VENUS: When Red meets Blue -- A multiply imaged Little Red Dot with an apparent blue companion behind the galaxy cluster Abell 383
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| Format: | Preprint |
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2025
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| author | Golubchik, Miriam Furtak, Lukas J. Allingham, Joseph F. V. Zitrin, Adi Akins, Hollis B. Kokorev, Vasily Fujimoto, Seiji Abdurro'uf Amorín, Ricardo O. Bauer, Franz E. Bezanson, Rachel Bradač, Marusa Bradley, Larry D. Brammer, Gabriel B. Chisholm, John Coe, Dan Conselice, Christopher J. Dayal, Pratika Dessauges-Zavadsky, Miroslava Diego, Jose M. Faisst, Andreas L. Fei, Qinyue Ferguson, Henry C. Finkelstein, Steven L. Frye, Brenda L. González-Otero, Mauro Greene, Jenny E. Harikane, Yuichi Hsiao, Tiger Yu-Yang Inayoshi, Kohei Jiménez-Teja, Yolanda Knudsen, Kirsten Koekemoer, Anton M. Labbé, Ivo Lucas, Ray A. Magdis, Georgios E. Matthee, Jorryt Messa, Matteo Naidu, Rohan P. Nakane, Minami Noirot, Gaël Pan, Richard Papovich, Casey Richard, Johan Ricotti, Massimo Robbins, Luke Stark, Daniel P. Sun, Fengwu Treu, Tommaso Tripodi, Roberta Vanzella, Eros Willott, Chris Windhorst, Rogier A. |
| author_facet | Golubchik, Miriam Furtak, Lukas J. Allingham, Joseph F. V. Zitrin, Adi Akins, Hollis B. Kokorev, Vasily Fujimoto, Seiji Abdurro'uf Amorín, Ricardo O. Bauer, Franz E. Bezanson, Rachel Bradač, Marusa Bradley, Larry D. Brammer, Gabriel B. Chisholm, John Coe, Dan Conselice, Christopher J. Dayal, Pratika Dessauges-Zavadsky, Miroslava Diego, Jose M. Faisst, Andreas L. Fei, Qinyue Ferguson, Henry C. Finkelstein, Steven L. Frye, Brenda L. González-Otero, Mauro Greene, Jenny E. Harikane, Yuichi Hsiao, Tiger Yu-Yang Inayoshi, Kohei Jiménez-Teja, Yolanda Knudsen, Kirsten Koekemoer, Anton M. Labbé, Ivo Lucas, Ray A. Magdis, Georgios E. Matthee, Jorryt Messa, Matteo Naidu, Rohan P. Nakane, Minami Noirot, Gaël Pan, Richard Papovich, Casey Richard, Johan Ricotti, Massimo Robbins, Luke Stark, Daniel P. Sun, Fengwu Treu, Tommaso Tripodi, Roberta Vanzella, Eros Willott, Chris Windhorst, Rogier A. |
| contents | 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 $μ_{\mathrm{A}}=16.2\pm1.2$ and $μ_\mathrm{B}=9.0\pm0.6$, respectively, and the predicted time delay between them is $Δt_{\mathrm{grav}}=5.20\pm0.14$ 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 $_{II}$]$\lambda158 \ μ$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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_02117 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | VENUS: When Red meets Blue -- A multiply imaged Little Red Dot with an apparent blue companion behind the galaxy cluster Abell 383 Golubchik, Miriam Furtak, Lukas J. Allingham, Joseph F. V. Zitrin, Adi Akins, Hollis B. Kokorev, Vasily Fujimoto, Seiji Abdurro'uf Amorín, Ricardo O. Bauer, Franz E. Bezanson, Rachel Bradač, Marusa Bradley, Larry D. Brammer, Gabriel B. Chisholm, John Coe, Dan Conselice, Christopher J. Dayal, Pratika Dessauges-Zavadsky, Miroslava Diego, Jose M. Faisst, Andreas L. Fei, Qinyue Ferguson, Henry C. Finkelstein, Steven L. Frye, Brenda L. González-Otero, Mauro Greene, Jenny E. Harikane, Yuichi Hsiao, Tiger Yu-Yang Inayoshi, Kohei Jiménez-Teja, Yolanda Knudsen, Kirsten Koekemoer, Anton M. Labbé, Ivo Lucas, Ray A. Magdis, Georgios E. Matthee, Jorryt Messa, Matteo Naidu, Rohan P. Nakane, Minami Noirot, Gaël Pan, Richard Papovich, Casey Richard, Johan Ricotti, Massimo Robbins, Luke Stark, Daniel P. Sun, Fengwu Treu, Tommaso Tripodi, Roberta Vanzella, Eros Willott, Chris Windhorst, Rogier A. Astrophysics of Galaxies 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 $μ_{\mathrm{A}}=16.2\pm1.2$ and $μ_\mathrm{B}=9.0\pm0.6$, respectively, and the predicted time delay between them is $Δt_{\mathrm{grav}}=5.20\pm0.14$ 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 $_{II}$]$\lambda158 \ μ$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. |
| title | VENUS: When Red meets Blue -- A multiply imaged Little Red Dot with an apparent blue companion behind the galaxy cluster Abell 383 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2512.02117 |