{"work":{"id":"8a5c8250-83f7-430e-b32b-e0016d487d09","openalex_id":null,"doi":null,"arxiv_id":"2512.02117","raw_key":null,"title":"VENUS: When Red meets Blue -- A multiply imaged Little Red Dot with an apparent blue companion behind the galaxy cluster Abell 383","authors":null,"authors_text":"VENUS: When Red meets Blue -- A multiply imaged Little Red Dot with an apparent blue companion behind the galaxy cluster Abell 383","year":2025,"venue":"astro-ph.GA","abstract":"We report the discovery of a doubly-imaged Little Red Dot (LRD) candidate behind the galaxy cluster Abell 383, which we dub A383-LRD1. Initially classified as a dropout galaxy in HST imaging with several ground-based emission line detections placing it at $z_{\\mathrm{spec}}=6.027$, new JWST/NIRCam observations taken as part of the cycle 4 VENUS survey now reveal that the source consists of two underlying components: A red point-source with a V-shaped SED consistent with LRD selection criteria, and a nearby ($\\sim 380$ pc) compact blue companion which was the main contributor to the previous rest-frame UV detections. Based on lensing symmetry and its SED, the LRD appears to lie at a similar redshift as well. The magnification of the two images of A383-LRD1 is $\\mu_{\\mathrm{A}}=16.2\\pm1.2$ and $\\mu_\\mathrm{B}=9.0\\pm0.6$, respectively, and the predicted time delay between them is $\\Delta t_{\\mathrm{grav}}=5.20\\pm0.14$ yr ($\\sim0.7$ yr in the rest-frame). After correcting for the lensing magnification, we derive an absolute magnitude of $M_{\\mathrm{UV,LRD}}=-16.8\\pm 0.3$ for the LRD, and $M_{\\mathrm{UV,BC}}=-18.2\\pm 0.2$ for the blue companion. We perform SED fits to both components, revealing the LRD to be best fitted with a black hole star (BH*) model and a substantial host galaxy, and the blue companion with an extremely young, emission-line dominated star-forming nebula. A383-LRD1 represents the second known multiply-imaged LRD detected to date, following A2744-QSO1, and to our knowledge, the first LRD system with a confirmed detection of [C $_{II}$]$\\lambda158 \\ \\mu$m emission from ALMA observations. Thanks to lensing magnification, this system opens a unique door to study the relation between a LRD, its host galaxy, and its environment, and represents a prime candidate for deep JWST spectroscopy and high-resolution ALMA follow-up observations.","external_url":"https://arxiv.org/abs/2512.02117","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-07-02T10:06:51.611846+00:00","pith_arxiv_id":"2512.02117","created_at":"2026-05-15T03:03:57.551071+00:00","updated_at":"2026-07-02T10:06:51.611846+00:00","title_quality_ok":true,"display_title":"arXiv e-prints , keywords =","render_title":"arXiv e-prints , keywords ="},"hub":{"state":{"tier_text":"hub","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":10,"external_cited_by_count":null},"tier":"hub","role_counts":[{"context_role":"background","n":1}],"polarity_counts":[{"context_polarity":"background","n":1}],"runs":{},"summary":{},"graph":{},"authors":[]}}