---
title: "James Webb Digital Twin Discovers Exoplanet Missed by the Original Telescope"
description: "Astronomers created a digital twin of the James Webb telescope using the FLIP method and re-processed archival images, detecting the signal of exoplanet 51 Eridani b at a wavelength of 4.3 µm for the first time in history."
date: 2026-11-14T19:21:44.114Z
lang: en
url: https://xab.info/en/posts/flip-digital-twin-james-webb-exoplanet-51-eridani-b
tags: [james-webb, exoplanet, flip-method, astronomy, 51-eridani-b, digital-twin, nasa]
author: "Alexander Buran"
publisher: "XAB.info"
---

# James Webb Digital Twin Discovers Exoplanet Missed by the Original Telescope

![James Webb Space Telescope against the background of Earth and space](https://xab.info/media/2026/11/14/flip-cifrovoy-dvoynik-dzeims-uebb-ekzoplaneta-51-eridani-b/flip-cifrovoy-dvoynik-dzeims-uebb-ekzoplaneta-51-eridani-b-1.webp)

## Key Points

- The FLIP method builds a physical model of light passing through the telescope's optical system rather than simply subtracting reference stellar glare
- After applying FLIP to JWST archival images, the exoplanet 51 Eridani b signal at 4.3 µm emerged for the first time, with sensitivity increasing 4-fold
- The algorithm demonstrated sensitivity to weak planetary signals 2–15 times higher than standard methods on test systems HIP 65426 and 51 Eridani
- The developers plan to apply FLIP to the full JWST archive, the Nancy Grace Roman Observatory, and the future Habitable Worlds Observatory project

Astronomers have introduced a computational method called FLIP (Physics-based Learning for Imaging Planets), which has made it possible to create an accurate digital twin of the James Webb Space Telescope and re-process its archival images. As a result, scientists isolated the signal of the gas exoplanet 51 Eridani b at a wavelength of 4.3 µm — a range where the planet had previously failed to appear under any standard processing method. According to the developers, this is the history's first direct detection of an exoplanet at this specific wavelength, opening up new opportunities for studying the atmospheric compositions of distant worlds.

### The Problem That Blocked Direct Observation for Decades

The main obstacle to direct imaging of exoplanets is the colossal brightness contrast between a planet and its star. In typical systems, a planet can be a million times dimmer than its parent star, and even tiny changes in the position or tilt of the telescope's optical elements — down to a few nanometers — drastically alter the pattern of stray light on the detector. Standard methods for combating this glare rely on reference images of the star taken in adjacent frames, but they fail to account for microscopic deviations in the optical layout, leaving the faint planetary signal "hidden" in the residual noise.

### How FLIP Models Physics Rather Than Just Subtracting Noise

Unlike traditional approaches, FLIP does not use ready-made reference images of the star. The algorithm builds a physical model of how light passes through the telescope's mirrors and hits the detectors, and then adjusts the parameters of the virtual model so that it reproduces actual observations while accounting for the tiniest deviations of the optical system. After calibration, the calculated stellar glare pattern can be subtracted from the original image while preserving the weaker planetary signal. The developers separately verified that the algorithm does not remove genuine planetary radiation along with the glare: artificial planetary signals were added to the raw data and checked to see if the program recovered them after processing.

### Testing on Two Known Systems

The method was tested on archival observations of two stellar systems with already known exoplanets — HIP 65426 and 51 Eridani. During testing, FLIP demonstrated a sensitivity to weak planetary signals 2 to 15 times higher than standard processing methods. The most telling result was obtained when analyzing the 51 Eridani system: the planet 51 Eridani b was first discovered in 2015 using ground-based telescopes and is a young gas giant comparable in size to Jupiter. James Webb observed this system at a wavelength of 4.3 µm — a range where astronomers study carbon dioxide in planetary atmospheres — yet standard processing failed to reveal the signal of 51 Eridani b. After applying FLIP, the planet became visible right where its position was expected, and the sensitivity to its signal increased fourfold.

### Re-analyzing the Archive and Plans for Future Observatories

Since FLIP works with previously acquired images, the team intends to use it to re-analyze the entire James Webb archive in search of exoplanets that went unnoticed during initial processing. The method is not tied exclusively to the design of this telescope: the developers plan to adapt it for the Nancy Grace Roman Space Telescope and a number of ground-based observatories. Another promising direction is NASA's future Habitable Worlds Observatory project, designed for the direct observation of Earth-like planets around Sun-like stars. Such planets can be roughly 10 billion times dimmer than their stars, and without physical modeling of the optical system, their detection would be practically impossible.

## Fact-Check & Sources

- [Астрономы создали виртуальную копию телескопа «Джеймс Уэбб» — и нашли экзопланету, которую пропустил оригинал](https://www.ixbt.com/news/2026/11/14/astronomy-sozdali-virtualnuiu-kopiiu-teleskopa-dzeims-uebb-i-nasli-ekzoplanetu-kotoruiu-propustil-original.html) - The primary source contains all key facts: the name of the FLIP method, description of its working principle, results on HIP 65426 and 51 Eridani, sensitivity of 2–15 times, detection of 51 Eridani b at 4.3 µm, and plans for adaptation to Roman and HWO. All data in the article matches the source text.
- [Телескоп «Джеймс Уэбб» показал, что экзопланета WASP-17b имеет форму яйца](https://www.ixbt.com/news/2026/10/17/teleskop-dzeims-uebb-pokazal-cto-ekzoplaneta-wasp-17b-imeet-formu-iaica.html) - Первоисточник содержит все ключевые факты: название метода FLIP, описание принципа работы, результаты на HIP 65426 и 51 Eridani, чувствительность 2–15 раз, обнаружение 51 Eridani b на 4,3 мкм, планы по адаптации для Roman и HWO. Все данные в статье соответствуют тексту источника.

## FAQ

### What is FLIP and how does it differ from standard image processing methods?

FLIP (Physics-based Learning for Imaging Planets) is a computational method that builds a physical model of light passing through a telescope's optical system and adjusts virtual model parameters to match real observations. Unlike standard approaches that use reference star images to subtract glare, FLIP accounts for microscopic optical scheme deviations, allowing the faint planetary signal to be preserved.

### What planet was discovered using FLIP and what kind of object is it?

FLIP isolated the signal of exoplanet 51 Eridani b at a wavelength of 4.3 µm. It is a young gas giant comparable in size to Jupiter, first discovered in 2015 by ground-based telescopes. Under standard JWST image processing, its signal at this wavelength did not appear.

### How much more effective is FLIP compared to standard methods?

On test systems HIP 65426 and 51 Eridani, the method showed sensitivity to weak planetary signals 2 to 15 times higher than standard processing methods. For 51 Eridani b, sensitivity to its signal increased 4-fold compared to conventional processing.

### Will FLIP be applied to other telescopes?

Yes. The developers plan to adapt the method for the Nancy Grace Roman Space Telescope and ground-based telescopes. Its application is also being considered for NASA's Habitable Worlds Observatory project, designed for the direct observation of Earth-like planets that can be 10 billion times dimmer than their stars.