Miriam Golubchik, Lukas J. Furtak, Joseph F. V. Allingham, Adi Zitrin, Hollis B. Akins, Vasily Kokorev, Seiji Fujimoto, Abdurrouf, R. Amorín, Franz E. Bauer, Rachel Bezanson, Maruša Bradač, Larry Bradley, Gabriel Brammer, John Chisholm, Dan Coe, Christopher J. Conselice, Pratika Dayal, M. Dessauges‐Zavadsky, J. M. Diego, Andreas L. Faisst, Qinyue Fei, Henry C. Ferguson, Steven L. Finkelstein, Brenda L. Frye, Mauro González-Otero, Jenny E. Greene, Yuichi Harikane, Tiger Yu-Yang Hsiao, Kohei Inayoshi, Yolanda Jiménez-Teja, K. K. Knudsen, Anton M. Koekemoer, Ivo Labbé, Ray A. Lucas, G. Magdis, Jorryt Matthee, Matteo Messa, Rohan P. Naidu, Minami Nakane, Gaël Noirot, Richard Pan, Casey Papovich, Johan Richard, Massimo Ricotti, Lucy Robbins, Daniel P. Stark, Fengwu Sun, Tommaso Treu, Roberta Tripodi, Eros Vanzella, Chris J. Willott, Rogier A. Windhorst
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 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. These consist of a red point-source with a V-shaped SED consistent with LRD selection criteria and a nearby (∼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 A = 16.2 ± 1.2 and μ B = 9.0 ± 0.6, respectively, and the predicted time delay between them is Δ t grav = 5.20 ± 0.14 yr (∼0.7 yr in the rest-frame). After correcting for the lensing magnification, we derived an absolute magnitude of M UV, LRD = −16.8 ± 0.3 for the LRD and M UV, BC = −18.2 ± 0.2 for the blue companion. We performed SED fits to both components, revealing the LRD to show the best fit with a black hole star (BH*) model and a substantial host galaxy, along with the blue companion with an extremely young, emission-line dominated star-forming nebula. If it is verified spectroscopically in the future, A383-LRD1 would represent the second known multiply imaged LRD detected to date, following A2744-QSO1. To our knowledge, it would also stand as the first LRD system with a confirmed detection of [C II ] λ 158 μm emission from ALMA observations. Thanks to the lensing magnification, this system opens a unique door to studying the relation between a LRD, its host galaxy, and its environment. It represents a prime candidate for deep JWST spectroscopy and high-resolution ALMA follow-up observations.