“LRD”的版本间差异
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（创建页面，内容为“little red dot # JWST上天后高红移宇宙最有意思的发现之一 ==观测特征== * compact morphology： majority of LRDs are not hosted by well-established, massive galaxies; instead, their nuclear BHs appear to be overmassive relative to the local BH-to-galaxy mass correlation, *UV-optical spectral energy distributions (SEDs) with a turnover wavelength around rest-frame ≃ 4000 ̊A, their broad-line emission properties, and the weakness in canoni…”） |
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* 气体吸收可以解释balmer break和Balmer吸收 arXiv:2512.03130 |
* 气体吸收可以解释balmer break和Balmer吸收 arXiv:2512.03130 |
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* 致宽不是运动学致宽，是电子散射 arXiv:2601.18864 （exponential form of the broad line wings） |
* 致宽不是运动学致宽，是电子散射 arXiv:2601.18864 （exponential form of the broad line wings） |
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:* Sirocco selfconsistently computes the cocoon’s ionisation structure and radiation field(57), |
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2026年1月29日 (四) 03:11的最新版本
little red dot
- JWST上天后高红移宇宙最有意思的发现之一
观测特征
- compact morphology： majority of LRDs are not hosted by well-established, massive galaxies; instead, their nuclear BHs appear to be overmassive relative to the local BH-to-galaxy mass correlation,
- UV-optical spectral energy distributions (SEDs) with a turnover wavelength around rest-frame ≃ 4000 ̊A, their broad-line emission properties, and the weakness in canonical AGN signatures such as hot dust and X-ray corona emission.
- However, deep JWST/MIRI and ALMA observations show no significant detection of reprocessed IR flux in LRDs
- To date, the JWST observational programs have not been originally designed for multi-epoch observations and make the detection of variability challenging.
模型
- A red optical from dust reddened, obscured AGNs and a blue UV excess from scattered light (dust and electrons) leaking through a patchy, partially covering medium.
- 气体吸收可以解释balmer break和Balmer吸收 arXiv:2512.03130
- 致宽不是运动学致宽，是电子散射 arXiv:2601.18864 （exponential form of the broad line wings）
- Sirocco selfconsistently computes the cocoon’s ionisation structure and radiation field(57),