Galactic Science with Ultra-High Angular Resolution X-ray Imaging
Abstract
Milli- to micro-arcsecond X-ray imaging will open a new observational regime for Galactic astrophysics by resolving physical scales that are inaccessible to current X-ray observatories. This white paper highlights the science enabled by such capabilities across four broad questions: how particles are accelerated, how stars die, how accretion is fueled, and what populations of X-ray sources inhabit the Galaxy. Ultra-high angular resolution will enable many new studies, such as resolving shocks and jets, measuring proper motions, parallaxes, and binary orbits, and providing secure multiwavelength counterpart identifications in crowded environments such as the Galactic Center and globular clusters. Combined with high-time-resolution observations, these measurements will connect variability and transient events to the physical structures in which they originate, while coordination with gravitational-wave, neutrino, γ-ray, radio, optical, and infrared facilities will provide spatial information needed to identify and characterize multi-messenger sources. In addition to defining the science cases, this paper presents a curated list of compelling targets spanning various angular resolutions and outlines the complementary specifications necessary to maximize the scientific outcome. Accomplishing these science goals will require an instrument with high angular resolution, precise astrometry, substantial collecting area, sufficient spectral and timing resolution, and high dynamic range imaging capabilities.
Related
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BibTeX
@misc{draghis2026galactic,
title = {{Galactic Science with Ultra-High Angular Resolution X-ray Imaging}},
author = {Paul A. Draghis and Jeremy Hare and Mayura Balakrishnan and Poshak Gandhi and Tyler Holland-Ashford and Margarita Karovska and Thomas Maccarone and Herman L. Marshall and Mark Reynolds and Malgosia Sobolewska and Ryan Tanner},
howpublished = {arXiv},
year = {2026},
month = aug,
doi = {10.48550/arxiv.2608.28746},
eprint = {2608.28746},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2608.28746},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Galactic Science with Ultra-High Angular Resolution X-ray Imaging
AU - Paul A. Draghis
AU - Jeremy Hare
AU - Mayura Balakrishnan
AU - Poshak Gandhi
AU - Tyler Holland-Ashford
AU - Margarita Karovska
AU - Thomas Maccarone
AU - Herman L. Marshall
AU - Mark Reynolds
AU - Malgosia Sobolewska
AU - Ryan Tanner
PY - 2026
DA - 2026/08/28
PB - arXiv
DO - 10.48550/arxiv.2608.28746
UR - https://arxiv.org/abs/2608.28746
AB - Milli- to micro-arcsecond X-ray imaging will open a new observational regime for Galactic astrophysics by resolving physical scales that are inaccessible to current X-ray observatories. This white paper highlights the science enabled by such capabilities across four broad questions: how particles are accelerated, how stars die, how accretion is fueled, and what populations of X-ray sources inhabit the Galaxy. Ultra-high angular resolution will enable many new studies, such as resolving shocks and jets, measuring proper motions, parallaxes, and binary orbits, and providing secure multiwavelength counterpart identifications in crowded environments such as the Galactic Center and globular clusters. Combined with high-time-resolution observations, these measurements will connect variability and transient events to the physical structures in which they originate, while coordination with gravitational-wave, neutrino, γ-ray, radio, optical, and infrared facilities will provide spatial information needed to identify and characterize multi-messenger sources. In addition to defining the science cases, this paper presents a curated list of compelling targets spanning various angular resolutions and outlines the complementary specifications necessary to maximize the scientific outcome. Accomplishing these science goals will require an instrument with high angular resolution, precise astrometry, substantial collecting area, sufficient spectral and timing resolution, and high dynamic range imaging capabilities.
ER -