Webb 对 GLIMPSE-17775 取得 30 小时光谱；由于 Abell S1063 星系团的 gravitational lensing 放大效应，等效观测时间达 80 小时。这使研究团队在这个小而红的源中辨识出超过 40 条 spectral lines，成为目前最详细的 LRD 光谱。其中，hydrogen、oxygen 与 helium 等多条谱线无法由简单旋转气体云模型解释，最佳模型需要 electron scattering，显示外层存在致密分层气体茧。
关键数值证据包括由 16 条 iron lines 组成的「iron forest」，以及特定 oxygen lines 的强度与比值；这些特征需要快速吸积黑洞等高能量来源。helium 的 fluorescence 与 absorption 也分别指向包围强大中心源的致密介质。Webb 与 Hubble 的 Frontier Fields、BUFFALO 资料共同显示，GLIMPSE-17775 周围有巨大宿主星系，使 Balmer break 比典型 LRD 更弱；该模型也解释多数 LRD 在 X-rays 中微弱，因为辐射可能被气体茧吸收。
Since the NASA/ESA/CSA James Webb Space Telescope first discovered little red dots (LRDs) in 2022, GLIMPSE-17775 has provided the strongest evidence yet supporting the “black hole star” model. A team led by Vasily Kokorev analyzed Webb’s deepest LRD spectrum and argues that the object is a supermassive black hole wrapped in a dense cocoon of partially ionized gas. The source has a cosmological redshift of 3.5, meaning it existed about 1.8 billion years after the Big Bang, while LRDs first appeared about 600 million years after the Big Bang.
Webb obtained a 30-hour spectrum of GLIMPSE-17775; because gravitational lensing by the Abell S1063 galaxy cluster magnified it, the exposure was equivalent to 80 hours of telescope time. This enabled the team to identify more than 40 spectral lines from the small red source, making it the most detailed LRD spectrum to date. Many lines, including hydrogen, oxygen, and helium, cannot be explained by a simple rotating gas-cloud model; the best model requires electron scattering, indicating a dense, layered gas cocoon.
Key numerical evidence includes an “iron forest” of 16 iron lines and the strengths and ratios of certain oxygen lines, which require a high-energy source such as a rapidly accreting black hole. Helium fluorescence and absorption also independently indicate a dense medium around a powerful central source. Combined Webb and Hubble Frontier Fields and BUFFALO data show a giant host galaxy around GLIMPSE-17775, weakening its Balmer break compared with typical LRDs; the model also explains why most LRDs are faint in X-rays, because such emission is likely absorbed by the gas cocoon.