We still know very little about giant supermassive black holes (SMBH). After 30 years of study, we don’t know precisely how these objects produce their power. This requires observations at X-ray wavelengths. The state-of-the-art for X-ray images is Chandra (~0.5-1 arcsecond resolution) but this is insufficient to image regions near SMBH where the most energetic behavior occurs. The Accretion Explorer (AE) is a mission architecture that will shatter new ground by creating X-ray images at scientifically crucial energies of 0.7-1.2 keV, 1.5-2.5 keV, 6-7 keV, up to 6 orders of magnitude better than Chandra, and will offer imaging at 4-5 orders of magnitude better than JWST (IR) and HST(optical/UV).
The specific X-ray energy bands the Accretion Explorer will cover contain vital X-ray line signatures that can distinguish between SMBH activity and stellar processes. The AE NIAC concept would be a game changer for NASA and astrophysics. X-ray interferometry will challenge and change the conversation around future mission possibilities for NASA’s flagships. It will also influence the Astrophysics 2030 Decadal Survey and will significantly contribute to our scientific knowledge base in astrophysics and other fields. AE has tremendous potential to generate enthusiasm for future missions and the potential to build advocacy to support it within NASA, society, and the aerospace community.
Alternative approaches to ultra high-resolution X-ray imaging technology are not currently being funded. They will focus on a large free-flying X-ray interferometer. They will design a multiple spacecraft system that provides the architecture to align individual mirror pair baseline groupings provided by individual collector spacecraft, with the pointing precision to achieve micro-arcsecond resolution. The study will assess the required pointing stability and determine optimal ways to nest and mount the collecting mirror flats within mirror modules. They will assess the required size for the detector array(s) to accommodate the wavelength coverage for detecting fringes, study how images will be created from fringes, and produce a simulated image from a design with accompanying optical element tolerance tables. They will document alternative approaches, how new factors substantially differentiate AE from prior efforts for X-ray interferometry, and identify technical hurdles.
Weaver and her team are focused on optimizing mirror positioning, required detector sensitivity, and the pointing stability needed to maintain coherence between the mirrorcraft and detector craft. The underlying technologies for precise positioning and stable control could have applications beyond this single mission.
These include establishing how small baseline interferometers can be flown with less risk in terms of spacing and tethering mirror modules, studies of very high levels of pointing precision for space-based interferometers, and extreme stability on target. Producing a simulated image from this design with accompanying tolerance tables can inform other space-based interferometry designs.
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