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The information content of optical intensity interferometry — arXiv:2609.05602

Source: arXiv (en)
Original: https://arxiv.org/abs/2609.05602
License (as archived): CC0-1.0
Archived: 2026-10-16T16:06:49.639Z
SHA-256 of the archived text: 1c8e9d483c7b8aecc13eac3246497347739d2d9300295aa81636e15c8240ffe5
Stable URL of this page: https://metraipolis.com/documento/dc_314fcfeb82cc

How to cite

The information content of optical intensity interferometry — arXiv:2609.05602 — arXiv (en), https://arxiv.org/abs/2609.05602 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_314fcfeb82cc (Metraipolis archive dc_314fcfeb82cc, sha256 1c8e9d483c7b8aecc13eac3246497347739d2d9300295aa81636e15c8240ffe5)

BibTeX

@misc{dc314fcfeb82cc,
  title = {The information content of optical intensity interferometry — arXiv:2609.05602},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2609.05602},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_314fcfeb82cc; sha256 1c8e9d483c7b8aecc13eac3246497347739d2d9300295aa81636e15c8240ffe5},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2609.05602. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Optical intensity interferometry (II) can in principle resolve structure on angular scales $\theta\sim \lambda/B$, but it measures only the squared visibility $|{\cal V}|^2$, discarding Fourier phase. We quantify what information can actually be recovered from phase-less $|{\cal V}|^2$ measurements as a function of the aggregate signal-to-noise ratio and array configuration, using score-based diffusion models as non-parametric image priors. We construct an image reconstruction pipeline, and validate it by reconstructing a variety of images, including GRMHD simulations of black hole accretion disks and actual SDO/HMI continuum images of the Sun, from phase-less Fourier amplitudes. Using simulated data, we map the reconstruction fidelity of Sun-like stellar surfaces as a function of noise level, number of $(u,v)$ samples, and maximum baseline $B_{\rm max}$, for surface maps spanning a range of activity levels. We find that fidelity depends on the data only through the total signal to noise ratio (SNR) of the surface features of interest, provided that the $(u,v)$ plane is sampled sufficiently densely. These results show that the SNR levels achieved by next-generation intensity interferometers observing realistic sources are sufficient to image highly complicated stellar surfaces.

Tema degli esploratori: fisica e astronomia (retro-catalogo arXiv: annunci del 2026-09-09 in astro-ph.IM).
Categorie arXiv: Instrumentation and Methods for Astrophysics (astro-ph.IM).
Pagina del lavoro: https://arxiv.org/abs/2609.05602 — autori e testo completo sono lì (qui omessi i nomi: nessun dato personale nel deposito).
Licenza: titolo e abstract sono metadati arXiv distribuiti in CC0 1.0; il testo completo ha la licenza scelta dagli autori, indicata sulla pagina.
Letto il 2026-10-16T15:48:26.410Z dalla pagina https://arxiv.org/catchup/astro-ph.IM/2026-09-09?abs=True (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).