T-REX
Time-Resolving Black Holes from LEO
Ref Bari, Brown University
Introduction
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What is a black hole?
Introduction
T-REX
What is a black hole?
How do you image a black hole?
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
T-REX Primary Science Objectives
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
T-REX Primary Science Objectives
T-REX (u,v) Coverage
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
T-REX Primary Science Objectives
T-REX (u,v) Coverage
T-REX Engineering Challenges
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
T-REX Primary Science Objectives
T-REX (u,v) Coverage
T-REX Engineering Challenges
T-REX SWaPC Requirements
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
T-REX Primary Science Objectives
T-REX (u,v) Coverage
T-REX Engineering Challenges
T-REX SWaPC Requirements
T-REX Concept of Operations
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
T-REX Primary Science Objectives
T-REX (u,v) Coverage
T-REX Engineering Challenges
T-REX SWaPC Requirements
T-REX Concept of Operations
T-REX Timeline & Funding
Introduction
T-REX
What is a black hole?
How do you image a black hole?
How do you record a black hole?
T-REX Primary Science Objectives
T-REX (u,v) Coverage
T-REX Engineering Challenges
T-REX SWaPC Requirements
T-REX Concept of Operations
T-REX Timeline & Funding
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
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Ref Bari
Physics MS, Brown
-
Radiation Reaction for Binary Black Hole Systems (under Prof. Brendan Keith, Brown)
-
Funded under NSF Neural DynAMO Grant
-
-
“Nitrogen Outgassing from Water Worlds” (R.Bari et. al., under review, The Astrophysical Journal 2025)
-
“Reflection from Relativistic Light Sails” (R. Bari, The Astronomical Journal 2024)
-
“Simulating the Action Principle in Optics” (R. Bari, The Physics Teacher 2023)
-
Spin Qubit CNN Researcher at the Meriles Condensed Matter Lab
-
“A Path Integral Derivation of Hawking Radiation” (MS Thesis)
Binary Black Holes
Physics MS, Brown
-
Analysis of Binary Black Holes via Neural Networks (Prof. Brendan Keith, Brown)
Spaceflight Heritage
EQUiSat
SBUDNIC
PVDX
Spaceflight Heritage
SBUDNIC
PVDX
- 1U CubeSat (1.3 kg, 10x10x10 cm)
- Payload: High-Power LED Array + LiFePO4 Batteries (<6 kg)
- ADCS: Passive Magnetic Atitude Control System
- Power Generated: 1.3W (Top+Bottom Panels) & .7W (Side)
-
Total Cost: $5000
- All components built in-house at Brown Engineering Lab
EQUiSat
- 3U CubeSat (3 kg, 30x10x10 cm)
- Payload: Ham Radio Transceiver, 2 Cameras, Arduino Nano
- ADCS: Spring-Loaded + Aerodynamic Drag Sail
- Power Generated: 1.3W (Top+Bottom Panels) & .7W (Side)
-
Total Cost: $10,000
- 3D-Printed Components at BDW
- 3U CubeSat (~6 kg, 30x10x10 cm)
- Payload: Perovskite Solar Panels + Robotic Arm + Digital Display
- ADCS: Magnetorquers
-
Total Cost: ~$30,000
- 3D-Printed Components at BDW
- CUBECOM S-Band Transceiver ($10,000)
Spaceflight Heritage
SBUDNIC
PVDX
EQUiSat
T-REX
Spaceflight Heritage
T-REX
Time Resolving Experiment Satellite
T-REX
Capture Time-Resolved Videos of M87 & Sgr A*
Time-Resolve Binary Black Hole Systems
Rapid mm-wave time-domain observations of transient targets
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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
Capture the first video of Sgr A*
T-REX
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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-REX
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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
Size
Weight
Power
Power
\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
Cost
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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-REX
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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-REX
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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
NASA Pioneers
Aspera
Pandora
StarBurst
PUEO
(Galaxy Evolution via UV)
(Exoplanet Explorer)
(Neutron Stars via Gamma Rays)
(Particle Physics via High-Energy Neutrinos)
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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-REX
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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-REX
Oct
-
NASA NIAC Phase I
- Submitted: July 15
- Decision: Sep 6
$175,000
>$4M
-
Templeton Grant
- Submitted: Aug 15
- Decision: Oct 10
-
AAS Splinter Meeting
- Submitted: Sep 25
- Decision: Oct 30
-
CSA FAST Grant
- Submitted: Oct 26
- Decision: Dec 15
>$400,000
Princeton
Physics
Canadian
Institutions
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Team
Advisors
Inner
circle
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Canadian
Institutions
T-REX
Team
Advisors
Inner
circle
T-REX
Joshua Escobar
Space Instrument Engineer (IMAP)
Margaret Shaw-Lecerf
Space Instrument Engineer (IMAP)
Jamie Raskin
Space Instrument Engineer (Parker Solar Probe)
Michael Galvin
Principal Mechanical Engineer (Princeton Space Physics Group)
Princeton
Physics
T-REX
Team
Advisors
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Inner
circle
Luke Anderson
Lead Mechanical Engineer (Orion Space Solutions)
Laura Fissel
Assistant Professor, Queen's University (PI, BVEX)
Locke Spencer
Associate Professor, University of Lethbridge (Experimental Astrophysics)
Jayshri Sabarinathan
Associate Professor, University of Western Ontario (Engineering)
Princeton
Physics
T-REX
Team
T-REX
Inner
circle
Canadian
Institutions
Rick Fleeter
Adjunct Associate Professor, Brown
Travis Fischer
ESA/AURA Astronomer, Space Telescope Science Institute
Krista Lynne Smith
Associate Professor, Texas A&M
Andrew Miller
Postdoc, Utrecht University (LIGO Collaboration)
Princeton
Physics
Inner
circle
Canadian
Institutions
Advisors
T-REX
Mia Frickey
BS, Applied Math (Brown)
Graham Neely
BS, Engineering (Brown)
Kaylee DeGennaro
BS, Astrophysics (Brown)
Alex Khosrowshahi
BS, CS & Physics (Brown)
Sebastian Abreu
MS, Engineering (Columbia)
Gayda Mohamed
Fulbright Scholar (UAE)
Noah Barton
MS, Physics (Brown)
Sharanya Palit
MS, Physics (Brown)
Princeton
Physics
Canadian
Institutions
T-REX
Team
Advisors
Inner
circle
T-REX
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
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R
Event Horizon
Singularity
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R
Event Horizon
Singularity
Photon Sphere
1.5R
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R
Event Horizon
Black Hole Shadow
1.5R
Photon Ring
2.6R_s
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R
Event Horizon
Black Hole Shadow
1.5R_s
Photon Ring
2.6R_s
Innermost Stable
Circular Orbit
3R_s
T-REX
ds^2 = -\left(1-\frac{2M}{R}\right)dt^2 + -\left(1-\frac{2M}{R}\right)^{-1}dr^2 + r^2 d\Omega^2
p^\mu p_\mu = -m^2 \to \left(\frac{dr}{d\tau}\right)^2=E^2-\left(1-\frac{2M}{r} \right)\left(1+ \frac{L^2}{r^2}\right)
Event Horizon
Photon Ring
Shadow
ISCO
T-REX
ds^2 = -\left(1-\frac{2M}{R}\right)dt^2 + -\left(1-\frac{2M}{R}\right)^{-1}dr^2 + r^2 d\Omega^2
p^\mu p_\mu = -m^2 \to \left(\frac{dr}{d\tau}\right)^2=E^2-\left(1-\frac{2M}{r} \right)\left(1+ \frac{L^2}{r^2}\right)
Event Horizon
Photon Ring
Shadow
ISCO
T-REX
ds^2 = -\left(1-\frac{2M}{R}\right)dt^2 + -\left(1-\frac{2M}{R}\right)^{-1}dr^2 + r^2 d\Omega^2
p^\mu p_\mu = -m^2 \to \left(\frac{dr}{d\tau}\right)^2=E^2-\left(1-\frac{2M}{r} \right)\left(1+ \frac{L^2}{r^2}\right)
Event Horizon
Photon Ring
Shadow
ISCO
Photon Ring
T-REX
ds^2 = -\left(1-\frac{2M}{R}\right)dt^2 + -\left(1-\frac{2M}{R}\right)^{-1}dr^2 + r^2 d\Omega^2
p^\mu p_\mu = -m^2 \to \left(\frac{dr}{d\tau}\right)^2=E^2-\left(1-\frac{2M}{r} \right)\left(\frac{L^2}{r^2}\right)
Event Horizon
Photon Ring
Shadow
ISCO
Photon Ring
T-REX
ds^2 = -\left(1-\frac{2M}{R}\right)dt^2 + -\left(1-\frac{2M}{R}\right)^{-1}dr^2 + r^2 d\Omega^2
p^\mu p_\mu = -m^2 \to \left(\frac{dr}{d\tau}\right)^2=E^2-\left(1-\frac{2M}{r} \right)\left(1+\frac{L^2}{r^2}\right)
Event Horizon
Photon Ring
Shadow
ISCO
ISCO
T-REX
R
T-REX
T-REX
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
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M87
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SED, Sgr A*
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
T-REX
Spectral Energy Distribution (Sgr A*)
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
radio
infrared
T-REX
SED, Sgr A*
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
T-REX
SED, Sgr A*
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
\theta\sim \frac{\lambda}{D}
\sim 50\mu as
T-REX
\sim 50\mu as
T-REX
\sim 50\mu as
T-REX
SED, Sgr A*
The Supermassive Black Hole at the Galactic Center (Melia & Falcke, 2001)
\theta\sim \frac{\lambda}{D}
\sim 50\mu as
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Knox et al., “Spatial coherence from ducks”, Physics Today, March 2010
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E_1
E_2
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V(r_1 ,r_2)=\langle E_1^*
E_2\rangle
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V(r_1 ,r_2)=\langle E_1^*
E_2\rangle
T-REX
V(r_1 ,r_2)=\langle E_1^*
E_2\rangle
T-REX
V(r_1 ,r_2)=\langle E_1^*
E_2\rangle
T-REX
V(r_1 ,r_2)=\langle E_1^*
E_2\rangle
E_1
E_2
T-REX
T-REX
T-REX
T-REX
T-REX
T-REX
T-REX
T-REX
T-REX
EHT
(2019)
Event Horizon Telescope (EHT)
BHEX
(2031)
Black Hole Explorer Satellite (BHEX) Mission
BHEX
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
T-REX
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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-REX
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}
- Time-scale of Sgr A* accretion disk: 4<T<30 minutes (0<J<1)
- Time-scale of LEO Orbit: 90 minutes, with 22-minute (u,v) coverage
T-REX
Sub-milli arcsecond angular resolution:
Dual short and long baseline lengths
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-REX
\text{To time resolve Sgr A*, we must have} \\f_{coverage}>50\% \text{ in } t < T_{ISCO} \sim 30 \text{ min}
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
T-REX
T-REX
Capture Time-Resolved Videos of M87 & Sgr A*
Time-Resolve Binary Black Hole Systems
Conduct VLBI Survey of AGN targets at 86 GHz
T-REX
Capture Time-Resolved Videos of M87 & Sgr A*
Time-Resolve Binary Black Hole Systems
Conduct VLBI Survey of AGN targets at 86 GHz
T-REX
Supplement (u,v) coverage at 86 GHz
Enable parameter estimation of Sgr A*/M87
400\text{ km}
Capture Time-Resolved Videos of M87 & Sgr A*
"Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope" Palumbo et. al. ApJ 2019
T-REX
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"Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope" Palumbo et. al. ApJ 2019
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"Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope" Palumbo et. al. ApJ 2019
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$$\alpha=-\frac{\xi}{\sin i}, \quad \beta= \pm \sqrt{\eta+a^2 \cos ^2 i-\xi^2 \cot ^2 i}$$
$$M=\frac{c^2 D}{G} \frac{\theta_{sh}}{\mathcal{F}(a, i)}$$
\xi=\xi(r, M, a), \, \, \, \, \eta=\eta(r, M, a)
T-REX
\dot{M} = -2\pi R \rho u_R
T(R) = 2\pi \nu \rho R^3 \frac{d\Omega}{dR}
\Omega(R) = \sqrt{\frac{GM}{R^3}}
T-REX
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}
Videos of M87 & Sgr A*
"The Black Hole Explorer: Motivation and Vision" Johnson et. al. arXiv 2024
T-REX
Capture Time-Resolved Videos of M87 & Sgr A*
Time-Resolve Binary Black Hole Systems
Conduct VLBI Survey of AGN targets at 86 GHz
T-REX
Time-Resolve Binary Black Hole Systems
T-REX
Time-Resolve Binary Black Hole Systems
T-REX
Time-Resolve Binary Black Hole Systems
T-REX
Capture Time-Resolved Videos of M87 & Sgr A*
Time-Resolve Binary Black Hole Systems
Conduct VLBI Survey of AGN targets at 86 GHz
T-REX
Conduct VLBI Survey of AGN targets at 86 GHz
"The Black Hole Explorer: Motivation and Vision" Johnson et. al. arXiv 2024
T-REX
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
T-REX
20000\text{ km}
400\text{ km}
\text{MEO Satellite}
\text{T-REX}
"Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope" Palumbo et. al. ApJ 2019
\text{T-REX}
\text{EHT}
\text{T-REX}
\text{EHT}
\text{LEO}
\text{MEO}
T-REX
\text{MEO Satellite}
F_d
$$\theta$$
F_d
$$\theta$$
\text{LEO}
\text{MEO}
\text{LEO}
\text{MEO}
\text{LEO}
\text{MEO}
\text{LEO: Radio Arm (RA)}
\text{MEO: Optical Arm (OA)}
\tau_{res}
\theta_{res}
\frac{P}{4}=\frac{1.5\text{ hr}}{4} = 0.38 \text{ hr}
\frac{\lambda}{D}=\frac{3.5\text{ mm}}{12,400 \text{ km}} =58\mu as
\frac{P}{4}=\frac{12\text{ hr}}{4} \sim 3 \text{ hr}
\frac{\lambda}{D}=\frac{500\text{ nm}}{>3 \text{ km}} \leq 35\mu as
\text{EHT} \\ 50\mu as
\text{T-REX RA}\\ 180\mu as
\text{T-REX OA}\\ 2 as
\text{LEO: Radio Arm}
\text{MEO: Optical Arm}
t_{res} = 0.38 \text{ hr}
\theta_{res}=58\mu as
t_{res} = 3 \text{ hr}
\theta_{res} \leq 5\mu as
\textbf{EHT}
\text{}\\
\text{RA ["]}
\text{Dec ["]}
50\mu as
\textbf{T-REX RA}
180\mu as
\textbf{T-REX OA}
2as
A
B
C
Direct Detection
Heterodyne
Quantum VLBI
Direct Detection
Heterodyne
Quantum VLBI
M87
Sgr A*
10:15
11:00
8:00
Sgr A*
T-REX
a=13,000 \text{ km}
a=26,000 \text{ km}
a=6,000 \text{ km}
t_{\text{res}}\sim22.5 min
\theta_{\text{res}}\sim 35 \mu as
t_{\text{res}}\sim1 hr
\theta_{\text{res}}\sim 10 \mu as
t_{\text{res}}\sim3 hr
\theta_{\text{res}}\sim 6 \mu as
T-REX
T-REX
t=30\min
t=60\min
t=24 \text{ hr}
86 \text{ GHz}
230 \text{ GHz}
320 \text{ GHz}
"Imaging the event horizon of M87* from space on different timescales" Shlentsova et. al. ApJ 2024
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
T-REX
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength angular resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength angular resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
a=6,000 \text{ km}
\text{M}87
\text{Sgr} A^*
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Multifrequency Black Hole Imaging for the Next-generation Event Horizon Telescope (Chael et. al., 2023, ApJ)
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength angular resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Decreased signal loss
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
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength angular resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength angular resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Potential Reduced ISM Scattering
Prospects of Detecting a Jet in Sagittarius A* with VLBI (Chavez et. al., ApJ 2024)
\text{T-REX}
\text{EHT}
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)
T-REX
\text{T-REX}
\text{EHT}
Potential Reduced ISM Scattering
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength resolution
32\mu as<\theta_{\text{T-REX}} < 1800 \mu as
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Dual-baseline capability
\text{BHEX}
Rapid coverage of (u,v) plane
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope (Palumbo et. al., ApJ 2019)
T-REX
\text{T-REX}
\text{EHT}
Dual-baseline capability
\text{BHEX}
Decreased signal loss from LEO
Decreased radiation environment in LEO vs. MEO
Metrics and Motivations for Earth–Space VLBI: Time-resolving Sgr A* with the Event Horizon Telescope (Palumbo et. al., ApJ 2019)
T-REX
\text{T-REX}
\text{EHT}
Dual-baseline capability
\text{BHEX}
\tau<\frac{1}{\omega D_\lambda \theta_{\mathrm{FOV}}}
\sigma=\frac{1}{\eta_{\mathrm{Q}}} \sqrt{\frac{\mathrm{SEFD}_1 \mathrm{SEFD}_2}{2 \Delta \nu \tau}}
\text{Coherence Time}
\text{Thermal Noise}
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Infrared Thermal Emissions
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Limited Ground Coverage
T-REX
\text{T-REX}
\text{EHT}
Limited Ground Coverage
T-REX
\text{T-REX}
\text{EHT}
Limited Ground Coverage
T-REX
\text{T-REX}
\text{EHT}
Rapid (u,v) coverage
Decreased signal loss
Decreased radiation environment
Infrared Thermal Emissions
Limited Ground Coverage
Aggressive Slew Rate Required
Potential Reduced ISM Scattering
mm-wavelength resolution
Dual-baseline capability
T-REX
\text{T-REX}
\text{EHT}
Aggressive Slew Rate Required
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
T-REX
T-REX
T-REX
T-REX SWaPC
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
NASA Pioneers
Aspera
Pandora
StarBurst
PUEO
(Galaxy Evolution via UV)
(Exoplanet Explorer)
(Neutron Stars via Gamma Rays)
(Particle Physics via High-Energy Neutrinos)
Mission Parameters
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\tau_{\text{Coherence, T-REX}}\lessapprox 2 \text{ min} \sim 120 s
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
SEFD
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 100K
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 100K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 100K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\text{SEFD}_{\text{BHEX}}\sim 18,000 \text{ Jy}
\text{SEFD}_{\text{ALMA}}\sim 74 \text{ Jy}
\text{SEFD}_{\text{SMA}}\sim 6700 \text{ Jy}
\text{SEFD}_{\text{SMT}}\sim 10,500 \text{ Jy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\sigma_{\text{T-REX - BHEX}}=\frac{1}{\eta_{\mathrm{Q}}} \sqrt{\frac{\mathrm{SEFD}_{\mathrm{BHEX}} \mathrm{SEFD}_{\text{T-REX}}}{2 \Delta \nu \Delta t}}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\sigma_{\text{T-REX - BHEX}}=\frac{1}{\eta_{\mathrm{Q}}} \sqrt{\frac{\mathrm{SEFD}_{\mathrm{BHEX}} \mathrm{SEFD}_{\text{T-REX}}}{2 \Delta \nu \Delta t}}
\sigma_{\text{T-REX - EHT}}=\frac{1}{\eta_{\mathrm{Q}}} \sqrt{\frac{\mathrm{SEFD}_{\mathrm{EHT}} \mathrm{SEFD}_{\text{T-REX}}}{2 \Delta \nu \Delta t}}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\sigma_{\text{T-REX - BHEX}}=\frac{1}{0.75} \sqrt{\frac{(18,000 \text{ Jy})(32,000 \text{Jy})}{2 (32 \text{GHz}) (100s)}}
\sigma_{\text{T-REX - EHT}}=\frac{1}{0.75} \sqrt{\frac{(6000 \text{ Jy})(32,000 \text{Jy})}{2 (32 \text{GHz}) (10s)}}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 2\pi \cdot f \cdot \sigma_t
\sigma_t = \sigma_f \cdot \Delta t
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 2\pi \cdot f \cdot \sigma_t
\sigma_t = \sigma_f \cdot \Delta t
\sigma_t = 8\cdot 10^{-15} (\text{LISA USO})
\Delta \phi = 2\pi \cdot (86\cdot 10^9 \text{ Hz}) \cdot 8\cdot 10^{-15}s\sim 10^{-3} \text{ rad}<1 \text{ rad}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\Delta t = \text{10 s})
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\Delta t = \text{10 s})
L = 1-\exp\left(-2\pi^{2}f^{2}t^{2}\sigma_y^{2}\right)
L = 1-\exp\left[-2\pi^{2}(86\cdot 10^9)^{2}(10)^{2}(5\cdot 10^{-11})^{2}\right]\sim 1\%
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})=N_{\text {bits }} \times \Delta \nu \times 2_{\text {pol }} \times 2_{\text {Nyquist }}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})=N_{\text {bits }} \times \Delta \nu \times 2_{\text {pol }} \times 2_{\text {Nyquist }}
\text{Rate}\times T_{orb} \times \text{Duty Cycle} = \text{Total Data (GB)}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\theta_{S-S} \sim \frac{\lambda}{D}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\theta_{S-S} \sim \frac{\lambda}{D}=\frac{3.5mm}{20,000 km}
\theta_{S-G} \sim \frac{\lambda}{D}=\frac{3.5mm}{400 km}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
Systems Design
\sim85.3 kg
\sim 437 W
\sim \$25\text{ million}
N/A
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
Systems Design
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\tau<\frac{1}{\omega D_\lambda \theta_{\mathrm{FOV}}}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
Systems Design
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\tau<\frac{1}{\omega D_\lambda \theta_{\mathrm{FOV}}}
\omega=\frac{2\pi}{P} = \frac{2\pi}{1.5 \text{ hr}\cdot \frac{3600 s}{1 \text{hr}}}=1.16\times 10^{-3} rad/s
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\tau<\frac{1}{\omega D_\lambda \theta_{\mathrm{FOV}}}
0.11 G \lambda < b_{s g}<3.5 G \lambda
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
Systems Design
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\tau<\frac{1}{\omega D_\lambda \theta_{\mathrm{FOV}}}
\theta_{FOV} = 180 \mu as
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
Systems Design
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\tau<\frac{1}{\omega D_\lambda \theta_{\mathrm{FOV}}}=\frac{1}{(1.16\times 10^{-3} \frac{rad}{s}) (3.5 G\lambda)(1.6\cdot 10^{-7}s)}
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
\tau_{\text{T-REX}}\lessapprox \frac{15G\lambda}{3.5 G\lambda}\lessapprox 4.2 \text{ min}, \tau_{\text{Coherence, T-REX}}\sim 275 s
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
Systems Design
T^*_{sys} = [T_{rx}+\eta_{ff}T_{b, inc}](1+r)\sim 30K
T_{b,inc}=\frac{F_{tot}A_{eff}}{2k}\sim 3\cdot 10^{-3} K
T_{rx}=15K, \eta_{ff}=0.95, \eta_{A}=0.85, r= 1, F_{tot}\sim 2\pm 0.2 Jy
SEFD
USO
Data
\theta_{\text{Res}}
Orbit
\sigma_{\text{Noise}}
\tau_{\text{max}}
\Delta \phi = 4.3\cdot 10^{-3} \text{ rad } (\text{LISA USO})
L\sim 1\% \text{ (JUICE USO)}
\operatorname{Rate}(\mathrm{bps})\sim 8,750 \text{ GB }(T_{obs}=.5T_{orb}) \text{ over 1 orbit}
\text{Circular Highly-Inclined Polar LEO}, r\sim 400 km, e \sim 0, i>78^{\circ}
66.93s<\tau_{GS}<275s
\text{SEFD}_{\text{T-REX}}=\frac{2kT^*_{sys}}{\eta_A A}\sim 32,000 \text{ Jy}
\theta_{\text{T-REX -BHEX}}\sim 35 \mu as
\theta_{\text{T-REX - EHT}} \sim 1800 \mu as
\sigma_{\text{T-REX - BHEX}}\sim 12.65 \text{ mJy}
\sigma_{\text{T-REX - EHT}}\sim 40 \text{ mJy}
T-REX
T-REX
Antenna
T-REX
Antenna
T-REX
Antenna
T-REX
T-REX
Cryocooler
HiPTC Heat Intercepted Pulse Tube Cooler
T-REX
T-REX
Ultra-Stable Oscillator
T-REX
Ultra-Stable Oscillator
\Delta \phi = 2\pi \cdot f \cdot \sigma_t
\sigma_t = \sigma_f \cdot \Delta t
Phase Error
T-REX
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}
T-REX
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}
T-REX
Digital Backend
T-REX
Original Analog Radio Signal
T-REX
Sample the Signal every Unit Interval
f_s\geq 2f
Nyquist-Shannon Sampling Theorem
T-REX
Retain only the samples and record the sign of the voltage for each sample
T-REX
Reconstruct the original signal
T-REX
T-REX
T-REX
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
T-REX
T-REX ConOps
Optical Terminals
RF Tracking Stations
VLBI Ground Stations
\text{T-REX}
T-REX Data Center
Optical Terminals
RF Tracking Stations
VLBI Ground Stations
\mathbf{T-REX}
T-REX Data Center
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- T-REX Timeline & Funding Deadlines
T-REX
- Email BHEX Team
Jan 2025
T-REX
- Email BHEX Team
Jan 2025
T-REX
- Email BHEX Team
Jan 2025
T-REX
- Email BHEX Team
Jan 2025
Feb 2025
- Literature Review
T-REX
- Email BHEX Team
Jan 2025
Feb 2025
Mar 2025
- Literature Review
- Advised on BHEX Mini by Prof. Rick Fleeter
- Submit to Rhode Island Space Grant
Rick Fleeter
T-REX
- Email BHEX Team
Jan 2025
Feb 2025
Mar 2025
- Literature Review
Apr 2025
- Ivy Space Conference
- Ben Hudson (BHEX, KISPE)
- Luke Anderson (Orion Space Systems)
Ben Hudson
Luke Anderson
- Advised on BHEX Mini by Prof. Rick Fleeter
- Submit to Rhode Island Space Grant
T-REX
- Email BHEX Team
Jan 2025
Feb 2025
Mar 2025
- Literature Review
Apr 2025
May 2025
- Ivy Space Conference
- Ben Hudson (BHEX, KISPE)
- Luke Anderson (Orion Space Systems)
- Trained ~6 undergraduates to run simulations on BHEX Mini
- Jeffrey Olson (Cryocooler Engineer, Lockheed Martin
Jeffrey Olson
- Advised on BHEX Mini by Prof. Rick Fleeter
- Submit to Rhode Island Space Grant
T-REX
Jun 2025
Jul 2025
- Completed Antenna SWaPC Requirements
- Obtained Preliminary Grant Funding from Nelson Center
- Began correspondence with NASA JPL on Ultrastable Oscillators
- Constrained BHEX Mini SWaPC Requirements
- Approved by Brown Division of Research as PI for BHEX Mini
- Submitted to NASA NIAC Phase I Solicitation
- Accepted to SmallSat Europe 2026
Todd Ely
Joseph Lazio
Eric Burt
- Email BHEX Team
Jan 2025
Feb 2025
Mar 2025
- Literature Review
Apr 2025
May 2025
Jun 2025
Jul 2025
- Ivy Space Conference
- Ben Hudson (BHEX, KISPE)
- Luke Anderson (Orion Space Systems)
- Trained ~6 undergraduates to run simulations on BHEX Mini
- Jeffrey Olson (Cryocooler Engineer, Lockheed Martin)
- Rejected from RISG
- Completed Antenna SWaPC Requirements
- Obtained Preliminary Grant Funding from Nelson Center
- Began correspondence with NASA JPL on Space-Space VLBI
- Constrained BHEX Mini SWaPC Requirements
- Approved by Brown Division of Research as PI for BHEX Mini
- Submitted to NASA NIAC Phase I Solicitation
- Accepted to SmallSat Europe 2026
- Advised on BHEX Mini by Prof. Rick Fleeter
- Submit to Rhode Island Space Grant
Feb 2025
Mar 2025
- Literature Review
Apr 2025
May 2025
Jun 2025
Jul 2025
- Ivy Space Conference
- Ben Hudson (BHEX, KISPE)
- Luke Anderson (Orion Space Systems)
- Trained ~6 undergraduates to run simulations on BHEX Mini
- Jeffrey Olson (Cryocooler Engineer, Lockheed Martin)
- Rejected from RISG
- Completed Antenna SWaPC Requirements
- Obtained Preliminary Grant Funding from Nelson Center
- Began correspondence with NASA JPL on Space-Space VLBI
- Rejected from International Astronautical Congress
- Constrained BHEX Mini SWaPC Requirements
- Approved by Brown Division of Research as PI for BHEX Mini
- Submitted to NASA NIAC Phase I Solicitation
- Accepted to SmallSat Europe 2026
- Advised on BHEX Mini by Prof. Rick Fleeter
- Submit to Rhode Island Space Grant
- Meeting with MIT Lincoln Labs (8/15)
- Colloquium at Princeton IAS (9/04)
- Michael Johnson Colloquium at Brown (PI, BHEX) (9/22)
- Assemble Science/Engineering Leadership Team for NASA / CSA
Aug 2025
Sep 2025
- Accepted as NASA NIAC Finalist
- Accepted to 10th International VLBI Conference (Sweden)
- Accepted to Gravitational Wave Conference (Georgia Tech)
💰Funding Deadlines
June
💰Funding Deadlines
$5,000
-
Brown Nelson Grants
- Submitted: June 30
- Decision: Sep 15
July
💰Funding Deadlines
$5,000
$175,000
-
Brown Nelson Grants
- Submitted: June 30
- Decision: Sep 15
-
NASA NIAC Phase I
- Submitted: July 15
- Decision: Sep 6
Aug
💰Funding Deadlines
$5,000
$175,000
>$4M
-
Brown Nelson Grants
- Submitted: June 30
- Decision: Sep 15
-
NASA NIAC Phase I
- Submitted: July 15
- Decision: Sep 6
-
Templeton Grant
- Submitted: Aug 15
- Decision: Oct 10
Sep
💰Funding Deadlines
$5,000
$175,000
>$4M
-
Brown Nelson Grants
- Submitted: June 30
- Decision: Sep 15
-
NASA NIAC Phase I
- Submitted: July 15
- Decision: Sep 6
-
Templeton Grant
- Submitted: Aug 15
- Decision: Oct 10
-
AAS Splinter Meeting
- Submitted: Sep 25
- Decision: Oct 30
Oct
💰Funding Deadlines
$5,000
-
NASA NIAC Phase I
- Submitted: July 15
- Decision: Sep 6
$175,000
-
Brown Nelson Grants
- Submitted: June 30
- Decision: Sep 15
>$4M
-
Templeton Grant
- Submitted: Aug 15
- Decision: Oct 10
-
AAS Abstracts
- Submitted: Sep 25
- Decision: Oct 30
-
CSA FAST Grant
- Submitted: Oct 26
- Decision: Dec 15
>$400,000
- Introduction
- What is a black hole?
- How do you image a black hole?
- How do you record a black hole?
- T-REX Primary Science Objectives
- T-REX (u,v) Coverage
- T-REX Engineering Challenges
- T-REX SWaPC Requirements
- T-REX Concept of Operations
- The Request
T-REX
T-REX NASA NIAC Diagrams
By Ref Bari
