Astronomers report the discovery of β Pictoris d, a third giant exoplanet in the β Pictoris system, using multiple observing campaigns and instruments. One study detects β Pic d in non-coronagraphic VLT/ERIS data and confirms it with multi-epoch archival observations from JWST/NIRCam and VLT/SPHERE. Over an 11-year period, the team measures astrometry consistent with a gravitationally bound source showing orbital motion. Joint orbit fitting with the other known planets places β Pic d at a semi-major axis of about 26 au (with stated uncertainties) and an inclination near edge-on geometry, while finding its orbit is coplanar with the inner planets and consistent with sculpting the inner edge of the system’s debris disk. The other study first finds β Pic d serendipitously in JWST/NIRSpec IFU observations, then corroborates the detection with a second epoch using NIRSpec and MIRI/MRS. It extracts a spectrum showing absorption from CH4, CO, and H2O and finds the measured radial velocity consistent with its orbital position. Across analyses, estimated temperatures and masses fall in the approximate range of a few Jupiter masses, with reported evidence for atmospheric composition marked by strong CO2-related absorption in one dataset.
Astronomers confirm third directly imaged planet β Pictoris d
Astronomers report the discovery of β Pictoris d, a third giant exoplanet in the β Pictoris system, using multiple observing campaigns and instruments. One study detects β Pic d in non-coronagraphic V...
- β Pictoris d is confirmed as a third giant planet in the β Pictoris system.
- Detections come from multiple instruments and epochs, including JWST (NIRCam and NIRSpec/MIRI) and VLT (ERIS and SPHERE).
- Astrometric measurements over about 11 years are consistent with a gravitationally bound object showing orbital motion.
- Spectral data show molecular absorption features including CO, and one report also finds CH4 and H2O; another reports strong CO2 absorption.
- Orbital fits and stability modeling indicate a wide orbit (tens of AU) and consistency with clearing/sculpting the inner edge of the debris disk.
arXiv:2606.23801v1 Announce Type: new Abstract: We report the direct imaging discovery of a third exoplanet in the $\beta$ Pictoris system. We detect $\beta$ Pictoris d in non-coronagraphic observations obtained with VLT/ERIS as well as multi-epoch archival datasets from JWST/NIRCam and VLT/SPHERE. Astrometric measurements over an 11-year baseline demonstrate that it is consistent with a gravitationally-bound source with orbital motion. Joint multi-planet orbit fits of all three planets in the system yield a semi-major axis of $26.0^{+2.2}_{-6.1}$ au and inclination $89.0^{+0.7}_{-0.6}$ deg for planet d. $\beta$ Pictoris d has a larger orbital semi-major axis than the other known planets in the system, but is coplanar with the inner two planets, and its orbit is consistent with sculpting the inner edge of the debris disk. $\beta$ Pictoris d has a contrast of $\Delta L^{\prime}=12.11\pm0.15$ mag, with colors and luminosity that closely match those of 51 Eri b, another exoplanet in the $\beta$ Pictoris moving group. Its VLT/ERIS and JWST/NIRCam colors are distinct from those of free-floating planetary-mass objects of a similar age and temperature. Its red $F410M-F444W$ color indicates strong CO$_2$ absorption in its atmosphere and suggests significant enhancement in metals compared to free-floating objects. From the ATMO hot-start evolutionary models, we estimate an effective temperature of $600^{+45}_{-60}$ K and mass of $2.4\pm0.6$ $M_{\rm Jup}$, which also closely matches similar estimates for 51 Eri b. $\beta$ Pictoris d is among the lowest-mass exoplanets imaged from the ground. This discovery highlights the deep sensitivity achievable with ground-based imaging in the mid-infrared and the discovery potential of future high-contrast observations with the Extremely Large Telescope.
17 hours agoarXiv:2606.23789v1 Announce Type: new Abstract: We report the discovery of $\beta$ Pictoris d ($\beta$ Pic d), a third giant planet in the $\beta$ Pictoris system, which now becomes only the second directly imaged system with more than two confirmed planets. $\beta$ Pic d was serendipitously detected in JWST/NIRSpec IFU observations. A second epoch of NIRSpec and MIRI/MRS observations confirm the initial discovery. The extracted spectrum shows clear CH$_4$, CO, and H$_2$O absorption features, and $\beta$ Pic d's measured radial velocity is consistent with its orbital position. Radial velocity and astrometry measurements combined with orbital stability simulations suggest a semi-major axis $>$30 au, consistent with $\beta$ Pic d being responsible for carving the inner edge of the $\beta$ Pictoris debris disk. Using effective temperature estimates from atmosphere model grid fits combined with evolutionary models, we estimate a mass of 2--4 $M_\mathrm{Jup}$. $\beta$ Pic d is the first planet discovered using spectral template matching with moderate-resolution spectroscopy, highlighting its sensitivity to planetary molecular features hidden within bright extrasolar debris disks that are difficult to access with broadband imaging.
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