BHEX Mini

Direct Imaging Black Holes from LEO

Ref Bari | 06/29 Update

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

AI-Assisted Modular VLBI Constellation 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

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

One-line mission statement

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

One-line engineering innovation

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

What revolutionary science could it enable?

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

Motivation for telescope design

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

Why this? Why now? How does it advance NASA's stated goals?

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

Primary Science Objectives

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

Why is this TRL 1/2? Why is it revolutionary, not evolutionary?

Hybrid Observatory for Earth-like Exoplanets (HOEE)

John Mather, NASA GSFC

We propose the first hybrid observatory, combining a 100 m diameter starshade in space with a telescope on the ground. The Hybrid Observatory for Earth-like Exoplanets (HOEE) would convert the largest ground-based telescopes now under construction (Giant Magellan Telescope, Thirty Meter Telescope, and Extremely Large Telescope) into the most powerful planet finders yet designed. No other proposed equipment can match the angular resolution (image sharpness), sensitivity (ability to see faint objects in a given time), or contrast (ability to see faint planets near bright stars). The large telescope is needed because Earth-like planets are extremely faint. The starshade is needed to block the glare of the host stars; the sun is 10 billion times brighter than the Earth at visible wavelengths.  A starshade in an astro-stationary orbit would match position and velocity with the moving telescope, and cast a dark shadow of the star, without blocking the light of its planets.  Active propulsion would maintain alignment during the observation. Adaptive optics in the telescope would compensate for atmospheric distortion of the incoming images. The HOEE would address the highest priority recommendation of the Exoplanet Strategy report: observe reflected light from Earth-like planets with low resolution spectroscopy. This light is influenced by surface minerals, oceans, continents, weather, vegetation, and atmospheric constituents, temperature, and pressure. Observing many systems would help answer the question of why configurations like our own Solar System are rare; of the thousands of known exoplanet systems, none are quite like home, with inner rocky planets, a faint cloud of dust, an asteroid belt, and giant outer planets. Observing photosynthetic oxygen would answer the questions of whether life is rare or common, what it requires, and how long it takes to grow. But this starshade is not constructible with today’s designs. An ultra-lightweight redesign will be developed that can be built or assembled in space. Our objective is to cut the starshade mass by more than a factor of 10. There is no reason to require thousands of kg to support 400 kg of thin membranes. The HOEE depends on two major innovations:  a ground-space hybrid observatory,  and an extremely large telescope on the ground.  The tall pole requiring design and demonstration is the mechanical concept of the starshade itself.  It must satisfy conflicting requirements for size and mass, shape accuracy and stability, and rigidity during or after thruster firing. Low mass is essential for observing many different target stars. If it can be assembled or constructed after launch, it need not be built to survive launch. We believe all requirements can be met, given sufficient effort.  The HOEE is the most powerful exoplanet observatory yet proposed.

Memorable, superlative one-liner

Requirements for NASA NIAC Phase I

NASA NIAC Phase I Solicitations

First Impression: Overview Chart

NASA NIAC Phase I Solicitations

Overview Chart Example: ACTION

NASA NIAC Phase I Solicitations

Overview Chart Example: CLOVER

NASA NIAC Phase I Solicitations

3-Page Whitepaper: ACTION

NASA NIAC Phase I Solicitations

3-Page Whitepaper: CLOVER

NASA NIAC Phase I Solicitations

BHEX Mini Problems

NASA NIAC Phase I Solicitations

 

  1. Optical Downlink

    1. Problem: Limited Ground Coverage at LEO

    2. Radical Solution: Uplink to BHEX at MEO

  2. Atmospheric Decoherence

    1. Problem: Earth’s atmosphere adds noise to radio signals downlinked to ground stations, thus decreasing SNR

    2. Radical Solution: Delete the Earth’s Atmosphere

  3. Expensive SWaP Cryocooler Required

    1. Problem: We require an expensive, heavy Cryocooler to cool BHEX Mini’s primary receiver down to cryogenic sub-25K temperatures

    2. Radical Solution: Implement Passive Cooling Mechanisms (i.e., JWST’s Sunshield)

  4. (u,v) coverage limited to 86 GHz Regime

    1. Problem: Since BHEX Mini will be observing at only 86 GHz, its (u,v) coverage is restricted to a limited domain of the interferometric plane.

    2. Radical Solutions: (1) Employ a sandwich VLBI construction between BHEX + BHEX Mini or (2) Employ an intelligent swarm of VLBI SmallSats in LEO which can form many short and long baselines that provide dense and rapid (u,v) coverage

Radical Solution: Cryocooling

NASA NIAC Phase I Solicitations

Radical Solution: Cryocooling

NASA NIAC Phase I Solicitations

  1. 🎯 Introduction
  2. 🔭 Event Horizon Telescope
  3. 📻 BHEX (Black Hole Explorer Satellite)
  4. 🕰️ BHEX Mini
  5. 🕒 BHEX Mini Timeline
  6. 💰Funding Deadlines

BHEX Mini

  1. 🎯 Introduction
  2. 🔭 Event Horizon Telescope
  3. 📻 BHEX (Black Hole Explorer Satellite)
  4. 🕰️ BHEX Mini
  5. 🕒 BHEX Mini Timeline
  6. 💰Funding Deadlines

BHEX Mini

Black Hole (M87)

Event Horizon Telescope

(2019)

Event Horizon Telescope (EHT)

Event Horizon Telescope

(2019)

Event Horizon Telescope (EHT)

  1. 🎯 Introduction
  2. 🔭 Event Horizon Telescope
  3. 📻 BHEX (Black Hole Explorer Satellite)
  4. 🕰️ BHEX Mini
  5. 🕒 BHEX Mini Timeline
  6. 💰Funding Deadlines

BHEX Mini

Event Horizon Telescope

(2019)

Event Horizon Telescope (EHT)

Black Holes: An Intro

(2031)

Black Hole Explorer Satellite (BHEX) Mission

Imaging a Black Hole

(The black hole explorer: Motivation and vision, Johnson et. al., 2024)

  1. 🎯 Introduction
  2. 🔭 Event Horizon Telescope
  3. 📻 BHEX (Black Hole Explorer Satellite)
  4. 🕰️ BHEX Mini
  5. 🕒 BHEX Mini Timeline
  6. 💰Funding Deadlines

BHEX Mini

Spaceflight Heritage

EQUiSat

SBUDNIC

PVDX

Spaceflight Heritage

SBUDNIC

PVDX

EQUiSat

BHEX Mini

\text{MEO} (20000 \text{ km})
\text{LEO} (400 \text{ km})

BHEX Mini

Imaging a Black Hole

Todd Ely

Joseph Lazio

Eric Burt

Ben Hudson

Luke Anderson

Rick Fleeter

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

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

BHEX Mini

BHEX Mini

Antenna

BHEX Mini

Receiver

BHEX Mini

Cryocooler

BHEX Mini

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

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

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🕒 Prospective Timeline

June

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August

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  • NASA NIAC 2025 Phase I Step I
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September

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    • Nacer Chahat
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🕒 Prospective Timeline

June

July

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September

  • NSF Foundational Research in Robotics Grant (FRR)
  • Fall Walls Foundation Selections
  • Brown University Co-Lab 
  • NASA NIAC Phase I Round I Step B Selections Announced
  • Solar Panel Focus
    • DCubed Inc.
    • DHV Tech
  • NASA NIAC 2025 Phase I Step I
  • SpaceCom Conference 2026
  • Brown Nelson + Hazeltine Grants
  • Antenna Focus
    • Nacer Chahat
    • Emmanuel Decrossas
  • Cryocooler Focus
    • SunPower
    • Blue Marble

🕒 Prospective Timeline

June

July

Aug

Sep

  • Cryocooler Focus
    • SunPower
    • Blue Marble
  • NSF Foundational Research in Robotics Grant (FRR)
  • Fall Walls Foundation Selections
  • Brown University Co-Lab 
  • NASA NIAC Phase I Round I Step B Selections Announced
  • Solar Panel Focus
    • DCubed Inc.
    • DHV Tech
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NASA NIAC Phase I

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NASA NIAC Phase I

Oct

$175,000

$3,000

$250,000

💰Funding Oppurtunities