Kernel phase imaging with VLT/NACO: high-contrast detection of new candidate low-mass stellar companions at the diffraction limit. Issue 1 (28th March 2019)

• Record Type: Journal Article
• Authors: Kammerer, Jens; Ireland, Michael J; Martinache, Frantz; Girard, Julien H
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 486:Issue 1(2019)
• Page Start: 639
• Page End: 654
• Publication Date: 2019-03-28
• Subjects: planets and satellites: detection -- planets and satellites: formation -- techniques: high angular resolution -- techniques: image processing -- techniques: interferometric -- binaries: close; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz882
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: Directly imaging exoplanets is challenging because quasi-static phase aberrations in the pupil plane (speckles) can mimic the signal of a companion at small angular separations. Kernel phase, which is a generalization of closure phase (known from sparse aperture masking), is independent of pupil plane phase noise to second order and allows for a robust calibration of full pupil, extreme adaptive optics observations. We applied kernel phase combined with a principal component based calibration process to a suitable but not optimal, high cadence, pupil stabilized L '-band ($3.8\, {\mu \rm m}$ ) data set from the ESO archive. We detect eight low-mass companions, five of which were previously unknown, and two have angular separations of ∼0.8–1.2 λ/ D (i.e. ∼80–$110\, \text{mas}$ ), demonstrating that kernel phase achieves a resolution below the classical diffraction limit of a telescope. While we reach a 5σ contrast limit of ∼1/100 at such angular separations, we demonstrate that an optimized observing strategy with more diversity of PSF references (e.g. star-hopping sequences) would have led to a better calibration and even better performance. As such, kernel phase is a promising technique for achieving the best possible resolution with future space-based telescopes (e.g. James Webb Space Telescope ), which are limited by the mirror size rather than atmospheric turbulence, and with a dedicated calibration process also for extreme adaptive optics facilities from the ground.