter estimation of Sgr A*/M87
Achieve Space-Space VLBI
Survey of >25 AGN+BH Targets @86 GHz
Enable Population Modeling of SMBHs
Enable real-time imaging of dynamical accretion disk around Sgr A*
Enable multi-messenger gravitational astronomy w/ LIGO + LISA
Enable low-cost Space-Ground & Space-Space VLBI
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
Prospects of Detecting a Jet in Sagittarius A* with VLBI (Chavez et. al., ApJ 2024)
BHEX Mini
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
- What kind of targets can we observe with this angular resolution?
BHEX Mini
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
- What kind of targets can we observe with this angular resolution?
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
20,000\text{ km}
12000\text{ km}
400\text{ km}
BHEX Mini
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
- What kind of targets can we observe with this angular resolution?
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
20,000\text{ km}
12000\text{ km}
400\text{ km}
Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope (Palumbo et. al., ApJ 2019)
BHEX Mini
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
- What kind of targets can we observe with this angular resolution?
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
400\text{ km}
Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope (Palumbo et. al., ApJ 2019)
BHEX Mini
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
- What kind of targets can we observe with this angular resolution?
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
Multifrequency Black Hole Imaging for the Next-generation Event Horizon Telescope (Chael et. al., 2023, ApJ)
400\text{ km}
BHEX Mini
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
- What is the integration time for BHEX Mini on the (u,v) plane?
- Could BHEX Mini possibly enable direct imaging of dynamic accretion disk around Sgr A*? (i.e., creating a movie of a black hole!)
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Maximum data transmission rate (in bits per second); How fast can you send data from BHEX Mini to the earth?
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Power of Transmitted Signal: Strength of downlink signal in Watts (i.e., shouting louder to be heard further away!)
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Transmitter Gain: How well-focused your signal is when it leaves the satellite
(i.e., shouting into a megaphone instead of into the wind)
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Receiver Gain: How effectively the ground station collects and concentrates the incoming signal (i.e., ALMA's big dish listening to our incoming signal)
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Received Power: How strong is the signal once it hits the ground receiver? (after traveling through empty space)
P_r = P_tG_tG_r \left( \frac{\lambda}{4\pi R}\right)^2 \cdot \eta
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Receiver Gain: How effectively the ground station collects and concentrates the incoming signal (i.e., ALMA's big dish listening to our incoming signal)
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Distance: How much distance did the signal travel through free space? (LEO vs. MEO!)
P_r = P_tG_tG_r \left( \frac{\lambda}{4\pi R}\right)^2 \cdot \eta
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
Receiver Gain: How effectively the ground station collects and concentrates the incoming signal (i.e., ALMA's big dish listening to our incoming signal)
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
- Since BHEX Mini's laser downlink would suffer less signal loss from LEO than BHEX at MEO, can we transmit more data?
- Can this be leveraged to use 2-bit quantization instead of 1-bit quantization?
BHEX Mini
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
Sub-milli arcsecond angular resolution
Dual short and long baseline lengths
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
22\mu as<\theta_{\text{BHEX-Mini}} < 1800 \mu as
5.6 G \lambda < b_{s s}<9.3 G \lambda
0.11 G \lambda < b_{s g}<3.5 G \lambda
T_{orb}=90 \text{ min}
Decreased ISM scattering at LEO than MEO
R_{\max } \approx \frac{P_t G_t G_r \eta}{k T_b B}\left(N_{\bmod }\right)
P_r = P_tG_tG_r \left( \frac{\lambda}{4\pi R}\right)^2 \cdot \eta
BHEX Mini
Decreased ISM scattering at LEO than MEO
Orbit design for mitigating interstellar scattering effects in Earth-space VLBI observations of Sgr A* (Aditya Tamar, Ben Hudson, Daniel C.M. Palumbo, A&A, 2025)
BHEX Mini
Decreased ISM scattering at LEO than MEO
V_{obs}(b) = S\cdot \exp\left(-\frac{\pi^2 b^2\theta^2}{4\ln 2}\right)\exp \left(-\frac{1}{2} C_\phi^2 b^\alpha r_F^{2-\alpha}\right)
Intrinsic Gaussian Source
b=\frac{\lambda}{D}\to \text{BHEX Mini: } 0.1G\lambda b_{sg}<3.5G\lambda
b=\frac{\lambda}{D}\to \text{BHEX:}\geq 20G\lambda
BHEX Mini
Decreased ISM scattering at LEO than MEO
V_{obs}(b) = S\cdot \exp\left(-\frac{\pi^2 b^2\theta^2}{4\ln 2}\right)\exp \left(-\frac{1}{2} C_\phi^2 b^\alpha r_F^{2-\alpha}\right)
ISM Scattering
C_{\phi}\propto \lambda^2 (\lambda_{\text{BHEX Mini}}=3.5 mm)
- At MEO, BHEX is 20x the orbital altitude of BHEX Mini
- BHEX observes at a f=320 GHz, 4x higher than BHEX Mini
BHEX Mini
Decreased ISM scattering at LEO than MEO
V_{ratio}(b) = \frac{e^{-b_{\text{BHEX-Mini}}^2} e^{-\lambda_{\text{BHEX-Mini}}^2 b^\alpha}}{e^{-b_{\text{BHEX}}^2} e^{-\lambda_{\text{BHEX}}^2 b^\alpha}}
\lambda_{\text{BHEX Mini}}=3.7\lambda_{\text{BHEX}}, b_{\text{BHEX Mini}} = \frac{1}{5}b_{\text{BHEX}}
\lambda_{\text{BHEX}}=1.33mm, b_{\text{BHEX Mini}} \sim 20G\lambda
V_{\text{BHEX-Mini}}\sim 10V_{\text{BHEX}}
BHEX Mini Visibility Amplitude Advantage
Regardless of Source Flux Density!
V_{obs}(b) = S\cdot \exp\left(-\frac{\pi^2 b^2\theta^2}{4\ln 2}\right)\exp \left(-\frac{1}{2} C_\phi^2 b^\alpha r_F^{2-\alpha}\right)
BHEX Mini
Decreased ISM scattering at LEO than MEO
BHEX Mini
BHEX Mini
Antenna
BHEX Mini
Receiver
BHEX Mini
Cryocooler
BHEX Mini
Solar Panels
BHEX Mini
Ultra-Stable Oscillator
BHEX Mini
Ultra-Stable Oscillator
\Delta \phi = 2\pi \cdot f \cdot \sigma_t
\sigma_t = \sigma_f \cdot \Delta t
Phase Error
BHEX Mini
Ultra-Stable Oscillator
\sigma_f = 5\cdot 10^{-11}, f_{obs}=86 \text{ GHz}
\Delta t = 1s:
\sigma_t = 5\cdot 10^{-11} \cdot 1s = 5\cdot 10^{-11} s
\Delta \phi = 2\pi \cdot (86\cdot 10^9 \text{ Hz}) \cdot 5\cdot 10^{-11} s=27.01 \text{ rad}
\Delta t = 10s:
\sigma_t = 5\cdot 10^{-11} \cdot 10s = 50\cdot 10^{-11} s
\Delta \phi = 2\pi \cdot (86\cdot 10^9 \text{ Hz}) \cdot 50\cdot 10^{-11} s=270.01 \text{ rad}
\Delta \phi<1 \text{ rad for Phase Coherence}
BHEX Mini
Ultra-Stable Oscillator
Allan Deviation
f=86 \text{ GHz}, t=10s, \sigma_y = 5\cdot 10^{-11}
L = 1-\exp\left[-2\pi^{2}(86\cdot 10^9)^{2}(10)^{2}(5\cdot 10^{-11})^{2}\right]
ABRACON SMD OCXO
L = 1-\exp\left(-2\pi^{2}f^{2}t^{2}\sigma_y^{2}\right)
L\sim 1\%<10\% \text{ required for Phase Coherence}
BHEX Mini
Digital Backend
BHEX Mini
Original Analog Radio Signal
BHEX Mini
Sample the Signal every Unit Interval
f_s\geq 2f
Nyquist-Shannon Sampling Theorem
BHEX Mini
Retain only the samples and record the sign of the voltage for each sample
BHEX Mini
Reconstruct the original signal
BHEX Mini
\eta_{Q}(N_{bit})\sim 1-\frac{\pi}{2}\cdot 2^{-2N_{bit}}
SNR = \eta_{corr}\times \frac{T_{source}}{T_{system}}\times \sqrt{\Delta \nu \cdot \tau}
\operatorname{Rate}(\mathrm{bps})=N_{\text {bits }} \times \Delta \nu \times 2_{\text {pol }} \times 2_{\text {Nyquist }}
\eta = \sqrt{\eta_1\eta_2}
BHEX Mini
\eta_{Q}(N_{bit})\sim 1-\frac{\pi}{2}\cdot 2^{-2N_{bit}}
SNR = \eta_{corr}\times \frac{T_{source}}{T_{system}}\times \sqrt{\Delta \nu \cdot \tau}
\operatorname{Rate}(\mathrm{bps})=N_{\text {bits }} \times \Delta \nu \times 2_{\text {pol }} \times 2_{\text {Nyquist }}
\eta = \sqrt{\eta_1\eta_2}
Quantization Efficiency: how much of the analog SNR is retained after digitization
\eta_{Q}(1)\sim 63\%
\eta_{Q}(2)\sim 88\%
BHEX Mini
\eta_{Q}(N_{bit})\sim 1-\frac{\pi}{2}\cdot 2^{-2N_{bit}}
SNR = \eta_{corr}\times \frac{T_{source}}{T_{system}}\times \sqrt{\Delta \nu \cdot \tau}
\operatorname{Rate}(\mathrm{bps})=N_{\text {bits }} \times \Delta \nu \times 2_{\text {pol }} \times 2_{\text {Nyquist }}
\eta = \sqrt{\eta_1\eta_2}
SNR: Signal to Noise Ratio
SNR = 0.88\times \frac{1K}{100K}\times \sqrt{32 \text{GHz} \cdot 10\text{s}}=4.98
BHEX Mini
\eta_{Q}(N_{bit})\sim 1-\frac{\pi}{2}\cdot 2^{-2N_{bit}}
SNR = \eta_{corr}\times \frac{T_{source}}{T_{system}}\times \sqrt{\Delta \nu \cdot \tau}
\operatorname{Rate}(\mathrm{bps})=N_{\text {bits }} \times \Delta \nu \times 2_{\text {pol }} \times 2_{\text {Nyquist }}
\eta = \sqrt{\eta_1\eta_2}
Data Generation Rate: In Bits per Second
\text{Rate} = (2+2)\times 32 \text{ GHz} \times 2 \cdot 2=512 \text{Gb/s}
BHEX Mini
\eta_{Q}(N_{bit})\sim 1-\frac{\pi}{2}\cdot 2^{-2N_{bit}}
SNR = \eta_{corr}\times \frac{T_{source}}{T_{system}}\times \sqrt{\Delta \nu \cdot \tau}
\operatorname{Rate}(\mathrm{bps})=N_{\text {bits }} \times \Delta \nu \times 2_{\text {pol }} \times 2_{\text {Nyquist }}
\eta = \sqrt{\eta_1\eta_2}
Cross-Correlation
BHEX Mini Next Steps
Phy
- What are BHEX Mini's primary science objectives?
- To what extent can BHEX Mini achieve its objectives?
Eng
- SWaPC Requirements for Instrumentation
Fund
- Write Grant Proposals for Nelson Grants
- Write Abstract for SpaceCom 2026
- Write De-scoped BHEX Mini #1 & #2
BHEX Mini | Ben Update 07/04
By Ref Bari
