Exoplanets and Stellar Physics

Abstract:

A key science goal for the Planetary Camera and Spectrograph (ELT-PCS) instrument is to image rocky exoplanets in reflected light around nearby M- and K-dwarfs. These observations will require a contrast of 10−9 at 100 mas angular separation, and 10−8 at 10 mas. To achieve such an extreme performance, every instrument design choice must be carefully evaluated. For ELT-PCS’s science instruments, perhaps the most critical design choice is which integral field unit (IFU) technology to use. To this end, we have developed a modular, lab-based integral field spectrograph test bench with which to compare the performance of two popular IFU technologies: image slicers and lenslet arrays. The test bench implements a Lyot coronagraph and a spatial light modulator to simulate a high-contrast imaging system, which feeds each IFU with a diffraction-limited PSF image. Each IFU is coupled to the spectrograph, which achieves R≈3000 with the image slicer and R≈100 with the lenslet array. The calibration and data reduction for each IFU design are described and the initial results of a contrast comparison are presented. The lenslet array achieves a deeper contrast at angular separations of less than 6λ/D. The image slicer, however, gains more at small separations from applying spectral deconvolution, with a 3.4× greater gain at 4λ/D. Spectral deconvolution further yields a contrast curve close to the detector noise floor. Further work will focus on carrying out a fully-controlled characterisation of the lenslet array IFU and a more comprehensive study into the effects of adaptive optics residuals on the contrast.

Abstract:

Abstract The PLATO Stellar Variability Mitigation Working Group designed a radial-velocity (RV) data challenge to assess the precision and accuracy achievable on RV semi-amplitudes in the context of the future PLATO follow-up. Using Sun-as-a-star observations obtained with HARPS-N, we generated three multi-planet systems with realistic sampling, an effective signal-to-noise ratio of S/N ~ 450, an exposure time of Texp = 15 minutes, and a total of N ~ 1000 observations. The resulting data set is publicly available and can serve as a benchmark for the community to test and compare RV analysis methods. Eight independent teams participated in the challenge, aiming to recover the semi-amplitudes of both transiting and non-transiting planets. A meta-analysis of the submitted results shows that, with current data analysis methods, HARPS-N-like stability and the observing strategy studied in this paper, achieving a precision on semi-amplitudes better than 10% for habitable-zone signals around a solar-type star is challenging, and is typically limited to planets with masses of ~8–10 $\rm{$\mathrm{M}_{\oplus }$}$. This performance is expected to improve for K dwarfs, where planets down to ~2–5 $\rm{$\mathrm{M}_{\oplus }$}$ may be characterized at a similar level of precision. Finally, based on the results of this challenge and the occurrence of false positives, we derive an empirical detection threshold for RV surveys, which can be used to distinguish robust planetary detections from candidates.

Abstract:

Simulated PLATO light curves generated at the University of Oxford in 2025. The light curves were used to test light curve filtering and transit detection algorithms. The light curves were generated in python using the PLATO Solar-like Light curve Simulator (PSLS), PySpot, and PyTransit codes. The data are primarily stored in feather files, which in python can be read using the pandas and pyarrow packages. Detailed information on the included files and contents are provided in the README file.

Abstract:

Ultrahot Jupiters (UHJs; Teq ≳ 2000 K) enable simultaneous detection of volatile (ice-forming) and refractory (rock-forming) elements in planetary atmospheres, providing a powerful diagnostic of planet formation and atmospheric processing. We present a comprehensive high-resolution cross-correlation spectroscopy analysis of the UHJ MASCARA-1 b (Teq ≈ 2600 K) using the IGRINS and IGRINS-2 spectrographs. We detect robust (signal-to-noise ratio > 4) signals from H2O, CO, OH, Fe i, Mg i, Ca i, and Ti i, marking the most complete atmospheric inventory of MASCARA-1 b to date. Using a chemically consistent atmospheric inference framework, we constrain elemental abundances to a typical precision of ≈0.2 dex, retrieving a solar atmospheric metallicity ([M/H]⊙ (Formula presented) =0.07−0.13+0.17 ≈1.2 × solar), a C/O ratio (C/O (Formula presented) =0.65−0.08+0.08 ) consistent with solar value (C/O = 0.59), an enhanced refractory abundance ([ (Formula presented) R /H]⊙= (Formula presented) 0.40−0.17+0.23≈2.5× solar; ≈3.8 × stellar), and a moderately supersolar refractory-to-volatile ratio ([ (Formula presented) R/V ]⊙ =  (Formula presented) 0.36−0.09+0.11 ≈ 2.3× solar). Comparison with formation models suggests that MASCARA-1 b most likely accreted material between the soot–H2O or H2O–CO snowlines (at 68% confidence). We additionally find stellar values for atmospheric Ti/Fe and Ca/Fe ratios (at 68% confidence). The Mg/Fe is also found to be consistent with stellar value at 95% confidence. Therefore, we do not find strong indication of nightside cold trapping in MASCARA-1 b. As homogeneous refractory-to-volatile measurements expand across the UHJ population, particularly with upcoming Extremely Large Telescopes, these diagnostics will enable statistically robust tests of emerging trends in giant planet formation and atmospheric evolution.

Abstract:

We report the direct imaging discovery of a third exoplanet in the β Pictoris (β Pic) system. We detect β Pictoris d (β Pic d) in noncoronagraphic observations obtained with the Very Large Telescope (VLT) Enhanced Resolution Imager and Spectrograph (ERIS), as well as multi-epoch archival datasets from the JWST Near Infrared Camera (NIRCam) and VLT/SPHERE. Astrometric measurements over an 11 yr 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 semimajor axis of 26.0−6.1+2.2 au and inclination 89.0−0.6+0.7 deg for planet d. β Pic d has a larger orbital semimajor 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. β Pic d has a contrast of ΔL′=12.11±0.15 mag, with colors and luminosity that closely match those of 51 Eri b, another exoplanet in the β Pic 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 CO2 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 600−60+45 K and mass of 2.4 ± 0.6 MJup, which also closely matches similar estimates for 51 Eri b. β Pic 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.