Candidate Dyson Sphere Detections Are Regular Stars with Black Hole Galaxy Behind

Dyson spheres are solar systam sized shells enclosing stars supposedly manufactured by hyper advanced civilizations.

Nice idea, however almost any imagined solution runs out of materiel.  However, I can imagine a one mile diameter ring rotating on a hub generating one g at the rim.  This allows space factories and residences in earth Orbit and ultimately around any other object in our solar system as we perfect the tech.

any such Rim habitat system can be a mile wide easily providing  over three square milles of buildable surface with many plausible floors as well.  Ten stories alone will give us most of thirty square miles of floor.

The real potential for just this design is thousands, each holding up to a million folks or a space habitat population in the billions throughout our solar system and all as safe as can be.  again, we do not need to manage gravity for this.

We may need superior protection out there but that is quite different from advancing new physics.  for prtotection, we can turn the moon into swiss cheese but never adapt to the moon.s gravity.

The RIM station is operational any time we want to stsrt lifting components.  The hub could even be made from quality cement for protection.

think of a cross sectional slab fitting simply to the next slab until you have a circular hub.  Then turn cables about this hub naturally compressing the assemblage.  No connectors needed at all.  The only connectors on the cables will then be on the rim at one g..

I postulate that any advanced civilization will actually build thousands of these objects.

Candidate Dyson Sphere Detections Are Regular Stars with Black Hole Galaxy Behind

February 7, 2025 by Brian Wang

Astronomers looked more closely at one of seven stars that looked like possible Dyson sphere candidates from earlier observations.

https://www.nextbigfuture.com/2025/02/candidate-dyson-sphere-detections-are-regular-stars-with-black-hole-galaxy-behind.html#more-200871

They used high-resolution e-MERLIN and EVN (e-VLBI) observations of a radio source associated with Dyson Sphere candidate G, identified as part of Project Hephaistos. The radio source, VLASS J233532.86−000424.9, is resolved into three compact components and shows the typical characteristics of a radio-loud active galactic nucleus (AGN). The European VLBI Network (EVN) observations show that it has a brightness temperature in excess of 100 million degrees kelvin. No radio emission is detected at the position of the M-dwarf star. This result confirms an earlier hypothesis, that at least some of the Dyson Sphere candidates of project Hephaistos are contaminated by obscured, background AGN, lying close to the line of sight of otherwise normal galactic stars. High-resolution radio observations of other Dyson Sphere candidates can be useful in distinguishing truly promising candidates from those contaminated by background sources.

Project Hephaistos recently published a list of Dyson Sphere candidates selected from 5 million sources with distances measured by Gaia to  parsecs. Seven candidates were identified all of which are M-dwarf stars exhibiting an infrared excess in the WISE bands W3 and W4. These peculiar stellar Spectral Energy Distributions (SEDs) are consistent with simple Dyson Sphere models. Suazo et al. (2024) considered several natural explanations for the candidate SEDs, including warm debris discs which can also produce excess mid-infrared (MIR) emission (Cotten & Song 2016). However, the characteristics of these candidates challenge natural explanations: debris discs around M-dwarfs are extremely rare, and these candidates show higher temperatures and larger fractional luminosities than typical debris discs. While young stellar discs can have larger fractional luminosities, the seven candidates lack the variability typically associated with young stars. In addition, extreme debris discs (EDDs; Balog et al. 2009), which can have high fractional luminosities and higher temperatures (Moór et al. 2021), have never been observed around M-dwarfs.

High-resolution e-MERLIN and EVN radio observations of J2335−0004, associated with Project Hephaistos Dyson Sphere candidate G, reveal compelling evidence that the MIR excess previously attributed to a potential Dyson Sphere is instead the result of contamination by a background AGN. The combination of e-MERLIN and EVN data demonstrates that the source exhibits the typical characteristics of a radio-loud AGN in terms of its brightness temperature, component spectral indices, and source morphology.

Analysis of the positional offsets between the radio, MIR (WISE), and optical (Gaia) data reinforces this interpretation. While the W1 and W2 infrared bands align closely with the M-dwarf star, the W3 and W4 bands are offset towards the AGN (J2335−0004), indicating that the latter dominates the MIR emission. This contamination explains the SED anomaly that initially identified the G as a Dyson Sphere candidate.

Our findings align with the hypothesis that some, if not all, of the Dyson Sphere candidates from Project Hephaistos are affected by similar background AGN contamination. The likely culprits are ‘hot, dust-obscured galaxies’ (hot DOGs), which are faint in the optical and NIR but are well detected in the MIR. The absence of X-ray counterparts further supports the scenario of a heavily obscured, Compton thick AGN, also consistent with the properties of hot DOGs.

Finally, we note the absence of any detectable radio emission at the precise Gaia position of candidate G. All these findings underscore the critical role of high-resolution radio imaging in clarifying the origins of anomalous astrophysical data and highlight the necessity of meticulous background subtraction, particularly in the infrared, for the robust identification of Dyson Sphere candidates. Future high-resolution radio observations targeting other Project Hephaistos Dyson Sphere candidates (e.g. candidates A and B), would be invaluable for further testing the selection criteria and distinguishing truly promising candidates from those affected by background contamination. The challenge of differentiating genuine MIR excess sources from background AGN contamination is equally significant in searches for EDDs (Moór et al. 2021; Contardo & Hogg 2024). This highlights the need for careful source characterisation and follow-up observations to mitigate the risk of false positives in such studies.