Beyond Sgr A* and M87*: Sub-Microarcsecond Black Hole Shadow Detection via Lunar-based Extremely Long Baseline Interferometry

TL;DR

This paper proposes using lunar-based very long baseline interferometry to achieve sub-microarcsecond resolution, enabling detection of black hole shadows in a larger sample of SMBHs beyond current Earth-based capabilities.

Contribution

It introduces a lunar-based VLBI concept for black hole shadow imaging, identifying target SMBHs and analyzing observational feasibility with different telescope sizes and locations.

Findings

Six SMBHs have detectable shadows with a 5 m lunar telescope.

Larger telescopes (20 m, 100 m) are needed for some targets.

Photon ring detection is feasible with space telescopes filling baseline gaps.

Abstract

The 1.3 mm ground-based very long baseline interferometry (VLBI) array, the Event Horizon Telescope (EHT), is limited by the Earth's diameter and can image the supermassive black hole (SMBH) shadows of only M87* and Sgr A*. Extending the array with an assumed lunar-based telescope could achieve $\sim 0.85\ \mu$as angular resolution at 230 GHz, enabling black hole shadow detection for a larger SMBH sample. The concept is motivated by space VLBI missions and lunar exploration, including the ongoing Lunar Orbit VLBI Experiment (LOVEX) aboard QueQiao-2 (Chang'E-7) and the planned International Lunar Research Station (ILRS). We assess shadow detectability for 31 SMBH with predicted large angular sizes, exploring different telescope location and antenna size. Assuming a telescope at the lunar antipode, we simulate the Moon-Earth (u,v) coverage and show that source geometry relative to the Moon's orbit determines whether the primary indicator of shadow, first visibility null, can be sampled. Using a geometric ring model, we identify six high-priority targets: M104, NGC 524, PGC 049940, NGC 5077, NGC 5252, and NGC 1052. Shadows of M104, NGC 5077, and NGC 1052 are detectable with a 5 m lunar-based telescope; PGC 049940 requires 20 m; NGC 524 and NGC 5252 require 100 m. Photon ring detection for Sgr A*, M87*, NGC 1600, and M31 is possible if space telescopes fill the baseline coverage gaps and sensitivity requirements are met. These results provide a clear scientific and technical motivation for lunar-based telescopes in future black hole shadow studies.